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SP-1288 SP-1288 Research and Scientific

Report on the activities of the Support Department Research and Scientific Support Department 2003 – 2004

Contact: ESA Publications Division c/o ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands Tel. (31) 71 565 3400 - Fax (31) 71 565 5433 Sec1.qxd 7/11/05 5:09 PM Page 1

SP-1288 June 2005

Report on the activities of the Research and Scientific Support Department 2003 – 2004

Scientific Editor A. Gimenez Sec1.qxd 7/11/05 5:09 PM Page 2

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ESA SP-1288 Report on the Activities of the Research and Scientific Support Department from 2003 to 2004

ISBN 92-9092-963-4 ISSN 0379-6566

Scientific Editor A. Gimenez

Editor A. Wilson

Published and distributed by ESA Publications Division

Copyright © 2005 European Space Agency

Price €30 Sec1.qxd 7/11/05 5:09 PM Page 3

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CONTENTS

1. Introduction 5 4. Other Activities 95

1.1 Report Overview 5 4.1 Symposia and Workshops organised 95 by RSSD 1.2 The Role, Structure and Staffing of RSSD 5 and SCI-A 4.2 ESA Technology Programmes 101 1.3 Department Outlook 8 4.3 Coordination and Other Supporting 102 Activities

2. Research Activities 11 Annex 1: Manpower Deployment 107 2.1 Introduction 13 2.2 High-Energy Astrophysics 14 Annex 2: Publications 113 (separated into refereed and 2.3 Optical/UV Astrophysics 19 non-refereed literature) 2.4 Infrared/Sub-millimetre Astrophysics 22 2.5 Solar Physics 26 Annex 3: Seminars and Colloquia 149 2.6 Heliospheric Physics/Space Plasma Studies 31 2.7 Comparative Planetology and Astrobiology 35 Annex 4: Acronyms 153 2.8 Minor Bodies 39 2.9 Fundamental Physics 43 2.10 Research Activities in SCI-A 45

3. Scientific Support Activities 53

3.1 Astrophysics Missions Division 56 3.2 Solar and Solar-Terrestrial 64 Missions Division 3.3 Planetary Missions Division 70 3.4 Fundamental Physics Missions Division 78 3.5 Space Telescope Operations Division 80 3.6 Science Operations and Data Systems 83 Division 3.7 Science Payload and Advanced Concepts 89 Office Sec1.qxd 7/11/05 5:09 PM Page 5

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1. INTRODUCTION

1.1 Report Overview workshops organised by the Department, support to the Directorate’s science communication activities, and This report on the activities of the Research and various other activities. Scientific Support Department (RSSD) covers the 2-year period of 2003-2004. It is prepared as input to the While this Biennial Report provides perspective on the Department’s Advisory Committee, a group of breadth and quality of the activities of the staff, both in independent external scientists invited by the Director of their research and functional work, it is not intended to be ESA’s Scientific Programme to review the Department’s comprehensive. Up-to-date information on the Depart- activities. It forms the basis of the oral reports made to ment’s activities can be obtained at http://www.rssd. ESA’s Space Science Advisory Committee and the esa.int and for SCI-A at http://sci.esa.int/science-e/ Science Programme Committee every second www/area/index.cfm?fareaid=65 year. Through the publication of the report as an ‘SP’ (Special Publication) by the ESA Publications Division, the activities of the Department are brought to the 1.2 The Role, Structure and Staffing of RSSD attention of the scientific community and to a broader and SCI-A audience. RSSD, one of the two Departments of ESA’s Scientific These Biennial Reports have been produced since 1980. Directorate, provides the direct interface to the scientific In this volume, a number of changes introduced in the community throughout all mission phases. Following last report have been kept. The report also covers the in-orbit checkout and commissioning, it is also respons- activities of the Science Payload and Advanced Concepts ible for the management of the missions. In addition, the Office (SCI-A) owing to its close links with many Department plays its part in the dissemination of activities in RSSD and its history as the previous Science scientific knowledge to the public and for educational Payload Technology Division. purposes.

The report is divided into four Chapters plus four In essence, the role of RSSD is to ensure the best possible Annexes. Chapter 1 deals with the Department’s role and scientific performance of ESA’s Scientific Programme organisation. A brief summary is given because its missions. To this end, the Department is responsible for mandate and structure did not change significantly the implementation of all science management aspects of during the reporting period. Reference should be made to the missions in the Science Directorate throughout their the previous report (ESA SP-1268) for further study and operations phases. information. The names of staff, their locations, their functional duties and scientific research interests are In particular, the Department is responsible for providing given in Annex 1. scientific expertise to studies and projects in all phases, and for ensuring that maximum scientific return within Chapter 2 addresses the scientific research of the practical technical and budgetary constraints is Department’s staff, broken down according to maintained as a target through all phases of a scientific ‘discipline’ rather than divisional structure. A complete mission. The Department also manages, through its study listing of the scientific papers published in the literature or project scientists, the activities of each mission is given in Annex 2. Some 340 refereed papers were science team. published during 2003 and 2004, and more than 350 conference papers and other publications appeared. RSSD is responsible for all aspects of science operations (definition, development, implementation and execution) Chapter 3 provides a top-level summary of the mission- through all phases of missions and manages the related activities at Divisional level. For the four operations phases of missions following in-orbit Missions Divisions, the prime contributions to the commissioning, supported, as necessary, by system scientific support of the various elements of the Science engineering expertise from the Scientific Projects Programme are summarised. For the two Operations Department. Support Divisions, special mention is also made of post- operational and archiving phases. The activities of SCI-A In very close coordination with SCI-A, RSSD provides are included. scientific and payload expertise within the Agency in all phases of scientific missions, including to other Finally, Chapter 4 addresses a variety of activities carried directorates of the Agency (e.g. on International Space out by RSSD in its support role to the community. The Station payloads). It works with external science teams Chapter summarises important scientific symposia and to define the science requirements for future mission Sec1.qxd 7/11/05 5:09 PM Page 6

6 introduction

Head of Research and Scientific Support future missions as well for new payload technologies in Department support of the Cosmic Vision long-term Scientific SCI-S Programme. The Office works, in close liaison with the RSSD study scientists and the science community, to Chief Scientist SCI-SR determine the science and technological needs of this programme. In addition, SCI-A provides payload support/expertise to missions under development, both to RSSD Project Scientists as well as the Science Projects Astrophysics Missions Science Operations and Division Data Systems Division Department. The Office is also responsible for laboratory SCI-SA SCI-SD support throughout the Directorate, including those

Planetary Missions Space Telescope RSSD research activities requiring such support. Division Operations Division SCI-SB SCI-SN The organigram of RSSD is shown in Fig. 1.2/1. In Solar & Solar-Terrestrial addition, the office of the Department Head is supported Missions Division SCI-SH by a budget control group including three integrated project controllers from SCI-M. The role and functions Fundamental Physics Missions Division of the six Divisions, and those of SCI-A, are described SCI-SP further in Chapter 3.

Figure 1.2/1: The structure of RSSD. The staff of the Department (37 at the end of 2004) and of SCI-A (21, including 2 advanced recruitments) hold posts within the overall ESA staff complement. Staff associated with Science Operations Teams are generally studies and associated payloads and passes these to supernumerary positions. By the end of 2004, there was SCI-A for follow-up. a complement of 68 supernumeraries (3 in SCI-A). Fig. 1.2/2 depicts the structure of SCI-A. It should be It is, of course, very important that the scientific staff of noted that, in these teams, many contractors and often both RSSD and SCI-A maintain their scientific staff from Principal Investigator (PI) institutes work proficiency by undertaking personal research. together in an integrated structure. An overview of the staff in post at the end of 2004 is given in Table 1, In order to discharge its responsibilities and tasks in an integrating personnel from RSSD proper and SCI-A. efficient manner, the Department is structured into four Figure 1.2/3 gives the distribution of staff according to Missions Divisions: functions within RSSD.

— the Astrophysics Missions Division; Department staff are located not only at ESTEC, close to — the Planetary Missions Division; the Science Directorate’s project teams and the Technical — the Solar and Solar-Terrestrial Missions Division; Directorate, but also in Villafranca (ISO and XXM- — the Fundamental Physics Missions Division; Newton science operations teams), in Garching and Baltimore (Space Telescope Operations Division) and and two Operations Support Divisions: Greenbelt (SOHO Project Scientist Team at NASA Goddard Space Flight Center). During 2004, the Villa- — the Science Operations and Data Systems Division; franca facilities were integrated into the European Space — the Space Telescope Operations Division. Astronomy Centre (ESAC). Figure 1.2/4 shows the distribution according to location of personnel from The Office for Science Payload and Advanced Concepts RSSD. (SCI-A) is under the direct authority of the Director of the Scientific Programme. This Office is responsible for While not formally on the ESA staff complement, the assessment phase and the strategic approach for Internal Research Fellows, on contracts of maximum

Figure 1.2/2: The structure of SCI-A. Sec1.qxd 7/11/05 5:09 PM Page 7

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Table 1: RSSD Staff in Post at end of 2004.

Head of Department: A. Gimenez Assistant Administrator: C. Bingham Project Controller: R. Fontaine* Divisional Assistants: S. Ihaddadene, B. Schroeder, C. Villien R. Davis* G. D’Aquino* Chief Scientist: B.H. Foing *seconded from SCI-M

Astrophysics Missions Division J. Clavel (Head) M. Fridlund R. Laureijs A. Parmar T. Prusti T. Boeker A. Heras S. Leeks M.A.C. Perryman J. Tauber J. de Bruin P. Jakobsen A. Marston G.L. Pilbratt R. Vavrek F. Favata

Solar and Solar-Terrestrial Missions Division H. Opgenoorth (Head) C.P. Escoubet B.G. Fleck* H. Laakso L. Sanchez Duarte* S. Haugan* R.G. Marsden T.R. Sanderson *located at SOHO/EOF, NASA Goddard Space Flight Center

Planetary Missions Division G. Schwehm (Head) A. Chicarro J.-P. Lebreton R.M. Schulz K. Wirth D.V. Koschny P. Martin L.H. Svedhem O. Witasse

Fundamental Physics Missions Division R. Reinhard (Head) L. Cacciapuoti O. Jennrich

Space Telescope Operations Division D. Machetto (Head) M.R. Rosa A. Clampin-Nota M. Miebach M. Sirianni D. Sforna H. Jenkner B. Mobasher E. Villaver ST-ECF (Garching) I. Kamp N. Panagia T. Wiklind R. Albrecht STScI (Baltimore) J. Maiz-Apellaniz M. Robberto R.A.E. Fosbury A. Aloisi A. Micol S. Arribas

Science Operations and Data Systems Division M.F. Kessler (Head) F. Jansen M.J. Szumlas G. Thoerner C. Winkler C. Arviset* N. Schartel* D. Texier** A. Toni J.J. Zender K. Bennett *located at ESAC **located at Geneva

Integral Science Operations L. Hansson (Head) P. Barr L. O’Rourke A. Orr J. Sternberg

ISO Data Centre (ESAC) A. Salama (Head) P. Garcia Lario R. Lorente E. Verdugo

XMM-Newton Science Operations (ESAC) L. Metcalfe (Head, Science Support) M. Arpizou M. Guainazzi A. Pollock J. Munoz Peira (Head, Instrument Operations) M. Ehle J. Hoar M. Santos-Lleo B. Altieri J.C. Gabriel M. Kirsch

Herschel Science Operations Development J. Riedinger S. Ott

Science Payload and Advanced Concepts Office (Science Payloads Technology Division) A. Peacock (Head) T. Beaufort P. Falkner D. Klinge J. Romstedt S. Andersson J.F. van der Biezen Ph. Gondoin D. Lumb L.C. Smit T. Appourchaux B.A.C. Butler J. Heida D. Martin U. Telljohann H.J. Arends A. van Dordrecht B. Johlander N. Rando J. Verveer M. Bavdaz C. Erd Sec1.qxd 7/11/05 5:09 PM Page 8

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Figure 1.2/3: Distribution of RSSD staff according to Figure 1.2/4: Distribution of RSSD staff according to prime function. location.

2 years and funded by the Agency’s Education budget, 1.3 Department Outlook play a major role in the Department’s research activities. Typically, some 15 Research Fellows were in post at any During the past 2-years, time was devoted to one time during the reporting period. The Department consolidating the reorganisation of the Department in and SCI-A also hosted several Young Graduate Trainees line with its new role and goals. In addition, some on 1-year contracts, and offered numerous opportunities refinements in the internal working procedures of the for trainees and stagiaires. Directorate were found necessary. The next 2 years are expected to see a review of the effectiveness of the Highlights for the Department in the reporting period structure in place and the performance of the staff at all include: levels, with the possibility of more changes if required for the achievement of the overall goals of the — the successful launches of Mars Express, SMART-1, Department. Moreover, further discussions are expected Rosetta and Double Star, and the very promising first within the Directorate to improve interfaces with the data from all their instruments; Projects Department and other Offices, and new areas of — the successful arrival of Cassini-Huygens at Saturn cooperation with other Directorates, such as the newly and the release of the Huygens probe towards Titan; created programme for Exploration, will need to be — the excellent scientific results from Mars Express expanded. during its first year in orbit around the Red Planet; — RSSD and SCI-A contributions to the planning of At the level of the Scientific Programme, the challenges ESA’s long-term Scientific Programme ‘Cosmic of the coming years are clearly dominated by the Vision’, covering the decade 2015-2025; definition of the new Cosmic Vision plan for the decade — the completion, testing and delivery of 2015 to 2025. Many discussions and evaluations will Co-Investigator contributions to Rosetta and have to be done in close cooperation with the scientific SMART-1 instruments; community and our Advisory Bodies to define the — the continued excellent science return from the HST, themes, and then the missions to be implemented, to Ulysses, SOHO, Cluster and XMM-Newton achieve the selected scientific goals. While the last missions in orbit; 2 years were devoted to implementing a previously — maintaining a high level of research with a signifi- approved programme under increasingly difficult cant number of publications in spite of the increasing budgetary circumstances, we can now look into the pressure of the scientific support activities; future for new targets and science. Of course, we are still — the active organisation of a number of symposia and not clear of the problems with the current programme, workshops for the space science community; but we certainly have to start the discussion on what — transfer of the BepiColombo mission to Mercury missions should be launched in little more than 10 years from the assessment phase to implementation phase. from now, in order to keep a stable European contribution to space science. In 2004, RSSD achieved an all-time record of missions in orbit under its responsibility. A total of 11 space The way to define and implement missions is also missions (comprising 14 spacecraft) were being changing considerably. For example, the use of themes, operated, with an impact on the Department’s efforts in rather than the usual call for ideas, is allowing us to study the area of science operations despite the frozen level of new technologies not constrained by existing studies or complement. projects and to look for the actual scientific needs in the Sec1.qxd 7/11/05 5:09 PM Page 9

introduction 9

reference decade instead of trying to just do ‘more of the One of the important responsibilities of RSSD – the same’. In particular, SCI-A is responsible for the science operations of the various scientific missions – assessment of all future missions within the Directorate continues to require our full attention as well as the and is therefore closely linked to RSSD and the further development of skills and tools to cope with an technology development activities. In the implement- increasingly demanding activity. The availability of ation of missions, lessons learnt have been introduced properly processed scientific data, to the full satisfaction together with a more systematic risk analysis for each of the scientific community at large and valid for both mission. In particular, for the Department’s domain, the observatory-type missions, with its high pressure from design and implementation of science operations has the scientific community, and PI-type missions, is a clear become more pro-active and new ideas will have to be objective. implemented in the next years to ensure a more efficient performance of the operation of planetary missions. For SCI-A, one of the key tasks is the technical assessment of all future missions within the Directorate Concerning the research activities in the Department, the coupled to long-term planning, both at mission level and coming years will focus on the increasing recognition, for technology development. Such technology planning and evaluation, of the results achieved by the staff. is assisted by a parallel Technology Research and Another point of importance is the rapidly increasing Development Programme. need to devote time to functional activities to the detriment of the time available for research – a dangerous To conclude, while the need to maintain and, where situation that should be avoided. Nevertheless, research necessary, to improve the links with the research cannot be dictated and an average allocation of 20% of institutions in Member States through active cooperative the time may not be enough for competitive science. It is programmes remains a prime goal of the Department, important to see how these activities develop and other aims for the future include the continued provision whether further adjustments will be necessary in the light of properly processed scientific data to the community of experience. and support to the development of science communica- tions and science education activities in ESA. Our opportunities for the analysis of data provided by missions in orbit are now enhanced by those offered by SMART-1, Mars Express, the arrival of Cassini at Saturn and the very recent entry of the Huygens probe into the atmosphere of Titan. In astronomy, the data exploitation of successful missions such as Integral, XMM-Newton and HST or ground-based observatories continues, as well as that of data archives from previous missions like ISO that are currently being enhanced through the development of virtual observatories. In the area of the Solar System, research flourishes, in close collaboration with partners in the scientific community, thanks to Ulysses, SOHO and Cluster data. New flight instrumentation is under development through contributions to the COROT and STEREO missions. Finally, we have seen in the past 2 years the beginning of an effort in the area of Fundamental Physics research that should develop further.

Scientific support activities to missions under development or study will require close attention. Continued efforts will be devoted to the preparation of Herschel and Planck, which are entering critical phases of their development, as well as to the European contribution to JWST. On the other hand, Gaia will begin its implementation phase and the preparation of the very demanding science operations will require special attention. The gravitational wave observatory LISA and its technology mission LISA Pathfinder will require special efforts in this emerging area of space science. In the Solar System domain, our activities will focus on Venus Express, to be launched in 2005. Equally, the preparations for BepiColombo, travelling to Mercury, and of Solar Orbiter will need to be intensified. sec2.qxd 7/11/05 5:12 PM Page 11

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2. RESEARCH ACTIVITIES IN RSSD AND SCI-A

2.1 Introduction 2.7 Comparative Planetology and Astrobiology

2.7.1 Mars research 2.2 High-Energy Astrophysics 2.7.2 Lunar studies 2.7.3 Cassini-Huygens data analysis preparation 2.2.1 Stellar coronae and star-formation regions 2.7.4 Ground-based observations of Titan winds 2.2.2 X-ray binaries 2.7.5 Earth comparative planetology 2.2.3 Galaxies and active galactic nuclei 2.7.6 Astrobiology 2.2.4 Ground-based photon-counting studies

2.8 Minor Bodies 2.3 Optical/UV Astrophysics 2.8.1 The MIDAS instrument on the Rosetta mission 2.3.1 The Helix Nebula: when opportunity knocks 2.8.2 Determination of isotopic ratios in comets 2.3.2 Central stars of planetary nebulae 2.8.3 Characterisation of the new Rosetta target comet 2.3.3 Identifying core-collapse SN progenitors 2.8.4 Comet modelling 2.3.4 Metals in the dwarf starburst galaxy NGC 1705 2.8.5 Ground-based observations of comets 2.3.5 Luminous IR galaxies: a key galaxy population

2.9 Fundamental Physics 2.4 Infrared/Sub-millimetre Astrophysics 2.9.1 Interferometer design for LISA Pathfinder 2.4.1 Solar System studies 2.9.2 A phasemeter for LISA Pathfinder 2.4.2 Interstellar medium studies 2.9.3 Frequency stabilisation for LISA 2.4.3 Star formation 2.4.4 Stellar studies 2.4.5 Extragalactic studies 2.10 Research Activities in SCI-A

2.10.1 Development of superconducting cameras 2.5 Solar Physics 2.10.2 Advanced semiconductor sensors 2.10.3 Development of advanced optics 2.5.1 Chromospheric oscillations 2.10.4 Advanced instrumentation research for 2.5.2 Dynamics of transition region blinkers planetary missions 2.5.3 Comparison of blinkers and explosive events 2.5.4 Coronal magnetic fields

2.6 Heliospheric Physics/Space Plasma Studies

2.6.1 Energetic particles from the October/November 2003 solar events 2.6.2 Energetic particles in the high-latitude, high- speed solar wind 2.6.3 Acceleration of electrons in the auroral region 2.6.4 Magnetospheric observations 2.6.5 Examples of other associated activities within SCI-SH sec2.qxd 7/11/05 5:12 PM Page 13

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2.1 Introduction contracts, as well as Portuguese and Spanish Trainees on 2-year grants funded by their respective nations. The Research in RSSD and SCI-A is an integral part of the Department also hosted a number of Stagiaires for activities of the scientific staff, needed to maintain and durations of up to 6 months, as part of their research or develop its scientific skills, peer recognition and hands- graduate engineering studies, as well as externally on experience in space science. Active involvement in supported research students. The scheme for Internal research is necessary for Staff Scientists to remain part of Research Fellows, Trainees and Stagiaires, besides the community when performing their mission-related offering training and experience at RSSD, permits a duties. continuous exchange and collaboration with their institutes of origin or with their future destinations. A The overall research programme is organised in thematic number of Master or PhD theses were co-supervised by research groups covering different areas in astrophysics RSSD and SCI-A staff scientists and colleagues from (high-energy, optical/UV, IR/sub-mm); solar physics, academic institutes. heliospheric and space plasma physics; comparative planetology and astrobiology; minor bodies; funda- Mention should also be made of the role of 20 ESA mental physics; development and exploitation of external post-doctoral Research Fellows, funded to work superconducting cameras for astronomy. These topics 1 or 2 years in ESA Member States’ institutions. They reflect the breadth of the Cosmic Vision programme contribute in the building of research networking in within the different fields related to ESA science support of ESA missions. There are two calls per year missions. The results of these research activities, as well (applications due end of March and end of September) as new proposals for the following year, are reviewed covering all aspects of post-doctoral research related to annually, and the overall RSSD research programme is ESA activities in space science as well as Earth assessed by an external visiting committee every 2 years. observation, microgravity and human spaceflight and The activities have been influenced by the opportunities space technologies. given by the ESA Science Programme, but are constrained by the limited time available to scientists RSSD and SCI-A scientists publish, on average, some owing to increased workload on projects, studies and 180 refereed papers per year (those published or accepted other functional activities. In addition, in support of in 2003 and 2004 are listed in Annex 2). They still future missions and long-term planning, SCI-A conducts manage to maintain a leading role in more than a third of an independent laboratory-based Technology Research their research papers, despite the functional workload in and Development Programme in close coordination with scientific support to projects, thanks to their commit- other Programmes of the Agency. ment, collaborations within research groups and with the outside community, and the contributions by Research RSSD and SCI-A staff undertake research collaborations Fellows. with external institutes from all the Member States and with the international community, both in instrument RSSD staff organised Workshops or Symposia in support development and data exploitation for ESA and of ESA science missions or in relation to scientific international space science missions. External themes or collaborative research topics (Section 4.1). researchers have also contributed to the scientific output They also contributed to several coordination and of the department in the form of extended visits to RSSD supporting tasks (Section 4.3), as well as science and SCI-A. communications and education activities (Section 4.4). A programme of seminars for the Department (also open to The Research Groups provide a basis for the integration other interested scientists) invites external scientists to and daily research activities of Research Fellows and present results or reviews over a wide range of space Trainees, with the Chief Scientist responsible for their science topics (Annex 3). The successful colloquia overall supervision. ESA Internal Research Fellows, on programme presenting prestigious speakers to all ESTEC post-doctoral contracts of up to 2 years, play a major role staff continued during the reporting period (Annex 3). in the Department’s research activities. On average, some Also, within a programme of internal seminars, RSSD 15 internal Research Fellows are in post at any one time, scientists report on their ongoing research activities or covering the large range of topics in RSSD. They are give tutorials for their colleagues across disciplines. recruited through the standard ESA process of interviews. The excellence and publication record of The following Sections are arranged according to the candidates, their research programme matching RSSD individual research lines. research priorities, and the training opportunities at RSSD for their future career prospects are prime selection criteria. RSSD is also hosting a Post-Doctoral Researcher funded through the EU European Network collaboration scheme. The Department, together with SCI-A, hosts Young Graduate Trainees on 1-year sec2.qxd 7/11/05 5:12 PM Page 14

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2.2 High-Energy Astrophysics

The High-Energy Astrophysics research group uses primarily XMM-Newton observations coupled with extensive ground-based facilities to address a wide range of issues. Topics such as stellar physics and accretion- driven objects are the focus of the group’s attention.

2.2.1 Stellar coronae and star-formation regions

Using XMM-Newton data, Favata et al. (2004) reported the first clear evidence for an X-ray cycle in a star other than the Sun. During the 11-year solar cycle, the X-ray luminosity of the Sun varies in the 0.7-2.5 keV band by some 2 orders of magnitude, yet the X-ray luminosity of most active stars (which have X-ray luminosity 100-1000 Figure 2.2.1/2: The coronal abundances of λ And, times greater than the Sun) is remarkably constant, plotted with its measured photospheric abundances. within a factor of 2 or so, across several years. A Note how both differ in a similar way from the solar dedicated programme has been set up to monitor, at photospheric composition (from Sanz-Forcada et al., 6-month intervals, the X-ray luminosity of the solar 2004). analogue HD 81809, which has an X-ray activity level comparable to the Sun (thus much lower than the typical targets of X-ray spectroscopic observations). The results of the first 3 years of the programme are given in Fig. 2.2.1/1; they show that the X-ray luminosity of continues throughout 2005 and will be re-proposed for HD 81809 has varied by more than one order of each future AO, aiming to observe at least one complete magnitude in the last 2 years, and, according to the phase cycle (HD 81809 has a chromospheric cycle duration of of the known chromospheric cycle observed in the Ca II 8.2 years). H&K lines, is expected to bottom out between 2005 and 2006. The XMM-Newton observing programme Chemical abundances of the coronal plasma in active stars are an ongoing subject of debate. The discovery from early ASCA spectra that the coronal plasma does not have the composition of the solar photosphere (with generally lower abundances reported) sparked a long Figure 2.2.1/1: Three years of XMM-Newton discussion about the actual abundance patterns and the observations of HD 81890 (square symbols), together possible fractionation mechanisms. Progress has, with the Mt. Wilson observations of the Ca II however, been hampered by the lack of photospheric chromospheric activity index of the same star abundances for most active stars – the only stars (crosses). The very large long-term variation in X-ray sufficiently X-ray bright for their high-resolution X-ray luminosity, with a maximum in mid-2002, is easily spectrum to be observed and coronal abundances seen. (From Favata et al., 2004). derived. A long-term programme to determine both the photospheric and coronal chemical abundances of individual active stars is being carried out in RSSD in collaboration with a number of institutions. The most recent results (Fig. 2.2.1/2) come from the analysis of XMM-Newton and Chandra high-resolution spectra of a number of active stars (Sanz-Forcada et al., 2004). This has shown that, in a number of specific cases, the coronal abundances, which would be very different to solar photospheric abundances, are actually very similar to their stellar photospheric abundances. However, these RS CVn-type active binary stars have themselves rather strange photospheric abundances (Morel et al., 2004).

The structures of the coronae in active stars and their comparison with the solar corona, the only spatially resolved corona we can observe, have been open questions since the beginning of imaging X-ray astronomy. The advances in both collecting area and sec2.qxd 7/11/05 5:12 PM Page 15

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spectral resolution brought by XMM-Newton and Chandra have allowed new statistics to be exploited, namely the rotational modulation of spectral Doppler shifts and of the global X-ray luminosity. Hussain et al. (2005) studied the prototypical young main sequence star AB Dor with a long Chandra LETG observation, and found significant modulation in both the Doppler velocity of the O VIII coronal line (with an amplitude of about 60 km/s) and in the X-ray luminosity (at the 10- 15% level). This implies a highly non-homogeneous corona, with the X-ray emission dominated by a small number of compact emitting regions located at high latitudes. These observations also rule out a corona Figure 2.2.2/1: XMM-Newton EPIC pn residuals composed of very big magnetic loops (significantly when the best-fit model is fitted to XB 1254-690 larger than the star itself), which were in the past thought spectra for observations when a deep dip is present to be present on very active stars. (2001 Jan) and no dipping is evident (2002 Feb). The absence of any overall change in absorption line The origin of the observed strong X-ray activity in properties indicates that their presence is not related intermediate mass young stars (Herbig Ae/Be stars, to the presence, or absence, of dips. HAeBe in short) remains a puzzle: these stars are not expected to have a convective zone sustaining a dynamo, and their winds are thought not to be energetic enough to generate the observed X-rays through a wind shock mechanism (thought to be the origin of the X-ray from MXB 1659-298, GX 13+1 and 4U 1624-49. In the emission observed in the more massive O and early B last 2 years, these results have been extended by stars). In a number of cases, low-mass companions have observations of two more dip sources, XB 1254-690 been discovered to be the origin of the observed X-rays; (Boirin & Parmar, 2003) and XB 1916-053 (Boirin et al., however, there remains a significant number of 2004). Ongoing analysis of all the dip sources observed apparently single HAeBe stars. Combining XMM- by XMM-Newton is allowing their global properties to Newton and Chandra data, Giardino et al. (2004) have be investigated. for the first time detected flaring activity from an apparently single HAeBe star, V892 Tau. The During Exosat observations, the LMXB XB 1254-690 characteristics of the flares, one of which has a peak exhibited irregular dips in X-ray intensity that repeated temperature of around 90MK, require the plasma to be every 3.88 h. The dips are almost certainly due to magnetically confined, ruling out classical wind shock obscuration in the thickened outer regions of an models (in which the plasma is essentially unconfined). azimuthally structured accretion disc. One of the While the origin of the magnetic field is still unclear, peculiarities of this source is that, during some detailed analysis of the flares constrain the magnetic field observations, deep (up to 80%) dipping is present but in at around 500 G. others it is completely absent, while the overall X-ray intensity is unchanged. During an XMM-Newton obser- References vation in January 2001 a deep X-ray dip was seen while, Favata, F., Micela, G., Baliunas, S.L. & Schmitt, true to form, in a second observation a year later no dips J.H.M.M., 2004, A&A 418, L13. were evident. The 0.5-10 keV EPIC spectra from both Giardino, G., Favata, F., Micela, G. & Reale, F., 2004, non-dipping intervals were very similar, being modelled A&A 413, 669-679. by a disc-blackbody and a power-law continuum with Hussain, G.A.J., Brickhouse, N.S., Dupree, A.K. et al., additional structure around 1 keV and narrow absorption 2005, ApJ 621, 999. features at 7.0 keV and 8.2 keV that are identified with Morel, Th., Micela, G., Favata, F., Katz, D. & the K-alpha and K-beta absorption lines from H-like Fe. Pillitteri, I., 2004, A&A 412, 495. The low-energy structure may be modelled as a 175 eV- Sanz-Forcada, J., Favata, F. & Micela, G., 2004, A&A wide emission line. The absorption line properties show 416, 281. no obvious dependence on orbital phase and are similar in the two observations (Fig. 2.2.2/1), suggesting for the first time that the occurrence of such features is not 2.2.2 X-ray binaries directly related to the presence of dipping activity.

The outstanding spectral resolution and sensitivity of The discovery of narrow Mg XII, Fe XXV and Fe XXVI XMM-Newton continues to be exploited to investigate K-alpha X-ray absorption lines in the persistent emission narrow absorption features in low-mass X-ray binaries of the dipping LMXB XB 1916-053 during an XMM- (LMXBs). In the previous report, results were reported Newton observation in September 2002 has been sec2.qxd 7/11/05 5:12 PM Page 16

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consistent with a decrease in the amount of ionisation, as dipping activity progresses. This implies the presence of cooler material in the line of sight during dipping, consistent with the decrease in energy of the Fe feature as dipping becomes more intense (Fig. 2.2.2/2). The discovery of a 0.98 keV absorption edge in the persistent emission spectrum is also reported. The edge energy decreases to 0.87 keV during deep dipping intervals. The detected feature may result from edges of moderately ionised Ne and/or Fe, with the average ionisation level decreasing from persistent emission to deep dipping. This is again consistent with the presence of cooler material in the line of sight during dipping.

References Boirin, L. & Parmar, A.N., 2003, A&A, 407, 1079. Boirin, L., Parmar, A.N., Barret, D., et al., 2004, A&A 418, 1061.

2.2.3 Galaxies and active galactic nuclei

The X-ray emission from advection-dominated accretion flows in the elliptical galaxy NGC 3226 has been studied (Gondoin et al., 2004)). The continuum can be described by a bremsstrahlung model absorbed by neutral material. The absence of variability suggests that the emission originates from regions relatively far from the nucleus. Based on luminosity considerations, the mass of the central accreting black hole is be constrained to be 1.7- 50x107 solar masses.

The first systematic investigation of magnetic fields in barred spiral galaxies is now complete (Harnett et al., 2004; Beck et al., 2002). The radio surface brightness is found to be highest in galaxies with a long bar. The Figure 2.2.2/2: The variation in the Fe absorption derived regular magnetic fields are significantly different feature seen from XB 1916-053 during dipping from those in non-barred galaxies, allowing new intervals. The energy of the feature is indicated by constraints to be placed on dynamo-models. Individual vertical tick marks. The mean energy of the feature follow-up studies (including a comparison with X-ray decreases with increasing dip depth, consistent with observations) are continuing. the presence of increasingly cooler material. XMM-Newton observations of nearby star-burst galaxies have been analysed as part of a multi-wavelength investigation of all phases of the extra-planar interstellar medium (Ehle et al., 2004; Dahlem et al., 2003). This reported (Boirin et al., 2004). Such absorption lines from study was conducted in order to assess the importance of highly ionised ions are now observed in a number of haloes as repositories of a metal-enriched medium and high-inclination (close to edge-on) LMXBs, such as their significance in terms of galactic chemical evolution. XB 1916-053, where the inclination ranges between 60° The common goal of the multi-wavelength (X-ray, radio and 80°. This, together with the lack of any orbital phase continuum, H I and optical) project is to obtain a better dependence of the features (except during dips), suggests understanding of star-formation related outflows. The that the highly ionised plasma responsible for the galaxy NGC 4666 (Fig. 2.2.3/1) is an example of the absorption lines is located in a cylindrical geometry observed interplay between X-ray and optical filaments, around the accretion disc. Using the ratio of Fe XXV and star-formation regions in the underlying disc, and the Fe XXVI column densities, the photo-ionisation magnetic field structure. parameter was estimated to be 103.92 erg cm/s. Only the Fe XXV line is observed during dipping intervals and the Analysis of XMM-Newton’s observation of the Seyfert 1 upper-limits to the Fe XXVI column densities are galaxy ESO 141-G55 has revealed, in addition to an Fe sec2.qxd 7/11/05 5:12 PM Page 17

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Newton observation of Mkn 304 (Piconcelli et al., 2004), it seems likely that such absorbers are characteristic of X-ray weak quasars in general. They are different from the warm absorbers found commonly in AGNs that show much lower column densities and ionisation parameters. The X-ray spectrum of PG 1535+547 shows a relativistic Fe K-alpha disc line from fluorescence emission and is therefore only the second X-ray weak quasar with such an unusual characteristic. The occurrence of a variable relativistic Fe K-alpha fluorescence line in two out of the five well-studied X-ray weak quasars may indicate that such features are more common in these systems.

The discovery of two new occurrences of extreme variations in the column density obscuring nearby AGN has been reported (Guainazzi et al., 2004). The typical timescale of these phenomena is ~50 yr. This provides further support to a scenario in which gas associated with the host galaxy, or with dense regions of enhanced star Figure 2.2.3/1: A pn-MOS 0.5-0.9 keV image of NGC formation, is responsible for obscuration in 50% of the 4666 overlaid on an H-alpha and N II optical narrow- AGN in the nearby Universe, which is inconsistent with band image. In the halo, the most extended optical the predictions of the standard AGN Unification model. emission line filaments, which form an X-shaped structure, reach out to distances above the plane by The ongoing investigation of the star-formation up to ~7.5 kpc. Vectors mark the orientation of the processes in the nuclei of spiral galaxies has been magnetic field observed at 4.89 GHz with the VLA; expanded. Following up on the previous Hubble Space their lengths are proportional to the polarised Telescope survey of nuclear star clusters, Boeker and intensity. collaborators (Boeker et al., 2002) have used an isophotal analysis to demonstrate that many late-type spirals are indeed ‘pure’ disc galaxies in that they show no evidence for a spheroidal bulge component. The team has then used the IRAM 30 m telescope to search for molecular K-alpha fluorescence line (equivalent width of ~40 eV), gas in the central kpc of 47 bulge-less spirals in order to an absorption edge at 7.6±0.1 keV (Gondoin et al., measure the fuel reservoir available for nuclear star 2003a). Similar results have been obtained for the formation. The results demonstrate that a large fraction Seyfert 1 galaxy NGC 3227 by Gondoin et al. (2003b). of galaxies contain enough gas in the vicinity of the At soft energies, the spectrum of NGC 3227 shows nucleus to sustain at least a few modest (about 105 solar strong continuum absorption of 6.5x1022/cm2. masses in new stars) star-burst episodes. This is consistent with scenarios that invoke nuclear cluster XMM-Newton spectra of 40 quasars with redshifts growth through repetitive star-bursts. The challenge then < 1.72 from the Palomar-Green Bright Quasar Survey is to explain how the gas can lose its angular momentum sample have been analysed (Piconcelli et al., 2005; and be funnelled to within a few pc of the galaxy nucleus. Jimenez-Bailon et al., 2004). The hard X-ray continuum In order to advance observations at this level of detail, emission > 2 keV can be modelled by a power-law with Boeker and collaborators have performed a detailed case mean 2-12 keV photon index of 1.89±0.11. Below 2 keV, study of IC342, a nearby, late-type spiral with a a strong broad excess is present in most spectra, for prominent nuclear star cluster. Their observations with the which it is impossible to find an universal spectral shape. Owens Valley Radio Interferometer revealed a molecular Warm absorber features are present in around half of the disc that coincides with the nuclear star cluster and has a sources, in contrast to their rare occurrence (~5-10%) in radius of only 15 pc. This demonstrates that molecular gas previous studies. The XMM-Newton view of optically- can indeed accumulate on such scales, making repetitive selected bright quasars therefore suggests that there is no nuclear star-bursts a plausible scenario. significant difference in their X-ray spectral properties when compared with low-luminosity Seyfert 1 galaxies. References Beck, R., Shoutenkov, V., Ehle, M. et al., 2002, A&A Three X-ray weak quasars observed with XMM-Newton 391, 83. have been studied (Schartel et al., 2004). All three Boeker, T., Laine, S., van der Marel. R. et al., 2002, AJ objects are absorbed by ionised material with high 123, 1389. column densities and ionisation parameters. In Dahlem, M., Ehle, M., Jansen, F. et al., 2003, A&A 403, combination with the similar result from the XMM- 547. sec2.qxd 7/11/05 5:13 PM Page 18

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Ehle, M. & Dahlem, M., 2004, Mem. S.A.It. 75, 515. Gondoin, P., Orr, A. & Lumb, D., 2003a, A&A 398, 967. Gondoin, P., Orr, A., Lumb, D. & Siddiqui, H., 2003b, A&A 397, 883. Gondoin, P., Orr, A. & Siddiqui, H., 2004, A&A 420, 905. Guainazzi, M., Rodriguez-Pascual, P., Fabian, A.C., Iwasawa, K. & Matt, G., 2004, MNRAS 355, 297. Harnett, J., Ehle, M., Fletcher, A. et al., 2004, A&A 421, 571. Jimenez-Bailon, E., Piconcelli, E., Guainazzi, M. et al., 2004, A&A, in press. Piconcelli, E., Jimenez-Bailon, E., Guainazzi, M., et al., 2004, MNRAS, 351, 161. Piconcelli, E., Jimenez-Bailon, E., Guainazzi, M. et al., 2005, A&A 432, 15. Schartel, N., Rodriguez-Pascual, P.M., Santos-Lleo, M. et al., 2005, A&A 433, 455. Figure 2.2.4/1: The amplitude of the 10-min orbiter binary RX J1914+24, observed with S-CAM3 in July 2004. Immediately apparent in the colour ratio 2.2.4 Ground-based photon-counting studies (bottom panel) are not only the amplitude variation with orbital phase but also the colour dependency of The SCI-A technology development programme in the amplitude. Observations were made in superconducting detector arrays is being exploited within collaboration with Cropper & Ramsey, MSSL (UK). RSSD. This technology allows for optical photon counting with high efficiency, high time resolution, and photon energy determination, and has been under development for several years. It was last used at the William Herschel Telescope on La Palma in October very nice amplitude and colour modulation at the 2000, resulting in several publications mainly related to expected period. A series of exploratory observations of the determination of light curves and physical conditions pulsating white dwarfs and polar QPOs were undertaken in magnetic Cataclysmic Variables. Papers dealing with with R. Kotak (Imperial College, London). The high time temperature determination, and quasar redshift determin- resolution of the photon arrival time datation (of order a ation, both using the energy-resolved capabilities of the few microseconds) makes the device well suited to the device, have also been published over the last 3 years. long-running search for further optical counterparts of The array was recently upgraded from a 6x6 array radio pulsars: one millisecond pulsar and two normal (S-Cam2) to a 10x12 array (S-Cam3), and operated again pulsars were observed, under good photometric at the WHT for six nights in July 2004. conditions, with good reference astrometry allowing the expected position of the pulsar to be well centred on the The datasets arising from the S-Cam instrument are array. Preliminary estimates of the limiting magnitude of complex to analyse and interpret. In addition to the issues these observations, assuming a 10% pulsar duty cycle, of photometric stability and calibration of normal CCD are at around V = 26. cameras (e.g. atmospheric extinction and zenith angle variations) access to the photon arrival times means that the resulting datasets include time-dependent effects (seeing and sky background variations, as well as time- dependent differential atmospheric refraction, small amplitude telescope oscillations during short periods of high wind speed, etc) which must be calibrated as part of the pipeline processing. Detector and electronics enhancements made in the development from S-Cam2 to S-Cam3 have resulted in a very stable instrument.

A number of different observing programmes, granted through the Netherlands time allocation panel, have been undertaken. Eclipse mapping of three CVs was carried out in a programme led by P. Groot (Nijmijgen). Twelve successive cycles of the 12-min period ultra-compact binary RX J1914+24 were obtained (in a collaboration with G. Ramsay and M. Cropper at MSSL), showing sec2.qxd 7/11/05 5:13 PM Page 19

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2.3 Optical/UV Astrophysics

The optical/UV astrophysics research group has relied primarily on HST observations complemented by ground-based facilities to study a wide range of objects, including classical nebulae, the central stars of planetary nebulae, star formation in starburst galaxies and luminous IR galaxies.

2.3.1 The Helix Nebula: when opportunity knocks

The Helix Nebula (NGC 7293) lies about 600 ly away in Aquarius and has a diameter of about 2.4 ly, thus spanning as much as 14 arcmin. A substantial portion of the Helix has been imaged in two colours, using both ACS and WFPC2 by N. Panagia and collaborators. Fig 2.3.1/1 shows an image made by combining the new images from the HST-ACS and wide-angle images from the Mosaic Camera on the WIYN 0.9 m Telescope at Kitt Peak National Observatory. This is one of the largest and Figure 2.3.1/1: The Helix Nebula seen by combining most detailed celestial images ever made. the new images from the HST-ACS and wide-angle images from the Mosaic Camera on the WIYN 0.9 m These HST observations were made possible by a telescope at the Kitt Peak National Observatory. fortuitous combination of events. One of the most prominent meteor showers is the Leonids each November. The shower in 2002 was predicted to be especially rich and since those meteoroids pose a non- zero risk to spacecraft, HST had to carry out a special boundary between those stars that will evolve off the procedure to minimise the risk and any consequences. As AGB phase into Planetary Nebulae (PNe) and ultimately in the past several years, HST was required to point in a fade into white dwarfs, and those that will end their lives particular direction during the meteor shower in order to as type II Supernovae. keep the telescope’s aft end towards the stream, while minimising the cross-section of the solar arrays. This Studies of Central Stars (CSs) of PNe in the Galaxy are stand-down period was from 0 h to 14 h UT on 18 hampered by the poor knowledge of their distances, a November 2002. In preparing for this special effort, it problem that can be overcome by observing PNe in the was noticed that just outside the nominal pointing region Magellanic Clouds (LMC and SMC; Fig. 2.3.2/1). From lay the Helix Nebula, which had been imaged by Hubble ground-based observations, the unresolved nature of the in some small areas but never in its entirety. This was too nebula has, however, so far prevented us from taking full good an opportunity to miss! The HST Project at advantage of a known distance in the determination of Goddard Space Flight Center was immediately contacted the CS parameters. As a result, most ground-based and their concurrence in using HST slightly beyond its studies have had to rely heavily on photoionisation nominal pointing area was secured. Thus, it became modelling of the nebula in order to derive these CS possible to devote nine orbits of HST observing time to parameters. imaging a substantial portion of the large Helix Nebula in two colours, using both ACS and WFPC2, obtaining the HST offers a unique opportunity to study the CSs of PNe most detailed image ever of it. Apart from its outstanding in the Magellanic Clouds with unprecedented accuracy, beauty, such an image is also extremely valuable because largely because the stellar continuum can be measured it is a high-quality first-epoch dataset that is ideally directly. Villaver and collaborators have determined suited for later work on measuring the motions of the accurate masses of CSs of PNe for the two largest tight knots immersed in the nebula. samples of extra-galactic PNe ever studied, and have explored the connections among the fundamental properties of the stars and the physical properties of the 2.3.2 Central stars of planetary nebulae host nebulae (Villaver et al., 2003; 2004). Similar average masses in the LMC and SMC have been Stellar evolution predicts that stars in the range 1-8 solar established as well as an indication of a difference in the masses will lose most of their stellar envelopes through mass distribution of the two samples that cannot be mass-loss as they ascend the Asymptotic Giant Branch explained by a mass-loss rate dependency with (AGB) phase. It is the mass-loss that establishes the mass metallicity. As the immediate precursors of white dwarfs, sec2.qxd 7/11/05 5:13 PM Page 20

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Figure 2.3.2/1: A sample of HST (50 CCD STIS bandpass) images of LMC Planetary Nebulae. From left to right: SMP 4, SMP 10, SMP1 8, SMP 102. The field of view is 3 arcsec and the intensity scale is logarithmic.

the study of the mass distribution of the CSs of PNe type II-P SN 2003gd (Smartt et al., 2004). They found should help to constrain the initial-to-final mass relation that the star was an 8 solar-mass red supergiant, which is within environments of differing metallicity. consistent with the models of single stellar evolution.

Ground-based data from several telescopes have 2.3.3 Identifying core-collapse supernovae identified that the type II-P SN 2004dj took place in a progenitors 14 Myr-old, 24 000 solar-mass stellar cluster that included a number of red and blue supergiants (Maiz- With the only exception of type SN Ia, theory predicts Apellaniz et al., 2004). Post-explosion HST/ACS images that all other types of supernovae arise from the collapse obtained by Filippenko et al. were able to resolve the of the core of a massive evolved star that exhausts its supernova and the surrounding cluster (Fig. 2.3.3/1). nuclear fuel and cannot generate enough energy to support itself. After the explosion of one of these core- Images of the location of SN 1993J with HST/ACS have collapse supernovae, a neutron star or a black hole is all been obtained that allowed the identification of a bright that remains of the progenitor star. However, there are blue star that could have been the companion of the very few observations of the SN progenitors that can be previously red supergiant that exploded (Maund et al., used to confirm the theoretical predictions regarding 2004). The existence of such a companion had been their nature. Until 2003, only two SN had had their predicted by the theoretical models that had been progenitors unambiguously identified: SN 1987A and SN 1993J. The situation changed that year, when HST played a decisive role in the identification of two new progenitors and in the gathering of new information on one of the previous two.

A combination of pre-explosion HST/WFPC2 and Gemini/GMOS images and post-explosion HST/ACS images have been used to identify the progenitor of the

Figure 2.3.3/1: Three-colour ACS/HRC mosaic (red: F330W, green: F250W, blue: F220W) of the region around the cluster Sandage 96 in NGC 2403, where SN 2004dj took place, obtained 2 months after the explosion. The field is 90 pc on each side, with north towards the top. The central extended object is the cluster itself (blue owing to the blue giants and supergiants) while the reddish point source is the SN located about 1 pc to the south of the centre of Sandage 96. sec2.qxd 7/11/05 5:13 PM Page 21

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advanced to explain the peculiar evolution of the SN, the starburst environment. What we observe could thus which started out as a hydrogen-rich type II to later be the result of either chemical pollution of the medium transform into a helium-rich type Ib. closely surrounding the starburst or a metallicity gradient from the inner metal-rich galaxy to an outer metal-poor halo. The metal offset between the neutral and ionised 2.3.4 Metals in the dwarf starburst galaxy ISM has important implications for the chemical NGC 1705 evolution of dwarf starburst galaxies, since it implies that widespread enrichment episodes have preceded the NGC 1705 is one of the most intriguing nearby objects. current burst that dominates the bolometric luminosity of At a distance of 5 Mpc, it is a dwarf galaxy that is these systems. A potential scenario is one where star experiencing intense star formation, a so-called starburst. formation dates quite far back in the past, allowing the As a result, it hosts in its centre a compact and massive metals to be produced in the most central regions and young star cluster and shows evidence of a spectacular efficiently dispersed in the surrounding neutral gas of the large-scale outflow triggered by the simultaneous halo. The ISM non-homogeneity may also imply a larger explosion of a myriad of SNe II. The extreme physical loss of metals via galactic winds than previously thought, conditions of starbursts like NGC 1705 must have been thus favoring ‘bursty’ over low-level quasi-continuous much more common in the past, making them crucial star formation. targets against which observations of higher-redshift galaxies must be compared. 2.3.5 Luminous IR galaxies: a key galaxy population Dwarf starburst galaxies are characterised by a large reservoir of neutral gas. This is a fundamental ingredient Luminous IR Galaxies (LIRGs) are believed to be very for the star-formation onset, but it is also the place where common in the distant Universe, and are probably the most of the baryons may hide. A. Aloisi and local counterpart of the sub-mm galaxies that give rise to collaborators have studied the neutral ISM of NGC 1705 the far-IR background. The physical processes at work in by analysing the absorption lines detected in high- LIRGs (mergers of galaxies, dust-shrouded massive resolution UV spectra of its central cluster. The synergy starbursts, AGN formation, outflows, enrichment of the between the complementary spectral ranges of the intergalactic medium, etc) are likely to be the same as in HST/STIS and FUSE data used in this project has young galaxies in the early Universe. Therefore, they are allowed for the first time the issues involved in this type natural laboratories for understanding these processes in of analysis (e.g., saturation, ionisation and depletion) to detail, providing a local reference to high-z galaxy be tackled. The study shows that the metals abundance in population studies. the neutral gas of NGC 1705 are lower than in the ionised gas of the H II regions probed via optical nebular A project aimed at studying the internal structure and spectroscopy. This intriguing result unambiguously kinematics of a representative sample of LIRGs is indicates that the ISM in dwarf star-forming galaxies is underway. This study is based on Integral Field not homogeneous as previously suggested and usually Spectroscopy (IFS) using the 4.2 m William Herschel assumed in chemical evolution models, and may imply Telescope and HST imaging (WFPC2 and NICMOS). the existence of a lower metallicity halo that surrounds These two techniques are ideal and complementary to study the complex physical and kinematics properties of these objects. The analysis is mainly based on the rest frame optical spectral diagnostic features (and near-IR morphologies), which will be shifted towards longer wavelengths in the high-z galaxy populations to be studied with JWST. Furthermore, the linear resolutions to be obtained with JWST for high-z populations are coarsely of the order of those now obtained from the ground for local LIRGs.

Figure 2.3.5/1: HST/NICMOS (K-filter) image of the ultra-luminous IR galaxy IRAS 17208-0014, likely a merging of two galaxies in its final dynamical phase. The iso-contours indicate the ionised gas (H-alpha) velocity dispersion map (top) and velocity field (bottom) obtained with the fibre system on the 4.2 m WHT. sec2.qxd 7/11/05 5:13 PM Page 22

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Figure 2.3.5/1 presents the ionised gas (Hα) velocity 2.4 Infrared/Sub-millimetre Astrophysics dispersion map and velocity field of IRAS 17208-0014 (iso-contours), together with the near-IR image obtained The research group continues to utilise the ISO archive with HST/NICMOS (Arribas & Colina, 2003). It is extensively to further its research interests in a wide interesting to note that the peak of the velocity dispersion range of astronomical topics, ranging from Solar System map is centred on the near-IR continuum maximum, studies to analysis of deep fields. which indicates that for this galaxy the velocity dispersion seems to be a good mass tracer. Furthermore, the velocity field has a pattern compatible with rotation, 2.4.1 Solar System studies with its kinematical centre in positional agreement with the nucleus. This is a surprising result and differs from Salama, together with Coustenis et al., has continued the those obtained for most of the objects studied so far, analysis of the ISO Titan data taken by the SWS where the velocity fields are rather dominated by tidal instrument. The near-IR spectra of Titan show several induced forces. If velocity fields do not show rotation weak CH4 absorption regions, in particular centred near they cannot be used for obtaining dynamical masses, a 2.75 µm. Owing to interference from telluric CO2 key observational parameter for testing the hierarchical absorption features, only part of this region (2.9-3.1 µm) models of galaxy formation and evolution – these models has been observed from the ground. ISO observations predict an increase of galaxy masses over cosmic time. If show the 2.75 µm window in its full shape for the first velocity fields cannot be used for inferring dynamical time. Using a detailed microphysical model of Titan’s masses, such models have to be tested by more indirect atmosphere, information on the atmospheric parameters techniques. (haze extinction, single scattering albedo, tholin refractive index, etc.) has been derived by fitting the References methane bands. From the derived surface albedo Arribas, S., Colina. L., 2003, ApJ 591, 791. spectrum around 2.75 µm, some constraints on Titan’s Maiz-Apellaniz, J. et al., 2004, ApJL (10 November 2004 surface composition were determined. ISO data appear to issue). be compatible with H2O and CO2 ices. Maund, J.R. et al., 2004, Nature 427, 129. Smartt, S.J. et al., 2004, Science 303, 499. Villaver, E., Stanghellini, L. & Shaw, R.A., 2003, ApJ 2.4.2 Interstellar medium studies 597, 298. Villaver, E., Stanghellini, L. & Shaw, R.A., 2004, ApJ Work has progressed on the study of the dust emission of 614, in press. the interstellar medium of our Galaxy with balloon-borne sub-mm data (Dupac et al., 2003a) as well as with large- scale space-borne measurements. In addition, the dust emission of the NGC 891 galaxy was studied (Dupac et al., 2003b). This research was performed in collaboration with the Cold Universe group of CESR in Toulouse (F). In addition, the analysis of the Archeops balloon-borne experiment data, notably concerning the first detection of polarisation of the submillimetre dust emission (Benoit et al., 2004) and the measurement of the dust temperature- polarisation spectrum is ongoing. This work includes the measurement of the harmonic spectrum of the Cosmic Microwave Background fluctuations. In addition, in preparation for the Planck satellite operations phase, simulations of different scanning strategies for the cosmic microwave background is underway (Dupac & Tauber, 2005). Studies continue with CESR (Toulouse) into the gas/grain interaction in quiescent-dense inter- stellar medium (a filament in Taurus), using molecular lines and continuum tracers.

Studies of the dust properties in nine interstellar regions have also been fruitful, mostly from ISO observations at 60-200 µm (del Burgo et al., 2003), where an increased far-IR emissivity was observed in big dust grains (15- 110 nm) towards low temperatures. The relative abundance of very small grains (1.2-15 nm) with respect to the big grains shows significant variations from region sec2.qxd 7/11/05 5:13 PM Page 23

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Figure 2.4.2/1: CVF observation of the M31 bulge. Top: corrected images at 6 µm and 11.3 µm and, for comparison, the uncorrected 11.3 µm image. Bottom: spectrum of the M31 bulge obtained by linearly correlating the smooth radial gradient of the bulge emission at each wavelength with that measured at 6 µm (left), and the spectrum of the dust clouds that can be seen in the images (right).

to region at low column densities. Along lines of sight of proto-Oort cloud at distances of several tens of thousands higher column density, the data indicate the disappear- of AU from the binary. ance of small grains. These results can be interpreted in terms of coagulation of dust. The larger size and porous Analysis of a sample of high-luminosity star-forming structure of grains could explain the increased far-IR regions observed by ISO LWS indicate they are emissivity. The far-IR emission from large grains in characterised by strong far-UV stellar fields causing Taurus has been separated into warm and cold atomic ionisation. This work has shown how photo- components, from which the temperature and optical ionisation models can explain the observed fine structure depth of the components was determined and compared line luminosities and where other components, such as with the properties of the molecular gas. In addition, photodissociation emission and shock excitation by characterisation of the cirrus structure over the 90- outflows, have to be included to account for the observed 200 µm wavelength range continues (Kiss et al., 2003). spectra.

Improvements in the data reduction of the ISOCAM- As part of the GLIMPSE legacy team of the NASA CVF have been made that were motivated by the goal of Spitzer Space Telescope, a survey has been conducted of analysing extended emission data in less excited regions parts of the Galactic Plane in four IR wavebands between of the sky. The key features of the new data process are 3.6 µm and 8 µm. The early results of protostars in the the subtraction of the zodiacal emission and the Elephant Trunk Nebula and the discovery of a distant associated straylight, the improvement of the wavelength star-formation region have been published by Reach et calibration, and the astrometry. The scientific informa- al. (2004) and Mercer et al. (2004), respectively. tion that can be now extracted from the data is greatly enhanced for the large number of observed fields with Two research projects concerning low-mass brown extended emission fainter than the zodiacal light. Thanks dwarfs and planetary-mass objects in star-forming to all these corrections, reliable spectrum and spatial regions are also underway. The first is based on very structure of extended objects can be extracted. The deep ISOCAM images of the Taurus molecular cloud. results of the improved pipeline have been made The IR excess from the circumstellar disc of the forming available for public use in the ISO archive. stars is commonly used to identify young stars. It has been found that, in contrast to previous studies in which the presence of galaxies in the field was not taken into 2.4.3 Star formation account, the galaxies dominate the detections at these low flux-levels. These results have ramifications for the The investigation of the star-forming system in L1551 interpretation of the deep images of star-forming regions has continued. It is now clear that the inner parts of this acquired by the Spitzer Space Telescope. proto binary (class 0/1) is surrounded by a massive (> several solar masses) disc, from which the outflow The second project compares two different methods for lifts off. Aspects of the shocks within the outflow are identifying young stars. In general, mid-IR studies yield being investigated, particularly with respect to the a higher fraction of low-mass stars when compared to recently discovered X-ray source. In addition – for the optical and near-IR surveys. The questions addressed are: first time – methanol from the outer edges of this disc has ‘What is the cause of this discrepancy?’ and ‘Which been detected, which suggests that it could be due to a method gives the best measure of the true fraction of sec2.qxd 7/11/05 5:13 PM Page 24

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low-mass objects?’. Highly embedded regions (i.e. between CO and ONeMg novae (Lyke et al., 2003). For regions with very recent star formation) are best studied Nova V723 Cassiopae, the IR spectrum was dominated in the mid-IR because of the large extinction. This in the first year by H and He recombination lines, and at extinction may cause a strong bias in optical studies. For later times by coronal lines. From the H recombination older regions, optical surveys bring the advantage of lines, electron temperature and an electron density were increased sensitivity and higher spatial resolution. The derived. From the coronal lines abundance ratios of Chamaeleon star-forming region is the ideal intermediate S/Si ≈ 2.1, Ca/Si ≈ 1.6 and Al/Si ≈ 1.5 were found. The in which both methods have been applied. The candidate ejected mass was also constrained (Evans et al., 2003). lists from both mid-IR (ISOCAM) and near-IR surveys have been compared. They find that the effects of ISO/SWS IR spectra of oxygen-rich AGB stars with extinction in the optical are minimal and only a few stars optically thin dust shells continue to be exploited (Heras in the very densest part are undetected in the near-IR & Hony, 2005). The low mass-loss rate regime is of survey. particular interest because, owing to the low densities of the outflow, dust condensation may not be complete and Investigations into aspects of the process of star- and it is possible to observe the intermediate steps in the solar system-formation have continued. High-resolution dust condensation sequence. The composition of the spectra have been obtained with the VLT/UVES dust and the physical conditions in the shells were combination of the Beta Pictoris disc. The data maps the determined by modelling the SWS observations with gas distribution within the gas disc in more than 70 the radiative transfer code DUSTY. Through the absorption lines, demonstrating the warping of the disc. comparison with the CO observations found in the Gas can be traced from the inner parts out to more than literature, gas-to-dust ratios were calculated and the 400 AU. The origin of the gas remains unclear; the mass-loss rates derived. The results show that, even in investigation clearly shows that the gas is not the low-density environments studied, the dust accelerating outwards as it should do, given the radiation produced is enough to drive the stellar wind by pressure. An unseen molecular component may hold the radiation pressure. The composition of the dust and its atomic gas in place. dependence on the physical conditions at the inner shell is consistent with the thermodynamic dust condensation sequence. However, the temperatures derived for the 2.4.4 Stellar studies dust formation are lower than those estimated by current theories. A local interface dynamo model has been developed in order to reproduce the activity cycles of about 30 Sun- ISO/SWS spectra of S stars are also now being type stars, which have been detected by monitoring, examined. These AGB stars have abundances between since 1966, the photometric variation in two bands the oxygen-rich and the carbon-rich AGB stars. Owing centred in the Ca II H and K lines. The local model splits to this intermediate composition pattern, the molecules the dynamo equations into two systems, the first for the and solid components that form around such stars are overshoot region where the strong toroidal field is poorly known. In general, it is assumed that the solid assumed to be produced by the internal differential particles are predominantly silicates, i.e. oxygen-rich rotation, and the second for the base of the convection dust. The new ISO spectra present the first-ever zone where the so-called alpha-effect produces the detection of magnesium-sulphide grains around S stars. poloidal field. The model includes some new features, Such grains are otherwise observed only in carbon-rich such as the refraction of the magnetic waves from the environs. Furthermore, the spectra indicate that the overshoot region to the convection zone, and the scaling silicates present around these stars are systematically of the width of the shear layer where the differential different from those found around oxygen-rich AGBs. rotation is concentrated in the Sun. The observed trends A radiative transfer model has been developed in order in the magnetic cycle and rotation periods are well to derive physical parameters (size, distance, density) of reproduced by the model. The dependence of the detached dust shells around carbon-rich AGB stars magnetic intensites in the stellar interiors on the spectral based on their IR spectra (Hony & Bouwman, 2004). types, obtained with the model, agrees with that followed This model was also applied to two well-studied stars by the observed surface magnetic fields. with good agreement with other methods (CO mapping and imaging of light scattered from the dust). The new Nova continue to be studied through the use of method can be easily applied to more distant stars observations made by ISO SWS. For CP Crucis (Nova where these other techniques fail. It is intended to apply Crux 1996), abundance enhancements versus solar by and test the new model extensively by using new mass were found to be of 75, 17 and 27 for N, O and Ne, observations from the Spitzer Space Telescope in three respectively, from ISO and quasi-simultaneous ground- accepted programmes. based observations. Additionally, the Mg abundance in the ejecta is constrained to be approximately solar. The Studies of the dust shell around the peculiar post-AGB nova appears to be an example of the ‘missing link’ object HD 56126 (Fig. 2.4.4/1) have also been sec2.qxd 7/11/05 5:13 PM Page 25

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merging of multiple observations of the same source, about 16 500 mid-IR objects were confirmed with a confidence level of the detection probability to better than 99%. The catalogue will contain these sources and associated flags like source characterisation, detection quality and astrometric correction. The typical sensitivity limit reached in this survey is about 1 mJy, with a median of 3.9 mJy.

As a first scientific result derived from ISOCAM parallel results, a collaboration led by Haas (Ruhr Universitaet Bochum, D) discovered unique mid-IR excess sources. Various arguments suggest that they likely contain an AGN. The ongoing optical spectroscopy indicates 40% Figure 2.4.4/1: Multi-wavelength spectrum of the of the sample to be classical AGN and the remaining part post-AGB object HD 56126. The star is surrounded to be dust-shrouded sources. A survey of mid-IR selected by a shell of carbon-rich dust. The shell is easily AGNs was initiated to confirm this. In addition, identified in the mid-IR image (top-left), while the observing time was granted by Spitzer and TNG. star itself (indicated by the star symbol) is hardly detected. The spectrum is clearly divided in two Improvements in the ISO calibration has led to further components; the star dominates the UV and optical work in the areas of the far-IR source count analysis and light, while all the IR radiation originates from the luminosity function in the ELAIS fields (Heraudeau et dust in the shell roughly 2500 AU away. The various al., 2004; Serjeant et al., 2004) and cosmic far-IR dust components have been indicated. background (Rowan-Robinson et al., 2004).

A series of papers on the deep ISOCAM survey through gravitationally lensing galaxy clusters has been published. Metcalfe et al. (2003) presented the conducted (Hony et al., 2003). From the detailed catalogue of 7 µm and 15 µm observations of 148 mid- radiative transfer modelling of the IR spectrum and IR sources from the A370, A2218 and A2390 fields. imaging, stringent constraints are placed on the The fluxes of lensed background sources were composition and physical parameters of the shell. It has corrected for amplification to yield source counts been found that the star has relatively normal dust reaching three times deeper than other mid-IR surveys. properties but has exhibited an atypically high mass-loss These counts confirmed and extended earlier findings rate. of a factor of ten excess of 15 µm galaxies compared to models with no evolution. Most sources occur at The analysis of individual stellar sources evolving from 0.4 < z < 1.5 with median ~0.6, and resolve the bulk of the AGB to the PN stage, using multi-wavelength the cosmic mid-IR background. observations, has continued. In particular, in collabora- tion with A. Riera (U. Barcelona) and others, a detailed Clusters of galaxies have also been studied (Biviano et analysis was made of the remarkable highly collimated al., 2004; Coia et al., 2005a; 2005b) based on archival optical jets associated with the proto-PN Hen 3-1475 and published data to investigate the properties of (Garden Sprinkler Nebula), interpreted as the result of clusters of galaxies over a range of redshift episodic mass loss by a precessing binary system. A (0.18 < z < 0.4). Clusters A2219, Cl0024+1654 and detailed chemical abundance analysis of the PN Me 2-1 A1689 were included, for a total sample of about 75 was also carried out using a combination of ISO and IUE cluster sources, constituting a substantial fraction of the data, with optical spectra taken from the literature. ISO results on galaxy clusters beyond Virgo and Coma. Finally, two rare, new type I PNe belonging to the Comparing IR-based star-formation rates with optical Galactic Bulge population were identified as such and results shows up to 90% of cluster star-formation activity studied in detail. hidden from optical spectra by dust. Clusters were compared at 15 µm. Cl0024 has similar redshift to A370 but hosts ten times as many luminous IR galaxies 2.4.5 Extragalactic studies (LIRGs). No LIRGs were detected in A1689, A2218 or A2390, while a total of three might have been expected The ISOCAM Parallel Mode observations continue to be based on the results from Cl0024. The sources in Cl0024 exploited. A 27 sq. deg. area was observed with LW2, a are much more powerful than those in A1689 and A2218. broadband filter centred on 6.7 µm. The work on the A2218 galaxies were fitted by models of quiescent resultant point source catalogue is close to completion: ellipticals. The 13 galaxies detected in Cl0024 are after statistical cleaning, astrometric corrections and strongly star-forming. sec2.qxd 7/11/05 5:13 PM Page 26

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References 2.5 Solar Physics Benoît, A., Ade, P., Amblard, A., et al., 2004, A&A 424, 571. The research group continues to use SOHO observations Biviano, A., Metcalfe, L., McBreen, B., et al., 2004, A&A extensively to further its research interests in a wide 425, 33. range of topics in solar physics, such as studies of the Coia, D., McBreen, B., Metcalfe, L. et al., 2005a, A&A chromosphere, transition region dynamics and coronal 431, 433. magnetic fields. Coia, D., Metcalfe, L. McBreen, B., et al., 2005b, A&A 430, 59. del Burgo, C., Laureijs, R. J., Ábrahám, P., Kiss, Cs., 2.5.1 Chromospheric oscillations 2003, MNRAS 346, 403. Dupac, X., Bernard, J.-P., Boudet, N., et al., 2003a, A&A Investigations are underway to study the interaction of 404, L11. the topographic structure of the solar chromospheric Dupac, X., del Burgo, C., Bernard, J.-P., et al., 2003b, plasma with the wave modes observed (McIntosh & MNRAS 344, 105. Fleck, 2004; McIntosh et al., 2003). A distinct correlation Dupac, X. & Tauber, J., 2005, A&A 430, 363. between the inferred plasma topography and the phase Evans, A., Gehrz, R.D., Geballe, T.R., et al., 2003, AJ differences between and suppression of oscillations at 126, 1981. different levels in the solar atmosphere has been Héraudeau, Ph., Oliver, S., del Burgo, C., et al., 2004, established (Fig. 2.5.1/1). This can be interpreted as MNRAS 354, 924. evidence of interaction between the waves and the Hony, S., Bouwman, J., 2004, A&A 413, 981. extended magnetic ‘canopy’. Hony, S., Tielens, A.G.G.M., Waters, L.B.F.M., de Koter, A., 2003, A&A 402, 211. Coronal holes are the lowest density plasma components Heras, A. & Hony, S., 2005, A&A, in press. of the Sun’s outer atmosphere. They are associated with Kiss, Cs., Ábrahám, P., Klaas, U., et al., 2003, A&A 399, rapidly expanding magnetic fields and are the source 177. regions of the fast solar wind. The interfaces between Lyke, J.E., Koenig, X.P., Barlow, M.J., et al., 2003, AJ open and closed regions make them a topologically 126, 993. interesting place. McIntosh et al. (2004) have therefore Mercer, E.P., Clemens, D.P., Bania, T.M., et al., 2004, studied the propagation characteristics of chromospheric ApJS 154, 328. oscillations in and around an equatorial hole by applying Metcalfe, L., Kneib, J.-P., McBreen, B., et al., 2003, phase-difference and travel-time diagnostics to TRACE A&A 407, 791. time series in the 1700 Å and 1600 Å UV continua Reach, W.T., Rho, J., Young, E., et al., 2004, ApJS 154, bandpasses. Their results suggest a significant change in 385. atmospheric conditions at the base of the chromosphere Rowan-Robinson, M., Lari, C., Perez-Fournon, I., et al., inside the coronal hole relative to its boundary and quiet- 2004, MNRAS 351, 1290. Sun regions. Fig 2.5.1/2 shows a SOHO EIT 195 Å Serjeant, S., Carramiñana, A., Gonzáles-Solares, E., et context image from 2003 July 14, 00:08 UT. The TRACE al., 2004, MNRAS 355, 813. field-of-view is shown as the thick red rectangular region. The coloured contour levels qualitatively indicate the coronal hole boundary.

Figure 2.5.1/3 shows a travel-time map between the 1700 Å and 1600 Å signal. The travel-time (∆t) at any frequency (ν) is computed by applying a Gaussian filter, G(ν, δν), about ν with a width δν to each bandpass, cross-correlating the two filtered sequences and determining the shift of the cross-correlation function. The 1700 Å continuum is formed a few tens of km below the 1600 Å continuum. For upward travelling waves, the 1700 Å signal therefore leads the 1600 Å signal by a few seconds (negative travel-time according to the convention applied here).

There is a notable difference in travel-time between the coronal hole interior and exterior (~4 s). Interpreting the waves as being predominantly acoustic in nature, the ∆ ∆ observed travel-time, t ≈ z/cs, is directly proportional to the height difference between the two bandpasses, where cs is the local sound speed in the lower sec2.qxd 7/11/05 5:13 PM Page 27

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Figure 2.5.1/2: SOHO EIT 195 Å context image from 2003 July 14, 00:08 UT. The red rectangular region shows the TRACE field-of-view, while the yellow and orange contours show the 100 DN and 200 DN intensity levels in the image, respectively.

Figure 2.5.1/1: Upper left: spatial variation in the altitudes at which the plasma-β is of order unity in the TRACE field of view. Solid contours are added for reference, each separated by 0.25 Mm. The map is Figure 2.5.1/3: Travel-time map at full TRACE based on a potential field extrapolation of a time- resolution between the 1700 Å and 1600 Å band- average MDI longitudinal magnetogram. The passes. The coloured rectangles denote regions of presence of the network elements, where the β- coronal hole interior (red), coronal hole transition height is blue-violet in colour, is perhaps boundary/exterior (blue), and coronal hole arcade the most striking feature. The other panels show one (purple). example of the integrated oscillatory power in the 3- 8 mHz band of the 1700, 1600 and 1550 Å TRACE UV bandpasses, respectively. On each of these panels we have overplotted the contours of the β-transition height in the upper left. Note the clear correlation between the reduced power and the contours.

chromosphere (~6 km/s). For a filter frequency of 7 mHz, the 4 s difference can therefore be approximated to a difference in ∆z of 24 km between the coronal hole interior and its boundary, a not insignificant fraction of a scale height near the chromospheric temperature minimum (~100 km).

This is a quite unexpected and confounding result: Why would the largely hydrodynamic (high plasma-β) coronal hole interior plasma at the base of the chromosphere care sec2.qxd 7/11/05 5:13 PM Page 28

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about the fact that the magnetic field is open to the transition region, but the range of these enhanced interplanetary medium and stratify itself so? velocities is no larger than the typical spread of Doppler Conventional thinking would assume that the velocities in this region. The anticipated ranges of chromosphere should have little knowledge of the Doppler velocities of blinkers are 25-30 km/s in the quiet topologically open coronal holes above. Follow-up Sun (20-40 km/s in active regions) for O V. studies addressing a possible connection between the mixture of field polarities, proportion of open/closed Bewsher et al. (2003) also found that blinkers have magnetic structures, UV/EUV intensity/Doppler velocity preferentially larger non-thermal velocities than the contrast, and in situ solar wind measurements are on- typical background transition region. Again, the increase going. in magnitude of these non-thermal velocities is no greater than the typical ranges of non-thermal velocities. The range of non-thermal velocities of blinkers in both the 2.5.2 Dynamics of transition region blinkers quiet-Sun and active-regions are estimated to be 30- 45 km/s in O V. Blinkers are small-scale intensity enhancements observed in the transition region of the solar atmosphere. There are more blinkers with larger Doppler and non- They were first detected by eye in SOHO/CDS data, but thermal velocities than would be expected in the whole automated methods have been developed more recently of the transition region. The results have been used to to identify these events. Blinkers are best observed in help elaborate further the many mechanisms proposed to O V (which is formed at a temperature of 2.5x105K) and explain blinkers. have mean areas of 3x107 km2 and mean lifetimes of 16 min. They are either density enhancements or increases in filling factor, but not temperature events. 2.5.3 Comparison of blinkers and explosive events They occur above regions where one polarity of magnetic field dominates, including quiet Sun, plage Blinkers (intensity enhancements) are predominantly regions or sunspots. observed with the CDS instrument on SOHO and were discussed in the subsection above. Such blinkers can be further investigated by studying the relative Doppler and non-thermal velocities of quiet-Sun Explosive events, however, are characterised by strong and active-region blinkers identified in O V with non-Gaussian enhancements in the wings of spectral SOHO/CDS. It has been found that O V blinkers have a lines, and have large velocities (50-250 km/s) associated preference to be more redshifted than the normal with them. Explosive events have recently been observed with the SUMER instrument on SOHO but where first observed using HRTS. They have a mean area of 1 Mm2 and mean lifetime of 1 min. They are associated with regions of complex weak fields or on the edges of Figure 2.5.2/1: Three SOHO/CDS O V rasters taken unipolar. Models of the magnetic reconnection 7 min and 8 min apart. The circled region shows a configuration required for explosive events to occur have blinker in the second frame. also been presented.

There has been much speculation as to whether blinkers and explosive events are the same phenomenon, but observed differently with the CDS and SUMER instruments.

Bewsher et al. (2004a) have analysed co-spatial and co-temporal CDS and SUMER datasets and automatic- ally identified both blinkers and explosive events in both instruments data. They found that blinkers were identified in the SUMER data if the temporal resolution of the data was reduced to that of the CDS data, otherwise short-lived localised intensity enhancements were identified. Explosive events were identified in the CDS data if the width of the spectral line was significantly increased, and occasionally if an enhancement in the wing was present. In 3.5 h of data, they found only one case where a blinker and an explosive event coincided, ten examples of lone blinkers and seven examples of lone explosive events. This has sec2.qxd 7/11/05 5:13 PM Page 29

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(a) (b) Figure 2.5.3/1: (a) SUMER single slit image showing an explosive event labelled S1; (b) CDS raster showing blinkers labelled C1-3. The diamonds on the CDS raster mark the locations of blinkers and the vertical dashed line indicates the position of the SUMER slit. (c-d) lightcurves of the explosive event, S1 and blinker, C2 (which is closest spatially to the explosive event). (e-f) spectral line profiles of the explosive event S1 and blinker C2.

(c)

(d) Figure 2.5.4/1: Highly twisted magnetic flux tube inside an active region obtained from a non-linear force-free extrapolation technique based on photospheric vector magnetograms. The contours characterise the vertical magnetic field strength on the photosphere. (e) (f)

knowledge of the 3-D magnetic field is required. Considering that the observed solar region is in a force- free equilibrium state, the coronal magnetic field can be extrapolated from photospheric magnetic field measure- ments. Régnier and co-workers used vector magneto- graph measurements to study magnetic structures inside active regions (filaments or sigmoids) and their evolution led to the suggestion that blinkers and explosive events before and after flares. are not the same type of event. A theoretical statistical model was presented in Bewsher et al. (2004b), which Régnier & Amari (2004) have found that a filament and hypothesised that blinkers and explosive events are a sigmoid can both be described by a twisted flux tube random and not physically connected in any way. with a number of turns less than 1 and opposite electric current densities. They have also shown that the eruption associated with the studied active region is most likely 2.5.4 Coronal magnetic fields due to a highly twisted flux tube with a number of turns more than 1 (Fig. 2.5.4/1) different from the filament and To understand most of the phenomena in the solar the sigmoid. Studying the dynamics of an active region corona, such as flares, CMEs and filament eruptions, has also shown that the main progenitors of small flares sec2.qxd 7/11/05 5:13 PM Page 30

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identification of the source of the flare at a reversed-Y null point in the low corona.

References Bewsher, D., Parnell, C.E., Pike, C.D., Harrison, R.A., 2003, Solar Physics 215, 217. Bewsher, D., Innes, D.E., Parnell, C.E., Brown, D.S., 2004a, A&A, submitted. Bewsher, D., Brown, D.S., Innes, D.E., Parnell, C.E., 2004b, ESA SP-575, 465. Lundquist, L.L., Fisher, G.H., McTiernan, J.M., Régnier, S., 2004, ESA-SP 575, 306. McIntosh, S.W. & Fleck, B., 2004, ESA SP-547, 149. McIntosh, S.W., Fleck, B., Judge, P.G., 2003, A&A 405, Figure 2.5.4/2: Characteristic magnetic configuration 769. of the active region where most of the flares of McIntosh, S.W., Fleck, B., Tarbell, R.D., 2004, ApJ 609, October/November 2003 originate. Red field lines L95. describe the system of loops involved in the post-flare Régnier, S. & Amari, T., 2004, A&A 425, 345. phenomena. The background image is the Régnier, S. & Canfield, R.C., 2004, ESA-SP 575, 255. SOHO/MDI magnetogram at 10:00 UT Oct 28, 2003. Régnier, S. & Fleck, B., 2004, ESA-SP 575, 519. Welsch, B.T., Fisher, G.H., Abbett, W.P., Régnier, S., 2004, ApJ, 610, 1148.

in an active region are the transverse photospheric motions (sunspot rotation, magnetic flux emergence) and the complex topology (separatrix surfaces, separators) (Régnier & Canfield, 2004). The extrapolated coronal magnetic configurations are used to construct the synthetic X-ray and EUV emission maps by solving the energy equation along each individual coronal loop (Lundquist et al., 2004). The constructed maps are compared with observed images recorded by Yohkoh/ SXT and SOHO/EIT, giving some constraints on the coronal heating mechanism.

Vector magnetograms are also useful for determining the flow field on the photosphere. By combining the induction equation and the local correlation technique, Welsch et al. (2004) were able to self-consistently derive the three components of the flow field at the photospheric level. The flow fields as well as the force- free coronal magnetic configurations are the boundary conditions of magnetohydrodynamic (MHD) evolution codes.

Over 2 weeks in October/November 2003, the Sun featured unusually strong activity, with 12 X-class flares and two significant proton storms. Régnier & Fleck (2004) studied the magnetic properties of AR 10486 (the active region in which most of the events occurred) before and after the X17.2 flare on 28 October. Two methods were used: (i) the study of the active region dynamics by determining the potential coronal field from SOHO/MDI magnetograms with a high temporal cadence, as shown in Fig. 2.5.4/2; (ii) the analysis of a more accurate coronal magnetic configuration using a non-linear force-free extrapolation from a vector magnetogram taken before the flare, which led to the sec2.qxd 7/11/05 5:13 PM Page 31

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2.6 Heliospheric Physics/Space Plasma Studies

The scientists in SCI-SH have expertise in the observa- tions of electromagnetic fields and plasma particles, as well as in the detection of high-energy particles. Basically, their studies deal with two major areas. Firstly, how the solar wind originates and how it varies in the heliosphere; the team has particular expertise in solar energetic particles in the MeV range. Secondly, how the Earth’s plasma environment (the magnetosphere and ionosphere) is driven by the solar wind, particularly the transfer of particles between different regions as well as how particles are energised in the magnetosphere.

2.6.1 Energetic particles from the October/ November 2003 solar events

The research group has investigated heliospheric effects of the intense solar activity that occurred in October- November 2003 using observations of the COSPIN/LET Figure 2.6.1/1: Energetic particle observations of the instrument on the Ulysses spacecraft located near the COSPIN/LET instrument on Ulysses. solar equator at 5.2 AU from the Sun. COSPIN/LET was built by members of SCI-SH together with current members of SCI-A.

Figure 2.6.1/1 (top panel) presents the proton/alpha ratio 2.6.2 Energetic particles in the high-latitude, high- for the 42-day period after 17 October (DOY 290). speed solar wind Dashed vertical lines mark the times of forward (F) and reverse I shocks identified in the magnetic field data at A detailed study has been made of energetic particle Ulysses, where F-shocks labelled in red indicate events observed by COSPIN/LET during the recent probable CME-driven shocks. The lower panel contains second northern polar pass. For a short time during this heavy ion abundance ratios (1-day averages), all high-latitude pass, Ulysses was immersed in high-speed normalised to the solar energetic particle (SEP) solar wind from the newly formed northern polar coronal composition. Shown for reference is the 1.2-3.0 MeV hole. Four large SEP events were observed, permitting proton intensity. The onset time and duration of a large significant conclusions to be drawn concerning the CME associated with the October-November 2003 propagation of the particles to high latitudes. activity is marked by an inverted triangle. A topic of considerable debate triggered by Ulysses Solar wind conditions at Ulysses prior to the period of observations is the role played by perpendicular diffusion enhanced solar activity were dominated by recurrent in the transport of charged particles in the heliosphere. high-speed/low-speed stream interaction regions (SIRs). Based on the events studied here, no evidence has been As a result of the increased activity, and the associated found for local transport across the magnetic field. CMEs, this pattern was temporarily disrupted. The Indeed, the particle angular distributions at the onset at highest particle intensities occur at the time of the reverse all energies were considerably more isotropic than events shock on DOY 314/10 November, although the seen at lower latitudes, or even at 1 AU. preliminary analysis does not allow us to determine conclusively whether or not this is the result of local It must be stressed that the observations do not allow acceleration of the pre-existing SEP population. With the conclusions to be drawn about particle propagation close possible exception of He, which apparently shows a to the Sun. Even though, at the location of Ulysses, typical corotating interaction region (CIR) enhancement particles were propagating along the magnetic field lines (decrease in p/He, increase in He/O), the composition and not across them, there may be cross-field diffusion signatures suggest that the CIR reverse shock processed occurring close to the solar surface. Another possible the ambient SEP population (as evidenced by the SEP- mechanism is the large-scale distortion of the magnetic like C/O ratio). If real, the enhanced He content within field connecting Ulysses to the Sun at lower latitudes by, the CIR is presumably the result of accelerated for example, an outward-moving coronal mass ejection. interstellar pickup helium. The signature for Fe/O is suggestive of CIR composition, but very large scatter in Continuing the research group’s study of the relationship daily values prevents a firm conclusion. between the Sun and the heliosphere, the group is sec2.qxd 7/11/05 5:13 PM Page 32

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involved in a new instrument for NASA’s STEREO spacecraft. The instrument comprises a proton and electron telescope. Staff from SCI-A designed, manufac- tured and tested the overall electronics for the SEPT instrument for two NASA/STEREO satellites; the electronics is highly miniaturised using ASIC compo- nents. The instruments have been delivered for final testing at Caltech. The PI institute of the instrument is the University of Kiel (D); SCI-SH Co-I’s are R. Marsden and T. Sanderson.

2.6.3 Acceleration of electrons in the auroral region

One of the key issues in space plasma physics is the acceleration of charged particles. In the auroral region, electrons become highly accelerated before hitting the Earth’s atmosphere and causing auroral emission. The acceleration is often related to the occurrence of large electric fields, either DC or wave electric fields, which can be monitored with electric field instruments. The NASA Polar satellite (1996-) carries such an instrument that was in part built by the SCI-SH team together with current members of SCI-A.

Figure 2.6.3/1, taken from Janhunen et al. (2004c), provides one possible approach to the acceleration processes occurring in the auroral region. It appears that an island of density cavities (see the isocontours in the figure) and enhanced electric field structures occur at 4- 5RE radial distance in the evening and midnight Figure 2.6.3/1: Plasma processes that Alfvén waves magnetic local time (MLT) sectors in the auroral region cause in auroral regions. during disturbed conditions. At the same time, the ion beam occurrence frequency changes at the same altitude (these ions come from the Earth’s atmosphere). It is proposed that the mechanism involved in the electron acceleration is electron Landau resonance with incoming resonance region as well, leading to another density Alfvén waves. cavity at higher altitudes (see panel c) found by the authors in the earlier studies. After the Alfvén wave The auroral kilometric radiation (AKR) is the strongest activity has stopped, the cavity fills up on the ion time electromagnetic emission generated around the Earth and scale, so that it continues to exist for some time (panel d). it can be detected from large distances, even beyond the The low-altitude depletion is all the time maintained by heliosphere. Similar radiation can be observed from other processes that are independent of Alfvénic activity. other planets featuring auroral displays, e.g. Jupiter and Normal AKR is emitted all the time near the lower Saturn. A new type of AKR emission is Dot-AKR, boundary of the cavity, although not shown. originating from 2-3 RE radial distance, has been found to occur during substorm onsets. This is suggested to be an effect of Alfvénic wave acceleration in a pre-existing 2.6.4 Magnetospheric observations auroral cavity. In Fig. 2.6.3/1 panel a presents a low- altitude auroral cavity associated with a stable auroral arc Double cusp and reconnection hypotheses in the atmosphere and maintained by ion Bernstein waves. At the substorm onset (panel b), Alfvén waves Magnetic reconnection has been successful in explaining arrive from the magnetosphere, causing electron the main features of mass, energy and momentum acceleration (via a resonance between waves and transfers from the solar wind into the magnetosphere. A electrons) and possibly also Dot-AKR emission in the key parameter ruling the magnetic reconnection process low-altitude cavity; the Dot-AKR emission is usually and therefore the whole solar wind-magnetosphere short-lived and probably requires strong transient Alfvén coupling is the interplanetary magnetic field (IMF) waves. If Alfvén wave activity lasts for some time, orientation. For southward IMF, reconnection takes place electron acceleration causes some ions to leave the at the low-latitude magnetopause, between the two cusps. sec2.qxd 7/11/05 5:13 PM Page 33

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Figure 2.6.4/1: Statistics of cusp observations from Cluster.

The signature of low-latitude reconnection is a strong anti-sunward convection in the cusp as well as an energy dispersion of ions (higher energies at lower latitudes). For northward IMF, on the other hand, reconnection takes place at higher latitude, poleward of one or both cusps. This drives a sunward convection in the cusp and the ion energy dispersion is then ‘reversed’ (higher energies at higher latitudes). Figure 2.6.4/2: WHISPER spectrograms from An intermediate case appears when the IMF is dominated Cluster 1 (top) to Cluster 4 (bottom) by its Y-component (dawnward or duskward IMF). Then, reconnection is thought to occur simultaneously at high and low latitudes. The discovery of the double cusp and the study of its consequences in the high-latitude ionosphere makes the coupling processes between the plasmasphere, particularly during high magnetic activity. solar wind and the magnetosphere more complicated This emission cuts off suddenly at the plasmapause, the than described above. outer boundary of the plasmasphere. Although the generation of hiss emission is not yet understood, it is Prior to the study of the double cusp, F. Pitout and believed that the decay of radiation belt electrons is C.P. Escoubet performed a statistical study of three significantly controlled by the hiss phenomenon. months of Cluster crossings of the mid-altitude (at 5- 6RE) cusp (Fig. 2.6.4/1). A few morphological features Using Cluster instrumentation (WHISPER, STAFF and of the cusp have been defined and then related to the WBD), an investigation into plasmaspheric hiss was prevailing IMF. The double cusp, which is thought to initiated which established a previously unknown occur when the IMF is dominated by its Y-component, is phenomenon, banded hiss emission (BHE) (Masson et searched for throughout this study. The preliminary study al., 2004). It appears below the electron gyrofrequency, reveals, among others, that textbook cases of cusps with Fce, but above the lower hybrid resonance, from 2 kHz nice ion dispersions do not occur that often. Instead, to 10 kHz. The waves were shown to propagate in the numerous irregular and discontinuous cusps are found, whistler mode. Based on the first year of Cluster among which there are interesting cases of discontinuous observations, the following properties of the BHE waves cusps occurring under stable IMF conditions. The latter were identified: (i) the location is strongly correlated are also good candidates for stable double cusps, which with the position of the plasmapause; (ii) no MLT require further studies. dependence was found; (iii) the spectral width is generally 1-2 kHz; (iv) the central frequency of their emission band varies from 2 kHz to 10 kHz and Banded hiss emissions in the plasmasphere correlates with the Kp index. All these features suggest that BHE is in fact mid-latitude hiss (MLH). The central The inner part of the magnetosphere contains two frequency correlation with Kp, found by this study, is a important regions: radiation belts that contain relativistic new property of MLH. It suggests either that MLH is electrons, and a plasmasphere that contains cold plasma generated in a given f/Fce range, or that there is a Kp- originating from the ionosphere. Plasmaspheric hiss (at dependent Doppler shift between the satellites and a 100-10 000 Hz) is observed throughout the Earth’s possible moving source of the MLH. sec2.qxd 7/11/05 5:13 PM Page 34

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Figure 2.6.4/2 shows an example of MLH as observed by References WHISPER on 2001 October 7, 14:45-18:30 UT. MLH Janhunen, P. et al. (inc. Laakso, H.), 2004, Ann. Geophys. occurs at 16:25-17:04 UT, indicated by white arrows. 22, 2213-2227. MLH is found to intensify with altitude and with time Masson, A. et al., 2004, Ann. Geophys. 22, 2565-2575. (note that the four Cluster satellites fly in a string-of- Sanderson, T.R., Marsden, R., Tranquille, et al., 2003, pearls formation near perigee). Geophys. Res. Lett. 30(19), 8036.

2.6.5 Examples of other associated activities within SCI-SH

In addition to the analysis of Cluster data, the team is also involved in the analysis of magnetospheric data from Double Star. The Double Star TC-1 spacecraft carries an ASPOC instrument that keeps the satellite potential near zero with respect to the ambient plasma. The team, through SCI-A, contributed both hardware and expertise on ion emitter development and in-flight operations to ASPOC. The ion emitter module was improved after experience gained on the Cluster mission. After the successful launch on 29 December 2003, ASPOC is functioning very well with a very good high-voltage ignition and very stable ion current. The PI institute of the instrument is the Space Research Institute in Graz (A).

Moving from the study of the Earth’s magnetosphere through the Cluster and Double Star missions, the research group is now turning its attention to the magnetosphere of Mercury. The team is involved in the challenging (owing to the very high temperature environment) development of an electric field instrument for the BepiColombo/MMO satellite. The team is responsible for the thermal analysis of the overall instrument, which is delegated to SCI-A personnel for implementation. The PI institute of the instrument is the Royal Institute of Technology in Stockholm (S). In addition, the study of ions from the surface of Mercury and their interaction with the planet’s magnetic field will be explored through the group’s involvement in the PICAM ion spectrometer on the BepiColombo MPO (Co-I C.P. Escoubet). Here, the design of the analogue- digital hybrid ASIC electronics together with the MCP detectors is the responsibility of SCI-A in support of the Co-I.

Finally, the SMART-1 satellite carries the SPEDE instrument that monitors the performance of the solar electric propulsion (SEP) engine of the satellite. The Division, together with SCI-A personnel, has been involved in the design and manufacturing of the two booms as well as the testing and calibration of the overall instrument. Measurements have been obtained since early October 2003, and currently the team is working with in-flight calibration issues. The PI institute of the instrument is the Finnish Meteorological Institute in Helsinki. Such experience will be invaluable for the BeppiColombo mission to Mercury, which also will use an SEP motor. sec2.qxd 7/11/05 5:13 PM Page 35

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2.7 Comparative Planetology and Astrobiology

Comparative planetology is an important study area in RSSD, because it is a necessary element in the preparation of ESA’s current and future planetary missions, and it maximises the scientific exploitation of these missions. Studies of the Moon, Mars, Venus, Titan and Mercury provide unique opportunities to improve our understanding of the processes and factors that have shaped our own planet. Mars Express, SMART-1 and BepiColombo have the potential for developing expertise and knowledge in comparative planetology focused on the terrestrial planets. Venus Express, to be launched in 2005, offers similar opportunities, in particularly for climatology. Huygens will provide detailed information on one of the most mysterious objects in the Solar System, Saturn’s moon Titan.

2.7.1 Mars research

Geologic evolution of the Martian surface

Gusev Crater is the landing site of one of the NASA Mars Exploration Rovers (MERs). During the early commissioning period of Mars Express, the HRSC took a number of images over the Gusev area. The study of this area, including the neighbouring highlands to the south and lowlands to the north, has been the subject of a stagiaire project. Data from Mars Global Surveyor, Mars Odyssey and the recent Mars Express image and altimetry data have all been used to produce a geological map and geological profiles of the region (Fig. 2.7.1/1). The basis for these geological profiles was provided by Figure 2.7.1/1: Geological map of the Gusev crater on HRSC digital elevation models (DEMs) derived from the Mars. The landing site of Spirit, one of the MER HRSC stereo images. The resolution of these DEMs is landers, is also shown. The map distinguishes various better than the available MOLA altimetry data (better rock units and is based on both image data and than 200 m for HRSC, compared to 600 m horizontal topography data from HRSC on Mars Express. resolution for MOLA). Geological mapping of the surface combined with geometrical analysis of the geological profiles make it possible to determine the stratigraphic sequence, including estimates of the thickness of the various units. This provides a much — characterisation of surface morphology and textures enhanced insight into the geological evolution of this at high/super resolution; terrain. Some of the main issues are: (1) a relative — characteristics of present and future landing sites. stratigraphic sequence of 16 units, including sediments and volcanic rocks; (2) mapping of tilted Noachian HRSC has obtained new evidence for geological activity terrains, indicating a dynamic early history of Mars; on Mars. Calderas on five major volcanoes in the Tharsis (3) correlation of two potential sedimentary units in the and Elysium regions have undergone repeated activation Gusev crater. and resurfacing during the last 20% of Martian history. Caldera floors as young as 100 Ma and flank eruptions as In addition, HRSC data have been used to study the young as 2 Ma have been found. These results confirm evolution of the Martian surface through time and that the volcanic edifices are characterised by episodic geological processes. Specific issues being addressed by phases of activity and suggest that volcanoes are HRSC Co-I B. Foing and collaborators are: potentially still active today.

— role of water and volatiles; HRSC images have provided convincing evidence of a — impact craters processes; current frozen body of water, with surface pack-ice, — evolution of volcanism and hydrothermal activity; around 5°N/150°E in southern Elysium (Murray et al., sec2.qxd 7/11/05 5:13 PM Page 36

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2005). The study of tropical to mid-latitude glaciation on The research team (B. Foing, D. Koschny, M. Almeida et Mars shows evidence of snow and ice accumulation and al.) is therefore actively involved in SMART-1, specific- flow in Mars Express HRSC data (Head et al., 2005). ally with the AMIE imaging and the D-CIXS X-ray Finally, very young volcanic and glacial activity at spectrometer teams. In particular, a new technique has Hecates Tholus has been discovered in HRSC images. been developed for remote sensing determination of lunar surface composition based on AMIE data. The In preparation for future missions to Mars involving a approach is based on spectral and composition data potential lander, Mutual Impedance Probes have been derived from a Lunar Soil Characterization Consortium built for atmospheric and surface investigations for a few, particle-size, separates of lunar soils, mapping (Huygens, Philae). The measurement of the electric the abundance of TiO2 and FeO, pyroxene content, properties of surface and subsurface materials is an maturity degree (Is/FeO), and a characteristic size of important issue for planetary missions. A prototype of a particles (Shkuratov et al., 2003). subsurface MIP has been developed, which will allow the measurement of the profiles of the electrical conductivity and permittivity along the path of a drill or mole, and 2.7.3 Cassini-Huygens data analysis preparation generate 2-D images of the electrical properties of materials along the walls of the borehole. The environ- Preparations for the arrival of Huygens at Titan: mental parameters and requirements for applications on Huygens radar tests Mars have been analysed. This will allow the investiga- tion of otherwise invisible subsurface structures, and the The main objective of the Huygens Radar Altimeter is detection and localisation of subsurface water deposits. the determination of the Probe altitude, which is very important for an optimised operation of the payload. In order to assess the performance of the radar at high Study of the upper Mars atmosphere altitudes, and verify the characteristics for concurrent operation of both radars, the research team supported a The research team is also closely involved in the study of series of radar tests on the ground and aboard the Martian atmosphere. Specifically, the UV stratospheric balloons (HASI Sicily flight June 2003, sky spectrometer SPICAM aboard Mars Express is test; PEASMA balloon flight November 2004). The radar performing a number of different scientific observations, signal reflected by Titan’s surface contains important including limb measurement. These observations aim at information about surface properties such as roughness studying the airglow (natural emission) of the upper and electrical parameters. The signal is processed via the atmosphere. From such data, information can be deduced PWA experiment, which is part of HASI. In addition to on the composition and thermal structure of the coupled verifying the altimeter performance, the balloon cam- neutral atmosphere/ionosphere, on both the dayside and paigns provided valuable datasets for the development the nightside, and on the interaction with the solar wind. and test of data analysis software, which will be used for SPICAM has provided the first spectra of the upper processing the radar data returned by Huygens in 2005. atmosphere since Mariner-9 in the 1970s. A number of limb data spectra are being analysed in detail and show + emissions of O, CO, CO2. A model of the ionosphere Preparations for the arrival of Huygens at Titan: the (Morel et al., 2004; Witasse et al., 2003) is being updated HASI-PWA experiment in order to model the lines and bands detected by SPICAM. The PWA experiment will explore the atmosphere of Titan during the Probe’s descent. It will measure the electric field (AC, Schumann resonances and lightning), 2.7.2 Lunar studies the atmospheric conductivity (Relaxation Probe and Mutual Impedance Probe), pressure variations (Acoustic The Moon bears the scars of countless impact craters, Experiment) and signals returned from the surface of and holds the only accessible record of the conditions in Titan by the Huygens Radar Altimeter. The preparations the Earth-Moon system over the past 4.5 billion years. for the processing and analysis of Huygens data are The recent Clementine and Lunar Prospector missions progressing in cooperation with partner institutes in provided the first views of global geochemistry. The Austria (IWF), France (CETP) and Spain (IAA). Final SMART-1 mission will add the first global IR dataset and hardware tests have been conducted in order to finalise the first global measurements using X-ray fluorescence, the calibration and validate various models required for which will map elemental Mg, olivine and pyroxenes data calibration. across the surface. These are critical to understanding the Moon’s crustal evolution and origin, which is intrin- A recent series of tests was designed to investigate the sically linked to the early evolution of the Earth, as well impact of the Huygens probe attitude on the measure- as other geological process in the Solar System, such as ment of electric fields (Fig. 2.7.3/1). Preparations at volcanism, tectonics, impact cratering and volatiles. ESTEC include logistics, finalising the calibration sec2.qxd 7/11/05 5:13 PM Page 37

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2.7.4 Ground-based observation of Titan winds

The study of winds on Titan is a scientific objective of the Cassini/Huygens mission. Earth-based observations are attempting to provide complementary information. All Earth-based techniques employ various implement- ations of the Doppler measurement technique. The technique used here, however, is based on the absolute accelerometry method developed for the detection of extrasolar planets. The reflected solar spectrum from a rotating body (in Titan’s case, its atmosphere) observed by a high-resolution spectrometer was analysed. The rotating atmosphere induces a Doppler shift in the whole spectrum. Observations of Titan were performed in 2001-2002, with the UVES spectrometer mounted on the ESO VLT. However, the data reduction, analysis and interpretation using the UVES pipeline data processing tools have led to results difficult to interpret. As a result, the approach was verified by applying the method to a Figure 2.7.3/1: Huygens balloon model in the electric rotating body with no atmosphere: Io. In that case, the field test chamber at Padua University, Italy. method consists of retrieving the surface rotation velocity, which is well known. Four observations of Io performed in early 2003 were analysed, yielding a rotation rate with an uncertainty < 2 m/s (Civeit et al., 2005). With the improved pipeline processing the software and preparing for the initial data analysis during method is being applied to analyse the observations of the Huygens arrival event. Titan, plus some recent observations of Saturn.

Reconstruction of the Huygens trajectory 2.7.5 Earth comparative planetology

The Huygens Project Scientist Team supported the Impact cratering studies scientific activities of the Descent Trajectory Working Group (DTWG). This group was created to ensure an Impact craters are the most common geological feature in orderly and efficient analysis, interpretation and delivery the Solar System. All of the planets have been struck by of the Cassini/Huygens engineering and instrument data countless asteroids, comets and meteoroids since its necessary for reconstructing the the Huygens probe entry formation 4.6 billion years ago. Impact craters thus and descent trajectory. One of the major activities of the represent a fundamental field of research in planetary group was the implementation and testing of a numerical studies. The emerging view of planets as geological tool that can reconstruct the trajectory. In this context, the objects makes the search for previously unknown impact Project Scientist Team built a synthetic dataset of the craters on Earth a fundamental element of planetary mission in order to test the algorithm. The philosophy of exploration. Various potential methods for the automated the approach, the assumptions made and the limitations recognition of impact craters from remote sensing data of the method are described in Perez-Ayucar et al. have been considered. As a result of the study, an (2004). algorithm based on the Hough transform was selected, implemented and demonstrated to be effective in identifying known craters from sample images of the Study of the upper atmosphere of Titan Earth, Mars and the Moon. The study also showed that the detection of new unknown impact craters requires the The upper atmosphere of Titan has been investigated by exploitation and fusion of data from multiple remote the Cassini Orbiter through two dedicated studies of the sensing missions and sensors, and therefore the ionosphere. The first is related to the ion production due development of more sophisticated recognition to electron impact (Lilensten et al., 2005a). The second algorithms. Envisat data are being exploited in the concerns the modelling of a doubly charged ion layer that framework of this work, to be followed by potential could be detected by the UVIS instrument (Lilensten et fieldwork of a few examples of identified structures. Of al., 2005b). This paper is the last of a series of three course, such an approach can also be applied to Mars studies on comparative planetology devoted to the craters and in particular Mars crater synthetic studies doubly-charged ions in planetary atmospheres (Mars: using coordinate registration by automated crater Witasse et al., 2003; Earth: Simon et al., submitted). recognition. sec2.qxd 7/11/05 5:13 PM Page 38

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Geological expedition to Pilbara terrain (Australia) Small Magellanic Clouds (LMC and SMC) offer a unique opportunity to link DIB behaviour to widely The Pilbara terrain in Western Australia is one of the varying environmental conditions (e.g. metallicity, UV planet’s oldest terrains – up to 3.5 billion years old. radiation field and star-formation activity). To this end, Because of its unique record of early life and conditions the absorption spectra of reddened OB stars in the on Earth, it is the focus of an international research effort Magellanic Clouds have been observed at unprecedented organised by the NASA Institute of Astrobiology. A field high resolution (R = 100 000) and high S/N with expedition to the Pilbara terrain was organised in August VLT/UVES. Analysis of the spectra of the LMC and 2004 to collect rock samples for three projects: SMC targets indicates that a delicate balance must exist for DIBs to be present. Noteworthy in this respect is the — spectral analysis of Archean volcanic rocks as 30 Doradus region in the LMC, where these special potential analogues for Martian geological units. conditions seem to prevail. Of all the LMC stars This project is in collaboration with the Geological observed, only the two in the 30 Dor region have Survey of Western Australia, CSIRO (Australia) and detectable DIBs. This balance appears to be strongly Technical University of Delft, ITC (Enschede, NL); dependent on the UV radiation field, which is — study of the early Earth magnetic field. The represented by the shape of the extinction curve (i.e. the behaviour of the Earth’s early magnetic field is presence of the 2200 Å bump and the steepness of the related to the formation of the inner core. Numerical far-UV rise). models of the geodynamo predict a weaker magnetic field at times prior to the formation of the solid inner The strongest diffuse interstellar bands ever were core. So far, no record of the early geomagnetic field measured using the VLT/UVES in the heavily reddened has been found. Granitic rocks in the Pilbara granite- line of sight towards the high-mass X-ray binary greenstone terrain have been sampled for isotopic 4U1907 +09. More than 180 DIBS could be detected in dating and paleomagnetic analysis to determine if this source. The relation between the DIB carriers, and such an early record is preserved in this terrain. This other species such as neutral hydrogen and K, could be project is in collaboration with MIT and Caltech, studied. where the measurements will be done; — sampling of units that possibly formed as a result of An astronomical search coupled to laboratory meteorite impacts. A 5 m-thick spherule layer was spectroscopy was conducted for C84: a prototype of discovered in the Coongan Greenstone Belt. large fullerenes. For the first time, a UV/Vis spectrum of a neutral and ionised fullerene (C84 isolated in Ne matrix) was obtained. It shows absorption bands that 2.7.6 Astrobiology have been compared to the optical DIB spectrum.

Large organics in space Finally, the ORGANICS experiment on Foton/Biopan has been prepared to study effects of UV and particle Spectroscopy of large PAHs, including laboratory studies radiation on selected PAHs and fullerenes, in order to and comparison with the Diffuse Interstellar Bands better constrain the destruction pathways of large organic (DIBs) have been performed by Foing and collaborators. molecules in interplanetary and interstellar environ- For the first time, laboratory spectroscopy of the UV-Vis- ments. NIR absorption spectra were obtained for a represent- ative set of large PAHs that have been selected for long- duration exposure experiment aboard the International Complex organics on Mars Space Station and Foton/Biopan. The PAH charge distribution and DIB carriers ware also studied. Physical The behaviour of organic compounds in a simulated parameters such as density, ionisation and temperature, Mars environment is under study. Viking Lander biology constrained by observed atoms and molecules, have been and molecular analysis experiments were re-analysed computed for the line of sight towards a single cloud and possible reasons why no organic compounds could towards HD 147889. It has been established that be clearly detected were identified (Ten Kate et al., different wavelength regions in the DIB spectrum 2003). The search for organic molecules and traces of life correspond to different charge states depending in the on Mars has been a major topic of planetary science for size distribution. The contribution of catacondensed several decades. The search for extinct or extant life is PAHs to the strong UV 200-300 nm absorption and to the the future perspective for several missions. A set of DIBs is constrained (Ruiterkamp et al., 2005). organic molecules has been selected for simulation experiments. Laboratory experiments under simulated The study of DIBs’ weak unidentified interstellar Mars conditions are performed in order to determine absorption bands observed towards reddened stars has what those missions should be looking for. This research continued. Their carriers are believed to be large has been developed as part of a Mars Express carbonaceous molecules (e.g. PAHs). The Large and Recognised Cooperating Laboratory (RCL). sec2.qxd 7/11/05 5:13 PM Page 39

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The Mars simulation chamber has been used to study thin 2.8 Minor Bodies layers of glycine exposed to low ambient pressures and UV lighting conditions similar to those on Mars. Scaling The Minor Bodies research group explores the physical times for sample alteration were determined for these and chemical properties of some of the oldest objects in Mars-like conditions. A sequence of Mars chamber the Solar System with a view to understanding how it studies is dealing with the Martian survival properties of was formed and providing insight into the formation and ice covered by or mixed with dust. This should provide evolution of extrasolar systems. Both topics are key an understanding of the remnants of glacier and ice aspects of current and future activities in the Agency’s deposits during the Mars obliquity cycles, as observed by science programme through such missions as Rosetta and Mars Express/HRSC. Darwin. To this end, the research group uses a variety of tools, spanning the development of key instruments and References observations from ground- and space-based observa- Civeit, T. et al., 2005, A&A 431, 1157. tories, both underpinned by a theoretical- and modelling- Cox, N. et al., 2004, A&A, submitted. based programme. Head, J. et al., 2005, Nature 434, 346. Lilensten, J. et al., 2005a, Icarus 174, 285. Lilensten, J. et al., 2005b, GRL 32(3). 2.8.1 The MIDAS instrument on the Rosetta Morel, L. et al., 2004, PSS 52, 603. mission Murray, J. et al., 2005, Nature 434, 352. Perez-Ayucar, M. et al., 2004, ESA SP-544. The MIDAS Atomic Force Microscope onboard the Ruiterkamp, R. et al., 2005, A&A 432, 515. Rosetta Orbiter was developed in collaboration with Shkuratov, Y. et al., 2003, Sol. Sys. Rev. 37, 251. IWF, Graz (A). This instrument will collect, image and Simon, C. et al., 2004, submitted. characterise the geometry of dust particles when in orbit Ten Kate, I. et al., 2003, LPI 1, 1313. around Comet 67P/Churyumov-Gerasimenko. Among Witasse, O. et al., 2003, GRL 30, 12. the key scientific goals is the 3-D characterisation of cometary dust with a resolution of better than 10 nm and the determination of dust flux variation and statistics of particles in the size range 10 nm to 5 µm. The AFM will study the morphology of dust grains around a comet in situ rather than requiring a far more expensive sampling and return mission.

After many years of development, manufacturing, integration and testing, the long-awaited successful launch of Rosetta came in March 2004. Since then, MIDAS has undergone its initial deployment and has been checked out in the majority of its operational modes. The instrument carries samples that allow a complicated but high-resolution in-flight calibration. The imaging conditions and parameters during the early commissioning phase are identical to those during the final orbit around Comet Churyumov-Gerasimenko. The data show that MIDAS is fully operational and its performance not only fulfils, but exceeds, the scientific requirements. Fig 2.8.1/1 shows an image of a calibration sample taken during flight. Repeated imaging on the same location confirms a reproducibility of the absolute dimensions of the sample in the range of a few nm. This result confirms the excellent mechanical performance of the instrument as well as the favourable imaging conditions aboard Rosetta. If all goes well with the instrument and the mission as it journeys to the comet, we shall for the first time be able to study the morphology of dust grains at the nm level from one of the early primitive bodies of the Solar System.

The interpretation of flight data and further optimisation of instrument operational parameters are supported by an intensive measurement programme using the flight spare sec2.qxd 7/11/05 5:13 PM Page 40

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Figure 2.8.2/1: A part of the CN R branch of the average reduced spectrum of comet C/2000 WM1 (LINEAR) compared with the synthetic spectrum. Top panel: synthetic spectrum (thick line) contains only 12C14N. Bottom panel: the synthetic spectrum also contains 13C14N and 12C15N, which result in an almost perfect fit to the observed spectrum.

Figure 2.8.1/1: The MIDAS flight instrument shortly Solar System. From the ground, such isotopic ratios can before integration on the spacecraft. Below: the first in principle be determined by high-resolution image taken in space during Rosetta’s commissioning spectroscopy (R ≥ 700 000) of the resonance- phase shows the cubed structure of an onboard fluorescence bands of certain simple molecules calibration sample. The 3-D view is rendered from containing the relevant element. In the case of the 12C/13C raw data. ratio, this has been done over the past two decades for a few bright comets, whereby the observed molecules were usually CN and C2, trace gas species typically present in cometary comae.

model installed in a vacuum chamber within the SCI-A The analysis of high-resolution spectra of comet C/1995 laboratories. This model is used as a testbed for new in- Q1 (Hale-Bopp) and C/2000 WM1 (LINEAR) resulted in flight procedures as well as a tool for the scientific the optical detection of 12C15N, which permitted the interpretation of the flight data from the comet. For this 14N/15N ratio in CN to be derived for the first time. The purpose, a large number of specific samples that 14N/15N ratios were determined to be 140±35 and 140±30, resemble different physical and chemical properties of respectively, which is significantly lower than the value cometary dust were installed. Data and experience in Earth’s atmosphere, usually referred to as the Solar gained during future studies will be collected and System value of 272 (Arpigny et al., 2003a; b). inserted into a database. This includes the growing knowledge of cometary materials from other space It should be noted that, over the past 2 years, the 12C/13C missions. The PI-team supported by the RSSD Co-I and 14N/15N isotopic ratios were determined in the CN activity should be well-prepared to face the rigours of the coma of 12 comets of different dynamical histories encounter in order to exploit and maximise the return (Jehin et al., 2004a). For all the comets studied so far, the from this novel instrument. 12C/13C ratio is consistent with the Solar System value of 89, whereas the 14N/15N ratio is only half the Solar System value. The results for two periodic comets have been 2.8.2 Determination of isotopic ratios in comets published (Jehin et al., 2004b).

Isotopic ratios of the light elements in comets are Although remarkably similar values have been derived important clues to the origin and early history of the for the 14N/15N ratios in the CN coma of the different sec2.qxd 7/11/05 5:13 PM Page 41

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comets, this ratio is much lower than the ratio derived for vations on 11 February 2003, post-perihelion character- HCN from sub-mm measurements in comet Hale-Bopp isation of this comet is now available, covering its (323±46). HCN was generally believed to be the main evolution along the orbit between 2.29 AU and 3.22 AU. parent of CN. However, the observations of Hale-Bopp Broadband BVRI images and low-resolution long-slit indicate a discrepancy between the nitrogen isotopic spectra have been obtained for morphological, colour ratios in CN and HCN, which would suggest that here is and compositional analysis of the coma and for studying at least one additional, unknown parent of CN, with even the comet’s activity along its orbit (Fig. 2.8.3/1). Various higher 15N excess. Organic compounds like those found observational techniques have been used to collect data in interplanetary dust particles are good candidates for the analysis of long-term and short-term variability, (Aléon et al., 2003). These new findings are under from which conclusions on several nucleus properties detailed evaluation and sub-mm measurements have can be drawn (Schulz et al., 2004a, and references been initiated to retrieve the nitrogen isotopic ratio in therein). comets from HCN.

Water production rates from SOHO/SWAN observations 2.8.3 Characterisation of the new Rosetta target comet Since January 1996, the SOHO/SWAN instrument has been producing full-sky Lyman-alpha maps. The SWAN Post-perihelion monitoring in 2003 images can be used to study the hydrogen coma of comets down to a visual magnitude of ~12. After the A new target comet was identified for the Rosetta retargeting decision of the Rosetta mission, the SWAN mission after its launch to Comet 46P/Wirtanen, planned archive was searched for possible occurrences of for mid-January 2003, was cancelled. As soon as 67P/Churyumov-Gerasimenko. The comet was identified 67P/Churyumov-Gerasimenko became a likely new in Lyman-alpha images obtained during its 1996 target based on its classification and orbital parameters, apparition, and five values for the production rate of extensive monitoring of this comet began to determine a neutral hydrogen were obtained. As cometary neutral number of basic properties. Starting with the first obser- hydrogen comes predominantly from photodissociation of water, SWAN observations can be used to estimate the water production rate of a comet. The observations suggest a perihelion water production rate of about

Figure 2.8.3/1: Structurally enhanced broadband R images showing the evolution of the distinct features in the coma of Comet 67P/Churyumov-Gerasimenko between February and June 2003. The direction of the Figure 2.8.3/2: Colour-coded nucleus bulk density Sun and the comet velocity vector are indicated. (kg/m3) as a function of the spin axis obliquity, I, and MIDAS/AFM will provide the morphology of the argument Φ. Black areas: prolate ellipsoidal model associated dust grains when orbit about the comet is nuclei cannot reproduce the observed light curve achieved in 2014. amplitude. Dots: observed water production rates are most closely reproduced. Solid-line areas: empirical change in the longitude of perihelion is reproduced. Dashed-line areas: empirical change in the longitude of the ascending node is reproduced. sec2.qxd 7/11/05 5:13 PM Page 42

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8x1027 s–1 and a possible post perihelion increase of activity (Mäkinen, 2004a).

Nucleus properties estimated from non-gravitational force modelling

The nucleus size, shape, active area fraction, spin axis orientation, mass and bulk density of Comet 67P/Churyumov-Gerasimenko have been estimated using a sophisticated thermo-physical nucleus model. The model has to reproduce simultaneously the empirical nucleus light curve, water production rate versus time, and non-gravitational changes of the orbital period, longitude of perihelion, and longitude of the ascending Figure 2.8.4/1: A slice through an irregular body node (per apparition). The results suggest that the spin (outlined with solid grey at intersection surfaces) at axis argument is close to either 60° (obliquity 100-140°) 1 AU, depicting outgassing water molecule density. or 240° (obliquity 40-90°). Hence, the nucleus semi-axes The Sun is to the right. are likely to be roughly 2.5x1.9 km. The nucleus bulk density is at most 500 kg/m3 and the active area fraction is 4-11% (Fig. 2.8.3/2). If substantial deviations between observed and calculated water production rates are allowed (to account for uncertainties in the modelling five dust colours to five dust characteristics (power index and observational errors), the spin axis orientation and of the size distribution, the smallest and largest particle nucleus dimensions cannot be estimated, but a hard sizes, scattering efficiency averaged over the size range, upper limit on the nucleus bulk density of 600 kg/m3 can and albedo ratio for the smallest and largest particles) be determined (Davidson & Gutiérrez, 2004). was applied to spectrophotometric observations of comet C/1995 O1 (Hale-Bopp). The calculated solution demonstrates how physical characteristics of comet dust 2.8.4 Comet modelling change with the distance from the nucleus and how they vary for different dates of observations. The power of the As a part of a project to study the cometary particle size distribution was found to exceed values found for environment, the research team has built a complex other comets and is quantitative evidence for the particle simulator capable of producing fractal aggre- overabundance of small particles in Comet Hale-Bopp gates through collisional coagulation, and simulating (Kolokolova et al., 2003). their evolution and dynamics in a cometary coma after being expelled from the nucleus (Makinen, 2004b). This self-consistent ballistic rigid-body particle colliding 2.8.5 Ground-based observations of comets simulator can be used to study the physical properties of cometary particles, the particle environment of a comet, Comet 81P/Wild 2 and even the dynamics of a meteor in Earth’s atmos- phere. It is capable of producing fractal aggregates of icy The pre-perihelion monitoring of the coma morphology particles modelled by hard or soft (metaball) spheres, to of Comet 81P/Wild 2 revealed the presence of long- be used for creating test particles in future statistical lasting fan structures, which remained essentially studies of the cometary coma-particle interaction unchanged for at least 3 months. The compositional (Fig. 2.8.4/1). Instead of a predefined sticking probabil- coma analysis confirmed the depleted abundance of C2 ity, actual surface interactions are modelled and a method with regard to CN in this comet. The results of the for calculating internal stresses and fragmentation of an observations led to the prediction that distinct coma aggregate is described. Simulations suggest that taking features were likely to be present at the time of the fragmentation into account has two major consequences: Stardust flyby (Schulz et al., 2003); such features were increase in the fractal dimension of particles, and a indeed detected by that spacecraft. noticeable change in the mass spectrum of an ensemble.

The work continued on extracting the size distribution of Comet C/2000 WM1 (LINEAR) dust particles by using measurements of the scattered light at a number of wavelengths. The method is based on The gas and dust coma of comet C/2000 WM1 have been general light-scattering properties of particles with a characterised from the analysis of optical imaging and power-law size distribution and places no limitation on long-slit spectroscopy. The gas coma showed a double jet particle shape or structure. A set of equations that relates structure in CN and C2, which has no counterparts in the sec2.qxd 7/11/05 5:13 PM Page 43

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dust. The gas production rates, dust colour and particle 2.9 Fundamental Physics distribution in the coma have been investigated (Lara et al., 2004). Near-IR observations led to the discovery of Research in Fundamental Physics is concentrated on two sublimating components in the coma, which possibly supporting the LISA Pathfinder and LISA missions, originate from different kinds of organic material (Tozzi particularly in the area of high-precision phase measure- et al., 2004). ments and interferometry.

References The LISA Pathfinder spacecraft will carry the European Aléon, J. et al. (inc. Schulz, R.), 2003, Lunar and LISA Technology Package (LTP) and a similar US- Planetary Science 34. provided package (ST7). Both packages consist of two Arpigny, C. et al. (inc. Schulz, R.), 2003a, Science 301, free-floating test masses, each in capacitive sensor cages 1522. (‘gravitational reference sensors’), which are the heart of Arpigny, C., et al. (inc. Schulz, R.), 2003b, BAAS 35(4), the drag-free control and an essential part of the LISA 986. mission. The purpose of both packages is to test a variety Davidson, B.J.R., Gutiérez, P.J., 2004, BAAS, in press. of operational modes of the gravitational reference Jehin, E. et al. (inc. Schulz, R.), 2004a, presentation at sensors together with their associated µN-thrusters and 35th COSPAR. drag-free loops, and to verify their performance and Jehin, E. et al. (inc. Schulz, R.), 2004b, ApJ 613, L161. noise behaviour. Kolokolova, L. et al. (inc. Schulz, R.), 2003, J. Quanti- tative Spectroscopy & Radiative Transfer 79-80, 861. Lara, L.M. et al. (inc. Schulz, R.), 2004, A&A 422, 717. 2.9.1 Interferometer design for LISA Pathfinder Mäkinen, J.T.T. in The New Rosetta Targets, 2004a, Kluwer, The Netherlands. The LTP interferometer is the diagnostic tool used to Mäkinen, J.T.T., 2004b, Particle Accretion and Dissipa- monitor the test masses in all operating modes tion Simulator. I. Collisional Aggregation of Icy continuously by measuring the distance between the two Particles, submitted to Icarus. test masses, the position of one test mass with respect to Schulz, R., 2003a, Highlights of Astronomy, IAU, 13. the optical bench, the differential alignment of the two Schulz, R., 2003b, BAAS 35(4), 970. test masses (with two sets of measurements: DC and Schulz, R., 2004, CNES Magazine No. 21. differential wavefront sensing), and the alignment of one Schulz, R. et al., 2003, A&A 398, 345 test mass with respect to the optical bench. Schulz, R. et al., 2004a, in The New Rosetta Targets, Kluwer, The Netherlands, 15-24. In the LTP, three heterodyne interferometers obtain these Schulz, R. et al., 2004b, A&A 422, L19-L21. measurements, two to measure the distance and the Tozzi, G.P. et al. (inc. Schulz, R.), 2004, A&A 424, 325. alignment of the two test masses with respect to each other and with respect to the optical bench, and one interferometer to provide a reference signal (Fig. 2.9.1).

2.9.2 A phasemeter for LISA Pathfinder

To evaluate the change in optical path length, precise determination of the phase of the heterodyne signal (typically a few kHz) is needed. The implementation of the phasemeter chosen for LTP is based on digitising the datastream with a sufficiently high sampling rate (about 100 kHz). It obtains the in-phase and out-of-phase components of blocks of input data with respect to a reference signal derived from the nominal heterodyne frequency. These components are then used to calculate the phase of the interferometric signal with respect to the reference signal. Data output occurs with a rate of 10 Hz.

A laboratory prototype of this phasemeter (Fig. 2.9.2/1) has been employed successfully at the University of Hannover (D), with the active involvement of the RSSD reseach team, to measure the performance initially of a breadboard prototype of the LTP interferometer (Heinzel et al., 2004). The phasemeter, at that point still realised in software on a standard PC, was used during the test sec2.qxd 7/11/05 5:13 PM Page 44

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Figure 2.9.1/1: The Engineering Model of the LTP optical bench.

campaign of the Optical Bench EM for LTP to demonstrate the compliance of the EM. In a later stage, a full LTP phasemeter, with 12 channels, 16-bit A/D converters, and the software implemented in an FPGA has been realised.

Differential wavefront sensing

As LTP will use quadrant photodiodes (QPDs) for the sensing of all the interferometric signals, it is possible to obtain information regarding the alignment of the test masses by comparing the relative phase of the heterodyne signals coming from the four different quadrants of the QPD.

During the test campaign for the optical bench EM, an accuracy of better than 10 nrad/√Hz in the frequency range relevant for LTP was achieved using this Figure 2.9.1/2: Layout of the LTP optical bench. technique.

Figure 2.9.2/1: Schematics of the LTP phasemeter. sec2.qxd 7/11/05 5:13 PM Page 45

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2.9.3 Frequency stabilisation for LISA 2.10 Research Activities in SCI-A

One of the most critical issues for LISA is the need for a The Science Payloads and Advanced Concepts Office laser that is stable enough in frequency to allow the performs research focused almost exclusively on the detection of gravitational waves. All of the current needs of future ESA science missions, and specifically strategies to achieve the required stability rely on a on advanced payload technologies. Such technologies combination of pre-stabilisation and numerical post- are underpinned through a long-term coordinated processing of the data. material science and micro-electronics programme involving: A particularly promising approach for a laser frequency stabilisation is a control system in which the instant- — materials for advanced superconducting sensors; aneous laser frequency is compared to the laser — novel semiconductor sensor materials; frequency; a round-trip time of about 33 s. Owing to the — materials for low-resource optics; long intrinsic delay, the ensuing control loop is non- — application-specific integrated circuits (ASICs). trivial in design, and transients and the damping of the initial conditions become important issues. García et al. (2005) have successfully demonstrated the feasibility of 2.10.1 Development of superconducting cameras the stabilisation scheme, replacing the 5 million km LISA arm by a 300 m delay line and the laser with a The superconducting sensor programme is one of the voltage-controlled crystal oscillator. They were able to longer-term advanced sensor development programmes demonstrate a noise suppression of about 40 dB up to the focusing on applications from the near-IR to the soft frequencies comparable to the inverse delay. The initial X-ray band. It has considerable heritage and combines conditions on closing the control loop, i.e. the change of basic research on the properties of novel superconducting the laser frequency during one round-trip time, were thin films with direct and immediate applications of more predicted to be critical for the performance of the traditional superconducting materials. Developments of stabilisation scheme. García et al. showed that the practical sensors are aided by proof testing on the ground influence of the initial conditions could be minimised by on astronomical telescopes, which provides RSSD and a suitable time-dependence of the control loop’s gain community astronomers with the latest astronomy when closing the loop. instruments.

References A considerable effort by SCI-AI in the Superconducting García, A. et al., 2005, Class. Quantum Grav. 22(10), Tunnel Junction (STJ) development programme was S235-S242. focused on completing the next-generation optical Heinzel, G. et al., 2004, Class. Quantum Grav. 21(5), spectrophotometer, S-Cam3, for its first observation run S581-S587. in July 2004. This system is capable of measuring individual optical photon energy, position (imaging) and arrival time (to ~1 µs). The improvements of the new system over its S-Cam2 predecessor can be summarised as:

— FOV increase from 4x4 arcsec to 11x9 arcsec. This has major system-level implications as well as bringing the S-Cam instrument closer to an astronomical instrument with wider applications; — optimised IR rejection filters, while extending the ‘red’ response; — increased energy resolution; — increased electronics readout speed and hence the system’s photon rate capability; — improved data-acquisition software robustness.

The first objective was met by a redesign of the detector. The S-Cam3 detector is an array of 10x12 pixels, each 33x33 µm with 4 µm inter-pixel gaps. The increased pixel size corresponds to ~0.8x0.8 arcsec on the sky. The combined effect of a significant increase in pixel number and slightly larger pixel size ensures uncompromised photometry on point sources, even under poor seeing conditions, and a more accurate background subtraction. sec2.qxd 7/11/05 5:13 PM Page 46

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Figure 2.10.1/2: Comparison of the overall detection efficiency of S-Cam2 and S-Cam3. Future S-Cams are intended to develop the read response beyond 1 µm.

Figure 2.10.1/1: The S-Cam3 array of 10x12 pixels each of 33x33 µm. Note the large amount of wiring required to connect yet isolate individual pixels Figure 2.10.1/2 is a comparison of the total efficiency of electrically. S-Cam3 versus S-Cam2. These curves take into account the measured transmissions of all optical elements as well as the detector’s efficiency. The peak efficiency has increased from ~22% in S-Cam2 to ~30% in S-Cam3. The bandwidth (at 10% of maximum) has also increased Also, simultaneous imaging of more than one object from 335-690 nm to 330-745 nm. With the combined becomes possible, which is useful when observing effect of reduced IR load and higher detector extremely weak objects. Fig. 2.10.1/1 shows a responsivity, we have been able to measure a photon micrograph of the S-Cam3 array and highlights the wavelength resolving power R = 13 at 500 nm, up from complex photolithography involved in this technology. R = 8 in S-Cam2.

The layup of the detectors is identical to the S-Cam2 The electronic readout system for S-Cam3 was arrays: 100 nm Ta with 30 nm Al trapping layers on completely redesigned. It allows in situ verification of each side of a very uniform and thin oxide layer. The each individual pixel by means of I-V curve tracing. best arrays show 100% pixel yield: all 120 pixels are Furthermore, the preamplifier signals are immediately low-leakage STJs with typical leakage currents of converted to the digital domain at up to 40 MHz ~30 pA. The responsivity (defined as the total collected sampling rates. A Finite Impulse Response filter is charge in electrons per eV of incident photon energy) implemented for each channel in FPGAs, which can be for the selected array is slightly increased from reprogrammed ‘on the fly’. This allows an optimisation ~15000 e–/eV in S-Cam2 to ~18000 e–/eV in the current of the filter algorithm for either higher energy resolving devices. power or higher speed. After event detection, the data stream is split in two. One is logged on a RAID system For these kinds of detectors, the rejection of thermal-IR for off-line post-processing, while the other will be photons is of crucial importance. The low energy gap of processed in the programmable hardware for quick-look Ta/Al STJs makes them sensitive to wavelengths up to purposes. In this way, light curves and spectra are ~1 mm. Since the detector is optically coupled to a 300K displayed in real-time and updated every second without environment, the IR-rejection filters have very tight compromising raw data logging or running the risk of requirements. Simple calculations of attenuation factors system failure due to computing or data-stream bottle- in the vicinity of the peak of the 300K blackbody necks. Maximum count rates are > 8000 counts/s/pixel radiation could not, however, explain the excess in sub- and > 500 000 counts/s over the whole array. With such gap current measured in S-Cam2. It was therefore a capability, astronomers now have an additional tool concluded that we were suffering from residual very with which to investigate very high-speed phenomena in long-wavelength radiation. In order to optimise the a wide range of objects. suppression of the longer wavelengths, while simultaneously improving the throughput in the visible, In order to cool the detector to its operating temperature the filter glasses were changed and an additional filter of ~0.3K, a dewar in combination with sorption coolers was added at 300mK. This, in combination with was used. This dewar can contain ~12 litres of liquid improved baffling and shielding, reduced the IR load per helium. Contrary to S-Cam2, S-Cam3 uses a hybrid unit detector area by more than an order of magnitude. 4He–3He sorption cooler combination. The hold time at sec2.qxd 7/11/05 5:13 PM Page 47

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Figure 2.10.1/4: Processed S-Cam3 image of a 16th magnitude star showing the effect of differential atmospheric refraction. With its intrinsic ability to detect and measure the colour of every single photon with a time resolution of below 1 µs, a wide range of astronomical applications can be envisaged for this technology.

Figure 2.10.1/3: S-Cam 3 cryostat (blue) with the four banks of preamplifier units (32 channels per bank) mounted. In the foreground are the relay optics and filter wheel.

the base temperature of 285mK is in excess of 24 h. In combination with ~18 h hold time of the helium bath, this allows for uninterrupted stable operation throughout the night and convenient recycling during daytime. The complete system can be seen in Fig. 2.10.1/3.

S-Cam3 saw first-light during a 7-night observation Figure 2.10.1/5: A processed S-Cam3 image of a campaign at the 4.2 m William Herschel Telescope at La 9x11 arcsec field showing multiple points sources and Palma (E) in July 2004. The instrument performed a single extended source, in this case a galaxy. Future extremely reliably, with only 15 min of observation time S-Cams will extend the field coverage to about lost due to instrument problems. The observation 1 arcmin, allowing intrinsic multi-colour deep-field programme focused on the detection of temporal and imaging for extragalactic studies. spectral variability in a number of targets. Data processing and analysis is underway. Fig 2.10.1/4 shows a processed image of a point source under fairly poor seeing conditions. Using the detector’s intrinsic wavelength resolution, the effect of differential space-based applications in future science missions are atmospheric refraction is clearly seen. Fig 2.10.1/5 is a not so far away. processed image of 9x11 arcsec in which five different sources can be distinguished, including a galaxy in the lower right part of the image. The star in the upper left 2.10.2 Advanced semiconductor sensors part is Mv = 19. Note that there is some distortion in this image because some pixels were lost through While superconducting sensors will have serious electrostatic discharge in the course of the S-Cam3 final applications in future astrophysics missions, sensors assembly. based on new semiconductor materials should also be beneficial to not only astrophysics but also planetary S-Cam3 has taken the development and application of missions. superconducting sensors further along the road to practical systems providing meaningful astronomical Long-term developments in semiconductor detector data. Further developments focusing around far larger research have included the production of pixellated fields of view (~1x1 arcmin) and closed-cycle cooling detectors fabricated from GaAs. Previous work on are now underway. Such developments may mean that monolithic diodes and small pixel arrays have shown sec2.qxd 7/11/05 5:13 PM Page 48

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Bump Dedicated ASIC Pixel p-layer

Insulating I-Layer (40-400 µm)

Substrate N-Layer (2 µm)

X-ray Illumination

Figure 2.10.2/1: The approach to bump-bonding a dedicated ASIC to a large-format GaAs array so that each pixel can be read out independent of all others. The inset shows an SnPb bump bond ~20 µm in diameter.

Figure 2.10.2/3a: Left, the limiting energy resolution achievable for a range of compound semiconductors as a function of band-gap energy at 5.9 keV. For completeness, included are the superconductors on which S-Cam3 is based. Curves are given for average values of the Fano factor: 0.22 for superconductors and 0.14 for semiconductors. NBG and WBG show the regions in which the narrow band gap and wide band gap semiconductors lie. Materials science research within SCI-AT/AI is covering the majority of these materials.

unprecedented performance as X-ray spectrometers due to the focus within SCI-AT on the fabrication of extremely high-quality epitaxial GaAs material. Figure 2.10.2/2a: The Medipix GaAs array (64x64 Spectroscopic performance approaches that of pixels) together with the vias for the SnPb bump- conventional silicon detectors, but with important bonds (inset). advantages of higher temperature operation (owing to its larger energy bandgap) and enhanced radiation damage tolerance.

The most recent activity has centred on the production of larger arrays that can be bump-bonded to readout ASICs (Fig. 2.10.2/1). A method of thinning away the supporting semiconductor substrate to expose the detecting volume and processing the contacts to allow a low temperature bonding to the readout chip matched to the detector pixels has now been demonstrated.

In lieu of a spectroscopic readout ASIC that is still in development, an imaging system of the same physical dimensions has been adopted from the medical imaging community. A complete end-to-end demonstration of a representative imager system has thus been possible, not only demonstrating the necessary packing technology for Figure 2.10.2/2b: An X-ray image of a sardine taken future space mission applications, but also affording a with the SCI-AT GaAs array coupled to a Medipx significant spin-off in terms of improving existing ASIC (top). The optical image (bottom is shown for medical imager technology – GaAs can replace Si pixel comparison). arrays with the benefit of improved spatial resolution and sec2.qxd 7/11/05 5:13 PM Page 49

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Figure 2.10.3/1: The improvements in the stacking and orientation of fibres used in micro-channel plate optics. On the left is the old technology with rounded edges that impede stacking. At right is the current improvement, together with a high-resolution image Figure 2.10.2/3b: Measured 241Am and 55Fe energy loss of a few micro-channels, each ~10 µm in width. spectra in (a) 1 mm2, 500 µm-thick Si detector; (b) a 1mm2, 40 µm-thick GaAs detector; (c) a 3.142 mm2, 2.5 mm-thick CdZnTe detector; (d) a 7 mm2, 500 µm- thick HgI2 detector. These wide-bandgap semi- conductors are all suitable for applications in hard 2.10.3 Development of advanced optics X-ray and gamma-ray planetary physics and astronomy. To enable future low-mass (hence lower cost) astro- physics missions, SCI-AT has been developing light- weight optics using a number of different technologies for applications at X-ray and gamma-ray wavelengths. Future developments include expanding this area of lower patient dose through the enhanced detection research to optical and IR wavelengths in support of the sensitivity (Fig. 2.10.2/2a, b). Cosmic Vision programme.

This work is expected to continue with the transfer of the As an example of the power of this type of focused same technology to the bump-bonding of a spectroscopic research and development, consider the case of micro- readout ASIC. This will be concluded by the channel plate-based optics. Micro-channel plate glass demonstration of simultaneous imaging and spectro- technology has been adapted for X-ray reflecting optics, scopy at X-ray wavelengths. Such a technology would where square pore glass micro-channels efficiently then be suitable for a low-resource X-ray planetary reflect X-rays up to a few keV in energy. When such a surface mapper, that in combination with suitable optics glass plate is slumped to an appropriate shape, and two (see Section 2.10.3) can map the surface distribution of plates located back-to-back, an approximation to chemical elements. Indeed, this technology development classical Wolter X-ray optics can be obtained. Recent has already led the scientific community to want it to activities have centred on improving the metrology and form the baseline for the X-ray imaging spectrometer on preparation of drawn glass fibres, together with ESA’s BepiColombo mission to Mercury. improvements in fibre stacking. Major improvement in the quality of the micro-channels has allowed In addition to this specific development in GaAs, improvements in performance (Fig. 2.10.3/1). Measure- research continues on a number of other materials ments made at synchrotron facilities confirm a suitable for hard X-ray and gamma-ray astrophysics. The significant improvement in attainable resolution, to study of imaging sensors based on the wide bandgap ~30 arcsec. The large open area factor guarantees a very semiconductors HgI2 and TlBr are particularly promising low density of the optics, such that a geometric area of (Fig. 2.10.2/3) for room-temperature operation in the 1m2 will weigh only 25 kg. Clearly, such low-mass gamma-ray regime. optics have applications not only in astrophysics missions but also as the optical part of an imaging X-ray Finally, low-bandgap semiconductors are also now being spectrometer for future planetary missions, such as the studied for the UV, EUV and soft X-ray part of the BepiColombo mission to Mercury. spectrum as potential imaging photon-counting sensors for astrophysics. Here the energy resolution would be Notwithstanding this dramatic demonstration of improved over Si-based sensors while the needs for very performance, a number of future applications in low-temperature cryogenic cooling, such as required for astrophysics demand a much higher angular resolution in superconducting sensors, may be relaxed (Fig. order to resolve distant populations of galaxies forming 2.10.2/3a). early in the Universe. For the XEUS mission, for sec2.qxd 7/11/05 5:13 PM Page 50

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(Fig. 2.10.3/3). This facilitates a mission concept for XEUS that allows a 10 m2-class telescope to be transportable to an L2 orbit.

It is through these types of developments, when coupled with novel deployment techniques, that high-precision low-mass optics may have serious applications on future ESA science missions over a number of different wavelengths. This may enable more demanding scientific missions to be realised while still constraining costs.

2.10.4 Advanced instrumentation research for planetary missions

The Planetary Exploration Studies Section is involved in Figure 2.10.3/2: An X-ray image of a point source a wide range of research and development activities for observed through the micro-pore optics. The remote sensing and in situ instrumentation for planetary resolution is ~3 arcsec. Such a technology will have applications of future missions. The aim is to develop wide applications for future ESA astrophysics scientific instruments with reduced resource demands missions. (power, mass, volume, number of interfaces, etc) by miniaturisation, integration and use of the most recent technologies. This approach leads to sophisticated instrument suites for smaller and less demanding science missions and enables new mission profiles at reduced costs. Breadboards of several key instruments and instrument suites are under development to demonstrate scientific performance under environmental conditions and to allow a better understanding of the operational needs of future missions and the associated scientific instrumentation.

Exploitation of missions in orbit or under development, such as SMART-1, Mars Express, Venus Express, Figure 2.10.3/3: The low-mass micro-pore optics with Rosetta and Huygens, is also supported to investigate a resolution of ~3 arcsec and an area-mass density at 1 keV of 200 kg/m2 (left). At right is the full-sized high-mass XMM optics, having a resolution of ~14 arcsec and an area-mass density of 2300 kg/m2. Figure 2.10.4/1: Refraction and total reflection at an interface between two media with refractive indices n1 and n2 (n1 < n2). The exponential decay of the electric field in a layer close to the interface, in the example, a requirement (goal) of 5 (2) arcsec is necessary case of total reflection, is indicated and the symbol of to avoid confusion between faint objects. Another a water molecule on the surface is shown. technological solution has been developed to address this need. With a long focal length, a conical approximation to Wolter optics can be obtained with excellent resolution. Such a conical approximation is realised with silicon micropores that are fabricated by a chemo- mechanical ribbing of highly polished silicon wafers. The structure is in principle light and self-supporting. Prototype modules produced in the last year have been measured at synchrotron facilities (Fig. 2.10.3/2) and shown already to offer an angular resolution of ~3.5 arcsec FHWM, sufficient to meet the requirements of XEUS. The area density of this technology allows a significant area-mass density advantage over, for example, the XMM-Newton replicated optics approach sec2.qxd 7/11/05 5:13 PM Page 51

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current limitations, fields for further improvements, applicability of technology development and to define further needs of future enabling key technologies.

Listed below are the most important activities currently under study. These developments are performed in close cooperation with various scientific institutes, industrial partners, national agencies and several ESA departments. A summary of a few of these developments are also provided below to complement the list. Note: FM = Flight Model, LM = Laboratory Model; BB = bread- board; dev/ment = development..

Research & Development Status Target level Highly Integrated Payload Suites (HIPS) dev/ment BB Figure 2.10.4/2: The Nanokhod rover under Laser altimeter (surface topography study BB development within D/TEC. The payload cab can from orbit) accommodate the LMS together with a micro-camera Atomic Force Laboratory, FM LM, or an alternative geochemistry package under metrology and MIDAS FM development within SCI-AP, comprising an alpha- Rover (surface science with mobility) BB EM proton-X-ray and Mossbauer spectrometer. Mole (subsurface science) LM BB Heat flow and physical properties study BB package (for the Mole) Geochemistry package (for Rover) LM BB [alternative to LMS] Laser Mass Spectrometer (LMS) BB BB LIBS-RAMAN spectroscopy study BB Attenuated Total Reflection BB Spectrometer (ATR) Luminescence surface dating study BB (sample age determination) Melting probes (subsurface science) dev/ment BB 3-axis fluxgate magnetometer FM- front-end ASIC ASIC & BB Subsurface & surface radar study BB (topography & subsurface science) Figure 2.10.4/3: Laboratory prototype of a packet- sized mass spectrometer. The oversized power connector and lens holder would be eliminated for a Attenuated Total Reflection (ATR) Spectrometer flight version.

The starting approach here has been to consider the detection of water sublimations on subsurface soil grains on Mars with a miniaturised spectrometer based on the Fahrenfort principle (Fig. 2.10.4/1). Initial tests with commercial equipment have led to promising results that indicate the elemental composition of the grain itself may also be derived. The goal for the instrument front-end is a diameter smaller than 3 cm, so as to be accommodated as part of the payload of the mole that isalso under development for subsurface investigations.

Laser mass spectrometer (LMS)

This instrument is being developed together with the Figure 2.10.4/4: LMS flight-like electronics for the University of Berne to be accommodated inside the second prototype spectrometer (laser control payload cab of a microrover (Fig. 2.10.4/2). Early results circuitry and high-voltage power supply). sec2.qxd 7/11/05 5:13 PM Page 52

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from the first rover prototype LMS, with dimensions of a few cm, its total mass and a laser source similar to those envisaged for the flight model are very promising (Fig. 2.10.4/3). A mass resolution and transmission in good agreement with simulations have been achieved. The mass resolution is sufficient to resolve adjacent isotopes clearly when used with laboratory data- acquisition hardware. Work is ongoing to improve the hardware: final miniaturisation of the electronics and optics, and setting up a laboratory testbed for performance verification and further improvements (Fig. 2.10.4/4).

3-axis flux gate magnetometer

An ASIC containing the complete front-end electronics for a 3-axis fluxgate magnetometer is under develop- ment. An integrated sigma-delta converter is used to sample the output of the three magnetometer coils. The output is passed through an integrated decimation filter unit. Up to four housekeeping data channels are supported on chip. Data output and instrument control is provided via a synchronous serial interface. All required excitation signals are also provided by the ASIC. Experience gained through the successful and completed development and application of the Particle Detector Front End (PDFE) ASIC, which is due to fly on the NASA STEREO mission within the IMPACT instrument suite, has been used to ensure that an instrument on a single chip can be developed. The development, research and verification of the magnetometer ASIC is expected to be a leading example for further integration of instrument front-ends on ASICs.

MIDAS

An atomic force microscope has been successfully developed into a flight model and accommodated on the Rosetta mission. Laboratory tests are beingperformed with a commercial AFM and with the spare FM to build a reference database. This experience may well lead to the design of a much lower-resource instrument for incorporation into the payload of future planetary missions based around mini-satellites. sec3.qxd 7/15/05 10:01 AM Page 53

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3. SCIENTIFIC SUPPORT ACTIVITIES IN RSSD & SCI-A

3.1 Astrophysics Missions Division 3.4 Fundamental Physics Missions Division

3.1.1 Introduction and overview 3.4.1 Introduction and overview 3.1.2 Herschel 3.4.2 LISA Pathfinder 3.1.3 Planck 3.4.3 LISA 3.1.4 Eddington 3.4.4 ACES 3.1.5 COROT 3.4.5 Microscope 3.1.6 Gaia 3.1.7 JWST 3.1.8 Astro-E2 3.5 Space Telescope Operations Division 3.1.9 Darwin 3.1.10 XEUS 3.5.1 HST observation programme 3.1.11 Lobster-ISS 3.5.2 Special HST programmes 3.1.12 ROSITA 3.5.3 Instrument status 3.1.13 EUSO 3.5.4 The European Coordination Facility 3.5.5 HST operational status

3.2 Solar and Solar-Terrestrial Missions Division 3.6 Science Operations and Data Systems 3.2.1 Introduction and overview Division 3.2.2 Ulysses 3.2.3 SOHO 3.6.1 Introduction and overview 3.2.4 Cluster 3.6.2 ISO 3.2.5 Double Star 3.6.3 XMM-Newton 3.2.6 Solar Orbiter 3.6.4 Integral 3.2.7 Solar-B 3.6.5 Astro-F 3.6.6 Herschel Science Centre development 3.6.7 Information technology support activities 3.3 Planetary Missions Division 3.6.8 Archive and Virtual Observatory activities

3.3.1 Introduction and overview 3.3.2 Cassini/Huygens 3.7 Science Payload and Advanced Concepts 3.3.3 Rosetta Office 3.3.4 Mars Express 3.3.5 Venus Express 3.7.1 Science Payload Instrument Section (SCI-AI) 3.3.6 BepiColombo 3.7.2 Science Missions Section (SCI-AM) 3.3.7 SMART-1 3.7.3 Planetary Exploration Studies Section (SCI-AP) 3.7.4 Advanced Technology Section (SCI-AT) 3.7.5 Darwin special project group sec3.qxd 7/15/05 10:01 AM Page 55

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Section 3 addresses the contributions of RSSD and commissioning. Responsibility for the development and SCI-A staff to the mission-related activities of the execution of science operations and, after completion of Department and Office. These encompass ESA’s science the in-orbit commissioning phase, for the mission missions in their orbital and post-operations phases, the management rests with the Science Operations and Data approved missions under or awaiting development, and Systems Division. Responsibility for mission manage- missions under study. ‘Europeanised’ missions led by a ment of Solar, Solar-Terrestrial and Planetary Missions national agency and potential International Space during operational phases remains, however, with the Station (ISS) payload elements are also included. respective Mission Division. The Space Telescope Operations Division hosts the ESA staff supporting the The chapter is structured by Division, reflecting the Hubble Space Telescope Science Institute (STScI) in RSSD organisation at the end of the reporting period Baltimore (US) and the European Coordinating Facility (see Table 1). As stated in Section 1, RSSD has four (ST-ECF) in Garching (D). Mission Divisions (Sections 3.1-3.4) and two Operations Divisions (Sections 3.5 and 3.6). The For the sake of brevity, the instruments, Principal responsibilities of the Science Payload and Advanced Investigators, mission or interdisciplinary scientists, Concepts Office, which are independent of RSSD science team members etc. of the missions described are although closely associated, are summarised in not tabulated here. Such information may be found in Section 3.7. ESA’s Report to COSPAR, the most recent being ESA SP-1276 (July 2004), produced by the RSSD Project For astronomy missions (excluding HST), the Scientists, and in the relevant Web pages (the addresses Astrophysics Missions Division has responsibility for are included here as footnotes with each mission Project and Study Scientist support until in-orbit description).

Table 2: Research and Scientific Support Department 2004 – Projects and Studies.

Division Astrophysics Solar & Planetary Fundamental Space Science Ops. Missions Terrestrial Missions Physics Telescope & Data Missions Operations Systems

Missions in Ulysses Cassini/ HST ISO Operation or SOHO Huygens XMM Post-Operation/ Cluster Rosetta -Newton Archive Phase Double Star Mars Express Integral SMART-1

Missions in or Herschel Solar Orbiter Venus Express LISA Astro-F awaiting Planck BepiColombo Microscope Herschel development Eddington LISA Pathfinder science ops. JWST ACES Gaia COROT

Mission and Darwin ILWS ISS Payload XEUS Solar-B Studies ISS*

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3.1 Astrophysics Missions Division Madrid, Spain, the location of the Herschel Science Centre during operations. 3.1.1 Introduction and overview With five staff in place, the small team in the Planck The past 2 years brought their share of good and bad Science Office is now complete. The development is well news. On the sour side, the financial situation of the under way by RSSD of the software tool needed to Science Programme forced the cancellation of the evaluate the quality and completeness of the survey data Eddington mission by the SPC at the end of 2003. This and replan Planck operations if necessary. The was particularly sad given the strong scientific case of publication of the first WMAP results suggest that the Eddington and its wide support in the scientific detection of the so-called CMB polarisation B mode by community. The latter is illustrated by the highly Planck is a real possibility, thereby enhancing the successful Eddington workshop organised by the scientific case for the mission even further. Division in April 2003 in Palermo. The excellence of Eddington was also reaffirmed in 2004 by the SPC, who RSSD activities in support of Gaia have also picked up recommended that it should be the first mission to momentum. Most prominent is the development, under implement if additional money could be found. RSSD responsibility, of a prototype data-analysis system. This Gaia Data Access & Analysis Study (GDAAS) is The Columbia Shuttle accident in 2003 and the US intended to demonstrate the feasibility of reducing the decision to terminate the ISS and Shuttle programmes 1000 TB expected from the 5-year mission and of soon after 2010 were serious drawbacks to various iteratively extracting the positions and proper motions of projects under study in the Division. The Division’s ~1 billion sources. A milestone was achieved in late Study Scientist, supported by the D/HME Study 2004, with the processing of 18 months of simulated data Manager, expended considerable effort in investigating and the successful recovery of 200 000 stars. alternative launch scenarios for the EUSO high-energy cosmic-ray payload. However, mostly due to its large RSSD activities in support of JWST have also gained size and mass, it soon became clear that there would be significant momentum over the last 2 years, as the no credible transportation system to lift EUSO into orbit project transitioned from its definition phase into and install it on the ISS. Irrespective of these implementation. In late 2003, one new staff member was programmatic uncertainties, the AWG and FPAG jointly added to the Division to assist the JWST Project re-examined the science case of EUSO during Spring Scientist. Both have been busy defining the scientific 2004. Both working groups confirmed that the scientific capabilities and detailed technical specification of potential of EUSO was excellent but not among their top NIRSpec, an instrument that is being developed and priorities, and therefore did not recommend its financed by ESA. They prepared the JWST Science continuation into Phase-B. Management Plan, which was subsequently approved by the SPC. The NIRSpec Instrument Science Team was The early retirement of the ISS was also potentially bad later appointed, to provide scientific guidance to the news for XEUS because the original mission profile Project Scientist. foresaw assembling the mirrors in orbit at the Station. Fortunately, a breakthrough in the development of light X-ray mirror technology by SCI-A meant that the ISS is 3.1.2 Herschel no longer needed and that a 10 m2 mirror spacecraft can be injected directly into an L2 orbit by an Ariane-5-type The Herschel Space Observatory is a multi-user launcher at a much reduced cost. observatory-type mission targeting the 57-670 µm range in the far-IR and sub-mm, providing observation The gradual build-up of the Herschel Science Centre opportunities for the entire astronomical community. (HSC) operations team continued throughout the period. Herschel is scheduled for launch in mid-2007. Members of the team spent extensive periods at the PI institutes, working together with the PI teams to prepare Herschel is designed to address the ‘cool’ Universe; it for the scientific operations of Herschel, and for the has the potential of discovering the earliest epoch proto- calibration of its instruments. They were deeply galaxies, revealing the cosmologically evolving AGN- involved in the Instrument Level Tests (ILTs) starburst symbiosis, and unravelling the mechanisms successfully carried out in Autumn 2004. The Herschel involved in the formation of stars and planetary system Common Science System (development led by RSSD) bodies. A major strength of Herschel is its photometric was used to support the ILTs and archive the test data. mapping capability for performing unbiased surveys This rather hectic period ended happily with the delivery related to galaxy and star formation. Redshifted ultra- of the instrument cryo-qualification models to ESA in luminous IRAS galaxies (with SEDs peaking in the 50- late 2004. The HSC team is now busy preparing the first 100 µm range in their rest frames), as well as class 0 call for observing proposals, which will be issued in proto-stars and pre-stellar object SEDs, have their 2006. In April 2005, the team will relocate to ESAC near maximum emission in the Herschel prime band. Herschel

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shared with Planck. It will operate from the vicinity of L2, which is situated 1.5 million km away from the Earth in the anti-sunward direction. It offers a stable thermal environment with good sky visibility. Commissioning and performance verification will take place en route to L2. Once these crucial mission phases have been accomplished, Herschel will enter routine science operations for a minimum of 3 years.

The scientific operations of Herschel will be conducted in a novel decentralised manner. The operational ground segment comprises six elements:

— the Herschel Science Centre (HSC), provided by ESA; — three dedicated Instrument Control Centres (ICCs), one for each instrument, provided by their PIs; — the Mission Operations Centre (MOC), provided by ESA; — the NASA Herschel Science Centre (NHSC) provided by NASA.

The HSC acts as the interface to the science community and outside world in general, supported by NHSC for the US science community. The HSC/NHSC provides information and user support related to the entire life- cycle of an observation, from calls for observing time, the proposing procedure, proposal tracking, data access and data processing, as well as general and specific information about using Herschel and its instruments.

RSSD is responsible for building the science ground- segment infrastructure for performing these tasks, Figure 3.1.2/1: An artist’s view of the Herschel together with the ICCs. One single system that evolves satellite as developed by Alcatel. over time, rather than having separate systems for different mission phases, is being built. The initial version of this system has been delivered to the instrument teams and was successfully used to support the instrument-level tests during Autumn 2004. The is also well equipped to perform spectroscopic follow-up observation planning subsystem is based on the NASA observations and further characterise interesting Spot tool used by Spitzer. In this way, not only is the individual objects. effort that went into building Spot reused, but previous Spitzer users will immediately feel at home, increasing Herschel’s telescope is passively cooled (to maximise their scientific productivity. SCI-SA personnel are size), while the three focal-plane instruments are housed deeply involved in providing scientific guidance and inside a superfluid helium cryostat, on top of which the supervision to the HSC software developers and telescope is mounted. The instruments are provided by performing the usual user acceptance tests. In the course consortia led by PIs who get guaranteed observing time of 2004, SCI-SA personnel in the HSC spent a large in return. The Photodetector Array Camera and amount of time collocated at the PI institutes together Spectrometer (PACS) is a camera and low- to medium- with the instrument teams, first preparing and later resolution spectrometer for wavelengths up to 210 µm. executing the ILTs. In this way, they not only provided The Spectral and Photometric Imaging Receiver (SPIRE) useful support to the PI teams, but they also acquired is a camera and low- to medium-resolution spectrometer first-hand experience with the Herschel instruments. for wavelengths longer than 200 µm. The Heterodyne The HSC SCI-SA scientists have also been busy Instrument for the Far-Infrared’ (HIFI) instrument is a preparing or upgrading the large amount of heterodyne spectrometer. It offers very high velocity documentation required for the scientific operations of resolution for a single pixel on the sky. Herschel, in particular concerning the observation scheduling, the calibration of the observatory and Herschel (Fig. 3.1.2/1) will be launched on an Ariane-5 support to the scientific community. sec3.qxd 7/15/05 10:01 AM Page 58

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In order to promote Herschel awareness in the scientific community, SCI-SA personnel have also been busy Telescope delivering talks and organising conferences related to Herschel science. In 2004 alone, there have been: Instruments — a special session on Herschel at American Astronomical Society Meeting 204 in Denver, USA Shields on 3 June 2004; — the Beyond Spitzer and Herschel conference in Pasadena, USA on 8 June 2004; — several Herschel presentations at the SPIE conference on Astronomical Telescopes and Service Module Instrumentation in Glasgow, UK on 21 June 2004; Solar array — The Dusty and Molecular Universe: A Prelude to Interface Herschel and ALMA conference in Paris on to Ariane 27 October 2004; — a workshop dedicated to the calibration of Herschel in Leiden, NL on 1-3 December 2004. Figure 3.1.3/1: The current configuration of the Planck satellite, as developed by Alcatel Space (F). On request from the Astronomy Working Group chairman, the Project Scientist also presented the status of Herschel to the AWG twice during the reporting period. space-based experiment to survey the whole sky with an At the time of writing, all SCI-SA personnel in the HSC angular resolution as high as 5 arcmin, a sensitivity are in the process of relocating to the European Space approaching ∆T/T ~10–6, and covering a frequency range Astronomy Centre (ESAC) near Madrid (E), from where wide enough to measure and remove all possible Herschel science operations will be conducted. foreground sources of emission. The main scientific result of the mission will be an all-sky map of the CBRF fluctuations and their polarisation. In addition, the sky 3.1.2 Planck survey will be used to study in detail the very sources of emission that ‘contaminate’ the cosmological signal, and In late 1992, the COBE team announced the detection of will result in a wealth of information on the dust and gas intrinsic temperature fluctuations in the Cosmic in both our Galaxy and extragalactic sources. Background Radiation Field (CBRF), observed on the sky at angular scales larger than ~10°, and at a brightness The Planck payload consists of a 1.5 m-diameter offset level ∆T/T ~10–5. In February 2003, the WMAP team telescope, with a focal plane shared by clusters of announced results on scales of about 15 arcmin with a detectors in nine frequency bands covering 30-900 GHz. similar sensitivity (see http://lambda.gsfc.nasa.gov for The three lowest bands (up to ~70 GHz) are covered by detailed descriptions of both COBE and WMAP). These HEMT-based receivers actively cooled to ~20 Kby an H2 fluctuations have been interpreted as due to differential sorption cooler. The higher frequency bands are handled gravitational redshift of photons scattered out of an by arrays of bolometers cooled to ~100mK; the H2 inhomogeneously dense medium. They thus map the sorption cooler provides pre-cooling for a Joule- spectrum of density fluctuations in the Universe at a very Thomson 4K stage, to which a dilution refrigerator is early epoch. This long-sought result established the coupled. Inflationary Big Bang model of the origin and evolution of the Universe as the theoretical paradigm. However, in Since 2002, the instrument development has intensified. spite of the importance of the COBE and WMAP The qualification models have been largely measurements, many fundamental cosmological manufactured and are now undergoing test. The first questions remain open. Building on the pioneering work delivery to ESA was made in late November 2004, for of COBE and WMAP, the main objective of the Planck integration into a full qualification satellite. This model mission is to map the fluctuations of the CBRF with an will be tested in early 2005 in a specially designed cryo- accuracy that is set by fundamental astrophysical limits, chamber at the Centre Spatial de Liege (B). The flight allowing us to address these fundamental questions. models are under manufacture and will be delivered to ESA in mid-2005. After long and complex testing, the Planck was selected in late 1996 as the third Medium satellite will be launched from Kourou in mid-2007. mission (M3) of ESA’s Horizon 2000 Scientific Programme, and is now part of its ‘Cosmic Vision’ At RSSD, activity in the past 2 years has concentrated on Programme. The observational goal is to mount a single the build-up of the Planck Science Office (PSO), which

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is in charge of overall scientific coordination, survey 3.1.4 Eddington planning, archiving of the final data products and their distribution to the community. Support scientists and The Eddington mission has two main scientific goals: engineers have recently joined the group, which will move in late 2006 to its final location at ESAC. Many — the detection of habitable planets orbiting other stars, new documents have been written by PSO staff during and the determination of their frequency of occurr- the reporting period, among which the Calibration ence and characteristics in different environments; Requirements document, the Planck Science Operations — the understanding of the formation and evolution of plan and the Calibration and Performance Verification stars across a wide range of key stellar character- Phase Science Operations Plan. PSO scientists have also istics (age, chemical composition, mass). defined the baseline Planck scanning strategy as well as the requirements on the Planck Survey Planning and While planets will be detected by looking for the small Performance evaluation Tool, and they continue to but measurable decrease in a star’s light caused by a provide scientific guidance and supervision to its planet’s transit, stellar structure and evolution science software developers. As for Herschel, the PSO scientists will make use of asteroseismic techniques. These will have spent long periods at the HFI and LFI institutes to study stellar oscillations, as has been done with the Sun support the ILTs. for a number of years. Both techniques require long-term very high-accuracy photometric time series (which can The cancellation of the LFI 100 GHz channel by ASI in be obtained only from space) and thus can naturally be 2002 was a severe blow to the Planck scientific carried out by the same payload. capability because it removed the possibility to measure the CMB polarisation at this critical frequency, where The original Eddington proposal, submitted in response contamination by foreground sources is minimal. The to the 2000 call for the F2/F3 missions, was based on a Project Scientist successfully sought a resolution from monolithic 1.2 m-diameter telescope with a large-area the AWG stressing the scientific importance of 100 GHz CCD mosaic. In May 2002, Eddington was approved as polarisation measurements. This resolution helped the an element of the Science Programme by the SPC, with HFI PI to convince NASA to provide the extra funds a 2009 launch date. Two parallel industrial definition required to finance the development by JPL of polarisa- studies were conducted, with Astrium Germany and tion-sensitive bolometers at this critical frequency. Alcatel as prime contractors. These involved the complete space segment, including the payload, which is The Project Scientist, assisted by the Planck Science baselined to be ESA-procured. Both contractors Team, has updated the scientific case for the Planck converged to a similar payload design, involving three mission. The revised document, which takes into account identical, parallel telescopes with a total collecting area the exciting results obtained by WMAP, will be released of ~0.7 m2 and a six-CCD focal plane. Each telescope has in mid-2005. Far from weakening the case for Planck, the a different filter, so that the resulting light curves offer WMAP data actually enhance it. In particular, the colour information (a unique characteristic of tentative detection of a very early re-ionisation epoch Eddington). makes it much more likely that Planck will be able to detect the so-called polarised B-mode signal of the CMB In parallel, a development activity carried out with E2V that carries information about primordial gravitational as prime contractor resulted in the development of the waves generated during the inflation era. The Project CCD chips for the Eddington focal plane, with the first Scientist also updated the Science Management Plan, the CCD chips produced and qualified. These are based on highest-level document governing the implementation of an existing design but are produced in a large, custom the Planck mission. The revised document was approved format tailored to the Eddington focal plane. by the SPC in early 2004. The most important modification is the introduction of an Early Release Organised by RSSD, the second Eddington workshop Compact Source Catalogue (ERCSC), to be published took place in Palermo (I) in April 2003, attracting more 9 months after the completion of the first all-sky survey. than 150 scientists. The new instrumental configuration The idea behind the ERCSC is to allow follow-up was presented to the community, and significant progress pointed observations with Herschel of the many compact was made in the selection of the candidate fields for the millimetric sources that Planck will discover, including 3-years planet-finding observation. This resulted in the several hundreds clusters of galaxy. selection of the Lacerta field announced a few months later. Later in 2003, an AO for the Eddington Science SCI-SA personnel have also organised several Team was run, and resulted in the selection by AWG of conferences and workshops to promote awareness of the eight scientists. Planck mission in the scientific community, including the Second Planck Symposium Setting the Scene, held in Unfortunately, at the end of 2003 the financial situation Orsay (F) in January 2004 and attended by more than 200 of the Science Programme required deep cuts in the scientists. programme. Notwithstanding the high scientific rating

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given to it by the ESA advisory structure, it was decided to remove Eddington from the programme, and to stop all development activities. At a meeting in 2004, the SPC reaffirmed the scientific interest of Eddington, and recommended that, should fresh resources become available to the Science Programme, Eddington would be the first mission to be implemented.

3.1.5 COROT

COROT is a CNES-led mission for high-accuracy photometry, with both asteroseismology and extrasolar planet-finding among its science goals. With its 27 cm- diameter telescope and 2.8x2.8° FOV, COROT will concentrate on a limited number of relatively bright targets, and will be the first mission to perform a space- based search for exoplanets with the transit method.

In return for its contribution to the telescope optics and to the payload test and integration, the ESA Science Programme has negotiated data rights for scientists based in ESA member countries. To this effect, an AO was issued in 2002, which drew a large response from the European astronomical community, and which has resulted in the selection of a number of teams that have since then become significantly involved in the development of the mission. Figure 3.1.6/1: Artist’s impression of the Gaia satellite. As a member of the COROT steering committee, the SCI-SA Study Scientist oversees the scientific aspects of the project, in particular the definition of the observing programme. His role is also to protect the scientific interests of the European teams involved in COROT. preparations for the mission involve the participation of some 15 working groups, taking responsibility for COROT is on track for launch in the third quarter of (amongst other aspects) the accuracy modelling, the 2006. radial velocity instrument optimisation, preparation of simulated data, and the development of a data processing framework to handle the complex and large (of order 3.1.6 Gaia 1 Petabyte) Gaia data set.

Since June 2002, Gaia has been a confirmed mission The status of the satellite and payload was presented to within the ESA Cosmic Vision 2020 science programme, ESA and the Gaia science team at the mid-term with a target launch date of mid-2011. Gaia will build on presentations of the definition phase, held in September the observational principles of Hipparcos to measure 2004 at ESTEC. The two industrial teams, Alenia/Alcatel detailed properties of the brightest 1 billion stars. and EADS-Astrium, separately presented the status of Astrometric accuracies of 10 microarcsec at 15th their detailed studies into all aspects of the Gaia satellite. magnitude should lead to 20 million stars measured with These definition studies will run until mid-2005. distance accuracies of better than 1%, and more than 100 Technical prototypes of many parts of the Gaia satellite million better than 5%. Tangential velocities will be are now under development, including the silicon carbide measured astrometrically at better than 1 km/s for about primary mirror, and engineering models of the 100 million stars, while the dedicated radial velocity astrometric focal plane with flight-representative CCDs. spectrometer will gather radial velocities to 1-10 km/s to 16-17 magnitudes, depending on spectral type. Gaia will The final catalogues resulting from the Gaia mission are provide multi-colour (in 11 medium and 5 broad bands), not expected to become available until at least 2-3 years multi-epoch (of order 100 epochs over 5 years) after the end of mission operations, i.e. in about 2018 photometry for each object to 20th magnitude, with great according to current planning. However, early release care being invested in devising the photometric bands to catalogues of astrometry and photometry are foreseen maximise their astrophysical diagnostic power. Scientific from early on in the mission phase.

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The Project Scientist interfaces with the ESA Gaia perpetual shadow by means of a large deployable Project Team, chairs the Gaia Science Team, which takes sunshade. Further cooling of the mid-IR instrument is overall responsibility for all aspects of the scientific achieved by a dedicated solid-hydrogen cryostat. development of the mission, including coordination of the scientific working groups, and leads a small team in ESA’s participation in the mission was formally ESTEC supporting the community in developing plans approved by the SPC in October 2000, and consists of for the analysis of the huge quantity of data that will four components: result from the mission. At the science team level, this involves monitoring and contributing to the satellite and — provision of NIRSpec, the Near-IR Multi-Object payload design through analysis and independent Spectrograph covering 1-5 µm; modelling, and directing and coordinating the work of — provision of 50% of MIRI, the Mid-IR combined the 14 scientific working groups. These cover payload- Camera/Spectrograph covering 5-28 µm (through related aspects (such as accuracy modelling, on-board special funding from the ESA member states); detection, photometric system instrument definition, — provision of the Ariane-5 launcher that will carry the radial velocity instrument definition); in-depth studies of observatory to L2; specific classes of objects that present particular — contributions to JWST operations. problems during the observations or data analysis phase (such as binary stars, double stars, Solar System objects, In return for its contributions, ESA will gain a ~15% and reference frame definition), and aspects related to the partnership in JWST and secure for astronomers from its data analysis (database design, prototype reduction member states full access to the JWST observatory on system development, Grid-related studies and algorithm identical terms to those enjoyed today on HST: they will coordination). Altogether, some 250 member-state have representation on all advisory bodies of the project scientists are participating in these Gaia activities. and will win observing time on JWST through a joint peer-review process, backed by a guarantee of a The RSSD Project Scientist support team, under minimum ESA share of 15%. direction of the Project Scientist, supports the scientific community in this coordination effort, and takes a lead in Over the reporting period, the JWST observatory and its the accuracy analysis, parameter database definition, instruments successfully transitioned from the definition CCD performance and calibration, telemetry definition phase to the implementation phase. Following the NASA and coordination of the data analysis prototype. selection of Northrop-Grumman Space Technologies as the US Prime Contractor, the observatory underwent an The status of the scientific contributions and preparations extended ‘re-plan’ exercise, the outcome of which for the Gaia mission were presented at The Three resulted in the present 16-element 6.55 m-diameter Dimensional Universe with Gaia, a major symposium telescope design and 4-instrument payload suite held at the Observatoire de Paris, Section de Meudon (F), (NIRCam, NIRSpec, MIRI and FGS-TF). during 4-7 October 2004, and attended by 240 participants. On the European side, the highlights and major achievements of the period included: Details at http://www.rssd.esa.int/Gaia include up-to- date news, meetings of the working groups, information — final approval of the inter-agency agreement sheets, presentation material, and outreach features. governing the European consortium that will provide the Optics Module of MIRI; — successful completion of the MIRI System 3.1.7 JWST Requirements Review; — initiation of the MIRI PDR; NASA, ESA and CSA have, since 1996, collaborated on — selection of EADS/Astrium GmbH as the Prime the successor to the Hubble Space Telescope, the James Contractor for NIRSpec; Webb Space Telescope (JWST). JWST is scheduled to — initiation of the NIRSpec PDR; launch in 2011 and consists of a passively cooled, — selection of the external members of the NIRSpec 6.55 m-diameter telescope, optimised for diffraction- Instrument Science Team; limited performance at near-IR (1-5 µm) and mid-IR (5- — approval of the ESA JWST Science Management 28 µm) wavelengths. Plan.

The JWST telescope proper and its three instruments are During 2003 and 2004, ESA’s participation in JWST was to be cooled in bulk to < 50K, a temperature determined supported by RSSD through the ESA Project Scientist, by the operating temperature of the HgCdTe detector joined by the Deputy Project Scientist starting in late arrays employed by the near-IR instruments. Cooling is 2003. Like the Faint Object Camera on HST before it, the to be attained passively by placing the observatory at L2 NIRSpec instrument is being built by European industry and keeping the telescope and its instrumentation in to ESA’s specifications and under ESA project

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leadership. Hence, considerable effort by RSSD staff Mid-IR spectroscopic observations will be able to detect went into defining the capabilities and detailed technical and measure ozone, carbon monoxide, water and specifications of NIRSpec. These specifications served methane absorption lines, which together constitute the as a basis for the contractual negotiations with industry. best possible tracers of biological activities. The JWST Project Scientist proposed a list of members for the NIRSpec Instrument Science Team (IST) and got Since Darwin relies on the new technology of nulling it approved by the AWG at its meeting in May 2004. interferometry, ESA and ESO are jointly studying the Through an AO, he later recruited the IST whose main potential GENIE precursor instrument. This is a nulling role is to provide scientific guidance to the project. The interferometer, using the infrastructure at VLTI, ESO’s Project Scientist also drafted the JWST Science interferometer at Paranal in Chile. This instrument is Management Plan, which was approved by the SPC in planned to achieve first-light some time after 2008, and February 2004. He also obtained a recommendation from will study the Darwin target stars in detail in order to the AWG for the addition of an Integral Field Unit to determine the dust level in the exosystems, as well as NIRSpec, which considerably enhances the scientific attempt spectroscopic observations of a number of the return of the instrument and provide a back-up in case of known ‘hot Jupiter’ exoplanets. failure of the Micro Shutter Array. In late 2003, both the GENIE Science Team and the Terrestrial Exo-Planet Science Advisory teams were 3.1.8 Astro-E2 appointed via a standard AO. Their role is to provide scientific advice to ESA and the Study Scientist for the Astro-E2 will be Japan’s fifth X-ray astronomy satellite. definition, implementation and operation of the GENIE The mission is being developed at the Institute of Space and Darwin projects. The two industrial GENIE Phase-A and Astronautical Sciences, which is now part of the studies are progressing satisfactorily. The Study Scientist Japan Aerospace Exploration Agency (JAXA), together is closely involved in the on-going large R&D with a number of US and Japanese institutes. The programme that is designed to develop the challenging planned launch date is 2005. Astro-E2 will cover the new technologies required for Darwin. energy range 0.4-700 keV with capabilities highly complementary to those of XMM-Newton and Integral. Following an interval when the data belong to the 3.1.10 XEUS Astro-E2 Science Working Group, a Guest Investigator Programme will begin. JAXA has kindly offered to XEUS (X-ray Evolving Universe Spectroscopy) is the allocate part of the Japanese time to proposals led by potential successor to XMM-Newton. The goals of European astronomers. RSSD coordinated this XEUS are to detect massive black holes in the earliest participation and an ESAAO was prepared. Following its AGN and estimate their mass, spin and redshift through release, ESA established a Time Allocation Committee to Fe line and continuum variability studies, to study the review the received proposals; the highest ranking have formation of the first gravitationally bound, dark matter- been forwarded to JAXA for inclusion in the Japanese dominated groups of galaxies and trace their evolution part of the observing programme. into today’s massive clusters, to study the evolution of metal synthesis to the present epoch using observations of hot intra-cluster gas and to characterise the mass, 3.1.9 Darwin temperature and density of the intergalactic medium using absorption line spectroscopy. The Darwin mission and its potential precursor experiment GENIE (Ground-based European Nulling The original intention was to launch two separate Interferometer Experiment) have continued develop- detector and mirror spacecraft into low-Earth orbit with a ment. Darwin is ESA’s mission to search for and study mirror area of 6 m2. The two satellites would fly in Earth-like planets orbiting nearby (25 pc) stars. It relies formation, separated by the 50 m focal length of the on the technology of nulling or destructive interfero- optics. The mirror area would be then expanded to 30 m2 metry, where the appropriate phase-delays are applied to by the addition of further mirror segments, delivered to the beams from telescopes separated by many tens or the ISS by the Shuttle. With the early retirement of the hundreds of metres, thereby accomplishing destructive Shuttle resulting from the Columbia tragedy, it became interference along the optical axis. This extinguishes the apparent that this approach was no longer realistic. light from the star – which is 10 orders of magnitudes Instead, a revised mission concept is being examined. brighter than an Earth-like planet – while enhancing the This consists of direct injection of separate spacecraft to light from the planet. Darwin is now projected to consist L2 by an Ariane-5 or similar, and a mirror area of around of three 3 m-class telescopes based on the Herschel 10 m2 with a spatial resolution of 2-5 arcsec. XEUS will telescope, each on a separate spacecraft, with a beam use SCI-A’s new high-precision micro-pore optics, which combiner and detector assembly on a separate satellite. provide higher performance and lower mass than the Two Soyuz-Fregats will launch the four spacecraft to L2. nickel replication used for XMM-Newton. RSSD has

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been closely involved in ensuring that the revised the handful seen so far from ground observatories. The mission scenario fulfils the scientific goals of the Phase-A study, jointly conducted by the Human mission, defining a possible payload, coordinating study Spaceflight and Science Directorates, was recently activities with the Japanese partners, and holding completed and the final report provided to the ESA discussions with other potential partners. Science Advisory Structure. Unfortunately, EUSO was not identified as one of the scientific priorities for implementation in the foreseeable future. Activities are 3.1.11 Lobster-ISS continuing to investigate alternative implementation scenarios. RSSD has supported the Phase-A study by Lobster-ISS ESA is a sensitive all-sky monitor under providing coordination between the separate instrument study as a potential external payload on the ISS. Lobster- and payload studies, and ensuring that the advice of the ISS will use a novel form of wide-FOV micro-channel independent Science Study Team is properly utilised. plate X-ray optics, and will be the first true imaging X-ray all-sky monitor. Lobster-ISS will locate X-ray sources to within 1 arcmin with a limiting sensitivity of 0.1 mCrab in a day. As well as providing an alert facility, the outstanding sensitivity will allow many topics to be studied using Lobster-ISS data alone. Lobster-ISS recently completed an industrial Phase-A study. RSSD staff ensured that the scientific capabilities of the payload were maintained while producing a design that fulfils the requirements of the Columbus External Payload Facility on the ISS.

3.1.12 ROSITA

ROSITA (Roentgen Survey with an Imaging Telescope Array) is a proposal to perform the first imaging 0.5- 11 keV all-sky survey using an array of telescopes on the ISS. The main scientific goals are to detect obscured accreting black holes, to study the hot intergalactic medium in clusters and the hot gas in cluster filaments, to find distant clusters of galaxies and to investigate the galactic X-ray source populations. Following an initial feasibility study, additional activities are on hold until the outcome of the ‘Dark Universe Observatory’ NASA SMEX proposal is known in 2005. DUO would perform X-ray scans of limited regions of sky, whereas ROSITA would perform an all-sky survey; the science goals of the two missions are somewhat similar. RSSD has provided support to the initial feasibility study and to subsequent discussions with D/HME on future activities.

3.1.13 EUSO

Understanding the origin of cosmic rays with energies > 5x1019 eV is one of the primary challenges in astrophysics. At such extreme energies, cosmic rays interact with the cosmic microwave background and the distance that a cosmic ray can travel is limited to our galactic neighbourhood. Intriguingly, all the astronomi- cal objects that could produce such energetic cosmic rays are likely to be much further away. The Extreme Universe Space Observatory (EUSO) will observe the light produced when such a cosmic ray interacts with the Earth's atmosphere. Looking down from the ISS, EUSO could detect around 1000 events per year, compared to

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3.2 Solar and Solar Terrestrial Missions Division formations, the Cluster mission continues to deliver outstanding results of small- and large-scale physical 3.2.1 Introduction and overview processes in near-Earth space. As expected, Cluster has now provided both evidence and direct in situ The Solar and Solar Terrestrial Missions Division observations of reconnection in the magnetic tail and the provides scientific support for all ESA missions in solar, dayside high-latitude magnetopause. It has furthermore heliospheric and solar-terrestrial science. The present confirmed the existence of large-scale boundary waves missions in operational phase are Ulysses, SOHO, and vortices at the magnetopause, found filamentary Cluster and Double Star. Solar Orbiter is in its study structures in the aurora, the cusp and the tail current, and phase within SCI-A. Apart from providing science explicitly measured the extreme thinness of the bow- support to these missions, the Division is also shock and the cross-tail current just before substorm responsible for their management once in their onset. It appears that the number of results from Cluster operational phases. is still growing at an exponential rate, promising an exciting future. Both SSWG and SSAC have recently Staff members of the Division are located at ESTEC, taken a positive stand towards plans for a further mission with the exception of the SOHO team, who reside at the extension to late 2009, allowing a number of new SOHO Experiment Operations Facility at the NASA adaptive or multi-scale configurations to be exploited Goddard Space Flight Center, Greenbelt, USA. and new magnetospheric regions to be visited (in particular, the important sub-solar magnetopause and the Ulysses has now been in orbit for over 14 years and is near-Earth tail around 10 RE). An important step in the presently on its way towards a third set of polar passes in direction of even more effective Cluster data exploitation 2006-2007 (south) and 2007-2008 (north), following the was the ESA SPC decision to fund the Cluster Active decision by SPC to extend the mission to March 2008. Archive, an open approach to delivering high-resolution Ulysses has also completed a distant encounter with Cluster data to the worldwide community. Jupiter, where the scientific highlights were observations of quasi-periodic radio bursts and distant observations of ESA’s first collaboration with China, the Double Star Jupiter dust streams. Ulysses also observed cometary Project, got underway with successful launches into ions in a coronal mass ejection. As in the past, Ulysses’ equatorial (December 2003) and polar (July 2004) orbits. results continue to feature prominently at international The orbits are designed to support the Cluster mission, meetings and workshops, and the science team maintains and most of the European-provided instruments are an exceptionally high publication record (over 120 identical to the Cluster payload. In spite of some papers during 2003-2004). Such activities are problems with boom deployment and attitude computers, coordinated by the RSSD Project Scientist Team and both missions are now operating nominally, and will extend to data dissemination, archives and long-term provide important data complementary to Cluster for at calibration issues. least the mission baseline period of 1 year.

The SOHO mission remains the flagship of solar and After reconfirmation following the reassessment of the heliospheric research, continuously supplying scientists Cosmic Vision programme in 2003, Solar Orbiter is and, increasingly, space weather experts, through the under assessment in the Science Payload and Advanced RSSD Project Science Operations Team, with data from Concept Office, with support from the Study Scientist the Sun. A dramatic incident occurred in mid-2003, when concerning science issues and contacts with the a problem with the high-gain antenna motor resulted in international scientific community. During 2003, the some data loss, which sent a shockwave through the Solar Orbiter Science Definition team reviewed the scientific community. Using on-board data storage and scientific goals of the mission, resulting in a well- clever roll manoeuvres of the satellite, the SOHO RSSD balanced and highly focused mission. Project Scientist team was able to keep the damage from the malfunctioning motor to a minimum, rescuing Several instruments built in previous years by members continuous helioseismology data even during periods of of the Division and SCI-A personnel continue to deliver low-gain antenna contacts. Apart from such problems, good data. The instruments presently operative in orbit SOHO operations and science exploitation have run are COSPIN on Ulysses, LOI on SOHO and EFW and smoothly throughout the reporting period. As usual, the ASPOC on Cluster. For NASA’s STEREO mission, parts SOHO RSSD team has been extremely active in science of the SEPT/IMPACT instruments were delivered by outreach and communications. The most spectacular SCI-A during the reporting period. The SEPT instrument highlight was the coverage of the extraordinary solar built by SCI-A with science guidance from division staff outbursts in Autumn 2003, which are still under scientific is the most recent link in a very successful series of study via a large number of spacecraft such as Cluster. energetic-particle instruments from the Division.

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taken on during the reporting period. However, it is hoped that staff of the Division will be involved in providing the science requirements and guidance to SCI- A for the thermal design and testing of hardware for the ion and electric field instrument on BepiColombo’s MPO and MMO, respectively.

Besides the primary occupation of the Divisional staff in supporting the missions in orbit, almost all staff members have pursued their own scientific research. In the absence of new hardware projects, other than those listed above, such activities have now concentrated on data analysis. The prime research fields of the divisional staff are in solar physics (Section 2.5), heliospheric physics Figure 3.2.2/1: An example of quasi-periodic (Section 2.6) and space plasma physics (Section 2.6). (~40-min period) radio bursts from Jupiter, detected The combined effort of RSSD staff in scientific data by URAP on Ulysses in October 2003. (Courtesy analysis has been supported by an active research fellow R.J. MacDowall) programme.

3.2.2 Ulysses

Ulysses is an exploratory mission being carried out jointly by ESA and NASA to study the properties of the interplanetary medium and solar wind in the inner heliosphere as a function of heliographic latitude and solar activity. The mission also focuses on the dust and gas components of the local interstellar medium that gain access to the heliosphere inside the orbit of Jupiter. The European-built Ulysses spacecraft was launched by the Space Shuttle on 6 October 1990, and a Jupiter gravity- assist in February 1992 deflected it into its final high- inclination heliocentric orbit. Major mission milestones to date include the south and north polar passes at solar minimum (1994/95) and again at solar maximum (2000/01). Following a distant encounter with Jupiter in February 2004 and aphelion passage in June 2004, Ulysses is now heading south prior to the third set of polar passes, in 2006/07 (south) and 2007/08 (north).

Scientific highlights during the reporting period included Figure 3.2.2/2: Ulysses observes ions from Comet observations of quasi-periodic radio bursts from Jupiter, McNaught-Hartley trapped inside a CME. Earth’s the most distant observations to date of dust streams from orbit is shown for reference. (Courtesy G. Gloeckler) Jupiter (Fig. 3.2.2/1), observations of the effects of the October/November 2003 violent solar outbursts at the orbit of Jupiter, and remote observations of cometary ions trapped in a CME (Fig. 3.2.2/2). switched on on a rotating basis. Starting in October 2004, A joint ESA-NASA Mission Operations Team at JPL the nominal ground station coverage via NASA’s Deep conducts spacecraft operations. A major priority during Space Network was reduced from 70 h to 35 h per week. the reporting period was to ensure that critical elements This reduced coverage, introduced as a result of the 2003 of the hydrazine system used for attitude control Sun-Earth Connections Senior Review in NASA, will remained above freezing. The low temperatures were the last for 2 years. Within these constraints, the spacecraft combined result of the diminishing power available from and payload are operating very well. the RTG power source and the large distance from the Sun. The ensuing power and thermal constraints required On the programmatic side, a major achievement was the the introduction of a power-sharing plan for the scientific approval by ESA’s SPC in February 2004 of funding to payload whereby a core set of instruments is operated continue spacecraft operations until March 2008. This continuously and a subset of the remaining payload is mission extension, the third for Ulysses, will enable

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measurements to be acquired up to and including a third set of polar passes. The scientific rationale for this is the desire to have out-of-ecliptic observations covering as much as possible of a complete Hale (22-year) solar magnetic cycle. Furthermore, the launch in 2006 of NASA’s twin STEREO probes will create a unique opportunity for multi-spacecraft observations during Ulysses pole-to-pole transit in 2007. Funding on the NASA side for 2007-2008 will be decided at a Senior Review in 2006.

During the reporting period, the ESA RSSD Mission Manager, together with his JPL counterpart, provided scientific advice to the operations team on all mission aspects and co-chaired the Science Working Team (SWT) meetings. In addition, the Mission Manager co- chaired the corresponding ESA-NASA Joint Working Group (JWG) meetings at which the overall policy issues related to the mission are discussed. Four JWG/SWT meetings were held in 2003-2004, two in Europe and two in the USA. A major topic of discussion at recent SWT Figure 3.2.3/1: Cover of the July 2004 issue of meetings has been the implementation of payload power- National Geographic, which includes the 32-page sharing. As part of his Project Scientist duties, the story ‘The Sun: Living with a Stormy Star’. Mission Manager assisted in the organisation of special sessions related to heliospheric research at international scientific meetings. Two collections of papers and a major review article, all focusing on the results from the recent solar maximum solar passes, appeared during the the prestigious Laurels for Team Achievement Award of reporting period. Individually, the Ulysses investigators the International Academy of Astronautics (IAA). The continued to publish prolifically, with more than 120 award recognises both the outstanding achievements in papers appearing in 2003-2004. designing, building and operating the mission, as well as the science it has performed. The Ulysses Data Archive is maintained at ESTEC by a small RSSD Ulysses team and is mirrored at JPL. SOHO is a busy observatory, with many coordinated Ulysses data are also archived by NASA at the National observations (covering well over half the observation Space Science Data Center (NSSDC), and form part of time) involving different instruments as well as ground- the Planetary Data System (PDS) archive. During the based observatories and other spacecraft. reporting period, key activities included the acquisition of additional sets of high-resolution time data, and the The coordination of science operations by the RSSD porting of the archiving software from the current VMS Project science team focuses on maximising the science system to Windows and UNIX platforms. output of the mission on both short and long time scales, serving current interests as well as possibilities for future analysis by facilitating requested and ad hoc collabora- 3.2.3 SOHO tions. It also involves identification and resolution of technical issues under a variety of operational situations. SOHO is a mission of international cooperation between ESA and NASA to study the Sun, from its deep core to After showing signs of degradation in May 2003, the the outer corona, the solar wind and its interaction with azimuth drive of the high-gain antenna was parked in an the interstellar medium. SOHO has provided the first optimal position in June 2003. Coupled with 180° images of structures and flows below the Sun’s surface spacecraft rolls twice per 6-month orbit, the parking and has identified the source regions and acceleration position introduces keyhole periods of 2-3 weeks every mechanisms of the fast solar wind. It has revolutionised 3 months, when the low-gain antenna must be used with both our understanding of solar-terrestrial relations as 34 m or 70 m DSN stations. Low availability of such well as our space weather forecasting capabilities by stations causes about 40% loss of telemetry during such providing a continual stream of images of the dynamic keyhole periods. Careful planning to take full advantage solar atmosphere, extended corona and activity on the far of all on-board recording capabilities has still made it side of the Sun. possible to ensure near-continuous time series for the GOLF and VIRGO instruments during the last three In September 2003 the SOHO Team was presented with keyholes (winter 2003 – autumn 2004), thanks to their

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doubly redundant telemetry streams. Concurrently, an and embassy staff, and several film crews making onboard software patch was developed by Saab Ericsson documentaries on the Sun (e.g. Discovery Channel) were Space to record only selected telemetry packets. The supported. patch was successfully tested during the last keyhole and will be used for future keyholes, hopefully ensuring continuous helioseismology data from the GOLF, 3.2.4 Cluster VIRGO and MDI instruments. The four Cluster satellites were launched in pairs on two The Internet-based approach to science operations Soyuz rockets in July and August 2000, into a polar orbit coordination and data dissemination that SOHO has targeting some of the most important near-Earth regions: pioneered since 1994 is still the cornerstone of the SOHO solar wind, bow shock, magnetosheath, cusp, magneto- information and data system, and it continues to grow: an pause, plasmapause and magnetotail. By providing average of almost 16 million requests were received, and unique 4-point measurements in the Earth’s magneto- more than 2700 GB of data were transferred from the sphere, Cluster is revolutionising our understanding of SOHO servers every month during the last 2 years (up the dynamics of space plasmas. Originally funded to from 7 million requests and 950 GB during the last operate for 2 years, and now in an extended mission period). Over the mission lifetime, the SOHO web phase until December 2005, the spacecraft and payload servers have received a total of 617 million requests and continue to perform well and are expected to do so for have delivered > 91 TB of data. several years to come. In order to fully realise the potential of the mission, a second extension will be Anticipating a reduction in the on-site staffing, emphasis proposed to the SPC early in 2005. has been placed by the RSSD Project Science team on streamlining all data-handling processes for automation Discoveries made by Cluster have demonstrated the and ease of maintenance. The system encompasses critical importance of making measurements on different processing, archiving, cataloguing, searching and spatial scales. For example, the substructure of the distribution of level-zero telemetry, ancillary data sets magnetopause reconnection layer on electron scales of and science processed data, as well as real-time products ~20 km; filamentary structure within the cusp over scales and general web pages for the public. of only 100 km; density irregularities at the plasmapause, including plasmaspheric plumes, over scales from The SOHO teams have set a new standard in providing 100 km to several 1000 km; observations of a tail current images and results through the World Wide Web, capturing the imagination of the science community and the general public alike, and inspiring students of all ages to seek more information about the Sun. SOHO images have become stock footage for news organisations Figure 3.2.4/1: 3-D cut-away view of Earth’s around the world. magnetosphere. The curly features sketched on the boundary layer are Kelvin-Helmholtz vortices SOHO maintains its high profile in the international observed by Cluster. They originate when the two media thanks to continued efforts to improve the SOHO adjacent flows travel at different speeds; in this case, web pages and by expanding the network of personal the magnetospheric flow on one side and the solar media contacts. SOHO images were featured on the front wind flow on the other. (Courtesy H. Hasegawa, covers of many popular science magazines, including the Dartmouth College) cover of the July 2004 issue of National Geographic, which featured a 32-page story on recent developments in solar science and space weather. Members of the SOHO RSSD Project Scientist Team worked closely with National Geographic staff, reviewing the article and consulting on the artwork and images.

Several special showings of the IMAX film Solarmax were arranged by the RSSD Project Science team, e.g. at the meeting of the American Metrological Society in Seattle and the International Astronautical Congress in Vancouver, Canada. The latter supported ESA’s education support programme at this conference. We have also supported ILWS exhibits at the United Nations in Vienna and New York with SOHO materials, models and real-time images. Numerous VIP tours to the SOHO operations facilities were hosted for European ministers

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sheet only ~0.1 RE thick; the scale of the quasi- Archive (CAA), funded by ESA, NASA and member perpendicular shock transition on the ion gyroradius states. From early 2005, this archive will provide free scale; propagating wave modes in the magnetotail with access for the entire scientific community to the full, wavelengths of several RE; and huge vortices on the calibrated, high-resolution Cluster data set (CSDS flanks of the magnetosphere. contains only low- and medium-resolution data). CAA will be a unique research tool for the worldwide During the last 2 years, the RSSD Project Scientist team magnetospheric science community for many years to has devoted a large part of its time to the operations of come. It consists of a core RSSD team with four people the Cluster mission and the distribution of data to the that will prepare and populate the database at ESTEC, scientific community. It chaired seven Cluster Science and one person in each of the 10 European PI teams to Operations Working Group meetings and four Science calibrate and deliver the data to the archive. The first Working Team meetings. Five Cluster workshops were CAA data were delivered before the end of 2004 and then organised between October 2002 and October 2004, to 2 years’ worth of data will be delivered annually. discuss Cluster data and prepare the plan for the spacecraft separation strategy. A special issue of Annales Geophysicae was published in July 2004 with Cluster 3.2.5 Double Star results presented during the 5th Cluster workshop in Orleans (F). A special ISSI book is being finalised on The two Double Star satellites were launched on Cluster results on the dayside boundaries of the 29 December 2003 and 25 July 2004 aboard Chinese magnetosphere Long March 2C rockets. Double Star is a China-ESA programme to study the effect of the Sun on the Earth’s The Cluster Science Data System (CSDS), which has environment. The Chinese National Space Administra- been specially developed to allow fast easy access to the tion built, launched and is operating the two satellites. Cluster physical parameters measured by the ESA provided eight European instruments, the support instruments, has been running smoothly since February for their integration in Europe, their science operations, 2001. Nine national data centres, in Austria, China, and the acquisition of 4 h of data per day using the ESA France, Germany, Hungary, Netherlands, Sweden, VILSPA II ground station. The orbits are designed to United Kingdom and the United States constitute the maximise collaboration with Cluster such that both CSDS. They are funded by their national agencies; ESA small-scale and large-scale observations of the through the Project Scientist team coordinates the system magnetosphere are collected simultaneously. and provides the user interface to allow a scientific user to query, retrieve and manipulate the data coming from The satellites and instruments are working well although all instruments. User access to the data system is a few anomalies occurred shortly after the launches. On gradually increasing every month. The average TC-1, one solid boom holding the STAFF (magnetic download by scientific users over a recent 3-month wave detector) did not deploy owing to a problem with a period was > 5.8 Gbytes/month. The physical parameters pyro-actuator. STAFF observations are contaminated by database contains more than 30 Gbytes. a strong background noise. Special software techniques are being developed to minimise this effect. In addition, A Joint Science Operations Centre (JSOC), at the a strong magnetic disturbance from the spacecraft solar Rutherford Appleton Laboratory (UK), was established array is observed by the FGM (magnetometer). The FGM to support the Project Scientist in coordinating the software has been modified to limit the effect. complex science operations of the mission. Its five main tasks are payload commanding, payload health On TC-2 the boom pyros were exchanged and the solar monitoring, planning and information dissemination, panel cabling modified, precautions that avoided the data management system delivery and maintenance, and problems encountered with TC-1. Unfortunately, both the CSDSweb (quicklook) delivery and maintenance. the main and redundant attitude orbit control computers The Cluster quicklook plots are available at failed within 2 weeks of launch. This lost the attitude http://www.cluster.rl.ac.uk/csdsweb/. JSOC has perform- control capability on the polar satellite; however, the ed its tasks successfully since the beginning of the attitude can be determined using the European- provided mission. A very active period for JSOC is during the magnetometer data. Spin axis pointing and spin rate are constellation manoeuvres, when instruments have to be nominal. Although the spin rate is expected to remain switched-off during thrusters firing and switched on stable over the mission, the spin axis is expected to drift again afterwards. Constellation manoeuvres consist slowly. Present drift predictions indicate that at least a typically of 50 thruster firings from a few seconds up to 1-year mission lifetime can be achieved for TC-2 without more than 1 h during a 1.5-month period and take place problems. once a year. 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3.2.6 Solar Orbiter

The key mission objectives of the Solar Orbiter mission are: to study the Sun from close up (48 solar radii, or 0.22 AU), permitting investigation of the solar surface at high spatial resolution; to study the links between the solar surface, the corona and inner heliosphere during perihelion passes that are matched to the Sun’s rotation; and to provide images of the Sun’s polar regions from heliographic latitudes in excess of 30°. Solar Orbiter was selected as an ESA Flexi-mission in 2000, and reconfirmed in 2004 to be implemented as a common development with the BepiColombo mission to Mercury. Launch is foreseen for either October 2013 or May 2015.

The model payload comprises the following state-of-the- art packages of heliospheric in situ and solar remote- sensing instruments: Plasma Package (ion and electron solar wind analysers); Fields Package (radio and plasma wave analyser, magnetometer); Particles Package (energetic particle detectors, interplanetary dust detector, Figure 3.2.5/1: Launch of the second Double Star solar gamma-ray and neutron detector); Solar Remote TC-2 satellite on 25 July 2004 from Tai Yuan. Sensing Package (visible-light imager and magneto- graph, EUV full-Sun and high-resolution imager, EUV spectrometer, X-ray spectrometer/telescope, corona- graph). mission, including the science operation of the European instruments and preparation of the data system. The In 2003, the Study Scientist formed a Science Definition Science Working Team is co-chaired by the Chinese and Team (SDT) that was given the task of reviewing and ESA Project Scientists. The RSSD Project Scientist refining the scientific goals to achieve a well-balanced co-chaired four DSP SWT meetings and four data system and highly focused mission. SDT meetings were held in implementation working group meetings between ESTEC in May and September, resulting in a Solar October 2003 and October 2004. Orbiter Science Requirements Document (Sci-RD), issued in December 2003. Throughout 2004, the Study Since the European contribution to Double Star consists Scientist supported the assessment activities lead by of Cluster spare or duplicate instruments, it was decided SCI-A, in particular with respect to payload-related to re-use as much as possible the data system developed issues, and maintained the interface to the external for Cluster. The European Payload Operation Centre scientific community. Other activities included presenta- (adapted from Cluster JSOC) updated the data tions at international meetings, and coordination efforts management system for Double Star and coordinates the in the framework of NASA’s Living With a Star commanding of the European payload. Similarly, the programme (specifically, Solar Probe and Sentinels), and Double Star Data System (DSDS), a subset of the Cluster the International Living With a Star initiative. data system, distributes data to the user community. The national data centres involved in the distribution of data are in Austria, China, France, The Netherlands and UK. 3.2.7 Solar-B The quicklook plot system has also been adapted to display the data from all instruments, European and Solar-B is a solar physics mission, led by ISAS, intended Chinese, a few days after data acquisition and is running to follow on from the highly successful Yohkoh at the Austrian data centre (http://edds02.iwf.oeaw.ac.at/ (Solar-A) mission. The payload comprises a coordinated dsdsweb). TC-1 operations began in March 2004 and for set of optical EUV and X-ray instruments to investigate TC-2 in early October 2004. The coordinated dual the interaction between the Sun’s magnetic field and satellite mission is planned to last at least until July 2005. corona. The final goal is to reach an improved under- standing of the mechanisms leading to solar variability The second Double Star workshop took place in Beijing and ultimately controlling the energy output. These on 8-10 November 2004. More than 50 papers, the processes are the main driving forces behind what is majority combining both Double Star and Cluster data, generally referred to as space weather. Solar-B is were presented during the 3 days. Very promising results scheduled for a launch in August 2006. emerged on magnetic reconnection, bow shock structures and surface waves on the magnetosphere. After having received an invitation to collaborate with

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ISAS on Solar-B, particularly on data analysis and 3.3 Planetary Missions Division operational ground support from a polar station, ESA received SPC approval in early 2003 to invest > 7 Meuro 3.3.1 Introduction and overview in providing an additional Norwegian ground station on Svalbard. This station, because of its high latitude, will The past 2 years were probably the most exciting period be able to provide downlink for almost all Solar-B passes for planetary science in Europe, and the staff of the in its Sun-synchronous low-altitude polar orbit. Closely Division played a major role in supporting the linked to the provision of the station, ESA is also community to contribute to this success. Three missions negotiating with Norway for a European data centre for were launched: Mars Express, SMART-1 and Rosetta. the full Solar-B database, supplying Europe’s solar Huygens was released from Cassini and completed its physics community with rapid access to the huge mission to study Titan’s atmosphere and surface on amounts of data expected from this mission. 14 January 2005. Venus Express, which was approved end-2002, is in its final stages of testing and will be ready ESA’s involvement in Solar-B can be considered as an for launch in November 2005. It was a demanding time initial ESA contribution to the International Living With for the Project Scientists and their teams, supporting the a Star Initiative (ILWS), which aims to increase our project reviews, monitoring the payload development understanding of how the variability of the Sun affects and testing, and preparing the commissioning activities the terrestrial and other planetary environments, in the jointly with the Experiment Teams and the Mission short- and long-terms. In particular, the effects of solar Operations Team at ESOC. variability on mankind and society are being investigated. The Division is responsible for the coordination of all payload operations for Mars Express, Rosetta and B. Fleck acts as the prime ESA contact person with SMART-1. The supporting facilities for these missions respect to JAXA/ISAS, and R. Marsden and H. Opge- have been developed and the various teams have taken noorth represent ESA in the ILWS steering committee, over responsibility for planning the operations of their which has been chaired by the latter for the last 2 years. specific mission. In addition to Huygens, the Division took over the responsibility for the mission management, during the exploitation phase, of Mars Express, Rosetta and SMART-1.

The launch delay of Rosetta required an additional effort to define the new mission scenario, monitor the new target comet and demonstrate, in a unique team effort with the Project Team and the Rosetta Science Working Team, that we had defined a viable mission to the new target, 67P/Churyumov-Gerasimenko. In addition, the RSSD Project Scientist team had to support a long launch campaign for the second time.

The successful redefinition of the baseline mission scenario for BepiColombo by SCI-A was supported by the Project Scientist. Unfortunately, the Mercury Surface Element had to be dropped for programmatic reasons. A successful mission profile involving two orbiters (one ESA and one Japanese) was developed that ensured a major science return could be maintained. The RSSD Project Scientist was heavily involved in maximising this science return from the low-resource model payload designed within SCI-A, as well as in the payload selection process and the accompanying negotiations to secure payload funding.

In close collaboration with the Science Operations and Data Systems Division, the ESA Planetary Science Data Archive was created using the tools developed for the archives for ESA’s astrophysics missions. The first data sets ingested were the results from Giotto and the Giotto Extended Mission and from the ground-based observation campaign of the Rosetta targets. The archive sec3.qxd 7/15/05 10:01 AM Page 71

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is operational and waiting for the data sets from the first 6 months in Martian orbit from the Mars Express instruments.

3.3.2 Cassini/Huygens

The Cassini-Huygens mission is a joint undertaking between NASA, ESA and ASI. It is designed to explore the Saturnian system and all its elements: the planet and its atmosphere, rings and magnetosphere, and a large number of its moons (icy satellites), in particular Titan, Saturn’s largest moon. The Cassini-Huygens spacecraft, launched in October 1997, was placed in orbit around Saturn on 1 July 2004. The interplanetary voyage of Figure 3.3.2/1: The Cassini-Huygens trajectory on 6.7 years included gravity-assists at Venus (April 1998 arrival at Saturn. The Huygens mission was carried and June 1999), Earth (August 1999) and Jupiter out on the third revolution around Saturn. Three (December 2000). Results obtained during the cruise Titan flybys were achieved before Huygens’ mission: phase and the planetary flybys have appeared regularly in T0 (2 July, closest approach 300 000 km); Ta the scientific literature. (26 October, 1174 km); Tb (13 December, 1200 km). The probe mission was carried out on Tc on Saturn approach science started in early 2004. It included 14 January 2005. More than 40 Titan flybys are a coordinated set of observations of Saturn’s auroras by expected to follow Huygens’ mission before the HST while Cassini monitored the solar wind conditions. orbiter’s mission ends in mid-2008. Remote sensing observations of the entire system during the approach phase allowed the study of what already appears to be a highly variable and dynamic system where all elements are interacting (Saturn and Titan atmosphere, rings, moons, magnetospheric plasma, dust). (INMS) on 26 October, as well as the two stellar Nineteen days before Saturn Orbit Insertion (SOI), a occultation data sets on 13 December by the UV Imaging 2000 km flyby of the large outer moon Phoebe was Spectrometer (UVIS), allowed, in combination with the performed. Spectacular observations indicated that ground-based data set obtained during the Titan Phoebe is most likely a captured object from the outer occultation in mid-November 2003, the upper Solar System. During SOI, Cassini-Huygens went atmosphere model of Titan’s atmosphere to validated and through a gap between the F- and G-rings. Unique ring updated, a key step in the validation of the performance observations were obtained by several remote-sensing of Huygens mission. instruments, including the Imaging Science Subsystem (two cameras) and various optical spectrometers During the reporting period, the RSSD Mission covering the UV to the far-IR. The fields & particles Manager/Project Scientist, supported by the Huygens instrument complement has begun to study the global Mission Team which is distributed across ESTEC, morphology of Saturn’s magnetosphere. Lightning was ESOC, NASA/JPL and Industry, assumed the overall detected in Saturn’s atmosphere by the plasma wave responsibility for the implementation of the Huygens sensors, indicating some change in its characteristics recovery mission, which was completed in December since the Voyager observations. 2003 when the required Probe onboard software patches were uploaded and validated. In 2004, the work By the end of 2004, Cassini had performed three Titan concentrated on preparation activities for the Huygens flybys: 2 July (300 000 km closest approach), mission itself. Three major Huygens reviews were 26 October (1174 km) and 13 December (1200 km) conducted in 2003-2004. An Agency-wide Delta Flight (Fig. 3.3.2/1). The surface of Titan, ‘seen’ by three Acceptance Review was conducted on the recovery remote-sensing instruments (camera, VIMS, radar) is mission from December 2003 to February 2004. The revealing itself to be more complex, exotic and review identified the need to consolidate the entry heat geologically diverse than ever anticipated. The flux and heat load calculations, because recent work on atmosphere’s thick haze is a challenge for the optical radiation flux during entry into a methane-rich nitrogen remote-sensing instruments in reaching their best atmosphere had raised questions on the work done in the resolutions. Remote observations by the Composite early 1990s. A special effort began in April 2004 with the Infrared Spectrometer (CIRS) and the Visual Infrared Huygens industry team, NASA and Ecole Centrale de Mapping Spectrometer (VIMS) on 2 July and Paris, where there is unique expertise high-temperature 26 October, and in situ measurements in the upper plasma radiation spectroscopy. The work concluded in atmosphere by the Ion and Neutral Mass Spectrometer late November 2004, allowing the latest methane

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Figure 3.3.2/2: Updated Titan atmosphere profile Figure 3.3.2/3: VIMS image of Titan after Ta after the T0, Ta, Tb flyby data set. The update profile, observations. The expected Huygens landing site is represented by he thick purple line, falls within the shown. envelope of the engineering model used for the Huygens mission design.

space debris. In order to arrive at a realistic concept, the study focused on the tracking of Huygens during its concentration in Titan’s atmosphere derived from the descent to Titan. The initial study was closely followed early Cassini observations to be taken into account by the RSSD Project Scientist. It demonstrated that the (Figs. 3.3.2/2 & 3.3.2/3). tracking of Huygens was achievable. Following the positive outcome of the initial study, further work was An ESOC-led Delta Ground Segment Readiness done jointly by the Technical and Science Directorates Review was held in September 2004. The to develop a project for Huygens VLBI observations. recertification of the entry performance was one of the The ESA studies were led by the Joint Institute for major topics addressed in a Joint ESA/NASA Mission VLBI in Europe (JIVE), in Dwingeloo (NL). The main Risk Review (MRR), which was conducted from mid- goal was to measure the position of the probe during its October to mid-December 2004. The MRR gave the descent and on the surface to an accuracy of the order green light, on 16 December, to proceed with of 1 km with a time resolution of a few seconds. At the preparations for the probe’s release. Huygens was initiative of JIVE, radio telescope time was applied for successfully released from Cassini on 25 December and obtained as part of the regular AO process in the US 2004 at 02:00 UTC. Thanks to excellent pointing and and in Australia through peer-review proposals, which performance of the Spin and Eject Device, Huygens were highly ranked during the evaluation process. was targeted at the nominal entry angle of –65º. A series Altogether, 18 telescopes in the USA, Australia, Japan of optical navigation images of the probe was obtained and China were involved in the observations. Two test by the two Cassini cameras, which contributed to observations were conducted in late August 2004 (using refining the probe trajectory and to confirming that the Cassini transmitting in the X-band as the RF source), entry ellipse uncertainty was only 0.8º (3º requirement). and in mid-November 2004 (using Cassini’s Radio At the end of 2004, it was known that Huygens was Science S-band transmitter and Mars Express’ S-band well on its way to Titan for an entry on 14 January 2005 transmitter). Those test observations allowed the at 09:06 UTC (Fig. 3.3.2/4). Huygens team to debug and coordinate the complex observation plan and were key to preparing for the real Following an initial study within the ESA General Huygens observations. Studies Programme (GSP) in mid-2003, initiated by the Technical Directorate, a project was developed for tracking the probe using Very Long Baseline Huygens successfully landed on Titan on 14 January Interferometry (VLBI). The objective of the study was 2005. All science instruments performed well, yielding a to investigate synergies available between large data set of the moon’s physical and chemical properties. effective apertures for radio astronomy and the needs of The amazing descent panorama and superb pictures from space applications like data downlinks (MARS/Venus/ the landing site can be found on http://saturn.esa.int or Mercury landers and/or small orbiters) and monitoring http://saturn.jpl.nasa.gov sec3.qxd 7/15/05 10:01 AM Page 73

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Operations Centre (RSOC) and have a fully operational system ready for the payload commissioning that started shortly after launch. It is responsible for consolidating the command sequences for the operation of the science payload. These command files are submitted to the Rosetta Mission Operations Centre (RMOC) at ESOC. In addition, the Project Scientist Team team supported all Project Reviews and the official RSOC Reviews as part of the Rosetta Ground Segment validation and commissioning.

The payload commissioning was split into three periods – two periods immediately after launch until early June – and the Pointing and Interference Campaigns in September and Figure 3.3.2/4: Huygens Entry, Descent and Landing October 2004. For the last period, RSOC took scenario. for the first time full responsibility for preparing the payload operations. This required very close interaction and collaboration with the Experiment Teams. The system worked flawlessly and proved the readiness of RSOC.

3.3.3 Rosetta The Mission Commissioning Results Review on 3 December 2004 at ESOC concluded that all goals of On 2 March 2004 Rosetta was launched from Kourou the spacecraft and payload commissioning had been on an Ariane-5G+. After the delay from early 2003 achieved and that the mission was operational. From owing to the failure of the new Ariane-5ECA, the mid-October the spacecraft was in quiet cruise mode, the Project and the RSSD Project Scientist team, in close next big event being the first Earth gravity assist on collaboration with the Rosetta Science Working Team, 4 March 2005. studied alternative mission scenarios. These had to meet three basic requirements: preserve the scientific Subsequently, for the operational phase of the mission objectives of the mission, minimise the technical risks, the management of Rosetta was transferred from the and minimise the financial impact on the overall Projects Department to RSSD. Science Programme. A mission to comet 67P/ Churyumov-Gerasimenko was finally identified that met these requirements. The RSSD Project Scientist 3.3.4 Mars Express team, in collaboration with the scientific community, mounted an observing campaign to characterise the new Mars Express is ESA’s first planetary mission and was target in support of defining the new mission scenario. launched on 2 June 2003 from Baikonur Cosmodrome In parallel, technical activities proceeded at an aboard a Soyuz-Fregat. Following a 7-month journey, it increased pace in order to meet the new launch date of was inserted into Mars orbit on 25 December 2003. The February 2004. Fortunately, the Rosetta orbiter did not Beagle 2 lander was released on 19 December and require changes to cope with the new mission scenario. should have landed on 25 December; it was considered However, considerable effort was needed to to be lost following extensive searches by the NASA demonstrate the compatibility of the Philae Lander Mars Odyssey orbiter, terrestrial radio telescopes and design with the new target. Churyumov-Gerasimenko Mars Express itself. has a radius of 2 km, in comparison to the 0.6 km radius of the original target 46P/Wirtanen. The greater The Mars Express orbiter is designed to achieve the gravitational attraction will produce a higher following science objectives: touchdown speed on the nucleus. All these technical hurdles were overcome and Rosetta was ready to be — global high-resolution (10 m) photogeology; launched at the end of February 2004. After two brief — super-resolution imaging at 2 m/pix of selected areas; launch delays due to bad weather and a technical — global mineralogical mapping at 100 m resolution; problem, respectively, Rosetta was finally launched. — global atmospheric circulation and mapping of composition; The Project Scientist team used the 1-year delay to — study subsurface structure at km-scale down to the improve the implementation of the Rosetta Science permafrost;

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— study surface-atmosphere interactions; — study interaction of the upper atmosphere with the solar wind.

The RSSD Payload Support Team (PST) at ESTEC acts on behalf of the RSSD Mission Manager, in consultation with the Science Operations Working Group (SOWG). The Mission Manager is advised by the Project Scientist and the Science Working Team (SWT) on all matters related to optimising the mission’s scientific return.

The SOWG is composed of PI team representatives assigned to address all science operations issues. The Payload Operations Service (POS) at RAL (UK) is contracted to support the PST, the PIs and the Mission Figure 3.3.5/1: Venus Express in fully operational Operations Centre (MOC) in conducting efficient configuration. As the solar input at Venus is about operations of the mission’s scientific instruments. The twice that at Mars, the solar panels are shorter than POS develops, implements, tests and operates the system for Mars Express. and tools required to support Mars Express.

For the detailed planning and the transition to and implementation of the commanding of each instrument’s operations, POS interfaces with the MOC on one side, operate well at the high temperatures expected at Venus, and with the PI institutes on the other. The PST plays a and the size of the panels has been halved. The payload key role in coordinating all the required inputs, is composed of a selection of instruments from Mars respecting the mission constraints and safeguarding the Express, Rosetta and two newly built instruments. balance in the scientific return of the Mars Express instruments. Venus Express will be launched from Baikonur Cosmodrome by a Soyuz-Fregat into a direct transfer Up to the launch, the PST focused on preparing for trajectory to Venus. The journey to Venus requires about mission science planning and operations. A large effort 150 days. The operational orbit is a highly elliptic 24 h was spent on preparing the Master Science Plan, a polar orbit, with a pericentre altitude of 250-350 km and document describing the full range of Mars Express an apocentre altitude of 66 000 km. The observations science goals and mission planning, from global will be split between the pericentre region, where high- overview to full detail. Following launch, emphasis resolution studies of small-scale features will be carried shifted to understanding and coordinating the mission out, and near-apocentre and intermediate observations, and its constraints in order to arrive at an efficient and where global features will be studied. optimised mission planning process. This also involved the first example of ‘interplanetary networking’, in Activities within the Planetary Missions Division have which some data from the NASA Mars rovers were concentrated on three areas. The first is the organisation routed through Mars Express to Earth. and lead of the Science Working Team and the related meetings, with, as an important result, the refinement of The PST has also been active in preparing the the scientific objectives and the definition of principles requirements for the Mars Express science archive. It for selecting observations for the different phases of the was decided that the best way to implement the archive mission. The second is the definition and the set-up of the would be through the reuse of the technology and Science Operations Centre within the Division. The third software used for ISO (and later XMM-Newton). The is interfacing with the ESA project team, ESOC and the archive was expected to be online in early 2005. industrial contractors to follow the development of the different elements of the project closely.

3.3.5 Venus Express A somewhat new top-down approach has been taken to the formulation of the scientific objectives. The The development of the Venus Express (Fig. 3.3.5/1) objectives are formulated as a set of fairly wide fields of mission is progressing well and is on schedule for a interest or ‘themes’, where each theme is broken down launch on 26 October 2005. The spacecraft is based on into several sub-themes. The sub-themes in turn, are the Mars Express platform, with modifications to the broken down into a set of observations to be made, where thermal control to handle the more challenging the physical parameters to be observed are defined. The environment around Venus. The solar panels have been observations are distributed over the different phases of redesigned and now use modern-technology cells that the mission based on the importance of the specific

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conditions like illumination, repetition rate, conjunc- tions, eclipses and available downlink capability. For each phase, all measurements that address all aspects of the defined observations, and the individual instruments that make the measurements, are identified. In this way, full traceability exists in both directions: it can be seen directly which theme is addressed by a specific measurement and it can be verified that each theme is properly covered with an adequate set of measurements. The following Science Themes have been defined,

— Atmospheric Dynamics; — Atmospheric Structure; — Atmospheric Composition and Chemistry; — Cloud Layers and Hazes; — Radiative Balance; — Surface Properties and Geology; Figure 3.3.6/1: An example of the MMO and MPO — Plasma Environment and Escape Processes. forming part of the BepiColombo composite stack together with the SEPM and CPM. The organisation of the Venus Express Science Operations Centre (VSOC) has been defined and its interfaces to ESOC and to the individual PI institutes are in the final state of definition. Experience from previous missions, in particular Mars Express, Rosetta and October 2000 as the 5th Cornerstone mission. The SMART-1, is used to synthesise a design that is flexible Mission consists of two orbiters, the Mercury Planetary and maximises the efficiency of the limited resources Orbiter (MPO), which is 3-axis-stabilised and nadir available. A generic software package, MAPPS pointing, and the Mercury Magnetospheric Orbiter (Mapping and Planning for Payload Science) for (MMO), a spinning satellite. The MMO is being assisting in the planning process is under development provided by JAXA. ESA is responsible for the overall in-house. A first version was distributed to the PIs and BepiColombo mission design, including launcher, other potential users during a dedicated workshop. The spacecraft composite, propulsion modules, ground intention is that this package will contain all functions segment and the delivery of both spacecraft into their needed for the planning the science observations. It reads dedicated orbits, as well as for the MPO and its the individual instrument request files, analyses and operations. The severe reduction of the science budget checks the required resources and produces the files that after the Ministerial Conference in November 2001 are passed to ESOC for further transmission to the resulted in a mission reassessment process, which started spacecraft. in October 2002 with the aim of maximising the scientific performance through the optimisation of the The project has been progressing at an unprecedented payload complement, while reducing costs and pace since the start in 2002. The RSSD Project Scientist programmatic risk. The reassessment was performed by team has interacted with the project team, ESOC and SCI-A in close cooperation with the Planetary Missions industry by participation, mainly by the Project Scientist, Division (SCI-SB), and was completed in June 2003. in numerous meetings and by closely following and commenting on the progress. The areas of payload The mission scenario that emerged from the reassess- development, accommodation and operation, and ment was to carry the MPO and MMO together on a spacecraft performance and operations have been single launcher (Soyuz-Fregat 2-1B) in mid-2012 prioritised. In some cases, when of direct interest to the (Fig. 3.3.6/1). The transfer to Mercury will be based on science performance, the performance and characteristics Solar Electric Propulsion with a travel time of about of spacecraft subsystems have been monitored. 4.6 years. Upon arrival, the Solar Electric Propulsion Contribution has been made to all major agency-level Module (SEPM) will be jettisoned and the Chemical reviews for spacecraft and ground system, as well as to Propulsion Module (CPM) will provide the required all payload reviews. thrust for Mercury capture and orbit insertion (Fig. 3.3.6/2).

3.3.6 BepiColombo The orbiters are dedicated to the detailed study of the planet and its exospheric and magnetospheric environ- BepiColombo is an interdisciplinary mission to explore ment. The MPO investigations include high-accuracy Mercury through a partnership between ESA and JAXA. measurements of the planet’s interior structure and a The mission was selected and approved by ESA’s SPC in global multi-wavelength analysis of the surface at a

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neutral and ion particle analyser, limb pointing camera, magnetometer), thereby maximising the mission’s overall science return. Considerable effort by the RSSD Project Scientist team went into further optimising this scientific return by ensuring that specific measurements from individual instruments could be correlated and would complement each other. An example of this approach is the correlation of the surface morphology based on the optical camera instruments with the mineralogical and elemental composition of individual surface features as derived from the IR and X-ray imaging spectrometers. In addition, simultaneous measurements from the MPO and MMO will resolve spatial and temporal ambiguities in the exosphere and Figure 3.3.6/2: MPO and MMO orbiting Mercury. magnetosphere that would arise from single-point observations.

In November 2003 the SPC approved this new concept for MPO payload procurement through the endorsement resolution of 500 m, providing its morphology as well as of the BepiColombo Science Management Plan. As a elemental and mineralogical composition. Thus surface result, the Request for Proposals for IFEs was issued on morphology will be correlated with surface composition. 26 February 2004; 20 proposals for the MPO payload Together with the MMO, it will provide the detailed were received. On 30 September 2004 the Payload structure of the magnetic field and a complete character- Review Committee recommended an MPO payload isation of Mercury’s exosphere. The MPO orbit produces complement for selection that reflects the Reference optimal coverage of the polar regions. Hence the material Payload. Considerable effort by the Project Scientist was of the radar-bright spots observed from Earth and required in support of the Payload Review Committee suspected to be either water ice or sulphur will be and subsequent negotiations with national funding identified. The detection of sulphur would strongly agencies and potential instrument consortia. As a result, support the presence of at least a partially molten core. with the payload selection process now complete and the mission deep into its definition phase, BepiColombo is At the start of the reassessment the Project Scientist, in now well placed for a launch in mid-2012. Arrival at close collaboration with the external Science Advisory Mercury and the start of the science exploitation phase is Group, formulated the detailed science requirements for expected for early 2017. the MPO scientific payload. In cooperation with the science community, these agreed requirements were then translated by SCI-A personnel into requirements on 3.3.7 SMART-1 instrumentation, which served as the basis for the development of the overall payload architecture. Specific SMART-1 was launched by Ariane-5 on 27 September science teams coalesced around particular themes of 2003. The commissioning of the spacecraft, its ion MPO measurements, such as imaging, IR-spectroscopy/ engine and instrument functional checks were completed radiometry, laser altimetry, UV/X-ray/gamma-ray/ during the first few weeks after launch. SMART-1 had to neutron spectroscopy, radio science, magnetic field and travel through the inner radiation belts, during which particle measurements, in order to develop the scientific very violent solar flares in October-November 2003 thrust of the mission. This effort resulted in a rather novel made the operation of the startrackers and the ion-driven payload concept based on a high level of integration. The spacecraft very difficult. The instruments were resultant MPO reference payload no longer consisted of commissioned in February 2004 and the first images and individual instruments, but of the front ends of these spectra from the Earth and the Moon were obtained. instruments (IFE), which share common subsystems After an eclipse period in March 2004, the spacecraft such as data processing, electronics and power. In expanded its spiral towards the Moon, until the lunar addition, advantage was taken of the fact that new resonant approaches on 19 August (when SMART-1 was technologies and miniaturisation techniques have been closer to the Moon than to Earth for the first time), on developed in recent years, which allow alternative 27 September and again on 12 October 2004. approaches in instrument design and increased perform- ances with lower use of precious resources (mass, power, SMART-1’s science objectives include studies of the etc.). This new payload concept led to a significant chemical composition of the Moon, of geophysical reduction in the mass of the reference payload which in processes (volcanism, tectonics, cratering, erosion, turn allowed for the inclusion of additional instruments deposition of ices and volatiles) for comparative (thermal-IR mapping spectrometer and radiometer, planetology, and high-resolution studies in preparation sec3.qxd 7/15/05 10:01 AM Page 77

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Figure 3.3.7/2: Images taken by SMART-1 during the lunar approach phase. The right image shows a slice of the Moon’s far side and north pole; this was seen for only the second time in the history of lunar exploration.

Figure 3.3.7/1: First image of Europe obtained by AMIE, from 70 000 km in July 2004. This began a series of synoptic Earth images for camera operation validation and calibration.

for future lunar exploration. The results could provide new insights into topics such as the accretion processes that led to the formation of rocky planets, and the origin Figure 3.3.7/3: Mosaic view of crater Pythagoras and evolution of the Earth-Moon system taken by AMIE on 29/30 December 2004 from an altitude of 4000 km. The SMART-1 science payload, with a total mass of 19 kg, features many innovative instruments and advanced technologies such as a miniaturised high- resolution camera (AMIE) for lunar surface imaging, a near-IR point-spectrometer (SIR) for lunar mineralogy ESOC, have been planning payload operations for the investigation, and a very compact X-ray spectrometer cruise phase and the first part of lunar phase. (D-CIXS) with a new type of detector and micro- collimator that will provide fluorescence spectroscopy The SIR IR spectrometer showed nominal performance and imagery of the Moon’s surface elemental when it measured the first near-IR space spectra of the composition. Moon in the range 0.9-2.5 µm. It also measured, by comparison, Earth reference spectra with atmospheric The cruise and lunar approach demonstrated a number of absorption. The comparison between lunar spectra has technologies (spacecraft, navigation, operations and demonstrated the ability of the instrument to distinguish instruments) that will be useful for the future. The the mineralogy of different areas on the Moon. mission’s prime objective, to demonstrate Solar Electric Propulsion, has been fulfilled. The RSSD Project AMIE has achieved a number of Earth pointings Scientist and support team, together with the Science and (Fig. 3.3.7/1) which have been used not only for Technology Operations Coordination (STOC) centre at educational and outreach purposes, but also to measure

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scenes of planetary interest using various colour filters 3.4 Fundamental Physics Missions Division (geologic features such as volcanic terrains). It has also observed the Moon at different distances and phases to 3.4.1 Introduction and overview validate the instrument performances and exposure times (Fig. 3.3.7/2 & 3.3.7/3). The Project Science team has The main activities in the Fundamental Physics Missions been heavily involved in the planning and execution of Division fall into three areas: direct detection and these operations during this early preparatory phase. observation of gravitational waves, high-precision tests of the Equivalence Principle (EP), and fundamental SMART-1 has been the only mission in lunar orbit since physics applications of laser-cooled atoms. it was captured by the gravity field on 15 November 2004. Beyond its remaining primary science objective, In the first area, two missions are supported by the the mission provides, both for ESA and Europe, an Division: LISA (Laser Interferometer Space Antenna) excellent strategic position from which to contribute to and LISA Pathfinder (formerly SMART-2). LISA is a future international lunar exploration collaborations with mission to detect and observe gravitational waves, jointly approved missions (Lunar-A, Selene, Chandrayaan-1, undertaken with NASA. LISA Pathfinder is a technology Chang’E, Lunar Reconnaissance Orbiter, Moonrise), and mission, aimed at demonstrating and validating key possibly within the framework of the new NASA technologies for LISA. During most of the reporting Exploration initiatives. period both missions were supported by an RSSD Project Scientist. In July 2004, ESTEC hosted the 5th Inter- By the end of 2004, more than about 110 papers related national LISA Symposium, organised by the LISA to SMART-1 had been published in the scientific Project Scientist. Various other workshops and meetings literature, including 23 refereed papers. There is a large associated with LISA and LISA Pathfinder took place public interest, as indicated by the media response, during the reporting period. articles and the web presence that showed Europe-wide visibility for SMART-1 science and technology. In the second area, the Division supports the Microscope mission. This is a CNES/ESA collaborative mission to test the EP in space, with a launch by the end of 2007.

The third area includes the Atomic Clock Ensemble in Space mission. ACES is under development for flight aboard the ISS, led by the Directorate of Human Spaceflight, Microgravity & Exploration (D/HME); the Division provides support in the form of a Project Scientist.

3.4.2 LISA Pathfinder (formerly SMART-2)

LISA Pathfinder (LPF) is primarily intended to demon- strate the key technologies for the LISA mission, especially the performance of the inertial sensors that cannot be tested on the ground. To this end, LPF will accommodate a LISA Technology Package (LTP), provided in large part by European institutes and industry, and a Disturbance Reduction System (DRS) that is very similar to the LTP and has the same goals but is provided by US institutes and industry. LTP and DRS will be accommodated on a single spacecraft, injected into an L2 halo-orbit. The projected mission duration is 180 days, shared between LTP, DRS and a joint operational mode. The mission goals for the LTP are:

— demonstrating drag-free and attitude control in a spacecraft with two proof masses in order to isolate the masses from inertial disturbances. The aim is to demonstrate a performance on the order of 10–14 m/s2/Hz1/2 in the frequency band 1-100 mHz. The corresponding requirement for LISA is 10–15 m/s2/Hz1/2; sec3.qxd 7/15/05 10:01 AM Page 79

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— demonstrating the feasibility of performing laser — determine the population of ultra-compact binaries interferometry in the required low-frequency regime in the Galaxy; with a performance as close as possible to — probe the physics of the early Universe. 10–12 m/Hz1/2 in the frequency band 1-100 mHz, as required for LISA; LISA is an ESA/NASA collaborative mission with a — assessing the longevity and reliability of the launch foreseen in the 2012-2013 timeframe. By the end capacitive sensors, thrusters, lasers and optics in the of 2004, the project had entered the formulation phase space environment. (Phase-A), both in Europe and in the US. As a means of ensuring good communication between the engineers As the environment of the LPF spacecraft will be and scientists, regular meetings involving both sides take comparatively noisy (in terms of temperature place. They are held typically three times per year, fluctuations and magnetic disturbances) compared to the alternating between the involved centres, ESTEC, GSFC LISA environment, the mission goal for LPF is to meet a and JPL. The RSSD Project Scientist and his US performance of the inertial sensor that is a factor of 10 counterpart coordinate this activity. more relaxed than is required for LISA. This will allow validation of the models derived and extrapolated from To develop the requirements and design for the mission ground testing, and further extrapolation to the LISA and oversee the definition and development, helping to requirements. make trade-offs and mission design choices, NASA and ESA formed a LISA International Science Team (LIST) The LTP represents one arm of the LISA interferometer, in early 2001. LIST has 11 European and 11 US the distance between the proof masses is shrunk from members, including the respective Project Scientists. As 5 million km to 20 cm. As in LISA, the proof masses the project entered mission formulation at the end of fulfil a double role: they serve as optical references 2004, LIST met for the last time in December 2004 (‘mirrors’) for the interferometer, and as inertial before being disbanded. The science team will be references for the drag-free control system. The drag-free reinstated with modified membership and charter in 2005 control system aboard the LTP consists of the inertial to support the mission formulation phase. sensor, a propulsion system and a control loop using capacitive sensing in all six degrees of freedom, as well In July 2004, ESTEC hosted the biennial International as the interferometric readout system. LISA Symposium, organised by the RSSD Project Scientist. The Symposium attracted over 160 scientists; After completing the two parallel system-level industrial about 80 papers and posters were presented. studies in 2003, both of which were actively supported by the Project Scientist. the implementation phase began in May 2004. A major milestone was passed by the 3.4.4 ACES successful completion of the System Requirement Review (SRR) in November 2004. The Atomic Clock Ensemble in Space (ACES) mission consists of a caesium-atom clock and a hydrogen-maser clock aboard the ISS, plus laser and microwave links to 3.4.3 LISA ground stations. It is managed by D/HME; the RSSD Project Scientist provides scientific support and SCI-A The objective of the LISA mission is the detection and has assisted in technical development and programmatic observation of gravitational waves from super-massive issues. black hole coalescences and galactic binaries in the frequency range 0.1-100 mHz. The mission includes The ACES atomic clocks will be used as high-sensitivity three identical spacecraft, located at the vertices of an sensors for experimental tests of general relativity. The equilateral triangle with a baseline of 5 million km. The mission will contribute to fundamental physics centre of the triangle is in the plane of the ecliptic, 1 AU experiments in two distinct areas: from the Sun, and trailing Earth by about 20º. By measuring the distance between the spacecraft — an improved measurement of the redshift by interferometrically, the effects of a passing gravitational comparing ultra-stable clocks aboard the ISS and the wave can be registered. The orbital motion of the ground. The expected improvement over Gravita- detector allows information about the position and tional Probe-A is a factor 25. A number of auxiliary orientation of the gravitational waves’ sources in the sky measurements, such as a high-precision test of the to be obtained. The scientific goals of LISA are: Sagnac effect and the search for a possible anisotropy of the one-way speed of light (the theory — determine the role of massive black holes in galaxy of special relativity), can be performed with evolution; significantly improved precision; — make precision tests of Einstein’s Theory of — the search for a possible drift of the fine structure Relativity; constant. This constant characterises the strength of

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the electromagnetic interaction. The principle of the 3.5 Space Telescope Operations Division experiment is to compare the rate of atomic clocks (using different elements) as a function of time. The Space Telescope Science Institute (STScI) is responsible for all aspects of HST operations and, in Another test of relativity is to search for a possible particular, its scientific productivity. The Space anisotropy in the one-way propagation of light. The Telescope Operations Division of ESA contributes to this comparison of ACES clocks with ground clocks effort with the assignment of 15 ESA staff scientists and distributed worldwide will involve propagation of engineers. Some of the senior staff members have electromagnetic waves (both optical and microwave) in achieved significant leadership roles within the very different directions. Institute’s structure and are influential in key areas of the decision-making process. In addition, activities in support of the Hubble programme are carried out at the 3.4.5 Microscope ST-European Coordinating Facility in conjunction with ESO. The Division manages and leads these activities. Microscope (MICROSatellite à trainee Compensée pour l’Observation du Principe d’Equivalence) will be the first The Hubble programme is considered to be one of the mission to test the EP in space. The accuracy is 10–15, 2-3 most effective science missions ever, as rated by citations orders of magnitude better than possible on the ground or in science news media. It has one of the most recognised with lunar ranging. names and it is routinely cited as a major reason for increased worldwide interest in astronomy. The demand The payload comprises two differential electrostatic for telescope time is at a record high: more than six times accelerometers, one testing a pair of identical materials as much time was requested in Cycles 12 and 13 than (to provide an upper limit for systematic errors), one was available. testing a pair of different materials (the EP test proper). The test masses are freely falling concentric cylinders of Highlights of the HST programme include notable platinum and titanium, respectively. A violation of the EP enhancements in Hubble’s ability to produce world-class would manifest itself as a differential movement of the science, along with several achievements that gained proof masses with the orbital frequency of the satellite. worldwide attention. By every measure, HST has more science capability now than at any time in its lifetime. It The 3-axis stabilised, 193 kg satellite is planned for has achieved a discovery power 10 times greater than at launch in November 2007 on a shared Dnepr rocket into the beginning of the reporting period; ESA staff a Sun-synchronous, quasi-circular orbit at about 700 km contributed to all phases of this improvement. altitude. The drag by the residual atmosphere at orbital altitude and solar radiation pressure will be compensated The year of 2003 began with the tragic loss of the Space by a drag-free control system using Field Emission Shuttle Columbia and its crew of seven on 1 February. It Electric Propulsion (FEEP) thrusters. The required drag- ended with Hubble returning data of unprecedented free performance is 3x10–10 m/s2/Hz1/2 in the measurement quality and size as a result of the instrument upgrades bandwidth. made by Columbia’s crew on its last mission before the disaster, Servicing Mission 3B. In between, we saw the Microscope is a CNES/ESA collaboration: ESA’s share is continued growth of new ideas to use Hubble to the procurement of the FEEP thrusters. In return, ESA understand the cosmos, stimulated by its evolution as the will have full access to all FEEP flight data, which will world’s only serviceable space telescope. provide a valuable technology test in space for a whole suite of future astronomy and fundamental physics Hubble was designed for an entirely different set of missions. scientific problems than those it is solving now. Most of the original problems were solved in Hubble’s first decade, and it is now concentrating on the most important topics of today, none of which was developed or even imagined during Hubble’s design. Yet Hubble is now a dominant force in these new topics, in some cases uniquely so.

A primary responsibility of the Institute, and an activity led by RSSD staff, is to optimise the HST science programme. There are several major areas where the Institute adds value to the Hubble science programme, and these are naturally the focus of our improvement activities. These include stimulating the best possible science programme from the astronomy community via

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the proposal selection process, achieving the highest Programs were selected and some are already fully possible observing efficiency with the telescope, completed. As an example, investigators from providing timely and accurate calibration of the Hubble programmes such as the Great Observatories Origins data, stimulating the use of the Hubble data archive for Deep Survey have already published more than 30 papers additional scientific results, and providing tools to describing their results in prestigious journals. The high support the astronomical community’s use of the quality of papers based on Hubble observations reflects telescope and the archive. the high degree of competitiveness of the proposal process.

3.5.1 HST observation programme Another important change was the start of the Hubble Theory Program, funded as part of the Hubble Archival 2004 saw continued evolution in the process for selecting Research programme. The Theory Program stressed the the Hubble science programme. Major improvements importance of promoting theoretical research in were made, starting with Cycle 12, by reducing the time conjunction with major observing facilities, in order to between submitting proposals and starting observations improve the interpretation and understanding of the data in an observing cycle. The Phase I deadline was moved from these facilities. from September to the end of January, with observations starting in July. Shortening the time between proposal A successful policy-related topic has been the deadline and cycle start helps to ensure that recent implementation of the project to trade observing time findings have greater influence on new Hubble between Chandra and HST. Both the HST and Chandra observations, quickening the pace of scientific advance. Time Allocation Committees and users are very supportive of the concept. Observatory operations continued at high efficiency, averaging 43.7% for prime science observations and 48.6% for prime plus snapshot observations. Almost 60% 3.5.3 Instrument status of Hubble’s observing time in the current cycle uses the Advanced Camera for Surveys (ACS), installed during With the demise of the imaging spectrograph (STIS), SM3B in April 2002. The science data rate increased by there has been renewed interest in the slitless capabilities more than a factor of two following the installation of the of ACS, particularly in the UV. In-orbit calibration data new instruments and the ground system has been are being reduced and a further calibration programme is upgraded to respond to this increase challenge. HST is being planned to ensure that users are able to obtain high- also becoming easier to use, thanks to the new tools fidelity spectra from these modes. Wide Field Camera 3, produced at the Institute; migration of the archive data to planned to be installed in HST in the next servicing magneto-optical media was completed in 2004. Several mission, is undergoing ground testing and ECF is new software tools in support of HST operations were involved in the testing of the three grisms, one for the released: the Astronomer’s Proposal Tool (APT), near-UV and two for the near-IR. The possibility of StarView and the Space Telescope Grant Management applying the extraction software to FORS2 MXU data is Systems (STGMS) are fully operational. These activities currently being investigated and some daytime involved considerable effort by RSSD staff. calibrations have been taken to determine the feasibility of this approach.

3.5.2 Special HST programmes Under the Extension of the NASA/ESA MoU on HST, the Instrument Physical Modeling group continued the STSci and, in particular, the ESA staff have provided work on upgrading the HST STIS calibration pipeline leadership in several important science policy issues. (STIS-CE) with physical model-based modules. This Two new programmes, Treasury and Theory, added work is the consistent further development of the idea opportunities for scientists to do research with Hubble that calibration should make use of all the a priori and its data archives. The Hubble Treasury Program was information that is available from the physical principles started in Cycle 11 to stimulate science that might not that are embedded in the instrument’s design and naturally be encouraged by the existing process, and, in construction. Earlier testimony to the advantages of this particular, to promote the creation of important data sets concept is the stability of the ESO VLT UVES pipeline that one would regret not having obtained when Hubble and the several solutions provided for calibration is ultimately decommissioned. Treasury programmes shortcomings of the HST FOS spectrograph. address multiple scientific problems with a single, coherent dataset. The data sets carry no proprietary rights. Recently compiled metrics support the conclusion 3.5.4 The European Coordination Facility that papers from larger programmes, such as the Treasury Programs, have considerably higher scientific impact The Hubble ESA Information Centre (HEIC), which was than those from smaller programmes. Several Treasury established at ST-ECF, continued to supply material to sec3.qxd 7/15/05 10:01 AM Page 82

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the media and public. With a unique graphical expression data flows through sophisticated applications will be in all lines of products, high scientific quality and deomstrated, along with the use of ‘registries’ to harvest innovative distribution methods, the group has received astronomical databases. international recognition for their achievements.

On a yearly basis, HEIC receives more than 1000 3.5.5 HST operational status requests from press, public, educators, scientists and others for printed products, information and electronic The HST spacecraft is operating nominally, but 2004 saw products. Apart from the production of news and photo the demise of STIS on 3 August. To make up for the loss releases, innovative educational material, CD-ROMs, of scientific programmes, an additional 45 proposals brochures and posters, the HEIC has made important have been approved. These had already been rank- contributions. With up to 16 million hits/month, more ordered by the original Cycle 13 TAC. A number of than 125 000 individual visitors and up to 2 TB of data already-approved programmes that originally used STIS delivered, the http://www.spacetelescope.org website are in the process of being converted to use other belongs in the top group of astronomical outreach web instrument modes, most notably ACS/SBC. RSSD sites. Production of PR images from raw data continues. institute staff were actively involved in these complex This work has been based on HST data, but also images replanning issues. from ESA missions such as ISO, XMM-Newton and Integral, as well as the ESO VLT and others, have been As the observatory ages, and in the event it has to operate produced. This work is the most advanced of its kind in with only two gyros before a refurbishment can take Europe, producing high-quality artist’s impressions in place, preparations and development for the Two-Gyro 2-D and 3-D using highly optimised, very sophisticated Science Mode continue, involving a number of the RSSD software and hardware technique. High-quality video division staff. Extensive documentation and user material for news releases can be produced on timescales information is available at the STScI website, including of a few days. The online distribution of broadcast- a Two-Gyro Handbook and a ‘movie’ showing target quality video material enables broadcasters to use the availability under the somewhat more restrictive HEIC material in the evening news on the same day. scheduling opportunities with two gyros. Detailed simulations show that the impact on image quality from Slitless spectroscopy from space is competitive with jitter is substantially less than originally assumed, so that ground-based spectroscopy with large telescopes in those a voluntary entry into Two-Gyro Mode is now being spectral regions where the atmospheric background is discussed in order to preserve the lifetime of the high. HST has exploited this advantage and offers slitless currently operating four gyros. In support of this spectroscopy facilities on NICMOS and ACS. The ECF decision, detailed studies are under way to determine has developed expertise in all aspects of slitless how many orbits per week can be scheduled in two-gyro spectroscopy through support of the HST slitless mode as compared to using three units. On-orbit tests are spectroscopy modes. Through well-defined agreements planned for February 2005. with the STScI, the ECF has undertaken full cover for these instruments, from involvement in ground testing, to provision of software to extract wavelength and flux calibrated spectra, to user support. Currently, most effort goes into support for the ACS slitless modes, which cover the red grism for the WFC and HRC, a near-UV prism for HRC and two prisms for the far-UV SBC.

The Virtual Observatory (VO) project is evolving quickly. The current ECF archive development includes the creation of a database layer to host ancillary information (metadata, which fully describe the HST products through VO-compliant interfaces), and a database of instrumental characteristics (initially for ACS and WFPC2). The next VO science demonstration is scheduled for January 2005 at ESAC. The VO project is driven by its strategy of regular scientific demonstrations of VO technology, held on an annual basis. The next, based on input from the Science Working Group, will revolve around two science cases: ‘Rich Clusters of Galaxies’ and ‘Asymptotic Giant Branch to Planetary Nebulae Transition’. On the technical side, the use of powerful, distributed workflow processes driving sec3.qxd 7/15/05 10:01 AM Page 83

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3.6 Science Operations and Data Systems pipeline products from residual instrumental artefacts). Division Dedicated projects were undertaken, mainly in collaboration with the national centres, to reprocess 3.6.1 Introduction and overview observations of selected observing modes. As of October 2004, the archive includes 19 such data sets, some also The Science Operations and Data Systems Division obtained from the community, equivalent to 18% of the (SCI-SD) is responsible for the development and archive scientific content. For version 7, released in June execution of science operations for astronomy missions. 2004, a new approach was defined in the assessment of After completion of the in-orbit commissioning phase, the data quality, upgrading from a small set of technical the Division becomes responsible for overall project quality flags to a well-structured quality report, based on management: a Mission Manager is put in overall charge a total of 85 flags. and must ensure that operations are performed in the most efficient manner possible within the constraints; the The astronomical community continues to use the ISO Project Scientist remains responsible for ensuring archive intensively. There are now 1600 registered users maximum scientific return. The Division also provides and new users are still registering at a rate of about 10-15 support in data systems to the entire Department and has per month. In the first 6 years of use, the equivalent of long-term responsibility for the science archives of the nearly nine times the total number of scientific Directorate. The staff of the Division is located at ESAC observations in the archive has been downloaded, an and ESTEC. During much of the reporting period, there average monthly retrieval rate of around 13%. was also one staff member collocated with the Integral Science Data Centre in Versoix (CH). Another major activity has been the integration of the ISO archive into the Virtual Observatory. The ISO archive already incorporated many elements of 3.6.2 ISO interoperability with other popular astronomical archives. The ad hoc implementation of these function- The Infrared Space Observatory (ISO) was the world’s alities has evolved into a system complying with the new first true orbiting IR observatory. With a pointing standards set by the VO international community. ISO accuracy at the arcsec level and four highly sophisticated was one of the first archives to be part of the European scientific instruments, ISO explored the Universe at VO prototype, as demonstrated in January 2004. wavelengths of 2.5-240 µm with unprecedented sensitivity and capabilities. During its highly-successful Documentation has also been a focus of activity. The in-orbit operational phase from November 1995 to April legacy version of the five-volume ISO handbook, the 1998, ISO made some 30 000 individual scientific definitive standalone guide to the ISO mission and to its observations of all types of astronomical objects. All the data products, was published in early 2004 (as ESA data are available to the community via the ISO Data SP-1262) and distributed to the PIs of the ISO observing Archive – follow the links from the ISO home page at proposals and to some 300 astronomical libraries http://www.iso.vilspa.esa.es. The ISO project is well into worldwide. The proceedings of two recent conferences its Active Archive Phase, which will run until December organised by the ISO Data Centre were also released in 2006. This final phase is designed to maximise the the period, Exploiting the ISO Data Archive – Infrared scientific exploitation of ISO’s extensive IR database and Astronomy in the Internet Age (SP-511) and The to leave behind a homogeneous archive with refined data Calibration Legacy of the ISO Mission (SP-481). products, as a legacy to future generations of astronomers. The ISO Active Archive Phase Mid-Term Review was held in June 2004. The Board, composed of external data RSSD has the cradle-to-grave responsibility for ISO providers and users, was impressed with the scientific operations and, from the end of the achievements of the ESA and National Data Centres over commissioning phase, overall responsibility for the the previous 2.5 years. Their recommendations focused project. The Division has a team of staff and contractors, on making ISO data and results as widely available as led by the Project Scientist, in ESAC. Activities of this possible, by (i) concentrating the activities during the team include maintaining the central data archive, remaining 30 months on maximising the content and providing expert support to the community across all visibility of the Highly Processed Data Products, (ii) instruments, and coordinating activities with the various continuing with the integration of the ISO archive into national ISO centres. the VOs, (iii) ensuring prompt publication of the planned special issue of ISO Space Science Reviews, a 400-page Archive maintenance and improvement activities have book reviewing the results of ISO. continued. Version 6 of the ISO Data Archive, released in July 2003, upgraded the functionality associated with, In the 2003-2004 period, around 250 papers based on and visibility of, the Highly Processed Data Products (the ISO appeared in the major refereed journals (1160 papers result of dedicated projects focused on cleaning the are known in total and tracked in the ISO data archive).

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With the ISO data archive having establishing itself as a general astronomical research resource and as an important tool for planning future missions, with activities continuing on enhancing its contents and functionality, many more astronomical surprises and discoveries from ISO are still expected.

3.6.3 XMM-Newton

XMM-Newton is an X-ray astrophysics observatory, launched on 10 December 1999 with a projected and designed lifetime of over 10 years. It enables astronomers to conduct sensitive X-ray spectroscopic observations of a wide variety of cosmic sources. It is specifically designed to investigate in detail the spectra of cosmic X-ray sources down to a limiting flux of 10–15 ergs/cm2/s. It is able to detect X-ray sources down to a few times 10–16 ergs/cm2/s; however source confusion starts to play a role at these flux levels. The principal characteristics of XMM-Newton, with its three Figure 3.6.3/1: These four images illustrate the telescopes and suite of complementary instruments XMM-Newton observtion of GRB 031203. The ring (EPIC, RGS, OM used simultaneously), can be structures expanding around the point source are the summarised as follows: first time-dependent light echo seen in X-rays.

— effective aperture of 4500 cm2 at 1 keV (12.4 Å) and 1000 cm2 at 10 keV (1.24 Å); — almost constant angular resolution across the full waveband of ~15 arcsec HEW; — tracking the maintenance and implementation of — X-ray field of view ~30 arcmin; change requests to the SOC operations subsystems — capability of performing sensitive medium- by external contractors; resolution spectroscopy with resolving powers 100- — defining, implementing and tracking procedures for 700 over the wavelength band 5-35 Å (350- operating the scientific instruments; 2500 eV); — implementing instrument calibration observations, — broadband imaging spectroscopy from 300 eV to coordinating and participating in their analysis, and 12 keV (1-40 Å); delivering finalised calibration files to the community; — simultaneous sensitive coverage of the wavelength — co-developing, pre-release checking and distributing band 1600-6000 Å (~17 arcmin FOV) through a the Science Analysis Software (SAS) and the dedicated optical monitor, co-aligned with the X-ray associated data products. telescopes; — continuous coverage of a source for up to 42 h. During the reporting period, the work still performed at ESTEC (except for mission management) was Further details, including access to the data archive, may transferred to ESAC. be found by visiting http://xmm.vilspa.esa.es. During Autumn 2003, the Division prepared the case for The Division has overall management responsibility for extending mission operations and presented it to the the project and is directly responsible for the execution of scientific advisory structure and to the SPC, which science operations. Mission operations for XMM- unanimously approved the principle of an extended Newton are conducted from ESOC, while science mission up to 31 March 2008. With such an outlook, operations are conducted from ESAC, where the Science efforts to streamline and reduce the cost of operations Operations Centre is located. The main tasks of the SOC continue. In this context, a reduction in (contractor) staff are: has already been implemented without affecting the overall performance of the observatory or the ground — monitoring payload operations in real time; segment. One of the other elements to ensure that an — performing mission planning and constructing an extended, cost-effective future is possible has been the optimally efficient schedule. This includes issuing decision to transfer the operating system for the mission and processing announcements of opportunity; control systems from SCOS-1b to SCOS-2000. This — maintaining and updating all XMM-Newton activity is nearing completion and will, inter alia, provide handbooks; a solid operating environment up to the end of the mission.

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A new general management structure for satellites in orbit scheme has been running for almost a year now and is was introduced. For XMM-Newton, this meant a under evaluation. There is a clear indication of increased separation of the role of Mission Manager and Project science output from the SOC team contributing to the Scientist. The Mission Manager continued to work 50% on 650 refereed XMM-Newton publications so far. XMM-Newton and a new Project Scientist was appointed at ESAC. This new set-up is working extremely well. 3.6.4 Integral The XMM-Newton users’ group now meets on an annual basis, instead of biannually, as it was felt the mission is The Integral gamma-ray observatory is dedicated to now routinely and reliably turning out all products spectroscopy and imaging of celestial gamma-ray sources expected by the community. In general, it is very positive in the energy range from 15 keV to 10 MeV. It was about the status of the mission. launched on 17 October 2002 by a Russian Proton rocket. The payload consists of two imaging gamma-ray With the improved knowledge and experience both in instruments, one optimised for spectroscopy (SPI) and one mission planning and schedule execution, the SOC can for high-resolution imaging (IBIS). These are supported now carry out the necessary replanning and get the by co-aligned X-ray (JEM-X) and optical (OMC) satellite repointed in response to a target of opportunity monitors. All three high-energy instruments use coded alert in as little as 4 h 40 min after receipt of the alert. masks for imaging. Further information is available at This is well beyond what the mission was designed for, http://astro.estec.esa.nl/Integral. The majority of Integral and provides spectacular science results (Fig. 3.6.3/1). observing time is available to the general astronomical community via calls for proposals, with a smaller amount The calls for observing proposals are now issued annually (currently 25%) used for survey-type Core Programme by the SOC and the process has become routine. The activities such as deep exposures of the galactic centre uptake by the community remains very high, with 692 region and regular scans along the galactic plane. Integral proposals submitted in response to AO-3 and 657 in operations continue smoothly, with the spacecraft, response to AO-4. The oversubscription factor is around instruments and ground segment performing well. A major 5-6. There is a clear and continuing trend to go for longer milestone was reached on 17 July 2004 when the first observations and multiple sources per proposal. Integral observations entered the public domain. These are available to the scientific community via the on-line A number of new releases of the XMM-Newton Science archive at the Integral Science Data Centre. Archive (XSA) and the Science Analysis Software (SAS) were made available to the community. The XSA has now The Division has overall management responsibility for become the standard tool for the community for retrieving the project and is directly responsible for the Integral (and searching) both proprietary and public data. A few Science Operations Centre, handling uplink and coordin- thousand public data sets are available through the XSA. ation activities. During the reporting period, ISOC was One of the major new components integrated into the located at ESTEC but is being moved to ESAC. XSA was the first XMM-Newton source catalogue Downlink science operations (data processing and (1XMM), generated by the Survey Science Consortium distribution) are the responsibility of the Integral Science (SSC, PI: M. Watson, Leicester, UK). Preparations for Data Centre (ISDC, Versoix, CH). Mission operations generating a second, extended, source catalogue have are conducted from ESOC. The main tasks of ISOC are: started inside the SSC, and ESAC is actively regenerating data sets wherever new processing (attitude, timing, etc.) — to issue Calls for Observing Proposals and to process provide improvements. The SAS (now at release 6.0) has the submitted proposals; become the de facto standard for analysing XMM- — to conduct the scientific mission planning, including Newton data; it is a complete suite of tools, which now processing ToO requests; contains the tools to analyse grism spectra from the — to operate, jointly with the ISDC, a web-based Optical Monitor. helpdesk to support Integral users who have ques- tions about any aspect of the mission, or their own The observatory has implemented support of COSPAR observations. regional education activities (New Delhi, 2003; Durban, 2004) and is routinely organising workshops at ESAC to Additionally, in close collaboration with the Integral teach people how to use the XMM-Newton data analysis Science Working Team, the ISOC works: system. — to finalise the Core Programme of guaranteed-time In order to support observatory staff in executing their observations for each AO-cycle and implement them science research objectives, the concept of a ‘science day’ into the ISOC scheduling system; has been introduced. This is a fixed day in the week that — to prepare and manage the instrument in-flight cali- is set aside for research. On this day, in principle, no bration during the nominal and extended mission meetings or other functional duties are scheduled. The phases;

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creation of the corresponding commands to be sent to the spacecraft. The Integral observing schedules, both short- term and long-term, are available on the web. The overall observing programme is summarised in the exposure map (Fig. 3.6.4/1), which includes all observations to February 2005.

The gamma-ray sky is highly variable and interesting new targets can, and do, appear unexpectedly anywhere in the sky. When this happens, a ‘Target of Opportunity’ Figure 3.6.4/1: Integral exposure map covering (ToO) request may be made. The Project Scientist, scientific observations from December 2002 (start of supported by the ISOC mission planners, evaluates the the nominal mission phase) until February 2005 (end request and decides on the basis of scientific merit and on of AO-2 observing programme). the impact of the rescheduling, whether to go ahead. If the request is granted, the ISOC generates a new observing programme for the interval concerned and, inter alia, makes this available on the WWW to aid astronomers planning coordinated observations. During — to support the instrument teams in instrument the reporting period, 36 requests for ToO follow-up configuration and operations (e.g. telemetry observations were received, out of which 16 were allocation, annealing of the SPI detector unit). accepted and successfully observed.

During Autumn 2003, the Division prepared the case for The achieved sensitivities of the Integral high-energy extending mission operations and presented it to the instruments are now close to the statistical limits derived scientific advisory structure and to the SPC, which from the background counting rates and effective areas. unanimously approved the principle of an extended The Mission Manager has coordinated the activities to mission up to 31 December 2008, with a review of the improve the achieved sensitivities through better science foreseen in Autumn 2006. An element of the observing techniques, background modelling and mission extension is to move ISOC from ESTEC to analysis software. ESAC in order to increase synergy with XMM-Newton. The Mission Manager is ensuring that this transition is One of the few major payload anomalies has been the conducted in the most cost-effective way, while loss of two of the 19 SPI detectors. Both of these losses maintaining full operational capabilities. A plan for the followed annealing, when the SPI detectors are ‘baked’ evolution of the ISOC manpower has been developed by to recover the loss of energy resolution caused by the ISOC manager and the activities defined in the plan radiation damage. The Mission Manager has coordinated are underway, with science operations transferring from the efforts to understand the failures, using both in-flight ESTEC to ESAC in February 2005. tests, ground tests on flight spare hardware, and computer modelling. Once the failures are understood, it During the reporting period, two Calls for Observing will be possible to decide on future annealing strategies. Proposals (AO-2 in 2003, AO-3 in 2004) were issued and processed. The response from the community remained The Project Scientist coorganised the 5th Integral Work- strong, with 142 and 108 proposals received, respect- shop (Munich, February 2004) and co-edited the proceed- ively, with over-subscription factors of 8 for AO-2 and 4 ings (SP-552). Support is being provided to organise an (equivalent to 6 if the duration of the AO is taken into Integral workshop in January 2005 (ESTEC) and the 6th account) for AO-3. After each AO, the pointing direct- Integral Workshop in 2006 in St. Petersburg (Russia). ions of the approved observations are scanned by ISOC staff for targets close together in the sky which can be Finally the Project Scientist, in coordination with the observed in a single pointing – hence saving observing ISWT, contributed to the definition of the terms of time through amalgamation of several independent reference for the new Integral Users Group and the research proposals. This is particularly important for associated update of responsibilities for the ISWT as laid Integral where the observations are, owing to the low down in the Science Management Plan. fluxes, generally long, but the fields of view of the gamma-ray instruments are very large (the fully coded fields of view are 16º for SPI and (9x9)º for IBIS). The 3.6.5 Astro-F accepted proposals are processed at the ISOC into an optimised observing plan consisting of a timeline of Astro-F is a Japanese mission with the prime goal of target positions, together with the corresponding instru- making a second-generation all-sky IR survey with ment configurations. These are then forwarded to the higher sensitivity and longer wavelength coverage than Mission Operations Centre (MOC) at ESOC for the IRAS. ESA is collaborating with JAXA to provide sec3.qxd 7/15/05 10:01 AM Page 87

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tracking support (use of a second ground station) and assistance with the survey data reduction (pointing reconstruction) in return for 10% of the observing opportunities during the non-survey parts of the mission, to distribute to the ESA community. The SPC approved this collaboration in Autumn 2000. During the reporting period, JAXA/ISAS have announced launch delays from February 2004 to end-2005 or early 2006. The Division has overall responsibility for all of ESA’s contribution to this mission.

Implementation of tracking support has been delegated to ESOC, who, during the reporting period, have designed, implemented and tested the various upgrades and customisations necessary to enable the Kiruna tracking station to provide the required service. All equipment is now in hibernation until launch preparations start Figure 3.6.6/1: A month-by-month history of HCSS 6 months before launch. Activities for pointing software problem reports (SPRs) and software reconstruction and community support are carried out by change requests (SCRs) and the change in the the Division’s team in ESAC. Work on the input number of open SPRs/SCRs (pink line). reference catalogues, needed for the pointing reconstruc- tion task, was completed as planned by end-2004. The Pointing Reconstruction User Requirement Document has been issued and the detailed software design is underway. Planning for the European Call for Proposals Centres, and observers using Herschel. Seen end-to-end, is based on issuing the call in the May-June 2005 these services include support for (i) proposal sub- timeframe, preceded by a call for letters of intent, once mission, (ii) proposal evaluation, (iii) helpdesk support, the launch date has been finalised. (iv) generation of observing schedules compliant with the interfaces agreed with the Mission Operations Centre, (v) reception and archiving of telemetry, (vi) 3.6.6 Herschel Science Centre development instrument data processing software, (vii) data products in the Herschel archive. The science ground segment of the Herschel Space Observatory (Section 3.1.2) is being implemented as a One of the top-level requirements driving HCSS distributed architecture with the science community development is that it supports the concept of smooth being supported by an ESA-provided Herschel Science transition, in which a nucleus of the system that is to be Centre located at ESAC (US astronomers supported by used for in-flight operations already supports Instrument- the NASA Herschel Science Center at IPAC, Caltech) Level Tests in the laboratories of the PI teams several and instrument operations being carried out from three years before launch. Owing to this requirement, HCSS Instrument Control Centres, located on the PIs’ premises. development started in early 2000. The key software ‘glue’ holding these centres together is the Herschel Common Science System (HCSS), being During the 2003-2004 reporting period, seven releases built jointly by the above parties, under the leadership of were made, emphasising the consolidation of the the Division’s Herschel Science Centre Development development and the software having matured from the Team. early prototypes into production-level code. The status of the development is: Within RSSD, the Astrophysics Missions Division has overall responsibility for the scientific integrity of the — the system is in daily use for Instrument-Level Tests mission, while the Science Operations and Data Systems of the Avionics/Cryogenic Qualification Models in Division is responsible for implementing the science the PI laboratories; operations in close collaboration with the instrument — the system has been integrated into the Instrument teams. From the end of the in-orbit commissioning EGSE for use in satellite-level tests; phase, the latter Division will take over overall project — significant progress has been made in the develop- management responsibility. ment of a Herschel Interactive Analysis framework, with a group of scientific end-users giving direction The HCSS is an ensemble of services supplied in the to and providing priorities for this resource-limited form of a single, coherent and mostly platform- development; independent software system. Its users include the — development of the next system release, which will Herschel Science Centre, the Instrument Control support submission and handling of Herschel sec3.qxd 7/15/05 10:01 AM Page 88

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observing proposals and a first implementation of in the case of Rosetta, a valuable Knowledge Base to take the scientific mission planning system, is well under forward through the long mission. way for delivery in 2005. Tools have been created to harmonise the working Examining the trends of the software problem reports methods; these include the Publication Data Base, a tool (SPRs) and software change requests (SCRs) handled by for registering and approving the publications of staff the HCSS Configuration Control Board gives a vivid members. This tool is integrated with the web services insight into the development of the system (Fig. 3.6.6/1). such that an accepted paper is available to the public on Initially, until the end of third-quarter 2003, there was a line. The same database may be used, in connection with steady but slow trickle of inputs. Then, a steady rise the developed Hermes community contact system, to started as both the number of users at the PI institutes and distribute electronically (or by paper if no e-mail address also the intensity of their use increased. In addition to the is available) staffs’ preprints, with the resulting saving in increase in average flow, the submission rate shows secretarial effort, printing and postal charges. rather pronounced peaks, well correlated with dates of user releases of the system. This indicates that the system The various RSSD web sites have been consolidated into tests performed by the developers and acceptance tests a unified RSSD site at http://www.rssd.esa.int. Here, all performed by the users do indeed detect software the information needed by end users of a science mission problems that are not encountered during normal use of may be posted with the necessary protection of the system. Note also that the difference in open SPRs/ proprietary data and personal information. All project SCRs from one month to the next remains almost scientists have access to a tool for developing their web constant despite the monthly influx, showing that the pages; it is optimally designed for us using PHP methods HCSS developers just about manage to keep up. and My_SQL database. Although the site is not completely finished, it means we have significantly reduced the maintenance overhead for the web sites, 3.6.7 Information technology support activities freeing up Project Scientist time.

The Division provides support in data systems to the The departmental computing architecture is SUN-Solaris entire Department. The focus is on consolidating and based – a highly reliable architecture. During the report- optimising the various services with the needs of the ing period, numerous obsolete items have been replaced community, the cost-effectiveness of the infrastructure by a small number of modern powerful file servers, with and the requirements of remote users kept firmly in obvious economic benefits in performance and main- mind. tenance. Where appropriate, Linux machines have been introduced, keeping in step with the academic commun- The Department’s highly valued technical mail service ity’s tendency towards Linux. Windows is both the allows ease of e-mail access to the peripatetic staff. The Agency’s and the general public’s preferred platform and mail service is closely integrated with the LDAP the Solaris team has developed a close working (Lightweight Directory Access Protocol) services set-up relationship with the Windows support team. Inter- on which is built the RSSD intranet. By sharing common operability is the keyword and facilities are shared among resources, we have created a virtual community of all the the office, laboratory, science, operations and research RSSD outstations. The RSSD web portal has been users, such as software licences, storage and printers. developed to offer secure Single-Sign-On access to shared services, including contact and personal information, documents, web-page creation and 3.6.8 Archive and Virtual Observatory activities maintenance, mailing lists, directory services, mailing labels, publication lists, etc. The Science Archives Group at ESAC has been consolidated to provide horizontal support for archive These elements make up a software tool-box that enables activities to many science projects, ranging from the establishment of virtual communities, not just for astronomical missions to planetary missions. Develop- RSSD at large but also the external project teams spread ment and maintenance of the various archives is done in around the world. Such virtual communities have already an efficient and cost-effective manner by using common been set up for Planck, Gaia and Huygens, and it is architecture, code and manpower. This is demonstrated expected that, with management support, more projects by the achievements of the group during the reporting will soon adopt this technology. period, including:

The Department’s documents are centrally managed — the ISO Data Archive allows ingestion and access to using the Document Management system (based on highly processed data products provided by expert Livelink). This permits staff to access their assets user groups, and now provides a more detailed (document libraries) while on the road, publish quality report for each ISO observation; documents directly to the web and create, as for example — the XMM-Newton Science Archive now includes sec3.qxd 7/15/05 10:01 AM Page 89

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powerful and friendly access to the XMM-Newton 3.7 Science Payload and Advanced Concepts point source catalogue as well as on-the-fly Office processing capabilities to offer users the most up-to- date data products; The Science Payload and Advanced Concepts Office — a mirror of the Integral Science Data Archive, (SCI-A) provides support to the Agency’s science together with an updated user interface based on missions and technology programmes as well as the those built for ISO and XMM-Newton, has been research programme of RSSD. The various sections developed to support calibration and monitoring focus their support in these three important areas as well activities within ESA, offering powerful query and as being responsible within the Directorate for the automatic data distribution systems; assessment of future science missions. — work has started on the Herschel Archive Browser for instrument-level and system-level test data. 3.7.1 Science Payload Instrument Section (SCI-AI)

Experience gained in the astronomy archives has been 2003-2004 saw the successful completion of a number of reused to develop the Planetary Science Archive (PSA). flight hardware activities. After the March 2004 launch This will be the single portal to all ESA planetary of Rosetta, MIDAS, RPC-MIP, OSIRIS and SESAME all missions data. Giotto data have already been ingested; successfully underwent their first commissioning. Mars Express, SMART-1 and Rosetta data will be SPEDE on SMART-1 and ASPOC on the two Double incorporated from early 2005. Huygens, Venus Express Stars are also performing as expected. and BepiColombo data sets will come in the future. The PSA also offers a data set validation tool to help the PI Two additional flight projects are nearing completion. teams to provide data sets compatible with the PSA/PDS The first is the COROT Digital Processing Unit. The data sets standards. Engineering Model was delivered to the project and is undergoing integrated tests. The assembly and electrical Activities on the Virtual Observatory (VO) have been tests of the flight and flight spare models (three in total) expanded in the second year of the reporting period. VOs were completed at Astrium GmbH and were in the SCI-A are defined as a collection of interoperating data archives laboratories by December 2004. and software tools that use the Internet to form a scientific research environment in which astronomical The second project is the Solar Electron Proton research programmes can be conducted. The ISO Data Telescope (SEPT) for the STEREO mission as part of the Archive and XMM-Newton Science Archive have IMPACT suite of instruments within the Solar Electron already been updated to support existing VO protocols, Proton package. SEPT consists of two dual, double- such as Simple Image and Spectra Access, and are, ended magnet/foil solid-state detector particle telescopes currently, two of the few VO-compliant astronomy that cleanly separate and measure electrons in the energy archives worldwide. Following this success, ESA is range 20-400 keV and protons of 60-7000 keV, while providing more VO-dedicated manpower in 2005 and 2006 to fully integrate our archives into the VO world, to develop tools to support the VO community, to increase ESA and member-state data centre involvement in world- wide VO activities, and to position ESAC as the Space Figure 3.7.1/1: Top view of the STEREO Flight Model Astronomy VO centre in Europe. analogue board. sec3.qxd 7/15/05 10:01 AM Page 90

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Fig. 3.7.1/2 the complete system integrated in its housing with the various detectors. The four SEPT Flight Models (plus one spare) are assembled and have undergone final environmental tests. They were formally delivered to the project in December 2004 after completion of the calibration campaign.

Figure 3.7.1/3 shows the first spectra obtained with the instrument using the electron conversion lines of a 207Bi source. The PDFEs were operated in full anti- coincidence mode. The green curve is related to CS1, the centre segment of D1. The red curve shows the fluence observed on CS2, the centre segment of D2. The blue curve is related to XT1, the cross-talk ring of D1. At top right is a basic sketch of the position of the source with respect to the detectors. The K conversion lines are nicely resolved. The different lines are also visible on CS2, shifted by ~110 keV, the average energy deposited Figure 3.7.1/2: The assembled STEREO Flight Model by electrons crossing D1. These results indicate that, by Models. focusing on a detailed design, an optimised low-resource instrument can be developed without loss of overall performance. This approach will continue to be developed in SCI-A through the study of Highly Integrated Payload Suites (HIPSs).

3.7.2 Science Missions Section (SCI-AM)

The Science Missions Section of SCI-A is responsible for providing support to science missions in orbit, under development and under assessment, and for planning longer-term future mission developments.

Support to the external scientific community is provided directly and indirectly. Directly, for specific requests related to instrument development, to payload reviews Figure 3.7.1/3: The first spectra obtained with one of and to programmatic aspects or by performing dedicated the telescopes and the dedicated electronics, using the studies on the payload complement baselined for future electron conversion lines of a Bismuth-207 source. missions. Indirectly, by assessing new missions, thus defining the requirements of future instruments and the related technology development needs, and by supporting missions already under development. As an example, over the last few years, SCI-AM staff have providing anisotropy information through the use of followed the development of the SMART-1 payload units several fields of view. Two SEPT units (NS: North-South closely, supporting PIs and the Project Scientist direction, E: Ecliptic) are located on each STEREO throughout the different mission phases, including spacecraft. commissioning after launch and performance verification. The electronics were designed and fabricated by SCI-A for RSSD, while the housing and sensors were provided In the 2003-2004 period, SCI-AM staff provided by the University of Kiel (D). The major challenge of technical payload support to both RSSD (SCI-S) and the SEPT involves the growing need for compact and highly Science Projects Department (SCI-P) for a number of integrated instruments. SEPT is based on the Particle missions under development, such as Planck and Detector Front End ASIC developed under ESA’s GSTP. Herschel (participating in project reviews) and Integral With 640 g and 600 mW per unit, the instrument (Instrument Final Acceptance Review and In-Flight demonstrates the technological development that is Performance Review). In 2004 SCI-AM contributed to possible and which will have to be matured further to the Systems Requirements Review of NIRSpec and respond to future, ever-more demanding space missions. MIRI, two major instruments provided by ESA to the Fig. 3.7.1/1 shows the assembled analogue board and James Webb Space Telescope. SCI-AM staff also sec3.qxd 7/15/05 10:01 AM Page 91

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module, as well as to assess the needs of a mission aimed at investigating the ‘Pioneer effect’ (deviation from the gravitational theory at large distances from the Sun). Another TRS is the Solar Polar Orbiter, a mission exploiting solar sailing and aiming to observe the Sun from very high heliospheric inclinations

SCI-AM staff are responsible for the Darwin Ground- based Nulling Interferometer Experiment (GENIE) definition phase, which involves conducting two industrial parallel competitive studies to establish the feasibility, performance, preliminary design and cost. GENIE may be installed at the VLT of ESO (Chile) as a precursor to the future Darwin payload. GENIE has a Figure 3.7.2/1: The Solar Orbiter orbiting the Sun at two-fold objective: to exercise, on the ground, nulling 0.2 AU during the science mission phase interferometry in prospect of the Darwin mission; to provide the scientific community with a sophisticated instrument capable of obtaining valuable scientific data. The industrial studies ran during 2004 and the definition study will be completed at the end of March 2005. contributed to the Gaia Mid-Term Review (September 2004), providing payload and detector expertise, Finally, SCI-AM personnel supported a number of space including integrated support to the Project Scientist in science instruments being studied or developed for the areas such as radiation damage and detector modelling. ISS. Examples of instruments under study are EUSO and Lobster. Support to the instrument team has been Considerable support on technical and programmatic provided in the case of SolACES, a UV radiometer under areas has been provided for the BepiColombo development. reassessment and the following AO and payload selection process. As part of its duties, SCI-AM contributed to the cost and risk assessments of several 3.7.3 Planetary Exploration Studies Section missions (such as BepiColombo, Darwin, Solar Orbiter (SCI-AP) and the MIRI instrument), including payload, flight and ground segments, with the final goal of estimating the The principal effort of the section has been the execution Cost-at-Completion of these future ESA science of the 9-month reassessment of the BepiColombo missions. mission to Mercury, with the aim of maximising the scientific performance and optimising the payload A major task under the responsibility of SCI-AM during complement, while reducing costs and programmatic 2003-2004 was the Solar Orbiter assessment study risk. The change of the mission profile from a split (Fig. 3.7.2/1). Activities included the preparation of all launch for MMO and MPO into a single Soyuz- mission reference documents, the conduct of a dedicated Fregat 2B launch brought a major reduction in cost. industrial study on the payload complement, the Coupled with a detailed cost and risk assessment, this has completion of two parallel competitive studies at system allowed the mission to move into the definition and level, the preliminary mission analysis and mission development phases. The section now provides support control study, and a complete mission cost-risk to the Project Scientist and project team in such areas as assessment. With such an in-depth study of all these payload architecture, and participated, in particular, in mission elements Solar Orbiter is well placed to move the evaluation of instrument proposals after the Request into the development phase in 2006. for Proposals in support of the Payload Review Committee. Technology Reference Studies (TRS) in astrophysics, fundamental physics and solar physics are also being The section provides support to a number of planetary developed by SCI-AM, based on the ideas put forward missions such as Venus Express, where the external by the scientific community following the ESA Call for magnetometer team was supported during qualification Ideas and the Cosmic Vision workshop that took place in of the instrument and its boom. In the case of Rosetta’s September 2004. SCI-AM staff are performing a MIDAS, a major effort went into the final design, preliminary study on a future Gamma-Ray Lens project, integration, testing and verification of the flight as a potential post-Integral mission and targeting photon instrument and flight spare. Commissioning of MIDAS energies even above 500 keV. Similarly, in fundamental after launch was successfully performed by SCI-AP physics, work is under way to assess requirements for a personnel in collaboration with the PI team. Parallel standard fundamental physics payload and spacecraft activities, supported by SCI-AI, are establishing a sec3.qxd 7/15/05 10:01 AM Page 92

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Figure 3.7.3/1: The Europa Mini-Satellite Orbiter with its ice-penetrating radar deployed. The lifetime is about 60 days after entering polar orbit, sufficient for two complete high-resolution mappings of the surface.

reference database to determine the magnetic properties of selected meteorites and prepare for the data return.

Support has been provided on specific instruments for Solar System research to the Instrumentation Section SCI-AI. For example, the ASIC development for STERO and the major contribution to the development of the Figure 3.7.3/2: The Interstellar Heliopause Probe DSP-based DPU for COROT, based on the experience (IHP) with its high-gain antenna, RTGs and boom with the DPU of Rosetta’s OSIRIS. system (top), and the conceptual design showing the instruments’ field of views (bottom). The sail would Finally, in preparation for future technology planning as be shed at about 5 AU since no further major gain in well as for establishing potential feasible mission acceleration could be achieved. The science phase scenarios at an early phase, the section has been would then begin using the plasma instruments. The prominent in running a TRS series related to Solar probe would reach the assumed heliopause (~200 AU) System science. These have included the following top- in about 25 years. level mission profiles:

— exploration of the Jovian system and specifically the mapping of Europa using a series of mini-satellites meaningful technical data to the future technology plans, (Fig. 3.7.3/1); as well as providing quantitative data for the future — in situ exploration of Venus via an aerobot coupled science programme through the Cosmic Vision process. with a series of microprobes; — a mini-satellite sample and return mission to the Martian moon Deimos; 3.7.4 Advanced Technology Section (SCI-AT) — a solar polar microsat orbiter using a solar sail to raise the ecliptic inclination to 90º; The Advanced Technologies Section provides support to — a microsat to explore the boundary of the the community in two ways: by developing basic heliosphere, heliopause and beyond through the use enabling technologies for future missions and instru- of a large solar sail to achieve initial high velocities ments, and by offering specific technology support to (Fig. 3.7.3/2). on-going activities or studies. The key areas are in the technologies required for science payloads and, in Such mission studies allow the section to contribute particular, in advanced optics and detectors. It is sec3.qxd 7/15/05 10:01 AM Page 93

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systems should be possible without recourse to the very low temperatures required for current sensors based on superconductors.

Finally, the section’s technology expertise has been used to support ESA missions past and future including:

— XMM-Newton in-flight instrument calibration; — radiation damage annealing studies on Integral; — radiation damage analysis for Gaia and Bepi- Colombo; — BepiColombo spectrometers and particle monitor design; — supporting the development of specific payload technologies for BepiColombo; — CCD design and systems analysis for the Eddington focal plane camera; Figure 3.7.4/1: The Wolter 1 micro-channel plate — establishing the Solar Orbiter Technology Develop- optics developed as a prototype a variant of which ment Plan; will form part of the imaging X-ray spectrometer — system design studies for XEUS instruments and instrument on the BepiColombo mission. mirrors; — developing the XEUS micro-pore mirror; — supporting the Darwin Technology Development.

particularly considered that precision lightweight optics 3.7.5 Darwin special project group will be a crucial enabling technology, allowing lower- cost missions with much higher sensitivities. Darwin, the near-IR nulling interferometer, is a special project under study in SCI-A. This mission requires Specific areas of development include lightweight X-ray multiple spacecraft to fly in formation at L2. The mission optics such as those based on glass microchannel plates objectives are to detect and determine the nature of (Fig. 3.7.4/1) and silicon micro-pore optics. These extrasolar terrestrial planets out to a distance of about technologies have been studied in detail for future 25 pc. This is achieved through nulling interferometry at mission applications such as Lobster, a wide-field X-ray 6-20 µm. The Darwin special project group has telescope, the X-ray surface fluorescence spectrometer concentrated on studying in detail the optical architecture on BepiColombo, and the XEUS large effective area of the mission with the aim of maximising the scientific X-ray mirror. In the case of XEUS, the section is also return while controlling the cost, complexity and risk. handling all mission-related aspects, including payload This has been achieved through the use of four accommodation, system engineering, mission analysis spacecraft: three identical spacecraft carry ~3 m- and mission profile optimisation, because the optics diameter mirrors pointed at the target star, while a fourth technology drives all other issues. At a later stage, the spacecraft combines the three transferred beams under mission will be transferred to SCI-AM for further accurate phase control, including achromatic phase mission development at system level. In addition to these shifts. In this way, the light from the central on-axis star specific soft X-ray optics technologies, optics can be effectively reduced by six orders of magnitude requirements for the hard X-ray and gamma-ray regions while the transmission map has off-axis regions close to are under active study or development, and preliminary the star, where terrestrial planets would be detectable studies of the needs at far-IR wavelengths have begun. depending on the planet’s orbital period and observation Essentially, the experience gained in the development time. Rotation of the constellation coupled with multiple and deployment of low-resource optics at X-ray observations would allow planets to be detected and their wavelengths for astrophysics and planetary missions will orbital periods to be established. Longer observations of migrate across to other wavelengths and disciplines. any planet, once detected, would allow its atmosphere to be characterised through broadband spectroscopy. The second area of key expertise is in advanced detector technologies, which have been studied and developed The Darwin team has been able to reduce the mission over a wide range of wavelengths. A programme for the complexity, and thereby its cost, by introducing a novel development of solid-state neutron detectors for way of beam combination. This technique is based on planetary science has also been introduced. Of particular multi-axial beam injection into a single mode waveguide. note is the study of low band-gap semiconductors for the Recognising that the waveguide injection losses would EUV and soft X-ray domains, where photon-counting also occur when using traditional beam combination sec3.qxd 7/15/05 10:01 AM Page 94

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techniques, such as beam splitter plates, where a waveguide would be used for wavefront filtering, and that the technique allows odd numbers of beam to be efficiently combined, the team determined that an efficient nulling interferometer, involving the minimum number of beams, could be realised. The concept has been developed and now forms the mission baseline. An initial laboratory verification of the concept has been completed and will be complemented by more refined breadboards. The team continues its studies in nulling interferometry by pursuing explorative work in system design and modelling.

It is envisaged to place the four spacecraft in orbit around L2 using a pair of Soyuz-Fregat launchers. The cruise duration to L2 is of the order 100 days. The Darwin team is looking further into the details of the payload and its accommodation, together with the development of the mission at the system level. sec3.qxd 7/15/05 10:01 AM Page 95

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4. OTHER ACTIVITIES

4.1 Symposia and Workshops organised by RSSD The proceedings were published in Nucl. Phys. B (Proc. Suppl.) 132 (2004). 4th Cluster Workshop ‘1st Cluster Tail Workshop’, Graz, Austria, 26-28 March 2003 ‘5th Cluster Workshop’, Orleans, France, 12-16 May About 60 people attended this workshop to discuss the 2003 structure and dymanics of the Earth’s magnetotail. A key topic was thin current sheets that are unstable to This workshop dealt with spatio-temporal analysis and magnetic reconnection processes that energise charged multi-point measurements with Cluster. About 100 particles, causing fast plasma flows and magnetic flux participants attended, and the main topics were the ropes. These events lead to precipitation of particles into dayside plasma boundaries of the magnetosphere and the the Earth’s atmosphere, triggering auroral displays. local characterisation of the space plasma. The magnetic reconnection that also occurs on the dayside magnetopause was widely discussed: here the ‘2nd Eddington Workshop: Stellar Structure and reconnection causes the transport of energy, momentum Habitable Planet Finding’, Palermo, Italy, 9-11 April and particles from the solar wind into the magnetosphere. 2003 The measurement of electric current was also discussed: the measurement is based on Ampere’s Law and requires While the programme of this workshop focused on some four satellites that are properly separated in order to specific aspects of the preparation of the Eddington derive the current flowing across the satellite mission (the choice of planet-finding field and the data constellation. processing approach), broad science topics in the fields of planet-finding and asteroseismology were also extensively covered. The workshop was attended by 150 ‘New Perspectives for Post-Herschel Far Infrared scientists from most ESA Member States as well as Astronomy from Space’, Madrid, Spain, 1-4 September Canada, USA, Australia, Hungary and the Czech 2003 Republic. One of the workshop’s key issues was the selection of the region of the sky where Eddington would With Herschel and its instruments well into their have searched for habitable planets. The workshop development and construction phase, it was timely to generated a broad interest in the media, resulting in discuss the long-term future of far-IR space astronomy coverage in national newspapers in Italy as well as and to design a development plan for the post Herschel national TV and radio coverage in some of ESA’s era. ESA has already created a framework plan (Cosmic Member States. Vision) for future missions based upon discussions and considerations from the Horizon 2000+ planning exercise. However, these activities took place some time ‘The Restless High Energy Universe’, Amsterdam, The ago, when ISO was beginning operations and before the Netherlands, 5-8 May 2003 implementation of Herschel got underway. More recently, in 2002, US astronomers considered the options About 140 people attended this conference dedicated to for future far-IR/sub-mm space astronomy and have results from the BeppoSAX mission. The Italian-Dutch constructed a roadmap for technology and mission X-ray astronomy satellite was launched in April 1996 development. and operated for 6 years. It revolutionised the study of gamma-ray bursts (GRBs) by discovering long-lived At this meeting, about 75 members of the European X-ray afterglows which, at long last, allowed the (far-)IR astronomical community (both scientists and redshifts of GRBs to be determined and confirmed their instrumentalists) met to discuss the long-term scientific cosmological distances. During the conference, these goals requiring observations in space in the 50-600 µm results and their legacy were reviewed together with range, to review the instrumentation capabilities to be BeppoSAX results on clusters of galaxies and supernova developed and to discuss a strategy for implementation. remnants, active galactic nuclei and the X-ray background, stellar-mass black holes and neutron stars. It is clear that results from the broadband (0.1-300 keV) ‘IAA/ESA Workshop on the Next Steps in Exploring Deep instrumentation on BeppoSAX played major roles in Space’, ESTEC, 22-23 September 2003 many areas of high-energy astronomy. The workshop also examined the legacy of the mission, showing how This workshop, organised by ESA and the IAA, was discoveries from the mission have helped to define the attended by more than 125 participants. It built on an scientific priorities of later missions such as Swift and ongoing IAA cosmic study ‘Next Steps in Exploring Integral. Deep Space’ in order to give a vision for the exploration sec3.qxd 7/15/05 10:01 AM Page 96

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of space by humans in the first half of the 21st century. ‘ILEWG5, International Lunar Conference 2003’, The purpose was to provide a roadmap for a systematic, Hawaii, USA, 16-22 November 2003 logical and science-enabled plan for exploration of the Solar System and observation of the Universe, a The International Lunar Conference ILC2003 was programme to gradually but systematically establish a organised under the auspices of the International Lunar permanent presence and infrastructure at each outpost Exploration Working Group (ILEWG). This meeting along the way. The workshop considered prorities attracted lunar explorers at large, including Apollo established by various communities and space agencies astronauts John Young and Harrison Schmitt, space across the world, and discussed the spaceflight professionals and enthusiasts from all over the world. infrastructure required to pursue these goals, including Among the topics discussed were the exploration and the relevant policy, international aspects and public utilisation of the Moon, and issues such as exploration, engagement. science, advanced technologies, lunar resources, robotic and human expansion, lunar bases, commercialisation, Moon/Mars synergies, lunar tourism and who owns the ‘6th Cluster Workshop’, ESTEC, 29 September – Moon were addressed ( http://www.spaceagepub.com/ 3 October 2003 program.html). This conference was an opportunity to hear the latest news from SMART-1, the first European About 100 participants attended this workshop, mission to the Moon. consisting of three parallel splinter sessions on various topics, including collisionless shocks, magnetopause, cusps, inner magnetosphere and identification of plasma 37th ESLAB Symposium, ‘Tools and Technologies for wave modes. Owing to the supersonic nature of the solar Future Planetary Exploration’, ESTEC, 2-24 December wind, a shock layer is formed in front of the Earth’s 2003 magnetosphere. The understanding of the shock essentially requires multisatellite observations. At the With various European space missions either on their shock, strong electric currents flow; a typical current way to, or already in orbit around, exciting planetary here is of the order of 106 A (note that this can be objects, it was felt timely to reflect on experiences measured only with Cluster). gained, and at the same time to set new focal points for future activities. The currently active or planned planetary missions reflect drastically different environ- 13th SOHO Workshop, ‘Waves, Oscillations and Small- ments, ranging from a cold and dark world on a comet Scale Transient Events in the Solar Atmosphere: A Joint through quite benign conditions in orbit at Mars to hot View from SOHO and TRACE’, Palma de Mallorca, environments around Venus and Mercury. Future Spain, 29 September – 3 October 2003 expeditions may lead us to exotic worlds such as the Jovian icy moons or in situ analysis of Martian soils. The 13th SOHO Workshop was held jointly with the There are high demands on innovative methods and on TRACE team on waves, oscillations and small-scale the technology needed to decipher the manifold transient events in the solar atmosphere. Detailed scientific questions. The meeting was well supported by observational studies with SOHO and TRACE have the scientific community and, as a result, a very balanced provided a strong stimulus to theoretical developments, and interesting programme could be accomplished. so much so that coronal seismology (the determination of coronal parameters by using information from the waves As a warm up in the first session, an overview was the medium supports) is rapidly developing and presented of ESA studies on reference exploration providing insight into some of the physical parameters scenarios, which are used to identify the technological and processes at work in the corona. Nearly 100 needs of future planetary space missions. The challenges participants discussed 110 papers in seven sessions of spacecraft and scientific payload developments were covering MHD Waves and Oscillations in Photospheric addressed equally. Starting from this inspiring exercise, Structures, Waves in the Chromosphere, Topological the symposium went on with innovative ideas and Changes and Magnetic Coupling, Waves and Oscillations technological highlights in remote sensing instruments. in Prominences, Transition Region Dynamics: Considerable interest was shown for in situ Transients, Jets, Wave Acceleration in Open Magnetic measurement techniques for planetary surfaces. New Regions and Coronal Seismology. payload instrumentation was introduced as well as carrier systems enabling exploration strategies on a large The proceedings were published by ESA SP-547. scale. The detection of water (a prerequisite for the existence of life) and the recognition of traces of life itself are of substantial interest and were reflected in a full session. The presented concepts and technologies demonstrated the advanced level of expertise within Europe. sec3.qxd 7/15/05 10:01 AM Page 97

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The symposium was concluded with the Director of what will be the state-of-the-art of the field at the time of Science’s outlook on the future of the scientific Planck’s launch. programme. Overall, the 37th ESLAB Symposium was a great success, combining the efforts of the European The bulk of the Symposium was devoted to scientific science community and ESA towards the future talks on the probable scientific return of Planck in view exploration of our Solar System and beyond. of currently ongoing and planned experiments. These talks covered the spectrum of Planck science, not only CMB-based cosmology, but also extragalactic science, as ‘Moon-Mars Workshop’, Bremen, Germany, 26 28 Sep- well as the study of the Milky Way. Critical issues of tember 2003; Vancouver, Canada, 1-8 October 2004 instrument technology and data processing were also addressed. Finally, a large number of high-quality posters The Moon-Mars Workshop (MMW) was a recommend- gave insight into many detailed aspects of Planck. ation from the Space Generation Summit (SGS) held at the World Space Congress in Houston in 2002. The Space The discussions held in the various sessions confirmed Exploration workgroups from SGS decided that it is very that the scientific potential of Planck remains of the important to look at current Moon and Mars exploration highest calibre, even in view of the recent release of plans and to highlight their commonalities in order to WMAP data, and of new and very powerful ground- or show how developments for one benefit the other. A balloon-based experiments that are planned in the single roadmap is needed for Moon-Mars exploration, coming decade. Although it was clear that, in just 3 days, and this should accelerate our pace in exploration and it was impossible to cover all the potential scientific colonisation of our near Solar System. The First Moon- return of Planck, the Symposium fulfilled its objectives Mars Workshop was held in Bremen in conjunction and and served as a valuable milestone on the road towards collocated with the Third European Mars Society the satellite’s launch. Conference (EMC3), in connection with the IAF.

The Second Moon-Mars Workshop was held in ‘5th Integral Workshop’, Munich, Germany, 16-20 Vancouver during IAF 2004 (http://moonmarsworkshop. February 2004 com/ and http://moonmars.org/) 230 participants from all over the world attended the 5th Integral workshop. Many key results from Integral ‘3rd VILSPA SAS Workshop’, VILSPA, Spain, 8-10 observations were presented, including one very exciting October 2003, and ‘4th VILSPA SAS Workshop’, VILSPA, result from Integral’s Galactic Plane Scan (GPS) Spain, 8-11 June 2004 programme: the discovery of a new type of highly obscured X-ray binary sources that had so far escaped The VILSPA Science Analysis System (SAS) Workshops detection with other instruments. These new sources are provide XMM-Newton users who have little or no located within the Norma spiral arm of our galaxy. experience of XMM-Newton data analysis with an introduction to the procedures and techniques for Integral also observed the centre of the Galaxy, which reducing and analysing XMM-Newton data. No specific contains a super-massive black hole and yet only shows knowledge of X-ray data analysis is in principle required relatively faint emission. The discovery of a source, IGR to attend the workshop. The 3-4 day workshops are J17456-2901, coincident with the Galactic nucleus organised as half-days of presentations, and half-days of Sgr A* to within 0.9 arcmin was reported. It is the first practical training (hands-on) sessions. In the practical observation of significant hard X-ray emission from sessions, the participants, supported by XMM-Newton within the inner 10 arcmin of the Galaxy and a SOC scientists, can accomplish reduction tasks on contribution from the galactic super-massive black hole XMM-Newton public databases, belonging to the SAS itself cannot be excluded. Detection of 91 gamma-ray Scientific Validation or extracted from the public sources towards the direction of the Galactic centre was archive. Attendance is strictly limited to 20 people, to reported, of which 26 are new discoveries (Nature 2004, ensure proper individual support. 428, 293). The sources detected by Integral account for the vast majority of the Milky Way’s (‘diffuse’) emission at soft gamma-rays observed for 30 years, leaving only a 2nd Planck Symposium, ‘Setting the Scene’, Orsay, minor role for diffuse processes. France, 28-30 January 2004 After 1 year in orbit, a comprehensive survey of Integral/ The objective of these meetings is to update the many IBIS Core Program survey data was presented individuals involved in all facets of Planck’s develop- incorporating both the GPS and GCDE. A total of 124 ment, and to stimulate discussion across Planck-related sources has been detected, of which 40% are low-mass topics. This Symposium carried the title ‘Setting the X-ray binaries and 31% are of undefined nature; 14 Scene’ because it was timely to take a detailed look at sources are completely new. sec3.qxd 7/15/05 10:01 AM Page 98

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The last session was devoted to Gamma-Ray Bursts the new insights into coronal physics obtained from high- (GRBs); 10 have been seen in the field of view so far. It resolution XMM and Chandra spectroscopy, new results was shown that the Integral Burst Alert System currently on stellar and planetary formation, and the impact of IR gives the best GRB localisations, in terms of speed and survey and spectroscopy on our understanding of low- accuracy, for follow-up observation of their afterglows. mass stars, brown dwarfs and planets. Cool Stars 13 experimented with the format of the meeting, with the organisation of splinter sessions left to individual ‘2nd Cluster Tail Workshop’, Mullard Space Science participants. This was a success, as all splinters were well Laboratory, Dorking, UK, 3-5 March 2004 attended. The generous sponsorship by ESA allowed the participation of a number of students and young Some 40 Cluster scientists gathered to discuss in researchers. particular the dynamical processes of the Earth’s magnetotail. A main topic was magnetic reconnection The proceedings will be published as ESA SP-560. that occurs everywhere in the Universe, but our geospace is the only place where we can monitor and investigate it in detail. Many other issues were also discussed, such as 38th ESLAB Symposium, ‘5th International LISA the characteristics of thin current sheets that precede the Symposium’, ESTEC, 12-16 July 2004 reconnection; characteristics and existence of ion beams; plasma flow reversals, flux robes, plasmoids and The 5th International LISA Symposium was held jointly vorticity in the magnetotail; effects of interplanetary with the 38th ESLAB Symposium. The Symposium shocks on the magnetotail, and so on. More information traditionally focuses on the science and technology of about the workshop can be found at http://www.mssl.ucl. LISA and is held every second year. The Symposium was ac.uk/www_plasma/missions/cluster/7thworkshop/ attended by about 180 participants who discussed about 90 papers covering all aspects of LISA, starting from the state of the mission in ESA and NASA, leading through ‘Titan from Discovery to Encounter’, ESTEC, 13-17 the technological aspects of LISA and its technology April 2004 demonstrator LISA Pathfinder, finally coming to the astrophysics of the sources. This international conference was held on the 375th birthday of Christiaan Huygens (born 14 April 1629). The proceedings will be published in a special issue of During the 17th century, Huygens was one of the most Classical and Quantum Gravity. respected European scientists; a highlight of his career was the discovery of Saturn’s largest moon, Titan. The aim of the conference was to bring together historians 14th SOHO Workshop, ‘Helio- and Asteroseismology: and space scientists to discuss not only Huygens the Towards a Golden Future’, Yale University, New Haven, person, the scientist and his relationship with other CT, USA, 12-16 July 2004 scientists of his time, but also observations of Saturn and its moons since the 17th century, as well as coming up to The 14th SOHO Workshop was held jointly with the date with the Cassini-Huygens mission and the latest annual meeting of the Global Oscillation Network observations on the way to encounter. The conference Group. It focused on the study of the interior of the Sun was attended by about 120 space scientists and from a seismic perspective and the prospects for similar historians, and the last day was open to the public, study of Sun-like stars. Nearly 120 participants discussed attracting more than 100 people. over 125 papers addressing a wide variety of topics, including the observational status of low-, medium- and The proceedings were published as ESA SP-1278. high-degree p-mode characterisation, low-frequency g- mode detection, solar structure and dynamics, mode excitation and damping, advances in local ‘13th Cool Star Workshop’, Hamburg, Germany, 5-9 July helioseismology, and the first results from the Canada’s 2004 MOST asteroseismology mission.

The ‘Cambridge Workshop on Cool Stars, Stellar The proceedings were published as ESA SP-559. Systems and the Sun’ is the major event of the cool stars community. Organised every 2 years, it now traditionally alternates between the USA and Europe. The 13th ‘The Moon: Science, Technology, Utilization and Human workshop was coorganised by the University of Exploration’, COSPAR 2004, Paris, France, 22-23 July Hamburg and RSSD. The workshop was a big success, 2004 with 293 registered participants from all over the world, making it one of the best attended since the start of the This event included solicited and contributed series in 1980. Among the major topics discussed were presentations, organised in topical sub-sessions such as sec3.qxd 7/15/05 10:01 AM Page 99

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Science of the Moon, A Keystone for Planetary giant planets, UV/X-ray output of stars, and chemistry of Research; Formation and Early Evolution of the Moon, nebular material. Earth and Terrestrial Planets; The Moon as a Laboratory for Comparative Planetology; Current Lunar Missions: Finally, an updated discussion of TPF and Darwin SMART-1, Lunar-A, Selene, Chandrayaan-1, South Pole designs and plans was also provided by ESA and NASA. Aitken Sample Return, Lunar Reconnaissance Orbiter; This included science requirements and technology Astronomy from the Moon; Life Sciences on the Moon; advances as well as more generic choices recently made, Future Exploration and Resources Utilisation; and such as mid-IR interferometry being the current driver in Astrobiology, Living and Working on the Moon and Europe, while visual coronography is the first choice of Mars. NASA.

‘Dust Disks and the Formation, Evolution and Detection 15th SOHO Workshop, ‘Coronal Heating’, University of of Habitable Planets’, San Diego, USA, 26-29 July 2004 St. Andrews, Scotland, UK, 6-9 September 2004 (Towards Other Earths (Darwin/TPF), Heidelberg, Germany, 22-25 April 2003) More than 130 participants presented and discussed over 140 papers addressing a wide variety of topics, organised The second joint Terrestrial Planet Finder/Darwin around eight sessions covering: what is the coronal conference was held in Mission Bay, San Diego, heating problem?, driving coronal heating, wave heating California in July 2004. Attracting about 250 participants of the corona, kinetic aspects of coronal heating, the role from all over the world, it followed the very successful of reconnection in the corona, the solar-stellar Heidelberg meeting in April 2003. The main purpose of connection, plasma strands and the determination of the this conference series is to provide a forum in which to local heating function, and where next in the search for a develop the field of extrasolar planet research with solution to the coronal heating problem? respect to the two missions Darwin and TPF. NASA and ESA have recognised two primary, near-term goals in The proceedings were published as ESA SP-575. arranging these joint conferences: (1) involve the community in establishing high-level goals for TPF and Darwin; and (2) address key areas of research relevant to ‘8th Cluster Workshop’, New Hampshire, USA, 29 these ambitious missions that are important to the design September – 1 October 2004 and architecture of TPF and Darwin, respectively. One hundred and thirty Cluster scientists gathered to There were three major topics for this conference. The discuss the most recent scientific achievements of the first addressed recent results on exo-zodiacal (EZ) discs Cluster mission and to chart out the next phase of the from Spitzer and other space and ground observations. mission. During the 3-day workshop, the scientists Also predictions of expected and exciting new results discussed several hot-button topics in four working from Spitzer, HST/ACS, Keck/LBTI Interferometers, groups: Herschel and ground-based sub-mm telescopes on the evolution, structure, composition and frequency of debris — bow shock processes, structure, and dynamics; discs in the near and more distant future were discussed. — physics of the inner magnetosphere; Among the issues debated were how to extrapolate from — reconnection processes at the magnetopause and in the outer zodiacal clouds (Kuiper belt) detectable with the tail; Spitzer to the inner zodiacal clouds that will be — cusp dynamics and structure and auroral processes. measurable with TPF or Darwin. What do the Spitzer measurements of the outer zodiacal cloud tell us about More information about the workshop can be found at the presence or absence of planets? http://atlas.sr.unh.edu/cluster8/

Secondly, the link between the physical conditions in the early solar nebula and astrobiology, e.g. how might ‘The Three-Dimensional Universe’, Paris, France, astronomical conditions in the Hadean/Archaen periods 4-7 October 2004 affect the formation and evolution of life? New data from, for example, GENIE and the Keck-nuller may This major symposium, dedicated to the scientific provide new information on the properties of zodiacal aspects of the Gaia mission, was held at the Observatoire discs in the first 500 million years of a planetary system’s de Paris, Meudon, as ‘Les Rencontres de l’Observatoire existence. What does a high level of exo-zodiacal 2004’. Attended by 240 delegates, the 4-day meeting was emission imply in terms of bombardment and infall? an opportunity to present the status of the Gaia mission What other astronomical properties of a star and to the scientific community, and to hear the results of planetary system might be relevant to the formation of investigations carried out in the various areas of the stable, habitable planets, for example, the dynamics of mission over the previous 4 years. sec3.qxd 7/15/05 10:01 AM Page 100

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Activities and overall progress of the 14 scientific in the optical (Hubble and large 8-10 m ground optical working groups (from relativistic aspects of the data instruments such as ESO’s VLT), in X-rays (Chandra, analysis to the quasar reference frame) formed a major XMM-Newton) and other wavebands and facilities. part of the symposium. Various reports on the massive data analysis preparations gave a detailed perspective on The meeting was organised such that the various groups the complexities and challenges facing the on-ground working on this scientific preparation could meet and data treatment: the overall simulation chain, the current exchange their ideas, orientate their work towards the prototype data analysis system, Grid-related studies, and best strategies, and plan complementary goals for early the photometric data analysis. science with Herschel and ALMA. About 200 participants delivered a large number of oral and poster Five participants accepted the delicate challenge of presentations. summarising the poster presentations in the various categories. This effort contributed significantly to the The proceedings were published as ESA SP-577. coverage of a large variety of topics in a limited time, and was greatly appreciated by the participants. A highlight of the Symposium was the award by the Paris ‘6th International Conference on Exploration and Observatory of the degree of Doctor Honoris Causa to Utilisation of the Moon’, Udaipur, India, 22-26 the Honorary Chair of the Scientific Organising November 2004 Committee, Adriaan Blaauw, who celebrated his 90th birthday earlier in the year. The 6th International Lunar Conference was hosted by PRL and ISRO, and cosponsored by ILEWG and ESA. Generous financial support by various organisations The President of India, Dr. Abdul Kalam, addressed the connected to Gaia permitted the attendance at the meeting and made some highly relevant recommend- symposium of an unusually large representation of ations for international activities in exploration of the younger scientists (PhDs and post-docs), many of whom Moon, ‘for the benefit of human kind’. Discussions and are already playing a key role in the preparation of the presentations by 200 scientists from 17 countries focused ambitious Gaia mission. Attendees also included on new and planned missions to the Moon as well as collaborators from Greece (a new Member State of ESA) roadmap concepts for long-term exploration of the Moon and some non-member countries (Slovenia, Lithuania, and the utilisation of lunar resources. The programme Estonia, Australia). included key elements of science overview and opportunities for young scientists. The programme can The proceedings were published as ESA SP-576. be found on http://www.prl.ernet.in/~ILC6/ and the conference declaration on Sci.esa.int/ilewg

‘The Dusty and Molecular Universe – A Prelude to Herschel and ALMA’, Paris, France 27-29 October 2004 ‘Herschel Space Observatory Calibration Workshop: Models and Observations of Astronomical Calibration The future sub-mm and far-IR facilities of Herschel and Sources’, Leiden, The Netherlands, 1-3 December 2004 ALMA will make a breakthrough in our knowledge of star formation, the bulk of it occurring in dusty and The main purpose of the workshop was to provide an obscured regions, that can be revealed only at these overview of the state-of-the-art of models, observations wavelengths. They will shed light on the physical and laboratory spectroscopic studies associated with processes of galaxy formation, the formation of the first Herschel calibration sources, and to facilitate the stars after the dark age, starbursts in interacting and discussion between experts. The workshop brought merging galaxies, and the fuelling of black holes. The together calibration scientists from the three Herschel physics and chemistry of the interstellar medium will be instruments, members of the Herschel Science Centre known in unprecedented detail. The production of dust and the NASA Herschel Science Centre, planetary and and various elements in stars, supernovae and stellar stellar modellers and observers, and calibration scientists winds will be tackled by the observation of the from ground and space observatories that cover similar circumstellar medium. Knowledge of cometary and wavelength regions, in particular from ALMA, Astro-F, planetary atmospheres will be considerably enhanced, ISO, JCMT, Planck, SOFIA, Spitzer Space Telescope and their molecular abundances revealed. and SWAS.

The scientific preparation for the utilisation of these Over 45 scientists from Europe, USA and Japan attended facilities, expected to become operational just a few the meeting. The workshop programme was organised in years from now, is already underway using the legacy of both plenary and splinter sessions. The four splinter IRAS and ISO and through the presently operating sessions focused on the topics of Mars and giant planets, ground-based (sub)mm telescopes and the recent Spitzer Asteroids and satellites, Stars and secondary calibrators, IR space telescope. Complementary surveys are obtained and Calibration and cross-calibration strategies. sec3.qxd 7/15/05 10:01 AM Page 101

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The talks in the plenary sessions covered subjects 4.2 ESA Technology Programmes common across the splinters. They included presentations on the Herschel mission and of the The ESA science directorate relies heavily on three Herschel instruments’ calibration strategies. Other talks programmes to ensure technology developments are in provided overviews on the use of Solar System objects as place to support future missions. These are: calibrators, of the current knowledge of solid-state features in the far-IR and of the work in progress to study — the Core Technology Programme, funded directly and model the far-IR background. The workshop from the Science Programme and covering the needs achieved its objectives and definitely helped in of embryonic future missions and of more mature determining the future path for the calibration missions either in assessment or under definition. preparatory work. This programme focuses on high-priority core technologies needed specifically within science and The viewgraphs of the presentations and a list of actions covers the complete range of technology readiness identified during the meeting are collected on the levels (TRLs 1-10). workshop web page (http://www.rssd.esa.int/Herschel/ — the Technology Research Programme (TRP), funded hcal_wkshop.shtml). The models and observations of by the ESA General Budget and accessed by all astronomical calibration sources will be consolidated, customer directorates. In general, it covers documented and made available to the calibration technology in the early stages of development scientists through a common database. (essentially TRL levels 1-3). — the General Support Technology Programme (GSTP), funded directly by those Member States RHESSI/SOHO/TRACE Workshop, ‘Coordinated Obser- vations of Flares and CMEs’, Sonoma, California, USA, 8-11 December 2004 Figure 4.2/1: The various programmes and their The RHESSI/SOHO/TRACE workshop was oriented relationship with the Technology Readiness Levels towards the synthesis of data from these three missions used within ESA. and ground-based data. The workshop was attended by over 140 participants. With the emphasis being on actual research work, there were no set presentations other than four introductory talks. To maximise the exchange of ideas and foster new research arrangements, the workshop was organised around seven parallel working groups covering: pre-event physics; magnetic reconnection & formation of current sheets; inter- relationships of flares/CMEs in ‘super’ events; solar origins of solar energetic particles; ribbons and foot- points; imaging spectroscopy of the thermal plasma; particle acceleration and transport.

Figure 4.2/2: The overall flow of the technology planning and implementation process. TDA: Technology Development Activity. TRM: Technology Reference Mission. sec3.qxd 7/15/05 10:01 AM Page 102

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interested in a specific technology item. Generally, it 4.3 Coordination and Other Supporting Activities matures technology for direct application and therefore covers TRL levels 4-10. EIROforum

Figure 4.2/1 illustrates the overall approach to these The EIROforum is a partnership between seven leading various programmes and the associated TRL level. European intergovernmental research organisations: CERN, EFDA, EMBL, ESA, ESO, ESRF and ILL. As Of course, the individual items entering the various world leaders within their respective fields of science, programmes, whatever the funding approach, are crucial the member organisations represent the vanguard of to the overall success. Fig. 4.2/2 illustrates this complex European science, proving that European scientists can process, which attempts to ensure that the correct be competitive at the forefront of research. These technology needs of the Science Programme are organisations have a vital role to play in the future of identified and eventually enter the programme at the European research. A primary goal of EIROforum is to right time. SCI-A conduct studies into test-case missions, play an active role in promoting the quality and impact of known as Technology Reference Missions (TRMs), that European research through effective high-level inter- examine technical feasibility, costs and technology organisational interaction and coordination. This is needs. These TRMs assist the programme in providing possible by exploiting the existing intimate links inputs to the science community with regard to possible between the member organisations and their respective future projects as well as identifying core technologies, European research communities. often at a very low TRL, that may need to be developed in the longer term. The Head of RSSD is a member of the ESA EIROforum delegation. During the reporting period, ESA has occupied the chairmanship of the group for the last 6 months, with the Director of Science representing the Director General of ESA. In this period, a decisive push has been given to the previously existing working groups on instrumentations, grid technologies, human resources and, in particular, the preparation of a knowledge data- base on the management of large infrastructures. From the policy point of view, an EIROforum vision paper was prepared during the last year that is now being presented to the organisations of the European Union and, in particular, to the Science and Research Commission.

AVO/EURO-VO

Work continues on the development of Virtual Observatory (VO) tools in cooperation with other European organisations. After the success of the Astrovirtel programme, members of the Department in ST-ECF and ESAC are preparing the next steps in this much-needed resource for modern astrophysical research using a variety of observational databases, both ground- and space-based.

The last demonstration of the Astrophysical VO (AVO) project, before the beginning of the implementation of its fully-fledged form, was performed at ESAC. The use of archival data (including ISO and XMM) for this type of research was found to be particularly useful. Cooperation with ESO, through ST-ECF, as well as other astronomical centres in Europe, is envisaged in the preparation of a proposal to the European Commission for funding of some of the components of AVO. More information is given in the Divisional sections of this report. sec3.qxd 7/15/05 10:01 AM Page 103

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Opticon Fellows, funded to work 1 or 2 years in ESA Member States’ institutions outside their home countries. These The ST-ECF, on behalf of RSSD, participated in the Fellows contribute to research networking in support of Opticon network. This is an ‘Integrated Infrastructure ESA missions. Research Fellows working with the ESA Initiative (I3)’ European Commission-funded pro- SOHO team at NASA/GSFC or at the STScI are also gramme that comprises networking, a trans-national recruited via this scheme. access programme and a series of six technology projects called Joint Research Activities. RSSD contributes to these activities through the ST-ECF group in Garching General Scientific Support (D); the involvement of other members of the Department is being encouraged in specific JRAs linked RSSD staff provided scientific advice and support to and more closely to space projects. participated in committee and working groups not directly within the purview of the Scientific Directorate or of ESA. These included: Europlanet — A. Gimenez is a member of the Council of the This is a new European Commission-funded network of European Astronomical Society and President of the coordinated activities in planetary sciences. It was set up IAU Commision on Binary Stars. to achieve a long-term integration of this discipline in — G. Schwehm continued to provide support to the Europe. Its aims are to increase the science return of Agency’s Space Debris Working Group and as as planetary projects, with emphasis on major exploration coordinator for all planetary protection activities missions, to initiate a long-term improvement of the within the Agency. European planetary work infrastructure, to improve — in coordination with ESA’s International Affairs European scientific competitiveness, to develop and Department, RSSD staff have continued to provide spread expertise in this area of research, and to develop support to the organisation and programme public understanding of and support for planetary science development of the UN/ESA Workshops on Basic and exploration. Space Science. This series of workshops has found a special niche in identifying opportunities to promote These goals will be achieved by maximising synergies space science in the developing nations, both in between different fields contributing to planetary order to provide opportunities for professional sciences: space observations, Earth-based observatories, scientists, and as a means of enhancing the role of laboratory studies, numerical simulations and the science in the educational systems of these nations. development of databases. In addition, the design and The results of the first ten of these Workshops were development of an Integrated and Distributed summarised in the book Developing Basic Space Information Service providing access to the full set of Science World-Wide (W. Wamsteker, R. Albrecht, data sources produced by the mentioned complementary H. Haubold, Eds. Kluwer, Dortrecht, 2004). The fields is a driver of the project. 11th UN/ESA Workshop, originally scheduled for November 2003 in Beijing, China, was rescheduled owing to the SARS epidemic, and held in May 2004, Astronet hosted by the government of P.R. China and the Chinese Space Agency. The emphasis was on Very recently, members of RSSD have been involved in promoting international and regional collaboration, the preparation of a proposal to the European and access to data from high-end facilities via the Commission for funding of a network of European Virtual Observatory. The concept of a World Space research agencies in astronomy. Though only associated Observatory, as an effective means of stimulating members rather than full partners, owing to the nature of space science in developing countries, and ESA as a European organisation, an ambitious work plan generating better opportunities for participation of has been designed aimed at structuring and coordinating scientists from developing countries in space science European astronomical research. This plan is based on a and education, was further pursued. Responsibility number of work packages, including networking, a for liaison with the United Nations was transferred to strategic review of European astronomy, an R. Albrecht (ST-ECF) after the retirement of infrastructure roadmap and coordinated actions to W. Wamsteker. strengthen astronomy and astrophysics in Europe — B.H. Foing is the ESA representative and Executive Director of the International Lunar Exploration Working Group (ILEWG), a body charged with External Research Fellows developing and coordinating an international strategy for the exploration of the Moon. He also In addition to the internal Research Fellowship participated in a Cosmic Study of the International Programme, there are about 20 External Research Academy of Astronautics on ‘Next Steps in sec3.qxd 7/15/05 10:01 AM Page 104

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Exploring Deep Space’, led by Dr. W. Huntress 4.4 Science Communications (Carnegie), released in July 2004. The IAA study outlines compelling scientific and cultural Supporting the ESA Corporate and Science Communi- imperatives that provide the context for a vigorous cation Services programme of robotic science missions and for a systematic and evolutionary architecture for human RSSD Project Scientists and staff supported a number of expansion into the Solar System. science communication activities related to their — RSSD staff were active in numerous scientific projects. These include text and pictures for leaflets, societies (EAS, EGS, EPS) and some of the posters and brochures, and contributions to 80 web Scientific Unions (COSPAR, IAU, IRSI, IUPAP), stories in 2003 and 67 stories in 2004 for the ESA public where they contributed to scientific meetings by website (www.esa.int) and ESA space science pages organising special sessions and discussions, and, in (www.esa.int/esaSC). Of the more than 90 and 140 ESA some cases, holding elective offices. For example, press releases in 2003 and 2004, respectively, 79 and 67 H. Svedhem is a member of EGU Council and were related to science. In addition, more than 82 press President of the Geophysical Instrumentation releases were issued by STScI over the 2 years. Section of the EGU. — RSSD staff also taught space sciences and related A large effort was made by RSSD staff to support the topics in Member State universities and in several development, input updating and maintenance of the instances were also appointed as jury members for ESA scitech website (sci.esa.int), aimed at the scientific Ph.D. theses. The direct contact between ESA staff and educated communities, with specific information on and students and staff at the Universities continues to all missions: status reports, announcements, upcoming be mutually rewarding. events, latest publications, mission background, science, spacecraft and science operations, services, image gallery and videos. The Chief Scientist proposed an overall structure for the thematic contents of the scitech site.

RSSD staff (in particular, Project Scientists) supported ESA Corporate PR services in the production of TV broadcast material related to ESA science missions, in a variety of formats: documentaries for the general public; documentaries for the technical public; Index, A- and B- rolls; video Index, chapter structured; Interviews; Video News Releases; and live action. This material was distributed by ESA PR at related events or broadcast on ESA TV to European channels.

Contents of ESA Science Communication Stories for the Public in 2003-2004

ESA’s PR emphasis is often directed towards launch campaigns. RSSD Project Scientists supported ESA PR offices, in coordination with project teams, by preparing material, text and pictures for stories about these science missions from complementary viewpoints at selected milestones: the science background and goals, prepara- tion and key events for the spacecraft, specific instru- ments and technologies, initial results and more complete results.

Mars Express was the subject of 51 web stories in 2003- 2004, including the preparation for launch in June 2003, the arrival at Mars on 25 December, the search for Beagle-2 and the related enquiry, and the results from the orbiter. These included the spectacular stereo imagery of Mars’ geology, volcanoes, water features, impact craters, the detection of polar water ice by the instruments, the detection of methane by the Planetary Fourier Spectro- sec3.qxd 7/15/05 10:01 AM Page 105

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meter, water loss in the atmosphere, evidence for recent and cycles, clusters of galaxies, dark energy, accretion volcanism and glacial activity. RSSD staff supported a onto rotating black holes and dead-star magnetism. With number of press events, covering both mission aspects Integral, the stories included the hot trail of Geminga, and research. gamma-ray bursts, hidden black holes, and the new view of the Milky Way. The ESA website also mirrored or The communications activities on SMART-1 included expanded some of the HST stories and imagery from promotion of lunar and planetary science, new STScI. In addition, some HST stories from STScI technologies, people and new methods for small space exploited the use of spectacular images, such as the light missions, and exploration. The Project Scientist echo around an erupting star. supported film crews working on interviews and documentaries on SMART-1 and lunar exploration. He Some general astronomical stories were produced on supported media briefing events in March 2003, as well virtual observatories, the space grid, the search for as the pre-launch campaign in September 2003. The first exoplanets, star formation, origin of the Universe, results from the commissioning, cruise, navigation and mapping the Milky Way and preparing the background lunar capture on 15 November 2004 were featured. The for the upcoming Herschel, Planck, Gaia and JWST SMART-1 team collaborated with ILEWG (sci.esa.int/ observatories. ilewg) and the Lunar Explorers Society, (lunarexplorer. org) in public events. PR events were organised at the RSSD scientists supported a large number of other ILEWG conferences in Hawaii (2003) and Udaipur, communication activities during 2003-2004, including: India (2004) in the presence of Apollo astronauts and the President of India, respectively. — Le Bourget, Farnborough and other space fairs. Animations included presentations on space science The Cassini/Huygens arrival at Saturn prompted 10 and technology for the press and the public, 3-D stories on the critical Saturn orbit insertion, four from visualisations and demonstration models from some Cassini flybys (Phoebe, Titan, new moons) and the ESA space missions. preparation for the release of Huygens over Christmas — RSSD Project Scientist staff organised or supported 2004, building up the interest for the 14 January 2005 science communication events aimed at the science atmospheric entry and landing. community at large during sessions at the EGU in Nice, IAF in Bremen and Vancouver, COSPAR in Rosetta also enjoyed high PR activities during 2003- Paris, IAU, the JENAM joint European astronomy 2004, with 19 web stories emphasising the launch meeting, and national astronomy meetings. They campaign, the delay to 2004 and the environmental assisted in the organisation of a number of exhibition testing, as well as the science involved, such as the events (co-sponsored by ESA) featuring ESA space origins of the Solar System and the delivery from comets science missions. of the ingredients for life. — RSSD staff contributed ESA space science communication activities (highlights from ESA RSSD staff also contributed to educational and outreach science missions, lunar and planetary exploration, activities related to astronomical events such as lunar astronomy, space science, etc.) at press conferences, eclipses, the Mercury transit in May 2003 and the Venus and scientific and public assemblies (COSPAR, transit on 8 June 2004. EGS/EGU, IAF, IAU). — RSSD staff supported collaborative science Observations and discoveries made with SOHO have communication events with museums, planetariums continued to make the headlines, with a number of CNN and educational institutions all over Europe. A news stories. Special stories include the giant Halloween network of space science communication partners superflare of October-November 2003, and the detection was further developed, such as the British Festival of (mostly by amateurs) of more than 750 comets with Science, Space Week and the Association of Science SOHO. The solution of the high-gain antenna problem Journalists. was also newsworthy. Articles about SOHO have appeared in several popular magazines. Several film and TV crews visited the operations facility, and SOHO was Supporting Education, Teachers and Student Outreach featured in a number of science TV programmes. SOHO Initiatives observations and images play a prominent role in the 40- min giant-screen IMAX documentary ‘SOLARMAX’ RSSD participated in outreach activities such as the (www.solarmovie.com). ‘Physics on Stage’ events for teachers at ESTEC in November 2003, and Life in the Universe, Moon, Mars, Astronomy missions had a modest level of PR and ESA planetary and astronomy workshops. They provided science communication activities, with seven ESA press lectures and tutoring as part of the ESA student initiative releases and 10 web stories in 2003-2004. Themes that allowed the participation of 300 students at IAF included X-ray astronomy, with stories on stellar coronae Bremen in October 2003 and IAF Vancouver in October sec3.qxd 7/15/05 10:01 AM Page 106

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2004. They also served as lecturers and as reviewers in student projects coordinated by the ESA Outreach and Education Office. They advised the Education Office on the science background of hands-on projects for students. Public outreach activities were conducted during astronomical events such as the Mercury and Venus transits. They contributed lectures during conferences, public events, festivals of science, and university and institute general lectures and open days.

ESA Science and Technology Website (Missions and News): http://sci.esa.int ESA corporate portal: www.esa.int, with public science website: www.esa.int/esaSC ILEWG site: http://sci.esa.int/ilewg/ HST news site: http://hubblesite.org sec4.qxd 7/12/05 9:52 AM Page 107

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ANNEX 1: MANPOWER DEPLOYMENT

Department Office, ESTEC ESA Research Fellows Boirin, L., (to September 2003), X-ray astronomy Head of Department Del Burgo, C., (to September 2004), Modelling of sky Gimenez, A. as seen by Planck Diaz Trigo, M., (from May 2004), Data analysis Chief Scientist concentrating on study of stellar coronae and Foing, B.H., SMART-1 Project Scientist, comparative absorption lines in compact sources planetary and astrobiology, solar-stellar physics. Dupac, X., (to October 2004), Planck-related science on cosmic background and interstellar dust Administrative staff Hony, S., (to January 2005), Interstellar medium, circum- Bingham, C., Departmental Assistant Administrator stellar envelopes, dust Ihaddadene, S., Divisional Secretary and Admin. Husain, G., (from October 2003), Stellar activity, Assistant coronae Schroeder, B., Divisional Secretary and Admin. McBreen, S., (from October 2004), Analysis of Integral Assistant and XMM data on compact accreting sources Villien, C., Divisional Secretary and Admin. Assistant Papadopolous, P., (to March 2003), Interstellar medium Sanz Forcada, J., (from February 2004), Astero- Project Controllers (seconded from SCI-M) seismology D’Aquino, G. Stankov, A., (to January 2004), analysis of stellar Davis, R. seismology Fontaine, R. Spanish/Portuguese Trainees Perez-Ramirez, D., (to January 2004), Reduction of Astrophysics Missions Division XMM-Newton data Silva, B., (to October 2004), Computer model to Clavel, J., Head of Division, Multiwavelength simulate number and distribution of planets that observational astronomy. Eddington could find Boeker, T., (from September 2003), JWST Scientist, Galaxy formation and evolution De Bruin, J., Gaia Support Scientist Solar and Solar-Terrestrial Missions Division Favata, F., Eddington Study Scientist, COROT Project Scientist, support to Gaia studies, cool stars and Opgenoorth, H., (from April 2003), Head of Solar and stellar activity, X-ray astronomy Solar-Terrestrial Missions Division Fridlund, M., IRSI/Darwin Study Scientist, astrophysics Brekke, P., (to November 2004), Support to SOHO of star formation Project Scientist, solar physics, science Heras, A., Herschel scientist, IR astronomy communication Jakobsen, P., JWST Study Scientist, optical/UV Escoubet, C.P., Cluster and Double Star Project astronomy with HST and ground-based astronomy Scientist, magnetospheric physics Laureijs, R., Planck Deputy Project Scientist, Fehringer, M., (to March 2003), Support to Cluster and interstellar medium, dust properties Double Star Project Scientist, Microscope Study Leeks, S., (from April 2003), Herschel Instrument and Scientist (under the Fundamental Physics Missions Calibration Scientist Division) Marston, A., (from April 2003), Herschel Instrument Fleck, B., SOHO Project Scientist, Solar Orbiter Study and Calibration Scientist Scientist, solar physics Parmar, A., Acting Integral Project Scientist, XEUS, Haugan, S., SOHO Science Operations Coordinator, Lobster, Rosita & EUSO Study Scientist, Leader for solar physics the SAX LEGSPC, X-ray astronomy (X-ray binaries Marsden, R.G., Ulysses Project Scientist and Project and AGNs) Manager, Solar Orbiter Study Scientist, ILWS Perryman, M.A.C., Hipparcos Project Scientist, Gaia support, energetic particle data interpretation Project Scientist, exploitation of Hipparcos data Sanchez, L., SOHO Science Data Ordinator, SOHO Pilbratt, G.L., Herschel Project Scientist, IR and archive sub-mm astronomy Sanderson, T.R., Cluster Archive Scientist, energetic Prusti, T., Herschel Scientist, IR astronomy particle instrument development and data Tauber, J., Planck Project Scientist, sub-mm astronomy interpretation Vavrek, R., (from April 2004), Herschel Instrument and Calibration Scientist sec4.qxd 7/12/05 9:52 AM Page 109

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ESA Research Fellows Young Gradutate Trainees Khan, H., (from August 2004), Magnetospheric physics Conan, Y., (to April 2004) research based on analysis of Cluster data Merikallio, S., (from August 2004), Spacecraft Pitout, F., (to December 2004), Magnetospheric charging research based on analysis of Cluster data Sarkarati, N., (from May 2004), Experiment modelling Regnier, S., (from February 2004), Study of structure and dynamics of solar surface fields (EU Fellow) Spanish/Portuguese Trainees Almeida, M., (from April 2003), SMART-1 AMIE ESA External Fellow calibration, science operations support McIntosh, S., (to February 2003), Criticality of solar Perez Ayucar, M., (to June 2004), Telecommunication flares and chromospheric dynamics Engineer – Huygens Simoes, F., (to September 2004), Water on Mars Vazquez Garcia, J.L., (to May 2004), Planetary Missions Division Telecommunications Engineer – SMART-1

Schwehm, G., Head of Division, Rosetta Project Stagiaires Scientist Andurand, P., (March-September 2003) Chicarro, A., Mars Express Project Scientist, planetary Civeit, T., (April-September 2003) geology Couturier-Doux, S., (April-October 2004) Grard, R.J.L., (to November 2003), BepiColombo Maloreau, S., (March-August 2003) Project Scientist, modelling and instrument Nicoll, R., (February-April 2003) development Piberne, R., (April-October 2004) Koschny, D., Support to Rosetta Project Scientist, Roussos, E., (April-July 2004) science operations planning, meteor research, Sarmiento Ares, E., (March-August 2004) planetary cameras Seoane Purrinos, L., (March-August 2004) Laakso, H., (from April 2003), Support to Cluster, Van Kan, M., (March-August 2004) magnetospheric plasma research Vicente, D., (March-August 2003) Lebreton, J.-P., Huygens Mission Manager, Solar Zeyen, B., (April-July 2003) System technology support, plasma physics instrument development Martin, P., Mars Express Operations Scientist Fundamental Physics Missions Division Ocampo, A., (to February 2004), Support to Mars Express and BepiColombo Reinhard, R., Head of Fundamental Physics Division, Schulz, R.M., Bepi Colombo Project Scientist (from LISA Pathfinder Project Scientist 2003), cometary studies Caccapuoti, L., (from December 2004), ACES Project Svedhem, L.H., Venus Express Project Scientist, Scientist (for D/HME) development of planetary instrumentation, cosmic Fehringer, M., MICROSCOPE Study Scientist (to dust studies March 2003) Witasse, O., Huygens, planetary atmospheres Jafry, Y., (to August 2004), drag-free control expert for Wirth, K., (from August 2003), Planetary fundamental physics missions Scientist/Applied Physicist Jennrich, O., LISA Project Scientist

Research Fellows Boudin, N., (to February 2004), Astrochemistry Space Telescope Operations Division Campbell, M., (to December 2003), Observations and monitoring of meteors Macchetto, D., Head of Division, AGN, Elliptical Cord, A., (from October 2004), Analysis of imaging galaxies, gamma-ray bursts Mars Express data Davidsson, B., (from May 2003), Comet nuclei ST-ECF, Garching thermophysical modelling and observations ESA scientific staff Makinen, J., (to December 2003), Cometary science Benvenuti, P., (to October 2004), HST Project Scientist, (data analysis and modelling) Head of ECF, extragalactic HII regions, SNRs Michael, G., (to April 2004), Comparative planetology. Albrecht, R., Deputy Head ECF, Head of Science Data Piot, A., (to February 2004), exploitation of Huygens and Software Group, minor bodies of the Solar test balloon data System, computer science Zegers, T., (from May 2003), Geology and hydrology of Dolensky, M., (to January 2003), Science archive and Mars with Mars Express WWW software specialist Fosbury, R.A.E., Head of HST User Support Group, galaxies and AGNs sec4.qxd 7/12/05 9:52 AM Page 110

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Micol, A., Science Archive Software Specialist, image gravitational lensing and cosmology, stellar processing techniques and information systems dynamics, photometry Rosa, M.R., Head Post-operational Archive Group, HII Miebach, M., Lead Engineer for Scientific regions, star formation, supernovae, evolution of Instruments galaxies Mobasher, B., STIS Instrument Scientist, Galaxy Sforna, D., Science Programmer, Systems Analysis surveys, dwarf galaxies, elliptical galaxies Padovani, P., (to August 2003), Multi-Mission Archive ESO staff (included here to give the full picture of Scientist, AGN: unified schemes, evolution, X-ray ST-ECF team staffing) spectra, blazars Freudling, W., Instrument Scientist, observational Panagia, N., NGST Science Lead, stars, interstellar cosmology, peculiar motion of galaxies medium, supernovae, galaxies, cosmology Haase, J., Astronomical Data Archive and Pipeline Robberto, M., WFC3 Instrument Scientist, star Software Specialist formation, massive stars, IR instrumentation Hook, R.N., HST Data Analysis Scientist, scientific Sirianni, M., ACS Instrument Scientist software support, image restoration applications Stanghellini, L., (to April 2004), Proposal Scientist, Kuntschner, H., Instrument Scientist, galaxy formation planetary nebulae and their central stars, and evolution extragalactic distance scale Pierfederici, F., ASTROVIRTEL Support Scientist Villaver, E., (from February 2004), Astronomer Pirenne, B., HST Archive Scientist, data storage Wiklund, T., NICMOS Instrument Scientist, AGN, technology, gravitational lenses Starburst Galaxies Pirzkal, N., Scientific Analyst/Programmer, pre-main- sequence stars ESA External Research Fellows Sjöberg, B., ST-ECF Admin. Assistant / Secretary van Bemmel, I., (from March 2003) Walsh, J.R., Instrument Scientist, planetary nebulae, HII regions Science Operations and Data Systems Division ESO staff under ESA contract Alexov, A., Post-Operation Instrument Scientific Staff Programmer Kessler, M.F., Head of Division, Infrared Bristow, P., Post-Operation Instrument Scientific Astronomy Programmer Bennett, K., Gamma-ray astronomy, Planck (Co-I) Christensen, L., HST Outreach Astronomer Jansen, F., XMM-Newton/Mars Express Mission Fourniol, N., Archive Operator Manager, X-ray astronomy Kerber, F., Post-Operation Instrument Scientist, early- Szumlas, M., Technical coordination, Data Bank type stars maintenance Kornmesser, M., HST Outreach Technical Editor Thoerner, G., Divisional system analyst/computer Pasquali, A., Instrument Scientist, stellar winds, manager, SAX data analysis and cosmology studies nebulae Toni, A., Senior data technician Winkler, C., Integral Project Scientist, gamma-ray astronomy data analysis STScI, Baltimore Wamsteker, W., (to November 2004), Multi- Aloisi, A., STIS Instrument Scientist disciplinary scientist, active galaxies, abundances at Arribas, S., NICMOS Instrument Scientist, AGN, high- high redshifts (located at Vilspa) redshift galaxies, cosmology Zender, J.J., Data handling/archiving management for Boeker, T., (to August 2003), NICMOS Instrument planetary science operations Scientist, galaxy formation and evolution, in particular gas dynamics in the central regions Research Fellows Clampin-Nota, A., Deputy Head, Science Division, Sanz Forcada, J. (from February 2004), Data analysis massive stars, late stages of stellar evolution, IMF on physics of stellar coronae and absorption studies De Marchi, G., (to 2003), ACS Instrument Scientist, Herschel Science Centre, ESTEC initial mass function, globular clusters, dark matter Staff haloes Riedinger, J., Herschel Science Centre Development Jenkner, H., HST Mission Deputy, Guide Star Catalog Manager II, microvariability studies using FGS photometry Mathieu, J-J., Interactive Analsysis (p.t., TOS support) Kamp, I., (from May 2004), Astronomer Ott, S., System Analyst, Interactive Analysis Mais-Appellaniz, J., Spectrographs Instrument Scientist, Coordinator HII regions, young clusters Prades-Valls, R., Quality Assurance (p.t., TOS Meylan, G., (to August 2004), Proposal Scientist, support) sec4.qxd 7/12/05 9:52 AM Page 111

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Integral Science Operations Centre (ISOC) Pollock, M. RGS Calibration Scientist Staff Santos-Lleo, M., XMM-Newton user support, Hansson, L., Integral Science Operations Manager observational astronomy Barr, P., Operations scientist, mission planning Schartel, N., XMM-Newton User Support and Mission Much, R., (to August 2004), Operations scientist and Planning Group Team Leader, observational Deputy Project Scientist, Observational astronomy astronomy O’Rourke, L., (from September 2004), Science Operations Engineer (ESAC) Research Fellows Orr, A., Operations scientist, JEM-X and OMC expert, Bianchi, S., (from October 2004), XMM-Newton data responsible for helpdesk analysis of AGN Sternberg, J., System engineering, ISDC liaison Gimenez Bailon, E., (from May 2003), Seyfert High Energy Integral Science Data Centre (Geneva) Piconcelli, E., (from April 2003), Study of AGN Staff Texier, D., (to August 2004), Resident Engineer Science Archives Group (VILSPA) Staff ISO Data Centre (IDC), (ESAC) Arviset, C., System engineering. Archive group leader Staff Garcia-Lario, P., ISO Resident Astronomer, cross- Mars Express calibration expert, Handbook co-editor, late stages of Staff stellar evolution Texier, D., (from August 2004), Mars Express Science Gry, C., (to October 2004), ISO Resident Astronomer, Operations Coordinator LWS expert, LWS Handbook, interstellar medium Lorente, R., ISO Resident Astronomer, ISOCAM expert Peschke, S., (to April 2003), ISO Resident Astronomer, Science Payload and Advanced Concepts Office ISOPHOT expert, comets Salama, A., ISO Project Scientist SWS expert, Titan, Peacock, A., Head of Office, STJ Research Team novae and symbiotic stars Leader Verdugo, E., Resident Astronomer, ISOPHOT expert, Andersson, S., Electronics engineering for advanced ISO Data Archive products quality technologies for semiconductors sensors Appourchaux, T., Solar Orbiter payload support, solar Research Fellows research. COROT instrument Research Team Garcia-Hernandez, A., (from September 2004), analysis Leader of stellar ISO archival data Adriaens, M., (to June 2002), Mechnical engineer Sanchez Fernandez, C., (to April 2004), ISO and XMM- Arends, H., Mechanical engineer and mechanical Newton data analysis laboratory coordinator Bavdaz, M., Advanced technologies sensors and optics, Young Gradutate Trainee Sensors and Optics Research Team Leader, Head of Carter, J., (from May 2004), Astronomer Advanced Technology Section (p.i.) Beaufort, T., Electronics engineer for COROT PDU Spanish Trainee Biezen, J.F. van der, Electronics and laboratory Del Mar Siere Gonzalez, M., (to Novembre 2004), ISO metrology support to advanced technology data reduction and XMM-Newton RGS wavelength programme. calibration Butler, B.A.C., Instrument development engineer Dordrecht, A. van., Advanced Sensors electronics XMM-Newton SOC (VILSPA) engineer Staff Erd, C., Sensor research and development, ESA Altieri, B., Software and payload support, observational missions support astronomy Falkner, P., Electronics research and development, Head Arpizou, M., Secretarial and administrative support of Planetary Exploration Section (p.i.) Ehle, M., XMM-Newton user support, observational Gondoin, Ph., Darwin-Genie instrument manager, astronomy XMM observational research Gabriel, C., XMM-Newton instrument support, Heida, J., Instrument support engineer supernova remnants, cosmology Jolander, B., Head of Instrument Support Group, Guainazzi, M., XMM-Newton user support, instrument development engineer observational astronomy Klinge, D., Instrument development engineer Kirsch, M. EPIC Calibration Scientist Lumb, D., Advanced sensor research, XEUS and ISS Metcalfe, L., XMM-Newton Science Support Manager payload and mission support, XMM observational Munoz Peiro, J., Instrument Operations Manager research sec4.qxd 7/12/05 9:52 AM Page 112

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Martin, D., SCAM3 instrument manager, Head of Infrastructure Section (p.i.) Rando, N., Payload support and development engineer. Head of Missions Section (p.i.) Romstedt, J., In-situ planetary instrument development, Rosetta-MIDAS (AFM) Lead Scientist Smit, L.C., Instrument development support engineer Telljohann, U., Instrument electronics engineer Verveer, J., Laboratory cryogenic systems support

Research Fellows Molster, F., Rosetta-MIDAS AFM

Stagiares Kilter, M., (August 2003-January 2004) Kozak, R., (July-August 2003) Larfors, K. Leyder, J.-C., (January-March 2004)

Trainees Moreira, O., (Portuguese Trainee from April 2002), Helioseismology Pitcher, K., (June-August 2001), International Law

RSSD acknowledges the valuable contribution made by the contractor staff to the work of the Department.

Erratum from previous Report (2001-2002): Head of Astrophysics Division (to October 2001) and Acting Head of Department (to May 2001); Taylor, B.G. sec4.qxd 7/12/05 9:52 AM Page 113

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114 publications

ANNEX 2: PUBLICATIONS 2003, New Directions for Close Binary Studies: The Royal Road to the Stars, 3, 19. Ribas, I., Jordi, C., Vilardell, F., Guinan, E.F., Hilditch, Head of Research and Scientific Support Department R.W., Fitzpatrick, E.L., Valls-Gabaud, D., Gimenez, Refereed Journals, 2003 A., Properties and Distances of Eclipsing Binaries in M31, 2003, Extragalactic Binaries, 25th meeting of Claret, A., Willems, B., Gimenez, A., Unveiling the the IAU, Joint Discussion 13, JD123E, 35R. internal constitution of components of close binary Shaver, P.A., Dilella, L., Gimenez, A., Astronomy, systems, 2003, Recent Research and Development in Cosmology and Fundamental Physics, 2003, Proc. Astronomy and Astrophysics, 375. ESO-CERN-ESA Symposium, ESA. Clausen, J.V., Storm, J., Larsen, S.S., Gimenez, A., Silver, E.H., Schnopper, H.W., Jones, C., Forman, W., Eclipsing binaries in the Magellanic Clouds. uvby Bandler, S.R., Murray, S.S., Romaine, S.E., Slane, CCD light curves and photometric analyses for HV P.O., Grindlay, J.E., Madden, N.W., Beeman, J.W., 982 (LMC), HV 12578 (LMC), HV 1433 (SMC), and Haller, E.E., Smith, D.M., Barbera, M., Collura, A., HV 11284 (SMC), 2003, A&A, 402, 509-530. Christensen, F.E., Ramsey, B.D., Woosley, S.E., Domingo, A., Caballero, M.D., Figueras, F., Jordi, C., Diehl, R., Tucker, G.S., Fabregat, J., Reglero, V., Torra, J., Mas-Hesse, J.M., Giminez, A., Hudcova, V., Gimenez, A., B-MINE, the balloon-borne micro- Hudec, R., The Input Catalogue for the OMC camera calorimeter nuclear line explorer, 2003, X-ray and onboard INTEGRAL, 2003, A&A, 411, L281-L289. Gamma-ray telescopes and Instruments for Astron- Gimenez, A., Lund, N., Preface, 2003, Adv. Space Res., omy, Proc. SPIE, 4851, 905-912. 31/Issue 2, 275. Mas-Hesse, J.M., Gimenez, A., Culhane, J.L., Jamar, C., McBreen, B., Torra, J., Hudec, R., Fabregat, J., Head of Research and Scientific Support Department Meurs, E., Swings, J.P., Alcacera, M.A., Balado, A., Refereed Journals, 2004 Beiztegui, R., Belenguer, T., Bradley, L., Caballero, M.D., Cabo, P., Defise, J.M., Diaz, E., Ribas, I., Jordi, C., Vilardell, F., Gimenez, A., Guinan, Domingo, A., Figueras, F., Figueroa, I., Hanlon, L., E.F., A program to determine a direct and accurate Hroch, F., Hudcova, V., Garcia, T., Jordan, B., distance to M31 from eclipsing binaries, 2004, New Jordi, C., Kretschmar, P., Laviada, C., March, M., Astronomy Reviews, 48/9, 755-758. Martin, E., Mazy, E., Menendez, M., Mi, J.M., de Miguel, E., Munoz, T., Nolan, K., Olmedo, R., Plesseria, J.Y. Polcar, J., Reina, M., Rnotte, E., Rochus, P., Sanchez, A., San Martin, J.C., Smith, A., Soldan J., Thomas, P., Timon, V., Walton, D., OMC – An Optical Monitoring Camera for INTEGRAL. Instrument and Description, 2003, A&A, 411, L261- L268. Ribas, I., Solano, E., Masana, E., Giminez, A., Effective temperatures and radii of planet-hosting stars from IR photometry, 2003, A&A, 411, L501-L504.

Head of Research and Scientific Support Department Proceedings and other Publications 2003

Favata, F., Gimenez, A., The Eddington Mission (co-authored by the Eddington Science Team), 2003, Solar and Solar-like Oscillations – Insights and Challenges for the Sun and Stars, 25 th Meeting of IAU, Joint Discussion 12, JD12E, 51F. Gimenez, A., The Future of Optical Astronomy in ESA’s Science Programme, 2003, ASP Conf. Proc. Hubble’s Science Legacy – Future Optical/Ultraviolet Astron- omy from Space, 136-2, 22. Gimenez, A., Concluding Remarks and Future, 2003, Extragalactic Binaries, 25th meeting of the IAU, Joint Discussion 13, 18 July 2003. Sydney, Australia, JD13E, 31G. Gimenez, A., Eclipsing Binaries and Stellar Astronomy, sec4.qxd 7/12/05 9:52 AM Page 115

publications 115

Astrophysics Missions Division sequence stellar emission in the L1551 star-forming Refereed Journals, 2003 complex, 2003, A&A, 403, 187. Favata, F., Micela, G., Coronal X-ray Astronomy, 2003, Bendo, G.J., Joseph, R.D., Wells, M., Gallais, P., Haas, Space Sci. Rev., 108, 577. M., Heras, A.M., Klaas, U., Laureijs, R.J., Leech, K., Franco, G., Fosalba, P., Tauber, J.A., Systematic Effects Lemke, D., Metcalfe, L., Rowan-Robinson, M., in the Measurement of Polarization by the Planck Schulz, B., Telesco, C., Dust Temperatures in the Telescope, 2003, A&AS, 405, 349. Infrared Space Observatory Atlas of Bright Spiral Fridlund, M., Gondoin, P., GENIE – The Darwin demon- Galaxies, 2003, AJ, 125, 2361. strator, 2003, Astrophysics & Space Science, 286, 93. Benjamin, R.A., Churchwell, E., Babler, B.L., Bania, Hony, S., Tielens, A.G.G.M., Waters, L.B.F.M., Koter, A. T.M., Clemens, D.P., Cohen, M., Dickey, J., de, The circumstellar envelope of the C-rich post- Indebetouw, R., Jackson, J.M., Kobulnicky, H.A., AGB star HD 56126, 2003, A&A, 402,211. Lazarian, A., Marston, A.P., Mathis, J.S., Meade, Jakobsen, P., Jansen, R.A., Wagner, S., Reimers, D., M.R., Seager, S., Stolovy, S.R., Watson, C., Whitney, Caught in the act- a helium-reionizing quasar near the B.A., Wolff, M.J., Wolfire, M.G., GLIMPSE. I. An line of sight to Q0302-003, 2003, A&A, 397, 891. SIRTF Legacy Project to Map the Inner Galaxy, 2003, Katz, D., Favata, F., Aigrain, S., Micela, G., The PASP, 115, 953. photospheric abuyndance of active binaries. I. Boirin, L., Parmar, A.N., Discovery of narrow X-ray Detailed analysis of HD 113816 (IS VIR) and HD absorption features from the low-mass X-ray binary 119285 (V851 Cen), 2003, A&A, 397, 747. X 1254-690 with XMM-Newton, 2003, A&A, 407, Laine, S., van der Marel, R.P., Rossa, J., Boeker, T., 1079. Mihos, J.C., Hibbard, J.E., Zabludoff, A.I., Hubble Boirin, L., Parmar, A.N., Barret, D., Paltani, S., Space Telescope/WFPC2 Investigation of the Nuclear Discovery of X-ray absorption lines from the low- Morphology in the Toomre Sequence of Merging mass X-ray binaries 4U 1916-053 and X 1254-690 Galaxies, 2003, AJ, 126, 2717. with XMM-Newton, 2003, Nuclear Physics B Lehtinen, K., Mattila, K., Lemke, D., Juvela, M., Prusti, T., Proceedings Supplements, 132, 506. Laureijs, R., Far infrared observations of pre-proto- Bridge, C.M., Cropper, M., Ramsay, G., de Bruijne, stellar sources in Lynds 183, 2003, A&A, 398, 571. J.H.J., Reynolds, A.P., Perryman, M.A.C., Variability Liseau, R., Brandeker, A., Fridlund, M., Olofsson, G., of the accretion stream in the eclipsing polar EP Dra, Takeuchi, T., Artymowicz, P., The 1.2 mm image of 2003, MNRAS, 341, 863. the beta Pictoris disk, 2003, A&A, 402, 183. Carpano, S., Aigrain, S., Favata, F., Detecting planetary Morel, T., Micela, G., Favata, F., Katz, D., Pillitteri, I., transits in the presence of stellar variability. Optimal The photospheric abundances of active binaries, 2003, filtering and the use of color information, 2003, A&A, A&A, 414, 459. 401, 743. Parmar, A.N., Kuulkers, E., Oosterbroek, T., Barr, P., Corbett, E.A., Kewley, L., Appleton, P.N., Charmandaris, Much, R., Orr, A., Williams, O.R., Winkler, C., V., Dopita, M.A., Heisler, C.A., Norris, R.P., Zezas, INTEGRAL observations of the black hole candidate A., Marston, A., COLA. II. Radio and Spectroscopic H1743-322 in outburst, 2003, A&A, 411, L421. Diagnostics of Nuclear Activity in Galaxies, 2003, Pillitteri, I., Micela, G., Sciortino, S., Favata, F., The ApJ, 583, 670. X-ray Luminosity Distributions of the high-metallicity Cropper, M., Barlow, M., Perryman, M.A.C., Horne, K., open cluster Blanco 1, 2003, A&A, 399, 919. Bingham, R., Page, M., Guttridge, P., Smith, A., Prisinzano, L., Micela, G., Sciortino, S., Favata, F., Peacock, A., Walker, D., Charles, P., A concept for an Luminosity and mass function of the galactic open STJ-based echelle spectrograph, 2003, MNRAS, 344, cluster NGC 2422, 2003, A&A, 404, 927. 33. Roxburgh, I.W., Favata, F., The Eddington Mission, Del Burgo, C., Laureijs, R.J., Abraham, P., Kiss, C., The 2003, Ap&SS, 284, 17. far-infrared signature of dust in high latitude regions, Stankov, A., Ilyin, I., Fridlund, C.V.M., Abundances and 2003, MNRAS, 346, 403. Radial Velocity Analysis of BW Vulpeculae, 2003, Dupac, X., Bernard, J.P., Boudet, N., Giard, M., Lamarre, A&A, 408, 1077-1086. J.M., Miny, C., Pajot, F., Ristorcelli, I., Serra, G., Steeghs, D., Perryman, M.A.C., Reynolds, A., Bruijne, Stepnik, B., Torre, J.P., Inverse temperature J.H.J. de, Marsh, T., Dhillon, V.S., Peacock, A., High- dependence of the dust submillimeter spectral index, speed energy-resolved STJ photometry of the 2003, A&A, 404, L11-L15. eclipsing dwarf nova IY UMa, 2003, MNRAS, 339, Dupac, X., Del-Burgo, C., Bernard, J.P., Giard, M., 810-816. Lamarre, J.M., Laureijs, R.J., Pajot, F., Ristorcelli, I., Steenbrugge, K.C., Bruijne, J.H.J. de, Hoogerwerf, R., de Serra, G., Tauber, J., Torre, J.P., The complete Zeeuw, P.T., Radial velocities of early-type stars in the submillimetre spectrum of NGC 891, 2003, MNRAS, Perseus OB2 association, 2003, A&A, 402, 587-605. 344/1, 105. Urquhart, J. S., White, Glenn J., Pilbratt, G. L., Fridlund, Favata, F., Giardino, G., Micela, G., Sciortino, S., An C. V. M., ISOCAM-CVF imaging of M16, 2003, XMM-Newton-based X-ray survey of pre-main A&A, 409, 193. sec4.qxd 7/12/05 9:52 AM Page 116

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Walter, R., Rodriguez, J., Foschini, L., de Plaa, J., Calibration of SWS, 2003, The Calibration Legacy of Corbel, S., Courvoisier, T.J.-L., den Hertog, P.R., the ISO Mission, ESA SP-481, 67. Lebrun, F., Parmar, A.N., Tomsick, J.A., Ubertini, P., Fridlund, C.V.M., Darwin – The Scientific Constraints, INTEGRAL discovery of a bright highly obscured 2003, Stellar Structure and Habitable Planets, ESA galactic X-ray binary source, 2003, A&A, 411, L427. SP-538, 293. Fridlund, M., The Darwin Mission, 2003, Scientific Frontiers in Research on Extrasolar Planets, 294, 621. Astrophysics Missions Division Gondoin, P., Absil, O., Erd, C., Fridlund, M., den Hartog, Proceedings and other Publications, 2003 R., Rando, N., The Darwin-GENIE Experiment – An ESA-ESO Partnership, 2003, Hubble’s Science Absil, O., Gondoin, P., Erd, C., Fridlund, M., den Legacy: Future Optical/Ultraviolet Astronomy from Hartog, R., Labadie, L., Rando, N., Candidate VLTI Space, 291, 288. Configurations for the GENIE Nulling Experiment, Hartog, R. den, Absil, O., Kaltenegger, L., Gondoin, P., 2003, Scientific Frontiers in Research on Extrasolar Wilhelm, R., Fridlund, M., Could GENIE detect hot Planets, 294, 557. Jupiters?, 2003, Proceedings of the Conference on Absil, O., Kaltenegger, L., Eiroa, C., den Hartog, R., Towards Other Earths: DARWIN/TPF and the Search Gondoin, P., Wilhelm, R., Fridlund, M., Can GENIE for Extrasolar Terrestrial Planets, ESA SP-539, 399. characterize debris disks around nearby stars?, 2003, Heras, A.M., Wieprecht, E., Nieminen, P., Feuchtgruber, Proceedings of the Conference on Towards Other H., Lahuis, F., Leech, K., Lorente, R., Morris, P.W., Earths: DARWIN/TPF and the Search for Extrasolar Salama, A., Vandenbussche, B., Summary of the SWS Terrestrial Planets, ESA SP-539, 323. Detector Radiation Effects, 2003, The Calibration Appleton, P.N., Marston, A.P., Jarrett, T., Charmandaris, Legacy of the ISO Mission, ESA SP-481, 203. V., Corbett, E., Dopita, M.A., Kewley, L., Zezas, A., Hony, S., Prusti, T., Ott, S., Siebenmorgen, R., An Norris, R.P., The Host Galaxies of Low-luminosity ISOCAM mid-IR survey of TMC-2, 2003, Open AGN and Starbursts in the Northern COLA Sample, issues in local star formation, ASSL, 299. 2003, Active Galactic Nuclei: from Central Engine to Hony, S., Waters, L.B.F.M., Tielens, A.G.G.M., The 21 Host Galaxy, 290, 477. and 30 micron emission features in Planetary Nebulae Boirin, L., Parmar, A.N., Barret, D., Paltani, S., with Wolf-Rayet central stars, 2003, Planetary Discovery of X-ray absorption lines from the low- Nebulae – their evolution and role in the universe, mass X-ray binaries X1916-053 and X1254-690 with 209, 299. XMM-Newton, 2003, Proc. of the SF2A conf. held in Kaltenegger, L., Absil, O., Eiroa, C., Stankov, A., Erd, Bordeaux, France, June 2003, 459. C., Gondoin, P., den Hartog, R., Fridlund, M., Del Burgo, C., Laureijs, R.J., Ábrahám, P., Kiss, C., Far- Wilhelm, R., Characterisation of disks around YSOs infrared colours of high-latitude dust regions, 2003, with GENIE, 2003, Proceedings of the Conference on Exploiting the ISO Data Archive. Infrared Astronomy Towards Other Earths: DARWIN/TPF and the Search in the Internet Age, ESA SP-511, 195. for Extrasolar Terrestrial Planets, ESA SP-539, 465. Eiroa, C., Fridlund, M., Kaltenegger, L., The DARWIN Kaltenegger, L., Fridlund, M., Absil, O., Details on target list – observational properties of the G-type DARWIN and the Search for Extrasolar Planets, 2003, stars, 2003, Proceedings of the Conference on Scientific Frontiers in Research on Extrasolar Towards Other Earths: DARWIN/TPF and the Planets, 294, 653. Search for Extrasolar Terrestrial Planets, ESA SP- Kaltenegger, L., Karlsson, A., Fridlund, M., Absil, O., 539, 403. Overview of the DARWIN mission, 2003, Feuchtgruber, H., Katterloher, R.O., Jakob, G., Lutz, D., Proceedings of the Conference on Towards Other Barl, L., Bauer, O.H., Becher, K., Beintema, D.A., Earths: DARWIN/TPF and the Search for Extrasolar Boonstra, A.J., Boxhoorn, D.R., Coti, J., Czempiel, Terrestrial Planets, ESA SP-539, 459. S., van Dijkhuizen, C., de Graauw, T., Drapatz, S., Laureijs, R.J., Klaas, U., Richards, P.J., Schulz, B., Evers, J., Frericks, M., Genzel, R., Glas, M., de Abraham, P., The ISO Handbook, Volume IV – PHT – Groene, P., Haerendel, G., Haser, L., Heras, A.M., The Imaging Photo-Polarimeter, 2003, The ISO Horinga, W., van der Hucht, K.A., van der Hulst, T., Handbook, 4. Huygen, R., Jacobs, H., Kamm, N., Kampermann, T., Marston, A.P., Molecular gas around the Wolf-Rayet star Kester, D.J.M., Koornneef, J., Kunze, D., Lahuis, F., WR 18 (WN4), 2003, A Massive Star Odyssey: From Lamers, H.J.G.L.M., Leech, K., van der Lei, S., van Main Sequence to Supernova, Proceedings of IAU der Linden, R., Luinge, W., Melzner, F., Morris, P.W., Symposium #212, 732. Ploeger, G.R., Price, S.D., Roelfsema, P.R., Salama, Perryman, M.A.C, Monte Rosa Conference Summary, A., Schaeidt, S.G., Sijm, N., Spakman, J., Spath, H., 2003, Gaia Spectroscopy, Science and Technology, Steinmayer, M., Stvcker, J., Sturm, E., Valentijn, 298, 391. E.A., Vandenbussche, B., Waelkens, C., Wesselius, Perryman, M.A.C., The Gaia Mission, 2003, Gaia P.R., Wieprecht, E., Wiezorrek, E., Wijnbergen, J.J., Spectroscopy, Science and technology, 298,3 Wildeman, K., Young, E., The Ground-based Roelfsema, P.R., Valentijn, E.A., Bauer, O.H., Beintema, sec4.qxd 7/12/05 9:52 AM Page 117

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D.A., Boxhoorn, D.R., Feuchtgruber, H., de Graauw, Kaplan, J., Lagache, G., Lamarre, J.M., Lange, A.E., T., Heras, A.M., Huygen, R., Kester, D.J.M., Lahuis, Macias-Perez, J.F., Madet, K., Maffei, B., Magneville, F., Leech, K., Lorente, R., Morris, P.W., Salama, A., C., Marrone, D.P., Masi, S., Mayet, F., Murphy, A., Schaeidt, S.G., Shipman, R.F., Vandenbussche, B., Naraghi, F., Nati, F., Patanchon, G., Perrin, G., Piat, Weiprecht, E., The ISO SWS Calibration – Strategy M., Ponthieu, N., Prunet, S., Puget, J.L., Renault, C., and Lessons Learned, 2003, The Calibration Legacy Rosset, C., Santos, D., Starobinsky, A., Strukov, I., of the ISO Mission, ESA SP-481, 31. Sudiwala, R.V., Teyssier, R., Tristram, M., Tucker, C., Sciortino, S., Favata, F., Micela, G., Parmar, A.N., The Vanel, J.C., Vibert, D., Wakui, E., Yvon, D., First physics of shocks in the proto-stellar environment – detection of polarisation of the submillimeter diffuse Herbig-Haro objects observed with XEUS, 2003, Galactic dust emission by Archeops, 2004, A&A, 424, XEUS – studying the evolution of the hot universe, 571. held at MPE Garching, March 11-13, 2002. Edited by Boeker, T., Sarzi, M., McLaughlin, D.E., van der Marel, G. Hasinger, Th. Boller, and A.N. Parmar, MPE R.P., Rix, H.-W., Ho, L.C., Shields, J.C., A Hubble Report 281, 2003, 281,311. Space Telescope Census of Nuclear Star Clusters in Shipman, R.F., Morris, P.W., Beintema, D.A., Boxhoorn, Late-Type Spiral Galaxies – II. Cluster Sizes and D., Feuchtgruber, H., Heras, A.M., Huygen, R., Structural Parameter Correlations, 2004, AJ, 127, 105. Kester, D., Lahuis, F., Leech, K., Lorente, R., Lutz, Boirin, L., Parmar, A.N., Barret, D., Paltani, S., Grindlay, D., Roelfsema, P., Salama, A., Schaeidt, S.G., J.E., Discovery of X-ray absorption features from the Valentijn, E., Vandenbussche, B., Wieprecht, E., SWS dipping low-mass X-ray binary XB1916-053 with In-flight Calibration, 2003, The Calibration Legacy of XMM-Newton, 2004, A&A, 418, 1061. the ISO Mission, ESA SP-481, 107. Bonito, R., Peres, G., Orlando, S., Favata, F., Rosner, R., Sidoli, L., Parmar, A.N., Oosterbroek, T., Discovery of The X-ray Emission Mechanism in the Protostellar Jet absorption lines in Low Mass X-ray Binaries – MXB HH 154, 2004, A&A, 424, L1. 1659-298 and GX13+1, 2003, Memoire of the Italian Brandeker, A., Liseau, R., Olofsson, G., Fridlund, M., Astronomical Society, 75, 480. The spatial structure of the beta Pictoris gas disk, Tothill, N.F., Marston, A.P., Martin, C.L., CO 2-1 Maps 2004, A&A, 413, 681. of Wolf-Rayet Star Envionments, 2003, Astronomy in CadolleBel, M., Rodriquez, J., Sizun, P., Farinelli, R., Antarctica, 25th meeting of the IAU, SS2, 17. DelSanto, M., Goldwurm, A., Goldoni, P., Corbel, S., Volonte, S., Fridlund, C.V.M., The search for exoplanets Parmar, A.N., Kuulkers, E., Ubertini, P., Capitanio, F., in the ESA Science Programme, 2003, Proceedings of Roques, J.P., Frontera, F., Westergaard, N.J., High- the Conference on Towards Other Earths: energy observations of the state transition of the X-ray DARWIN/TPF and the Search for Extrasolar nova and black hole candidate XTE J1720-318, 2004, Terrestrial Planets, ESA SP-539, 277. A&A, 426, 659. White, G.J., Thompson, M.A., Fridlund, C.V.M., Churchwell, E.B., Whitney, B.A., Babler, B.L., Huldtgren White, M., Towards a molecular inventory Indebetouw, R., Meade, M.R., Watson, C., Wolff, of protostellar discs, 2003, Proceedings of the M.J., Wolfire, M.G., Bania, T.M., Benjamin, R.A., Conference on Towards Other Earths: DARWIN/TPF Clemens, D.P., Cohen, M., Devine, K.E., Dickey, and the Search for Extrasolar Terrestrial Planets, J.M., Heitsch, F., Jackson, J.M., Kobulnicky, H.A., ESA SP-539, 653. Marston, A.P., Mathis, J.S., Mercer, E.P., Stauffer, J.R., Stolovy, S.R., RCW49 at Mid-IR Wavelengths – A GLIMPSE from the Spitzer Space Telescope, 2004, Astrophysics Missions Division ApJS, 154, 322. Refereed Journals, 2004 Diedenhoven, B. van, Peeters, E., Kerckhoven, C. van, Hony, S., Hudgins, D.M., Allamandola, L.J., Tielens, Ábrahám, P., Kóspál, Á., Csizmadia, S., Kun, M., Moór, A.G.G.M., The Profiles of the 3-12 Micron Polycyclic A., Prusti, T., Long-term evolution of FU Orionis Aromatic Hydrocarbon Features, 2004, ApJ, 611, 928. objects at infrared wavelengths, 2004, A&A, 428, 89. Dupac, X., Tauber, J., Scanning strategy for mapping the Aigrain, S., Favata, F., Gilmore, G., Characterising Cosmic Microwave Background anisotropies with stellar micro-variability for planet transit searches, Planck, 2004, A&A, (Accepted for Publication). 2004, A&A, 414, 1139. Favata, F., Micela, G., Baliunas, S., Schmitt, J.H.M.M., Benoit, A., Ade, P., Amblard, A., Ansari, R., Aubourg, E., Discovery of an X-ray activity cycle in the solar-type Bargot, S., Bartlett, J.G., Bernard, J.P., Bhatia, R.S., star HD 81809, 2004, A&A, 418, L13. Blanchard, A., Bock, J.J., Boscaleri, A., Bouchet, F.R., Feigelson, E.D., Hornschemeier, A.E., Micela, G., Bauer, Bourrachot, A., Camus, P., Couchot, F., Bernardis, P. F.E., Alexander, D.M., Brandt, W.N., Favata, F., de, Delabrouille, J., Desert, F.X., Dore, O., Douspis, Sciortino, S., The Chandra Deep Field-North Survey – M., Dumoulin, L., Dupac, X., Filliatre, P., Fosalba, P., XVII. Evolution of magnetic activity in old late-type Ganga, K., Gannaway, F., Gautier, B., Giard, M., stars, 2004, ApJ, 611, 1107. Giraud-Heraud, Y., Gispert, R., Guglielmi, L., Fridlund, C.V.M., The Darwin mission, 2004, Adv. Space Hamilton, J.C., Hanany, S., Henrot-Versille, S., Res., 34, 613. sec4.qxd 7/12/05 9:52 AM Page 118

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Giardino, G., Favata, F., Micela, G., Chandra observa- Churchwell, E.B., Discovery of a Distant Star Forma- tions of the massive star-forming region S106 – X-ray tion Region Using GLIMPSE, 2004, ApJS, 154, 328. emission from the embedded massive protostellar Morel, T., Micela, G., Favata, F., Katz, D., The photo- object IRS4, 2004, A&A, 424, 965. spheric abundances of active binaries III. Abundance Giardino, G., Favata, F., Micela, G., Reale, F., A large X- peculiarities at high activity level, 2004, A&A, 426, ray flare from the Herbig Ae star V892 Tau, 2004, 1007. A&A, 413, 669. 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Walcher, C.J., Marel, R.P. van der, McLaughlin, D.E., Mercer, E.P., Clemens, D.P., Bania, T.M., Jackson, J.M., Rix, H.W., Boeker, T., Haering, N., Ho, L.C., Sarzi, Rathborne, J.M., Shah, R.Y., Babler, B.L., M., Shields, J.C., Masses of star clusters in the nuclei Indebetouw, R., Meade, M.R., Watson, C., Whitney, of bulge-less spiral galaxies, 2004, ApJ, (Accepted for B.A., Wolff, M.J., Wolfire, M.G., Benjamin, R.A., Publication). Cohen, M., Dickey, J.M., Kobulnicky, H.A., Marston, Whitney, B.A., Indebetouw, R., Babler, B.L., Meade, A.P., Mathis, J.S., Stauffer, J.R., Stolovy, S.R., M.R., Watson, C., Wolff, M.J., Wolfire, M.G., sec4.qxd 7/12/05 9:52 AM Page 119

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Clemens, D.P., Bania, T.M., Benjamin, R.A., Cohen, Non-detection of the cyclotron line in the spectrum of M., Devine, K.E., Dickey, J.M., Heitsch, F., Jackson, the anomalous X-ray pulsar 1RXS J170849-400910, J.M., Kobulnicky, H.A., Marston, A.P., Mathis, J.S., 2004, The 5th INTEGRAL Workshop – The Mercer, E.P., Stauffer, J.R., Stolovy, S.R., Churchwell, INTEGRAL Universe, ESA SP-552, 471. E.B., A GLIMPSE of Star Formation in the Giant HII Parmar, A.N., Cosmology with ESAs Future High- Region RCW 49, 2004, ApJS, 154, 315. Energy Astronomy Programme, 2004, Proc. Mykonos Conference on Multi-wavelength Cosmology, 301, 305. Astrophysics Missions Division Parmar, A.N., Arnaud, M., Barcons, X., Bleeker, J., Proceedings and other Publications, 2004 Hasinger, G., Inoue, H., Palumbo, G., Turner, M., Science with XEUS – the X-ray Evolving Universe Cadolle Bel, M., Goldwurm, A., Rodriquez, J., Goldini, Spectroscopy Mission, 2004, Proceedings SPIE – UV P., Corbel, S., Sizin, P., Parmar, A.N., Kuulkers, E., and Gamma-Ray Space Telescope Systems, 5488, 388. Capatanao, F., Del Sanot, M., Ubertini, P., Roques, J.- Peeters, E., Allamandola, L.J., Hudgins, D.M., Hony, S., P., Bouchet, L., Farinelli, R., Frontera, F., Wester- Tielens, A.G.G.M., The Unidentified InfraRed Bands gaard, N.J., INTEGRAL, XMM-Newton and Rossi- after ISO, 2004, Astrophysics of Dust, Estes Park, XTE observations of the state transition of the X-ray Colorado, May 26-30, 2003, 309, 141. transient and black hole candidate XTE J1720-318, Perryman, M.A.C., Detection and Characterization of 2004, The 5th INTEGRAL Workshop – The Extra-Solar Planets, 2004, The Search for Other INTEGRAL Universe, ESA SP-552, 215. Worlds, 713, 283. Cassinelli, J.P., Neiner, C., Discussion session on Perryman, M.A.C., Hipparcos and Gaia – the Develop- magnetic fields and Be stars, 2004, The nature and ment of Space Astrometry in Europe, 2004, IAC evolution of disks around hot stars, (Accepted for Winter School 2003, (Accepted for Publication). Publication). Perryman, M.A.C., Our Galaxy in Three-Dimensions – Catala, C., Aricha, A., Boulade, O., Diaz, E., Epstein, G., the Jeremiah Horrocks Memorial Lecture, 2004, Favata, F., Horne, K., Kjeldsen, H., Lumb, D., Mas- Transit of Venus – New Views of the Solar System and Hesse, M., Roxburgh, I., Science requirements and Galaxy, IAU Coll 196, (Accepted for Publication). their translation into instrumental design, 2004, Sanz-Forcada, J., Dupree, A.K., Active Stars and He I Second Eddington Workshop: Stellar structure and 10830 A, the EUV Connection, 2004, High Resolution habitable planet finding, ESA SP-538, 39. Infrared Spectroscopy in Astronomy, (Accepted for Clavel, J., The Herchel submm Space Observatory, 2004, Publication). The interplay among Black Holes, Stars and ISM in Sanz-Forcada, J., Favata, F., Micela, G., The not-so- Galactic Nuclei – Proceedings IAU Symposium #222, MAD coronal abundances of active stars, 2004, 2004, 553. Chemical Abundances and Mixing in Stars in the Fridlund, C.V.M., Darwin – the scientific constraints, Milky Way and its Satellites, (Accepted for 2004, Second Eddington Workshop: Stellar structure Publication). and habitable planet finding, 9-11 April 2003, Sanz-Forcada, J., Favata, F., Micela, G., The not-so- Palermo, Italy., ESA SP-538, 225. MAD coronal abundances of active stars, 2004, 13th Hussain, G.A.J., Stellar surface imaging – mapping Cambridge Workshop on Cool Stars, (Accepted for brightness and magnetic fields, 2004, Astronomische Publication). Nachrichten, 325, 216. Sciortino, S., Micela, G., Favata, F., Giardino, G., Kuulkers, E., Bodaghee, A., Foschini, L., Guainazzi, M., Flaccomio, E., Damiani, F., X-ray Observations of Matt, G., Israel, G., Nicastro, F., Oosterbroek, T., Star Formation Regions – EPIC results in L1551 and Parmar, A., Rodriquez, J., Walter, R., GX 339-4 Upper Sco-Cen, 2004, Mem. S. A. It., 75, 428. detected by INTEGRAL, 2004, Astronomical Sidoli, L., Parmar, A.N., Oosterbroek, T., XMM-Newton Telegram, 240,1. results on the ultracompact low-mass X-ray binary 4U Lim, T., Swinyard, B., Aramburu, A., Bock, J., Ferlet, 1850-087 in the globular cluster NGC 6712, 2004, M., Griffin, D., Griffin, M., Hargrave, P., King, K., The 5th INTEGRAL Workshop – The INTEGRAL Leeks, S., Naylor, D., Ronayette, S., Sawyer, E., Universe, ESA SP-552, 389. Schulz, B., Sidher, S., Spencer, L., Smith, D., Sidoli, L., Parmar, A.N., Oosterbroek, T., The First Woodcraft, A., First Results From Herschel-SPIRE Broad-Band Persistent X-ray Spectrum of the Dipping Performance Tests, 2004, Proceedings of SPIE. Low Mass X-ray Binary EXO 0748-676, 2004, The Optical, Infrared, and Millimeter Space Telescopes, 5th INTEGRAL Workshop – The INTEGRAL 5487, 460-468. Universe, ESA SP-552, 385. Neiner, C., Hubert, A.M., Magnetic fields in Be stars, Tauber, J., Prospects for Polarimetry of the Interstellar 2004, The nature and evolution of disks around hot Medium with the Planck Satellite, 2004, The stars, (Accepted for Publication). Magnetized Interstellar Medium, 191. Oosterbroek, T., Parmar, A.N., Rens, N., Israel, G.L., Tielens, A.G.G.M., Peeters, E., Bakes, E.L.O., Spoon, Stella, L., Mereghetti, S., Haberl, F., Angelini, L., H.W.W., Hony, S., PAHs and Star Formation, 2004, sec4.qxd 7/12/05 9:52 AM Page 120

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ASP Conf. Ser. 323: Star Formation in the Interstellar Planetary Missions Division Medium Workshop, in Honor of David Hollenbach, Refereed Journals, 2003 Chris McKee and Frank Shu. Walter, R., Courvoisier, T.J.-L., Foschini, L., Lebrun, F., Arpigny, C., Jehin, E., Manfroid, J., Hutsemekers, D., Lund, N., Parmar, A., Rodiguez, J., Tomsock, J.A., Schulz, R., Stuewe, J.A., Zucconi, J.-M., Ilyin, I., Ubertini, P., IGR J16318-4848 & CO – A new Anomalous nitrogen isotope ratio in comets – possible population of hidden high mass X-ray binaries in the connection with interplanetary dust particles and Norma arm of the Galaxy, 2004, Proc. 5th INTEGRAL organic molecules, 2003, Science, 301, 1522-1524. Workshop, ESA SP-552, 417. Clausen, K.C., Hassan, H., Verdant, M., Couzin, P., Huttin, G., Brisson, M., Sollazzo, C., Lebreton, J.-P., The Huygens Probe System Design, 2003, Space Sci. Rev., Special Cassini/Huygens issue, 35. Heather, D.J., Dunkin, S.K., Geology and Stratigraphy of King Crater, Lunar Farside, 2003, Icarus, 163, 307-329. Heather, D.J., Dunkin, S.K., Wilson, L., Volcanism on the Marius Hills plateau – Observational analyses using Clementine multispectral data, 2003, J. Geophys. Res., 108/E3, 3-1. Kolokolova, L., Lara, L.M., Schulz, R., Stuewe, J.A., Tozzi, G.P., Color of an ensemble of particles with a wide power-law size distribution – application to observations of Comet Hale-Bopp at 3 AU, 2003, J. Quantitative Spectroscopy and Radiative Transfer, 79-80, 861-871. Lebreton, J.-P., Matson, D.L., The Huygens Probe – Science, Payload and Mission, 2003, Space Sci. Rev., Special Cassini/Huygens, 41. Michael, G.G., Coordinate registration by automated crater recognition, 2003, Planet. Space Sci., 51/9-10, 563. Molina-Cuberos, G., Witasse, O., Lebreton, J.-P., Rodrigo, R., Lopez-Moreno, J.J., Meteoric ion in the atmosphere of Mars, 2003, Planet. Space Sci., 51/3, 239-249. Schulz, R., Maximize the Outcome of a Comet Mission, but how?, 2003, Adv. Space Res., (Accepted for Publication). Schulz, R., Stuewe, J.A., Boehnhardt, H., Gaessler, W., Tozzi, G.P., Characterization of STARDUST target comet 81P/Wild 2 from 1996 to 1998, 2003, A&A, 298, 345-352. Trautner, R., Grard, R., Hamelin, M., Detection of Subsurface Ice and Water Deposits on Mars with a Mutual Impedance Probe, 2003, J. Geophys. Res., 108/E10, 8047. Witasse, O., Dutuit, O., Correction to “Prediction of a 2+ CO2 layer in the atmosphere of Mars”, 2003, Geophys. Res. Lett., 30, 12.

Planetary Missions Division Proceedings and other Publications, 2003

Aleon, J., Arpigny, C., Robert, F., Jehin, E., Manfroid, J., Hutsemekers, D., Zucconi, J.-M., Schulz, R., Stuewe, J.A., Sangely, L., Chaussidon, M., Marty, B., Engrand, C., Cometary organic macromolecules in inter- planetary dust particles?, 2003, Lunar and Planetary Science, XXXIV, 1308. sec4.qxd 7/12/05 9:52 AM Page 121

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Arpigny, C., Cochran, A.L., Jehin, E., Manfroid, J., Planetary Missions Division Hutsemekers, D., Zucconi, J.-M., Endl, M., Cochran, Refereed Journals, 2004 W.D., Schulz, R., Anomalous 14N/15N ratio in comets 122P/1995 S1 (de Vico) and 153P/2002 C1 Bolton, S.J., Hansen, C.J., Matson, D.L., Spilker, L.J., (Ikeya-Zhang), 2003, Bull. Am. Astron. Soc., 35/4, Lebreton, J.-P., Cassini/Huygens flyby of the Jovian 986. system, 2004, J. Geophys. Res., 109, 1-5. Collon, M., Buis, E.J., Beijersbergen, M., Kraft, S., Erd, Campbell-Brown, M.D., Koschny, D., Model of the C., den Hartog, R., Owens, A., Falkner, P., Schulz, R., ablation of faint meteors, 2004, A&A, 418, 751-758. Peacock, A., Design and performance of the payload Culot, F., Lathuillere, C., Lilensten, J., Witasse, O., The instrumentation of the BepiColombo Mercury OI 630.0 and 557.7 nm dayglow measured by WINDII Planetary Orbiter, 2003, Proceedings of the Fifth IAA and modeled by TRANSCAR, 2004, Ann. Geo- International Conference on Low-Cost Planetary physicae, 22, 1947-1960. Missions, ESA SP-542, 501. Hansen, C.J., Bolton, S.J., Matson, D.L., Spilker, L.J., Falkner, P., Schulz, R., The BepiColombo Mission to Lebreton, J.-P., The Cassini-Huygens Flyby of Jupiter, Mercury, 2003, Bull. Am. Astron. Soc., 35/4, 1001. 2004, Icarus, 172, 1-8. Fulchignoni, M., Ferri, F., Angrilli, F., Bar-Nun, A., Jehin, E., Manfroid, J., Cochran, A.L., Arpigny, C., Barucci, M.A., Bianchini, G., Borucki, W., Coradini, Zucconi, J.M., Hutsemekers, D., Cochran, W.D., Endl, M., Coustenis, A., Falkner, P., Flamini, E., Grard, R., M., Schulz, R., Anomalous 14N/15N ratio in comets Hamelin, M., Harri, A.M., Leppelmeier, G.W., Lopez- 122P/de Vico) and 153P/Ikeya-Zhang, 2004, ApJ, Moreno, J.J., McDonnell, J.A.M., McKay, C.P., 613, L161-L164. Neubauer, F.H., Pedersen, A., Picardi, G., Pirronello, Kazeminjad, B., Perez-Ayúcar, M., Lebreton, J.-P., V., Rodrigo, R., Schwingenschuh, K., Seiff, A., Sanchez-Nogales, M., Belló-Mora, M., Strange, N., Svedhem, H., Vanzani, V., Zarnecki, J., The Roth, D., Popken, L., Clausen, K., Couzin, P., Simula- Characterisation of Titan’s Atmospheric Physical tion and analysis of the revised Huygens probe entry Properties by the Huygens Atmospheric Structure and descent trajectory and radio link modelling., 2004, Instrument (HASI), 2003, The Cassini-Huygens Planet. Space Sci., 52, 799-814. Mission, 395-431. Lara, L.M., Tozzi, G.P., Boehnhardt, H., DiMartino, M., Kraft, S., Collon, M., Montella, J., Buis, E.J., Schulz, R., Gas and dust in comet C/2000 WM1 Beijersbergen, M., Erd, C., Falkner, P., Schulz, R., during its closest approach to Earth. Optical imaging Peacock, A., On the concepts of a highly integrated and long-slit spectroscopy, 2004, A&A, 422, 717-729. payload suite for use in future planetary missions, the Lilensten, J., Simon, C., Witasse, O., Dutuit, O., Thissen, example of the BepiColombo Mercury Planetary R., Alcaraz, C., A fast computation on the diurnal Orbiter, 2003, Proc. Fifth IAA International secondary ion production in the ionosphere of Titan, Conference on Low-Cost Planetary Missions, ESA 2004, Icarus, (Accepted for Publication). SP-542, 219. Lilensten, J., Witasse, O., Simon, C., Soldi-Lose, H., Schulz, R., Kern, Koma und Schweife, 2003, Sterne & Dutuit, O., Thissen, R., Alcaraz, C., Prediction of a ++ Weltraum Special: Kometen und Asteroiden, 2/03, 28- N2 layer in the upper atmosphere of Titan, 2004, 32. Geophys. Res. Lett., (Accepted for Publication). Schulz, R., Wirtanen – A short period comet, 2003, Michael, G.G., Beagle-2 position determination from the CNES Magazine, 18, 34. returned camera panoramas using MOLA data, 2004, Schulz, R., Rosetta goes to comet Wirtanen, 2003, The Planet. Space Sci., 52, 271. Observatory, 123/1174, 115-118. Morel, L., Witasse, O., Warnant, R., Cerisier, J.-C., Schulz, R., Falkner, P., Peacock, A., Erd, C., Rando, N., Blelly, P.-L., Lilensten, J., Diagnostic of the dayside Kraft, S., The BepiColombo Mission, 2003, ionosphere of Mars using the Total Electron Content Highlights in Astronomy, 13. Measurement by the Neige/Netlander experiment – an Schulz, R., Stuewe, J.A., Boehnhardt, H., Postperihelion assessment study, 2004, Planet. Space Sci., 52/7, 603- monitoring of Comet 67P/Churyumov-Gerasimenko, 611. the new Rosetta target, 2003, Bull. Am. Astron. Soc., Schulz, R., Stuewe, J.A., Boehnhardt, H., Rosetta target 35/4, 970. comet 67P/Churyumov-Gerasimenko. Postperihelion Thomas, N., Schulz, R., Falkner, P., The BepiColombo gas and dust prodution rates, 2004, A&A, 422, L19- Lander – MSE, 2003, Highlights in Astronomy, 13. L21. Trautner, R., Chicarro, A.C., Martin, P.D., Coordinated Tozzi, G.P., Lara, L.M., Kolokolova, L., Boehnhardt, H., Science Operations of Mars Express Orbiter and Licandro, J., Schulz, R., Sublimating components in Lander, 2003, Lunar and Planetary Science, XXXIV, the Coma of Comet C/2000 WM1 (LINEAR), 2004, 1634. A&A, 424, 325-330. Trautner, R., Simoes, F., Grard, R., Hamelin, M., A new instrument for measuring the low frequency electrical properties of planetary subsurface materials, 2003, ESA SP-543, 193. sec4.qxd 7/12/05 9:52 AM Page 122

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Planetary Missions Division Lebreton, J.-P., Sollazzo, C., Blancquaert, T., Witasse, Proceedings and other Publications, 2004 O., Maize, E., Matson, D.L., Mitchell, R., Spilker, L., Flamini, E., Talevi, M., [and the Huygens Mission DiMartino, M., Battistelli, E., Carbognani, A., Cellino, Team], High Ambitions for an Outstanding Planetary A., Koschny, D., Resti, A., Tommasi, L., The ‘Smart Mission. Cassini-Huygens, 2004, ESA Bulletin, 120, Panoramic Optical Sensor Head’ – A new Tool for 11-21. Detecting Luminous Transient Phenomena on Lebreton, J.-P., Matson, D., The Huygens Mission to Planetary Bodies, 2004, Geophysical Research Titan. Overview and Status, 2004, Proc. Planetary Abstracts, 6, 02852. Probe Atmospheric Entry and Descent Trajectory Diaz del Rio, J., Koschny, D., Meteor Orbit and Analysis and Science, ESA SP-544, 21-30. Trajectory determination Software (MOTS), 2004, Matson, D.L., Lebreton, J.-P., Spilker, L.J., The Cassini- Proc. Int. Meteor Conf., 19-21 Sep 2003, Huygens mission to the Saturnian system, 2004, Bollmannsruh, Germany, Int. Met. Org., Berlin, Proc., ESA SP-1278, 242/I-242/XVi. Germany, 23-28. Rohner, U., Benz, W., Whitby, J.A., Wurz, P., Schulz, R., Frew, D., Koschny, D., Harch, A., Planning the Romstedt, J., Miniaturised Time-of-Flight Mass commissioning of a multi-payload mission, 2004, Spectrometer, 2004, Proceedings of the 37th ESLAB Proc. SpaceOps 2004, May 17-21, 2004, Montreal, Symposium ‘Tools and Technologies for Future Canada. Planetary Exploration’, ESA SP-543, 131. Hoofs, R., Koschny, D., van der Plas, P., Planning Schulz, R., BepiColombo. Visit to Mercury, 2004, strategy and supporting tools for the science ERCA, From indoor air pollution to the search for operations of ESA’s planetary missions, 2004, Proc. Earth-like planets in the cosmos, J. de Physique IV SpaceOps 2004, May 17-21, 2004, Montreal, Canada, Proc., EDP Sciences, 6, 249. Canadian Space Agency. Schulz, R., The Mercury Planetary Orbiter of Hoofs, R., Titov, D., Svedhem, H., Koschny, D., BepiColombo, 2004, Geophysical Research Ocampo, A., Science Operations Planning for Venus Abstracts, 6, 04807. Express, 2004, Geophysical Research Abstracts, 6, Schulz, R., Anomalous Nitrogen Isotopic Ratio in 06373. Comets, 2004, ESA Space Science News, 6, 8-9. Josset, J.-L., Beauvivre, S., Almeida, M., Barrucci, A., Schulz, R., Comet 67P/Churyumov-Gerasimenko, the Cerroni, P., Chevrel, S., diSanctis, C., Ehrenfreud, P., new Rosetta Target, 2004, CNES Magazine, February Hofmann, B., Josset, M., Koschny, D., Langevin, Y., 2004, 18. Mancuso, S., Muinonen, M., Pinet, P., Plancke, P., Schulz, R., Stuewe, J.A., Boehnhardt, H., Monitoring Shevch, V., Shkuratov, Y., Sodnik, Z., First results comet 67P/Churyumov-Gerasimenko from ESO in from the Smart-1 AMIE Multi-Colour Micro-Camera, 2003, 2004, The New Rosetta Targets. Observation, 2004, Geophysical Research Abstracts, 6, 07866. simulations and instrument performances, Kluwer Koschny, D., Comparing two potential meteor cameras – Academic Publishers, Dordrecht, The Netherlands, the Mintron and the Watec 120N, 2004, Proc. Int. 15-24. Meteor Conf., 19-21 Sep 2003, Bollmannsruh, Simões, F., Trautner, R., Grard, R., Hamelin, M., The Germany, Int. Met. Org., Berlin, Germany, 59, 63. dielectric properties of Martian Soil Simulant JSC Koschny, D., Dhiri, V., Frew, D., Hoofs, R., Lumb, R., Mars-1 in the frequency range from 20 Hz to 10kHz, Schwehm, G., Wirth, K., Zender, J., Science 2004, Lunar and Planetary Conference, XXXIV, 205. Operations for Planetary Missions in the European Svedhem, H., Lebreton, J.-P., Zarnecki, J., Hathi, B., Space Agency, 2004, Proc. SpaceOps 2004, May 17- Using Speed of Sound Measurements to Constrain the 21, 2004, Montreal, Canada, Canadian Space Agency. Huygens Probe Descent Profile, 2004, Int. Workshop Koschny, D., DiMartino, M., Oberst, J., Meteor ‘Planetary Probe Atmospheric Entry and Descent observations from space – The Smart Panoramical Trajectory Analysis and Science’, Lisbon, Portugal, 6- Optical Sensor (SPOSH), 2004, Proc. Int. Meteor 9 October 2003, ESA SP-544, 221-228. Conf., 19-21 Sep 2003, Bollmannsruh, Germany, Int. Trautner, R., Bello-Mora, M., Hechler, M., Koschny, D., Met. Org., Berlin, Germany, 64-69. A new celestial navigation method for Mars landers, Koschny, D., Trautner, R., Zender, J., Knöfel, A., Diaz 2004, Lunar and Planetary Science, XXXV, 1106. del Rio, J., Jehn, R., The ESA Leonid campaign 2002 Trautner, R., Koschny, D., A new Application for to Spain, 2004, Proc. Int. Meteor Conf., 19-21 Sep Planetary Lander Cameras – Lander Position and 2003, Bollmannsruh, Germany, Int. Met. Org., Berlin, Attitude Determination using Night Sky Images, Germany,70-77. 2004, Geophysical Research Abstracts, 6, 03614. 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Jean, P., Knödlseder, J., Hernanz, M., Cisana, E., Moran, L., Hanlon, L., McBreen, B., Preece, R., Kaneko, Valsesia, M., Strong, A., Leleux, P., Kienlin, A., Y., Williams, O.R., Bennett, K., Kippen, R.M., Winkler, C., Wunderer, C., Search for a galactic 1275 Kienlin, A. von, Beckmann, V., INTEGRAL keV line emission with SPI/INTEGRAL, 2004, Proc. Spectrometer Analysis of GRB030227 & 5th INTEGRAL Workshop, ESA SP-552, 119. GRB030131, 2004, Gamma-Ray Bursts: 30 Years of Kaneko, Y., Hanlon, L., Preece, R.D., Gonzalez, M.M., Discovery, AIP 727/1, 225-228. Dingus, B.L., Williams, O.R., Bennett, K., Winkler, Moran, L., Mereghetti, S., Gotz, D., Hanlon, L., von sec4.qxd 7/12/05 9:52 AM Page 131

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Kienlin, A., McBreen, B., Tiengo, A., Preece, R., GRB0300329 at early and late times, 2004, Gamma- Kaneko, Y., Williams, O.R., Bennett, K., Kippen, Ray Bursts: 30 years of discovery (AIP Conference R.M., Mcbreen, S., McGlynn, S., Preliminary Proceedings), 727, 316. INTEGRAL Analysis of GRB040106, 2004, Proc. 5th Walter, R., Aubord, A., Bartholdi, P., Beck, M., INTEGRAL Workshop, ESA SP-552, 653. Beckmann, V., Binko, P., Borkowski, J., Chernyakova, Mowlavi, N., Knödlseder, J., Diehl, R., Dubath, P., M., Contessi, T., Courvoisier, T., Dubath, P., Ebisawa, Lichti, G., Meynet, G., Schanne, S., Winkler, C., K., Favre, P., Gaber, M., Götz, D., Jaffe, T., Jennings, Search for 26Al in gamma Velorum, 2004, Proc. 5th D., Kretschmar, P., Landriu, D., Lecoeur, I., Lerusse, INTEGRAL Workshop, ESA SP-552, 39. L., Lock, T., Meharga, M., Mereghetti, S., Morisset, Oosterbroek, T., Parmar, A.N., Rea, N., Israel, G.L., N., Mowlavi, N., Paltani, S., Peachey, J., Pottschmidt, Stella, L., Mereghetti, S., Haberl, F., Angelini, L., A K., O’Neel, B., Produit, N., Rohlfs, R., Sauvageon, A., study of the variable anomalous X-ray pulsar 1RXS Shaw, S., Türler, M., Diehl, R., Domingo, A., J170849-400910 using XMM-Newton data, 2004, Goldwurm, A., Hansson, L., Schmidt, M., Wester- Proc. 5th INTEGRAL Workshop, ESA SP-552, 471. gaard, N., Winkler, C., The INTEGRAL Ground Orr, A., Falanga, M., Cocchi, M., Laurent, P., Goldwurm, Segment, 2004, ADASS XIII, 314, 432. A., Extensive INTEGRAL observations of the HMXB Wamsteker, W., Albrecht, R., Haubold, H.J., Developing 4U 1700-377, 2004, Proc. 5th INTEGRAL Workshop, Basic Space Sciences World-Wide. A decade of ESA SP-552, 357. UN/ESA workshops., 2004, Developing Basic Space Orr, A., Torrejon, J.M., Parmar, A.N., An INTEGRAL Sciences World-Wide. A decade of UN/ESA work- Open Time observation of the HMXB 4U 1700-377, shops, Kluwer Academic Publishers, Dordrecht, The 2004, Proc. 5th INTEGRAL Workshop, ESA SP-552, Netherlands. 361. Wamsteker, W., [for WIC WSO/UV Implementation Paizis, A., Courvoisier, T.J.-L., Vilhu, O., Chernyakova, Committee], The World Space Observatory/ M., Tikkanen, T., Bazzano, A., Beckmann, V., Ultraviolet (WSO/UV) – Current Status, 2004, Chenevez, J., Cocchi, M., Ebisawa, K., Farinelli, R., Developing Space Science World-wide. A decade of Frontera, F., Gimenez, A., Goldoni, P., Hannikainen, UN/ESA workshops, Kluwer Academic Publishers, D., Kuulkers, E., Lund, N., Oosterbroek, T., Piraino, Dordrecht, The Netherlands, 373-387. S., Rodriguez, J., Santangelo, A., Walter, R., Wieprecht, E., Brumfit, J., Bakker, J., de Candussio, N., Zdziarski, A.A., Zurita Heras, J.A., The INTEGRAL Guest, S., Huygen, R., de Jonge, A., Mathieu, J.-J., LMXRB Monitoring Programme, 2004, Proc. 5th Osterhage, S., Ott, S., Siddiqui, H., Vandenbussche, INTEGRAL Workshop, ESA SP-552, 229. B., de Meester, W., Wetzstein, M., Wiezorrek, E., Perea Calderon, J.V., Garcia-Lario, P., The transition Zaal, P., The HERSCHEL/PACS Common Software phase from AGB stars to Planetary Nebula as seen by System as Data Reduction System, 2004, ASP Conf. TIMMI2, 2004, High Resolution Near Infrared Ser. 314: Astronomical Data Analysis Software and Spectroscopy (ESO Astrophysics Symposia), Systems (ADASS) XIII, 314, 376. (Accepted for Publication). Williams, O.R., Parmar, A., Oosterbroek, T., Barr, P., Perez-Martinez, R., Metcalfe, L., Coia, D., Biviano, A., Much, R., Winkler, C., Three INTEGRAL Observa- McBreen, B., Altieri, B., Sanchez-Fernandez, C., tions of 4U 1822-371, 2004, Proc. 5th INTEGRAL ISOCAM Observations of Intermediate-redshift Workshop, ESA SP-552, 423. Galaxy Clusters at 7 and 15 microns., 2004, IAU Winkler, C., INTEGRAL – status and outlook, 2004, colloquium 195 – Outskirts of Galaxy Clusters – New Astronomy Reviews, 48, 183. intense life in the suburbs, 195, 352. Winkler, C., INTEGRAL – overview and current status, Salama, A., Ortiz, I., Arviset, C., Dowson, J., García- 2004, Proc. 5th INTEGRAL Workshop, ESA SP-552, Lario, P., Gry, C., Hernández, J., Lorente, R., 7. Matagne, J., Osuna, P., Salgado, J., Verdugo, E., User Zand, J.J.M. in ‘t, Cornelisse, R., Kuulkers, E., Verbunt, provided reduced data, catalogues and atlases in the F., Heise, J., New BeppoSAX-WFC results on ISO Data Archive, 2004, Astronomical Data Analysis superbursts, 2004, AIP Conference Proceedings, 714, Software and Systems (ADASS) XIII, 13, 26. 257. Schartel, N., XMM-Newton Observations of Gamma- Zand, J. in ‘t, Verbunt, F., Heise, J., Bazzano, A., Cocchi, Ray Burst Afterglows, 2004, Gamma-Ray Bursts: 30 M., Cornelisse, R., Kuulkers, E., Natalucci, L., years of discovery (AIP Conference Proceedings), Ubertini, P., BeppoSAX-WFC monitoring of the 727, 229. Galactic Center region, 2004, Nucl. Instrum. Meth. B Sembay, S., Abbey, A., Altieri, B., Ambrosi, R., Baskill, Suppl. Ser, 132, 518. D., Ferrando, P., Mukerjee, K., Read, A., Turner, Zurita-Heras, J.A., Shaw, S.E., Kreykenbohm, I., M.J.L., In-orbit performance of the EPIC-MOS Kretschmar, P., Gotz, D., Mereghetti, S., Lutovinov, detectors on XMM-Newton, 2004, Astronomical A., Palumbo, G., Oosterbroek, T., Budtz-Jorgensen, Telescope and Instrumentation, SPIE, 5488, 264. C., Ubertini, P., INTEGRAL detects increased activity Tiengo, A., Mereghetti, S., Ghisellini, G., Rossi, E., from 4U 0115+63, 2004, The Astronomer’s Telegram, Ghirlanda, G., Schartel, N., The X-ray afterglow of 331,1. sec4.qxd 7/12/05 9:52 AM Page 132

132 publications

Solar and Solar-Terrestrial Missions Division Solar and Solar-Terrestrial Missions Division Refereed Journals, 2003 Refereed Journals, 2004

Bewsher, D., Parnell, C.E., Pike, C.D., Harrison, R.A., Bogdanova, Y.V., Klecker, B., Paschmann, G., Kistler, Dynamics of Blinkers, 2003, Sol. Phys., 215, 217-237. L.M., Mouikis, C., Moebius, E., Reme, H., Bosqued, Brynildsen, N., Maltby, P., Brekke, P., Fredvik, T., M., Dandouras, I., Sauvaud, J.A., Cornilleau- Kjeldseth-Moe, O., Search for a chromospheric Wehrlin, N., Laakso, H., Korth, A., Bavassano- resonator above sunspots, 2003, Adv. Space Res., Cattaneo, M.B., Marcucci, M.F., Phan, T., Carlson, 32/6, 1097-1102. C., Parks, G., McFadden, J.P., McCarthy, M., Harra, L.K., Brekke, P., UV Spectroscopy with SOHO, Lundin, R., Investigation of the source region of 2003, Adv. Space Res., 32/6, 965-976. ionospheric oxygen outflow in the cleft/cusp using Hochedez, J.F., Appourchaux, T., Belsky, A., Castex, multi-spacecraft observations by CIS onboard M.C., Deneuville, A., Dhez, P., Fleck, B., Hainaut, O., Cluster, 2004, Adv. Space Res., 34, 2459-2464. Idir, M., Kleider, J.-P., Lemaire, P., Monroy, E., Darrouzet, F., Décréau, P.M.E., De Keyser, J., Masson, Munoz, E., Muret, P., Nesladek, M., Omnes, F., Pau, A., Gallagher, D.L., Santolik, O., Sandel, B.R., J.-L., Peacock, A., Schühle, U., van Hoof, C., Imageur Trotignon, J.G., Rauch, J.L., Le Guirriec, E., Canu, diamant et nitrures pour l’observation UV du soleil, P., Sedgemore, F., André, M., Lemaire, J.F., Density 2003, Journal de Physique IV, 108, 227-231. structures inside the plasmasphere – Cluster observa- Marsden, R.G., Fleck, B., The Solar Orbiter Mission, tions, 2004, Ann. Geophysicae, 22, 2577-2585. 2003, Adv. Space Res., 32/12, 2699-2704. Janhunen, P., Olsson, A., Laakso, H., The occurrence McIntosh, S.W., Fleck, B., Judge, P.G., Investigating the frequency of auroral potential structures and electric Role of Plasma Topography on Chromospheric fields as a function of altitude using Polar/EFI data, Oscillations Observed by TRACE, 2003, A&A, 405, 2004, Ann. Geophysicae, 22, 1233-1250. 769-777. Janhunen, P., Olsson, A., Hanasz, J., Russell, C.T., Schmitz, F., Fleck, B., Towards an explanation of Laakso, H., Samson, J.C., Different Alfven wave features in the diagnostic diagram of a model acceleration processes of electrons in substorms at atmosphere – I. Linear wave equations with 4–5RE and 2–3RE radial distance, 2004, Ann. convenient invariants, 2003, A&A, 399, 723-730. Geophysicae, 22, 2213–2227. Tranquille, C., Marsden, R.G., Sanderson, T.R., and Janhunen, P., Olsson, A., Laakso, H., Vaivads, A., Hofer, M.Y., A survey of helium-3 enhancements at 2- Middle-energy electron anisotropies in the auroral 20 MeV/nucleon – Ulysses COSPIN/LET observa- region, 2004, Ann. Geophysicae, 22, 237-249. tions, 2003, Ann. Geophysicae, 21, 1245-1248. Keiling, A., Rème, H., Dandouras, I., Bosqued, J.M., Vontrat-Reberac, A., Bosqued, J.M., Taylor, M.G.G.T., Sergeev, V., Sauvaud, J.A., Jacquey, C., Lavraud, B., Lavraud, B., Fontaine, D., Dunlop, M.W., Laakso, H., Louarn, P., Moreau, T., Vallat, C., Escoubet, C.P., Cornilleau-Werhlin, N., Canu, P., Fazakerley, A., Parks, G.K., McCarthy, M., Moebius, E., Amata, E., Cluster observations of the high-altitude cusp for Klecker, B., Korth, A., Lundin, R., Daly, P., Zong, Q., northward interplanetary magnetic field. A case study, New properties of energy-dispersed ions observed 2003, J. Geophys. Res., 108, 10.1029/2002JA009717. simultaneously in the plasma sheet boundary layer observed by Cluster, 2004, J. Geophys. Res., 109, 5215. Solar and Solar-Terrestrial Missions Division Lavraud, B., Phan, T., Dunlop, M., Taylor, M., Cargill, Proceedings and other Publications, 2003 P., Bosqued, J., Dandouras, I., Rème, H., Sauvaud, J., Escoubet, C., Balogh, A., Fazakerley, A., The Fleck, B., Marsden, R.G., Solar Orbiter – a mission exterior cusp and its boundary with the overview and status update, 2003, Innovative magnetosheath – Cluster multi-event analysis, 2004, Telescopes and Instrumentation for Solar Astro- Ann. Geophysicae, 22, 3039. physics, SPIE Proc. Series, 4853, 150-157. Marchaudon, A., Cerisier, J., Bosqued, J., Dunlop, M., Hochedez, J.-F., Schuehle, U., Pau, J.L., Hainaut, O., Wild, J., Décréau, P., Förster, M., Fontaine, D., Pace, E., Alvarez, J., Appourchaux, T., Auret, D.F., Laakso, H., Transient plasma injections in the Belsky, A., Bergonzo, P., Castex, M.-C., Deneuville, dayside magnetosphere – one-to-one correlated A., Dhez, P., Fleck, B., Haenen, K., Idir, M., Kleider, observations by Cluster and SuperDARN, 2004, Ann. J.-P., Lefeuvre, E., Lemaire, P., Monroy, E., Muret, P., Geophysicae, 22, 141-158. Munoz, E., Nesladek, M., Omnes, F., Peacock, A., van Masson, A., Inan, U., Laakso, H., Santolik, O., Décréau, Hoof, C., New UV detectors for solar observations, P., Cluster observations of mid-latitude hiss near the 2003, Innovative Telescopes and Instrumentation for plasmapause, 2004, Ann. Geophysicae, 22, 2565- Solar Astrophysics, SPIE Proc. Series, 4853, 419-426. 2575. Kirby, A., Brekke, P., The Role of the Sun in Climatic McIntosh, S.W., Fleck, B., Tarbell, T.D., Change, 2003, Proc. 9th Information Youth Forum. Chromospheric Oscillations in an Equatorial Coronal Granada, Spain, 1-4 Nov 2001, ESA SP-519, 2.1. Hole, 2004, ApJ, 609, L95-L98. sec4.qxd 7/12/05 9:52 AM Page 133

publications 133

Pitout, F., Escoubet, C.P., Lucek, E.A., Ionospheric NATO conference – Multiscale processes in the plasma density structures associated with magneto- Earths Magnetosphere, from Interball to Cluster, pause motion – a case study using the Cluster II/178, 131. spacecraft and the EISCAT Svalbard Radar, 2004, Fleck, B., Eight Years of SOHO, 2004, Multi- Ann. Geophysicae, 22, 2369. Wavelength Investigations of Solar Activity, Thiebault, B., Hilgers, A., Sasot, E., Laakso, H., Proceedings IAU Symp. 223. Escoubet, P., Genot, V., Forest, J., Potential barrier in Fleck, B., Eight Years of SOHO – Some Highlights, the electrostatic sheath around a magnetospheric 2004, Solar Magnetic Phenomena, Proc. spacecraft, 2004, J. Geophys. Res., 109, 10.1029/ Kanzelhoehe Summerschool and Workshop, 2004JA010398. (Accepted for Publication). Fleck, B., Harrison, R.A., Marsden, R.G., Wimmer- Solar and Solar-Terrestrial Missions Division Schweingruber, R., Summary of the Solar Orbiter Proceedings and other Publications, 2004 Payload Working Group Activities, 2004, SPIE Proc. Series, 5171, 123-130. Bewsher, D., Brown, D.S., Innes, D.E., Parnell, C.E., Gramkow, B., Escoubet, C.P., Bond, P., Bergquist, K., Probability Analysis of Coincident Blinkers and Double Star – East meets west in near-Earth space, Explosive Events, 2004, Proc. SOHO-15, ESA SP- 2004, ESA Bulletin, 118, 22. 575. Lundquist, L.L., Fisher, G.H., McTiernan, J.M., Bewsher, D., Parnell, C.E., Pike, C.D., Harrison, R.A., Regnier, S., Using Synthetic Emission Images to Dynamics of Transition Region Blinkers using Constrain Heating Parameters, 2004, SOHO 15: SOHO/CDS, 2004, Proc. SOHO-13 ‘Waves, Coronal Heating, ESA SP-575. Oscillations and Small Scale Transient Events in the Marsden, R.G., Ulysses at Solar Maximum, 2004, Solar Atmosphere: A Joint View from SOHO and Astrophysics and Space Science Library, The Sun and TRACE’, ESA SP-547, 267-272. the Heliosphere as an Integrated System, 317, 91. Brekke, P., Chaloupy, M., Fleck, B., Haugan, S.V., McIntosh, S.W., Fleck, B., Spatial Correlations of Phase Overbeek, T. van, Schweitzer, H., Space Weather Relationships in TRACE Ultraviolet Bandpasses, Effects on SOHO and its Space Weather Warning 2004, Proc. IAU Symp. 219, S-219, CD-696. Capabilities, 2004, Effects of Space Weather on McIntosh, S.W., Fleck, B., Mapping the Chromospheric Technology Infrastructure, 109-122. Plasma Topography Through Chromospheric Oscilla- Brekke, P., Fleck, B., Nearly Eight Years of SOHO tions, 2004, Proc. SOHO-13: Waves, oscillations and Observations. Some Highlights, 2004, Proc. 8th other small-scale transient events in the solar Spacecraft Charging Technology Conference, October atmosphere, ESA SP-547, 149-154. 20-24, 2003, Huntsville, Alabama, NASA/CP-2004- Pickett, J.S., Santolik, O., Kahler, S.W., Masson, A., 213091, P2. Adrian, M.L., Gurnett, D.A., Bell, T.F., Laakso, H., Brekke, P., Fleck, B., Haugan, S.V., Is the Sun going Parrot, M., Decreau, P., Fazakerley, A., Cornilleau- crazy?, 2004, Spaceflight Now, 46, 50-51. Wehrlin, N., Balogh, A., Andre, M., Multi-point Brekke, P., Fleck, B., Haugan, S.V., van Overbeek, T., Cluster Observations of VLF Risers, Fallers, and Schweitzer, G., Chaloupy, M., Space Weather Effects Hooks at and near the Plasmapause, 2004, Multiscale on SOHO and its Role as a Space Weather Watchdog, processes in the Earth’s magnetosphere – From 2004, Proc. 8th Spacecraft Charging Technology Interball to Cluster, Kluwer Academic Publishers, Conference, October 20-24, 2003, Huntsville, Dordrecht, The Netherlands, 178, 307. Alabama, USA, NASA/CP-2004-213091, P1. Regnier, S., Canfield, R.C., How is Magnetic Energy Brekke, P., Fleck, B., Haugan, S.V., van Overbeek, T., Stored and Released?, 2004, SOHO 15: Coronal Schweitzer, H., Chaloupy, M., Space weather effects Heating, ESA SP-575. on SOHO and its leading role in the early-wearning Regnier, S., Canfield, R.C., Magnetic Energy and system for space weather, 2004, Proc. 84th American Helicity Budget in AR 8210 What are the Sources of Meteorological Society Meeting, (Accepted for Flaring Activity?, 2004, Multiwavelength Investiga- Publication). tions of Solar Activity, Proceedings IAU Symposium Brekke, P., Fleck, B., Haugan, S.V., van Overbeek, T., 223, (Accepted for Publication). Schweitzer, H., Simonin, B., Space weather effects on Regnier, S., Fleck, B., Magnetic Field Evolution of SOHO and its leading as a space weather watchdog, AR0486 before and after the X17 Flare on October 2004, Multiscale Coupling of Sun-Earth Processes, 28, 2003, 2004, SOHO 15: Coronal Heating, ESA (Accepted for Publication). SP-575. Escoubet, C.P., Fehringer, M., Cluster – new view on the Schuehle, U., Hochedez, J.-F., Pau, J.L., Rivera, C., boundaries of the magnetosphere, 2004, COSPAR Munoz, E., Alvarez, J., Kleider, J.-P., Lemaire, P., Colloquia Series – Frontiers in Magnetospheric Appourchaux, T., Fleck, B., Peacock, A., Richter, M., Plasma Physics, 16. Kroth, U., Gottwald, A., Castex, M.-C., Deneuville, Escoubet, C.P., Laakso, H., Godstein, M., Cluster – new A., Muret, P., Nesladek, M., Omnes, F., John, J., van measurements of plasma structures in 3D, 2004, Hoof, C., Development of imaging arrays for solar sec4.qxd 7/12/05 9:52 AM Page 134

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UV observations based on wide band gap materials, Space Telescope Operations Division 2004, SPIE Proc. Series, 5171, 231-238. Refereed Journals, 2003 Volpp, J., Escoubet, C.P., Foley, S., Godfrey, J., Hapgood, M., Pallaschke, S., Cluster constellation Aloisi, A., Savaglio, S., Heckman, T.M., Hoopes, C.G., change manoeuvres – Management and Operations, Leitherer, C., Sembach, K.R., Abundances in the 2004, SpaceOps 2004 Proceedings, 3, 238. Neutral Interstellar Medium of I Zw 18 from Far Ultraviolet Spectroscopic Explorer Observations, 2003, ApJ, 595, 760. Annibali, F., Greggio, L., Tosi, M., Aloisi, A., Leitherer, C., The Star Formation History of NGC 1705 – A Poststarburst Galaxy on the Verge of Activity, 2003, AJ, 126, 2752. Arribas, S., Colina, L., INTEGRAL Spectroscopy of IRAS 17208-0014. Implications for the Evolutionary Scenarios of Ultraluminous Infrared Galaxies, 2003, ApJ, 591, 791. Battaner, E., Mediavilla, E., Guijarro, A., Arribas, S., Florido, E., Axisymmetrical gas inflow in the central region of NGC 7331, 2003, A&A, 401, 67. Bemmel, I.M. van , Vernet, J., Fosbury, R.A.E., Lamers, H.J.G.L.M., Polarization and kinematics in Cygnus A, 2003, MNRAS, 345, L13-L17. Bertero, M., Boccacci, P., Custo, A., De Mol, C., Robberto, M., A Fourier-based method for the restoration of chopped and nodded images, 2003, A&A, 406, 765. Bik, A., Lamers, H., Bastian, N., Panagia, N., Romani- ello, M., Clusters in the Inner Spiral Arms of M51 – The Cluster IMF and the Formation History, 2003, A&A, 397, 473. Binette, L., Groves, B., Villar-Martin, M., Fosbury, R.A.E., Axon, D.J., High-z nebulae – Ionization by stars or by an obscured QSO?, 2003, A&A, 405, 975- 980. Boeker, T., Schinnerer, E., Lisenfeld, U., Molecular gas in the central regions of the latest-type spiral galaxies, 2003, A&A, 406, 87. Boeker, T., Stanek, R., van der Marel, R.P., Searching for Bulges at the End of the Hubble Sequence, 2003, AJ, 125, 1073. Bond, H.E., Henden, A., Levay, Z., Panagia, N., Sparks, W.B., Starrfield, S., Wagner, R.M., Corradi, R.L.M., Munari, U., An energetic stellar outburst accompanied by circumstellar light echoes, 2003, Nature, 422, 405. Chiaberge, M., Gilli, R., Capetti, A., Macchetto, F.D., The Nuclear Spectral Energy Distribution of NGC 6251 – A BL Lacertae Object in the Center of an FR I Radio Galaxy, 2003, ApJ, 597, 166C. Chiaberge, M., Gilli, R., Macchetto, F.D., Sparks, W.R., Capetti, A., What do the Hubble Space Telescope and Chandra Tell Us about the Jet and the Nuclear Region of the Radio Galaxy 3C 270?, 2003, ApJ, 582, 645C. D’Elia, V., Padovani, P., Landt, H., The Disc-Jet Relation in Strong-lined Blazars, 2003, MNRAS, 338/4, 1081. Della Valle, M., Panagia, N., The Rate and the Origin of Type Ia Supernovae in Radiogalaxies, 2003, ApJ, 587, L71. sec4.qxd 7/12/05 9:52 AM Page 135

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Kamp, I., Sammar, F., Circumstellar Disks around Young Space Telescope Operations Division Solar-Type Stars, 2004, Stars as Suns: Activity, Proceedings and other Publications, 2004 Evolution and Planets, IAU Symposium 219, 102. Kerber, F., Rosa, M.R., Nave, G., Reader, J., Sansonetti, Albrecht, R., HST Experience in Data Management, 2004, C.J., Bristow, P., Lercher, G., New Insights from the Astronomische Nachrichten, 325, 590. ST-ECF Lamp Project, 2004, ST-ECF Newsletter, 37, Albrecht, R., The Changing Role of the Telescope in 5. Astronomy, 2004, Developing Space Science World Maíz-Apellániz, J., Massive Young Clusters in the Local Wide, Kluwer Academic Publishers, The Netherlands, Group, 2004, The Local Group as an Astrophysical 1, 363. Laboratory, (Accepted for Publication). Allen, M., Genova, F., Arviset, C., Derriere, S., Didelon, Maíz-Apellániz, J., Massive Young Clusters, 2004, How P., Garrington, S., Mann, R., Micol, A., Ochsenbein, F., does the Galaxy work? 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SPIE ‘Focal Plane Arrays for Space Cosmology: Essential Science in Hubble’s Final Telescopes’, 5167, 166. Years, (Accepted for Publication). Sirianni, M., Mutchler, M., Clampin, M., Ford, H.C., Maíz-Apellániz, J., Bond, H.E., Siegel, M.H., Lipkin, Y., Illingworth, G.D., Hartig, G.F., van Orsow, D., Maoz, D., Ofek, E.O., Poznanski, D., SN 2004dj, a Wheeler, T., Performance of the Advanced Camera supernova in a nearby young compact cluster, 2004, For Surveys CCDs after two years in orbit., 2004, JENAM 2004: The many scales of the Universe, SPIE Proceedings, 5499, 173. (Accepted for Publication). Tuairisg, S.Ó., Butler, R., Golden, A., Shearer, A., Voisin, Micol, A., Pierfederici, F., Benvenuti, P., Review of the B., Micol, A., Automated reduction and analysis of ASTROVIRTEL Experience at the end of its Three images from multiple data archives, 2004, Approved Cycles, 2004, Astronomical Data Analysis Astronomical Data Analysis Software and Systems Software and Systems (ADASS) XIII, 314, 197. (ADASS) XIII, 314, 444. Modigliani, A., Rosa, M.R., Evaluation of Methods to Tuellmann, R., Rosa, M.R., Dettmar, R.-J., SOAP and Locate Emission Lines From Calibration Lamps in 2D the Interstellar Froth, 2004, Extra-planar Gas, ASP Spectroscopic Data, 2004, Astronomical Data conference proceedings, (Accepted for Publication). Analysis Software and Systems (ADASS) XIII, ASP Van Dyk, S.D., Weiler, K.W., Sramek, R.A., Panagia, N., Conference Proceedings, 314, 808. 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Weiler, K.W., Diamond, P.J., Van Dyk, S.D., Voisin, B., Micol, A., Tuairisg, S.Ó., Butler, R.F., Lundqvist, P., Panagia, N., Shapiro, I.I., Sramek, R.A., Golden, A., Shearer, A., Simulating instruments for High-resolution Radio Imaging of Young Supernovae, mining uncalibrated archives, 2004, Optimizing 2004, IAU Colloquium 192 – Cosmic Explosions – Scientific Return for Astronomy through Information Springer Proceedings in Physics, 99, 97. Technologies, held in Glasgow, 24 June 2004, 5493, Pierfederici, F., Dolensky, M., Micol, A., Pirenne, B., 294. ASTROVIRTEL, Tools and Operations, 2004, Toward Wiklind, T., Molecules in the Interstellar Medium, 2004, an International Virtual Observatory, Proceedings of Origin and Evolution of the Elements, Carnegie the ESO/ESA/NASA/NSF Conference held in Garch- Observatories Centennial Symposium IV, 4, 357. ing, Germany, 10-14 June 2002. ESO Astrophysics Symposia, 129. Prada Moroni, P.G., Straniero, O., De Marchi, G., Fundamental Physics Missions Division Paresce, F., White dwarf cosmochronology and M4, Refereed Journals, 2003 2004, Memorie della Societa’ Astronomica Italiana, 75, 81. Pollack, S.E., Jennrich, O., Stebbins, R.T., Bender, P., Pérez, E., Maíz-Apellániz, J., Mas-Hesse, J.M., NGC Status of LISA phase measurement work in the US, 604, the Scaled OB Association (SOBA) Prototype, 2003, Class. Quantum Grav., 20, S193-S199. 2004, JENAM 2004: The many scales of the Universe, Heinzel, G., Wand, V., Garcia, A., Jennrich, O., Brax- (Accepted for Publication). maier, C., Robertson, D., Middleton, K., Hoyland, D., Quinn, P.J., Allen, M., Andrews, K., Boch, T., Bonnarel, Rudiger, A., Schilling, R., Johann, U., Danzmann, K., F., Derriere, S., Dolensky, M., Fernique, P., Hill, M., The LTP interferometer and phasemeter, 2004, Class. Leoni, M.C., Linde, A., Micol, A., Pirenne, B., Quantum Grav., 21, S581-S587. 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Chief Scientist Shkuratov, Yuriy G., Stankevich, Dmitriy G., Kaydash, Refereed Journals, 2003 Vadim G., Omelchenko, Vitaliy V., Pieters, Carle M., Pinet, Patrick C., Chevrel, Serge D., Daydou, Yves H., Duke, M.B., Foing, B.H., Preface to Proceedings of Foing, Bernard H., Sodnik, Zoran, Josset, Jean-Luc, COSPAR 2002 Moon Session, 2003, Adv. Space Res., Taylor, Lawrence A., Shevchenko, Vladislav V., 31, 2291. Composition of the lunar surface as will be seen from Dunkin, S.K., Grande, M., Casanova, I., Fernandes, V., SMART-1 – A simulation using Clementine data, Heather, D.J., Kellett, B., Muinonen, K., Russell, S.S., 2003, J. Geophys. Res., 108,1. Browning, R., Waltham, N., Parker, D., Kent, B., Volp, J., Foing, B., www.lunarexplorer.org – Educating Perry, C.H., Swinyard, B., Perry, A., Feraday, J., the general public, 2003, Adv. Space Res., 31, 2455. Howe, C., Phillips, K., McBride, G., Huovelin, J., Muhli, P., Hakala, P.J., Vilhu, O., Thomas, N., Hughes, D., Alleyne, H., Grady, M., Lundin, R., Chief Scientist Barabash, S., Baker, D., Clark, P.E., Murray, C.D., Proceedings and other Publications, 2003 Guest, J., DUston, L.C., Maurice, S., Foing, B., Christou, A., Owen, C., Charles, P., Laukkanen, J., Boudin, N., Ruiterkamp, R., Foing, B.H., A survey of the Koskinen, H., Kato, M., Sipila, K., Nenonen, S., PAH electronic spectra and their search in the Holmstrom, M., Bhandari, N., Elphic, R., Lawrence, Interstellar Medium, 2003, Astrophysics of Dust, May D., Scientific rationale for the D-CIXS X-ray 26-30, 2003, 162. spectrometer on board ESA’s SMART-1 mission to the Cox, N., Ehrenfreund, P., Cami, J., Kaper, L., Foing, B., Moon, 2003, Planet. Space Sci., 51, 435. Cordiner, M., Sarre, P., Snow, T., Salama, F., Carbon Foing, B.H., Racca, G.D., Marini, A., Heather, D.J., chemistry and diffuse interstellar bands in the Koschny, D., Grande, M., Huovelin, J., Keller, H.U., Magellanic Clouds, 2003, Astrophysics of Dust, 43. Nathues, A., Josset, J.L., Malkki, A., Schmidt, W., Ehrenfreund, P., Cami, J., Foing, B.H., Kaper, L., Cox, Noci, G., Birkl, R., Iess, L., Sodnik, Z., McManamon, N., Jimenez-Vincente, J., Salama, F., Sarre, P., Snow, P., SMART-1 mission to the moon – Technology and T., Maier, J.P., Magellanic Diffuse Interstellar Bands science goals, 2003, Adv. Space Res., 31, 2323. and Carbon Chemistry, 2003, The Astrochemistry of Garcia-Alvarez, D., Foing, B.H., Montes, D., Oliveira, J., External Galaxies, 25th meeting of the IAU, Joint Doyle, J.G., Messina, S., Lanza, A.F., Rodono, M., Discussion 21, 21,2. Abbott, J., Ash, T.D., Baldry, I.K., Bedding, T.R., Foing, B.H., Neiner, C., 2003, Observing stellar activity Buckley, D.A., Cami, J., Cao, H., Catala, C., Cheng, from space, EAS Publications Series 9, 147. K.P., Domiciano de Souza, A., Donati, J.F., Hubert, Foing, B.H., ESA Cosmic Vision programme, 2003, A.-M., Janot-Pacheco, E., Hao, J.X., Kaper, L., SF2A Proceedings Societe Francaise d’Astronomie et Kaufer, A., Leister, N.V., Neff, J.E., Neiner, C., Astrophysique, 4. Orlando, S., OToole, S.J., Schaefer, D., Smartt, S.J., Foing, B.H., Racca, G.D., Marini, A., Grande, M., Stahl, O., Telting, J., Tubbesing, S., Simultaneous Huovelin, J., Josset, J.L., Keller, H.U., Nathues, A., optical and X-ray observations of flares and rotational Koschny, D., Malkki, A., ESA SMART-1 Mission to modulation on the RS CVn binary HR 1099 (V711 the Moon, 2003, Recent Progress in Planetary Tau) from the MUSICOS 1998 campaign, 2003, A&A, Exploration, 25th meeting of the IAU, Special Session 397, 285. 1, 35. Grande, M., Browning, R., Waltham, N., Parker, D., Garcia-Alvarez, D., Foing, B.H., Montes, D., Oliveira, J., Dunkin, S.K., Kent, B., Kellett, B., Perry, C.H., Doyle, J.G., MUSICOS 98 Collaboration 2003, Swinyard, B., Perry, A., Feraday, J., Howe, C., MUSICOS 1998: Observations of Rotational McBride, G., Phillips, K., Huovelin, J., Muhli, P., Modulation and Flares on the RS CVn Binary Hakala, P.J., Vilhu, O., Laukkanen, J., Thomas, N., HR1099, The Future of Cool-Star Astrophysics: 12th Hughes, D., Alleyne, H., Grady, M., Lundin, R., Cambridge Workshop on Cool Stars, Stellar Systems, Barabash, S., Baker, D., Clark, P.E., Murray, C.D., and the Sun (2001 July 30 - August 3), Eds. A. Brown, Guest, J., Casanova, I., DUston, L.C., Maurice, S., G.M. Harper and T.R. Ayres, (University of Foing, B., Heather, D.J., Fernandes, V., Muinonen, K., Colorado), 2003, 12, 958-963. Russell, S.S., Christou, A., Owen, C., Charles, P., Racca, G., Foing, B.H., A solar-powered visit to the Koskinen, H., Kato, M., Sipila, K., Nenonen, S., Moon. The SMART-1 mission, 2003, ESA Bulletin, Holmstrom, M., Bhandari, N., Elphic, R., Lawrence, 113, 14. D., The D-CIXS X-ray mapping spectrometer on TenKate, I.L., Ruiterkamp, R., Botta, O., Lehmann, B., SMART-1, 2003, Planet. Space Sci., 51, 427. Gomez Hernandez, C., Boudin, N., Foing, B.H., Shkuratov, Yu.G., Kreslavsky, M.A., Stankevich, D.G., Ehrenfreund, P., Simulations of Martian Surface and Kaydash, V.G., Pinet, P., Shevchenko, V.V., Foing, Subsurface Processes, 2003, 34th Annual Lunar and B.H., Josset, J.-L., The SMART-1 Mission – Photo- Planetary Science Conference, March 17-21, 2003, metric Studies of the Moon with the AMIE Camera, League City, Texas, 1313. 2003, Solar System Reviews, 37, 251. Washuettl, A., Strassmeier, K.G., Foing, B., MUSICOS- sec4.qxd 7/12/05 9:52 AM Page 142

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98 Team 2003, MUSICOS Observations of the Stagnaro, L., Almeida, M., Koschny, D., Frew, D., Chromospherically Active Binary Star EI Eridani, The Zender, J., Heather, J., Grande, M., Huovelin, J., Future of Cool-Star Astrophysics: 12th Cambridge Keller, H.U., Nathues, A., Josset, J.L., Malkki, A., Workshop on Cool Stars, Stellar Systems, and the Sun Schmidt, W., Noci, G., Birkl, R., Iess, L., Sodnik, Z., (2001 July 30 - August 3), Eds. A. Brown, G.M. McManamon, P., ESA’s SMART-1 Mission Launched Harper and T.R. Ayres, (University of Colorado), To The Moon: Technology And Science Goals, Proc. 2003, 12, 1008-1013. International Lunar Conference 2003, A.A.S./Space Age Publ. (Ed. S.M. Durst et al.), 3. Foing, B.H., Zegers, T.E., van Kan, M., Pischel, R., Chief Scientist Martin, P., Jaumann, R., Hauber, E., Greeley, R., Refereed Journals, 2004 Hoffmann, H., Neukum, G., The HRSC Co- Investigator Team, Gusev Crater and Early Martian Crespo-Chacón, I., Montes, D., Fernández-Figueroa, History: Clues from Mars-Express and MGS Study. M.J., López-Santiago, J., GarcÍa-Alvarez, D., Foing, Second Conference on Early Mars: Geologic, B.H., High Temporal Resolution Spectroscopic Hydrologic, and Climatic Evolution and the Observations of the Flare Star V1054 Oph, 2004, Implications for Life, LPI Publ., 8070. Astrophysics and Space Science, 292/1, 697-703. Greeley, R., Thompson, S., Whelley, P., Neukum, G., Foing, B.H., The case for the first Indian Robotic Squyres, S., Sullivan, R.J., Rafkin, S.C., Michaels, T., Mission to the Moon, 2004, Current Science, 87/8, Golombek, M.P., Arvidson, R., Foing, B.H., Richter, 1061-1065. L., Rongxing, L., Pinet, P., HRSC Science Team, Head, J.W., Neukum, G., Jaumann, R., Hiesinger, H., Athena Science Team, 2004, Wind Patterns at the Hauber, E., Carr, M., Masson, P., Foing, B., Mars Exploration Rover (MER) Sites Inferred from Hoffmann, H., Kreslavsky, M., Werner, S., Milkovich, Mars Express HRSC and MER Images, AGU Fall S., HRSC, C.I., Tropical to Mid-Latitude Glaciation Meeting 21, 5. on Mars – Evidence for Snow and Ice Accumulation Racca, G.D., Foing, B.H., Brinkmann, J., de Bijl, J., di and Flow in Mars Express HRSC Data, 2004, Nature, Napoli, L., Estublier, D., Evrard, E., Grnagel, R., (Accepted for Publication). Lumb, R., Marini, A., Rumler, P., Stagnaro, L., van Kozyrovska, O., Korniichuk, O.S., Voznyuk, T.M., Dooren, J., 2004, En Route To The Moon: SMART-1 Lytvynenko, T.L., Rogutskyy, I.S., Mytrokhyn, O.V., Final Preparation, Launch And Early Flight. Proc. Estrella-Lopis, V.R., Borodinova, T.I., Foing, B.H., International Lunar Conference 2003, A.A.S./Space Kordyum, V.A., Microbial community in a precursory Age Publ. (Ed. S.M. Durst et al.), 213. scenario of growing Tagetes patula in a lunar Zegers, T.E., Conan, Y.G., Foing, B.H., Noachian greenhouse, 2004, Kosmichna nauka i technologiya, Martian highlands; the habitat of ancient life?, 2004, 11, 10. Proc. Third European Workshop on Exo-Astrobiology, Prinja, R.K., Rivinius, T., Stahl, O., Kaufer, A., Foing, 18-20 November 2003, Madrid, Spain, ESA SP-545, B.H., Cami, J., Orlando, S., Photospheric and stellar 313. wind variability in 949 Ori (B0 Ia), 2004, A&A, 418, Zegers, T.E., Conan, Y.G., Foing, B.H., Geology of 727-736. Noachian Martian Highlands Surrounding the Gusev Unruh, Y.C., Donati, J.F., Oliveira, J.M., Cameron, A.C., Crater, 2004, 35th Lunar and Planetary Science Catala, C., Henrichs, H.F., Johns-Krull, C.M., Foing, Conference, March 15-19, 2004, League City, Texas, B., Multisite observations of SU Aurigae, 2004, LPI, 1767. MNRAS, 348, 1301-1320.

Chief Scientist Proceedings and other Publications, 2004

Foing, B.H., 2004., Preface to The Proceedings of Hawaii International Lunar Exploration Conference 2003, A.A.S./Space Age Publ. (Ed. S.M. Durst et al.), 531. Foing, B.H., Racca, G.D., Marini, A., Grande, M., Huovelin, J., Josset, J.L., Keller, H.U., Nathues, A., Heather, D., Koschny, D., Malkki, A., ESA’s SMART-1 Mission to the Moon – Goals, Status and First Results, 2004, 35th Lunar and Planetary Science Conference, March 15-19, 2004, League City, Texas, LPI, 35, 1413. Foing, B.H., Racca, G.D., Marini, A., Evrard, E., sec4.qxd 7/12/05 9:52 AM Page 143

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Science Payload and Advanced Concepts Office Nevalainen, J., Lieu, R., Bonamente, M., Lumb, D., Soft Refereed Journals, 2003 X-Ray Excess Emission in Clusters of Galaxies Observed with XMM-Newton, 2003, ApJ, 584, 716. Acker, A., Neiner, C., Quantitative classification of WR Owens, A., Bavdaz, M., Brammertz, G., Gostilo, V., nuclei of planetary nebulae, 2003, A&A, 403, 659. Graafsma, H., Kozorezov, A., Krumrey, M., Lisjutin, Bertuccio, G., Casiraghi, R., Maiocchi, D., Owens, A., I., Peacock, A., Puig, A., Sipila, H., Zatokola, S., The Bavdaz, M., Peacock, A., Andersson, H., Nenonen, S., X-ray response of TlBr, 2003, Nucl. Instr. & Meth. A, Noise Analysis of Gallium Arsenide Pixel X-Ray A497, 370. Detectors Coupled to Ultra-Low Noise Electronics, Owens, A., Bavdaz, M., Brammertz, G., Gostilo, V., 2003, IEEE Trans. Nucl. Sci., 50, 723. Haack, N., Kozorezov, A., Lisjutin, I., Peacock, A., Brammertz, G., Kozorezov, A.G., Wigmore, J.K., Zatoloka, S., Hard X-ray spectroscopy using a small Hartog, R. den, Verhoeve, P., Martin, D., Peacock, A., format TlBr array, 2003, Nucl. Instr. & Meth. A, A497, Golubov, A.A., Rogalla, H., Energy-dependent kinetic 359. model of photon absorption by superconducting Owens, A., Mosselmans, J., Peacock, A., Near K-edge tunnel junctions, 2003, J. Appl. Phys, 94, 5854. linear attenuation coefficients for amorphous and Ellery, A., Kolb, C., Lammer, H., Parnell, J., Edwards, crystalline GaAs, 2003, J. Radiation Physics and H., Richter, L., Patel, M., Romstedt, J., Dickensheets, Chemistry, 66,1. D., Steele, A., Cockell, C., Astrobiological instru- Reynolds, A.P., Bruijne, J.H.J. de, Perryman, M.A.C., mentation for Mars – the only way is down, 2003, Peacock, A., Bridge, C.M., Temperature determina- International J. Astrobiology, 1, 365-380. tion via STJ optical spectroscopy, 2003, A&A, 400, Gondoin, P., The corona of V390 Aurigae (HD 33798), 1209-1217. 2003, A&A, 355, 364. Verhoeve, P., Brammertz, G., Martin, D., Peacock, A., Gondoin, P., The corona of HD 223460 (HR 9024), 2003, Quasiparticle loss rates in Ta-based superconducting A&A, 409, 263. tunnel junctions, 2003, Nucl. Instr. & Meth., 520, 246. Gondoin, P., Orr, A., Lumb, D., XMM-Newton Verhoeve, P., Martin, D., Dordrecht, A. van, Verveer, J., observation of the Seyfert 1 galaxy ESO 141-G55, Hartog, R. den, Peacock, A., 120-pixel array of super- 2003, A&A, 398, 967. conducting tunnel junctions as spectro-photometer for Gondoin, P., Orr, A., Lumb, D., Siddiqui, H., XMM- optical astronomy, 2003, Nucl. Instr. & Meth., 513, Newton observation of the Seyfert 1 galaxy NGC 206. 3227, 2003, A&A, 397, 883. Gostilo, V., Owens, A., Bavdaz, M., Lisjutin, I., Peacock, A., Sipila, H., Zatoloka, S., A comparison of the X-ray Science Payload and Advanced Concepts Office performance of TlBr crystals grown by the Proceedings and other Publications, 2003 Bridgeman–Stockbarger and travelling molten zone methods, 2003, Nucl. Instr. & Meth., A509, 47. Absil, O., den Hartog, R., Erd, C., Gondoin, P., Lumb, D.H., Finoguenov, A., Saxton, R., Aschenbach, Kaltenegger, L., Fridlund, M., Rando, N., Wilhelm, B., Gondoin, P., Kirsch, M., Stewart, I., In-orbit R., GENIESIM – The GENIE Simulation Software, Vignetting Calibrations of XMM-Newton Telescopes, 2003, Proc. ‘Towards other Earths’, ESA SP-539, 2003, Experimental Astronomy, 15, 89. 317. Lumb, D.H., Rando, R., Peacock, A., Favata, F., Atzei, A.C., Falkner, P., Berg, M.L. van den, Peacock, A., Perryman, M.A.C., Focal plane cameras for ESA Jupiter Microsat Explorer Programme, 2003, 5th IAA optical astronomy missions, 2003, Nucl. Instr. & Conference on Low-Cost Planetary Missions, ESA Meth., A513, 112. SP-542, 189. Neiner, C., Geers, V.C., Henrichs, H.F., Floquet, M., Atzei, A.C., Falkner, P., Berg, M.L. van den, Peacock, A., Fremat, Y., Hubert, A.-M., Preuss, O., Wiersema, K., The Jupiter Microsat Explorer Programme, 2003, 37th Discovery of a magnetic field in the Slowly Pulsating ESLAB Symp., 2-4 December 2003, ESA SP-543, 17. B star zeta Cassiopeia, 2003, A&A, 406, 1019. Bavdaz, M., Peacock, A., X-ray Optics – new Neiner, C., Henrichs, H.F., Floquet, M., Fremat, Y., technologies at ESA, 2003, SPIE Proceedings – Preuss, O., Hubert, A.M., Geers, V.C., Tijani, A.H., X-Ray and Gamma-Ray Telescopes and Instruments Nichols, J., Jankov, S., Rotation, pulsations and for Astronomy, 4851, 421. magnetic field in V2052 Ophiuchi – a new He-strong Bavdaz, M., Peacock, A., Laan, T. van der, Parmar, A., star, 2003, A&A, 411, 565. The XEUS – approaches to mission design, 2003, Neiner, C., Hubert, A.-M., Fremat, Y., Floquet, M., SPIE Proceedings – X-Ray and Gamma-Ray Jankov, S., Preuss, O., Henrichs, H.F., Zorec, J., Telescopes and Instruments for Astronomy, 4851, 396. Rotation and magnetic field in the Be star omega Berg, M.L. van den, Falkner, P., Atzei, A.C., Peacock, A., Orionis, 2003, A&A, 409, 275. Venus Microsat Explorer Programme, an ESA Neumann, D.M., Lumb, D.H., Pratt, G.W., Briel, U.G., Technology Reference Mission, 2003, Proc. 5th IAA The dynamical state of the Coma cluster with XMM- conference on low-cost planetary missions, ESA Newton, 2003, A&A, 400,811. SP-542, 73. sec4.qxd 7/12/05 9:52 AM Page 144

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Bertrand, R., Del Bianco, A., Harnisch, B., Jessberger, detectors, 2003, SPIE Proceedings – X-Ray and E.K., Peuser, P., Romstedt, J., Rost, D., Schneider, K., Gamma-Ray Telescopes and Instruments for Weber, I., A minituarized laser instrument for Astronomy, 4851, 922. chemical and mineralogical in-situ analysis on Martin, D., Verhoeve, P., Hartog, R. den , Bruijne, J. de, planetary surfaces, 2003, Geophysical Research Reynolds, A., Dordrecht, A. van, Verveer, J., Peacock, Abstracts, 5, EAE03-A-05861. A., 12x10 pixels superconducting tunnel junction Erd, C., Owens, A., Brammertz, G., Lumb, D., Bavdaz, array based spectrophotometer for optical astronomy, M., Peacock, A., Nenonen, S., Andersson, H., 2003, SPIE Proceedings – Instrument Design and Measurements of the quantum efficiency and Performance for Optical/Infrared Ground-based depletion depth in gallium-arsenide detectors, 2003, Telescopes, 4841, 805. SPIE Proceedings – X-Ray and Gamma-Ray Miyaji, T., Griffiths, R.E., Lumb, D., Sarajedini, V., Detectors and Applications IV, 4784, 386. Siddiqui, H., XMM-Newton view of the Hubble Deep Falkner, P., Erd, C., Highly Integrated Payload Suites and Field-North and Groth-Westphal strip regions, 2003, Related Data Link Requirements, 2003, ISWS – Astron. Nachtrichten, 324, 24. International SpaceWire Seminar 2003, 1, 25. Neiner, C., Appourchaux, T., Global fitting of power Falkner, P., Erd, C., Kraft, S., Peacock, T., Remote spectra of solar-like stars, 2003, 2nd Eddington Sensing Instrument Suite for Planetary Exploration, Workshop: Stellar structure and habitable planet 2003, Geophysical Research Abstracts, 5, 12462. finding, ESA SP-538, 373. Falkner, P., Romstedt, J., Verhoeve, P., Peacock, A., Neiner, C., Hubert, A.-M., Floquet, M., Seismology of Instrumentation for in-situ measurements on the Be stars, 2003, 2nd Eddington Workshop: Stellar surface of Mercury, 2003, Geophysical Research structure and habitable planet finding, ESA SP-538, Abstracts, 5, 12557. 369. Fridlund, M., Gondoin, P., The Darwin Mission, 2003, Owens, A., Peacock, A., Bavdaz, M., Progress in SPIE Proceedings – Interferometry in Space, 4852, Compound Semiconductors, 2003, SPIE Proceedings 394. – X-Ray and Gamma-Ray Telescopes and Instruments Gondoin, P., Absil, O., Fridlund, M., Erd, C., Hartog, R. for Astronomy, 4851, 1059. den, Rando, N., Glindemann, A., Koehler, B., Rando, N., Murphy, E., Falkner, P., Peacock, A., The Wilhelm, R., Karlsson, A., Labadie, L., Mann, I., Laser Altimeter for Planetary Exploration (LAPE), Peacock, A., Richichi, A., Sodnik, Z., Tarenghi, M., 2003, Geophysical Research Abstracts, 5, 12399. Volonte, S., The Darwin Ground-based European Torkar, K., Riedler, W., Romstedt, J., Jeszensky, H., Nulling Interferometry Experiment (GENIE), 2003, Steller, M., Arends, H., The MIDAS atomic force SPIE Proceedings – Interferometry for Optical microscope for cometary dust – technical highlights Astronomy II, 4838, 700. and future perspectives, 2003, Geophysical Research Gondoin, P., Absil, O., den Hartog, R., Kaltenegger, L., Abstracts, 5, EAE-A-07246. Eiroa, C., Erd, C., Fridlund, M., Karlsson, A., Verhoeve, P., Hartog, R. den, Kozorezov, A., Martin, D., Peacock, A., Sodnik, Z., Volonte, S., Wilhelm, R., Dordrecht, A. van, Wigmore, J.K., Peacock, A., Schoeller, M., Glindemann, A., The Ground-based Integration time dependence of tunnel noise and European Nulling Interferometry Experiment energy resolution of superconducting tunnel junctions, (Darwin-GENIE), 2003, Proc. ‘Towards Other 2003, SPIE Proceedings – Instrument Design and Earths’, ESA SP-539, 121. Performance for Optical/Infrared Ground-based Gondoin, P. XMM-Newton observation of the Seyfert 1 Telescopes, 4841, 141. galaxy IC4329A, 2003, Active Galactic Nuclei: from Central Engine to Host Galaxy, ASP Conf. Series 290, 97. Science Payload and Advanced Concepts Office Grard, R., Falkner, P., The Bepi Colombo Mission to Refereed Journals, 2004 Mercury, 2003, Geophysical Research Abstracts, 5, 10727. Brammertz, G., Peacock, A., Verhoeve, P., Martin, D., Hartog, R. den, Absil, O., Kaltenegger, L., Gondoin, P., Venn, R., Optical photon detection in Al Super- Wilhelm, R., Fridlund, M., Could GENIE detect Hot conducting Tunnel Junctions, 2004, Nucl. Instr. & Jupiters?, 2003, Proc. ‘Towards Other Earths’, ESA Meth., A 520, 508. SP-539, 399. Gondoin, P., X-ray spectroscopy of the W UMa-type Hartog, R. den, Kozorezov, A., Verhoeve, P., Martin, D., binary 44 Bootis, 2004, A&A, 426, 1035. Noise in a Quatratran-based detector – a comparison Gondoin, P., The corona of HD 199178 (V 1794 Cygni), with Superconducting Tunnel Junctions, 2003, SPIE 2004, A&A, 413, 1095. Proceedings – X-Ray and Gamma-Ray Telescopes and Gondoin, P., X-ray spectroscopy of the W UMa-type Instruments for Astronomy, 4851, 1002. binary VW Cephei, 2004, A&A, 415, 1113. Hartog, R. den, Owens, A., Kozorezov, A., Bavdaz, M., Gondoin, P., Orr, A., Siddiqui, H., XMM-Newton obser- Peacock, A., Gostilo, V., Lisjutin, I., Zatoloka, S., vations of the dwarf elliptical galaxy NGC 3226, Optimization of array design for TlBr imaging 2004, A&A, 420, 905. sec4.qxd 7/12/05 9:52 AM Page 145

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Kozorezov, A., Wigmore, K., Owens, A., den Hartog, R., M., Kraft, S., Status of X-ray Optics Development for Peacock, A., The effect of carrier diffusion on the the XEUS Mission, 2004, Proceedings SPIE, 5488, characteristics of semiconductor imaging arrays, 829. 2004, Nucl. Instr. & Meth., A531, 52. Bavdaz, M., Peacock, A., Tomaselli, E., Beijersbergen, Lumb, D.H., Bartlett, J.G., Romer, A.K., Blanchard, A., M., Collon, M., Flyckt, E., Fairbend, R., Boutot, J.-P., Burke, D.J., Collins, C.A., Nichol, R.C., Giard, M., Progress at ESA on High Energy Optics Technologies, Marty, P., Nevalainen, J., Sadat, R., Vauclair, S., The 2004, SPIE Proceedings, 5168, 136. XMM-NEWTON Omega Project – I. The X-ray Beijersbergen, M., Kraft, S., Bavdaz, M., Lumb, D., Luminosity-Temperature Relation at z>0.4, 2004, Guenther, R., Collon, M., Mieremet, A., Fairbend, R., A&A, 420, 383. Peacock, A., Development of X-ray pore optics novel Martin, D.D.E., Peacock, A., Verhoeve, P., Fernandez- high-resolution silicon millipore optics for XEUS and Leon, A., Glass, B., Maehlum, G., 64-channel pre- ultralow mass glass micropore optics for imaging and amplifier ASICs for superconducting tunnel junction timing, 2004, Proceedings SPIE, 5539, 104. readout, 2004, Nucl. Instr. & Meth., A 520, 570-573. Beijersbergen, M., Kraft, S., Gunther, R., Mieremet, A., Martin, D.D.E., Verhoeve, P., Peacock, A., Dordrecht, A. Collon, M., Bavdaz, M., Lumb, D.H., Peacock, A., van, Verveer, J., Hijmering, R., A 12x10 pixels Silicon Pore Optics – novel lightweight high- superconducting tunnel junction array based spectro- resolution X-ray optics developed for XEUS, 2004, photometer for optical astronomy, 2004, Nucl. Instr. & Proceedings SPIE, 5488, 868. Meth., A 520, 512-515. Berg, M.L. van den, Falkner, P., Atzei, A.C., Peacock, A., Owens, A., XANES fingerprinting – a technique for Venus MicroSat Explorer Programme, an ESA investigating CCD surface structures and measuring Technology Reference Mission, 2004, Proc. dead layer thicknesses, 2004, Nucl. Instr. & Meth., Workshop on Planetary Probe Atmosphric Entry and A526, 391. Descent Trajectory Anaylsis and Science, ESA Owens, A., Peacock, A., Compound Semiconductor SP-544, 275. Radiation Detectors, 2004, Nucl. Instr. & Meth., Berg, M.L. van den, Falkner, P., Atzei, A.C., Peacock, A., A513, 18. Venus Entry Probe, an ESA Technology Reference Rando, N., Lumb, D., Bavdaz, M., Martin, D., Peacock, Mission, 2004, Tool and Technologies for future A., Space science applications of cryogenic detectors, planetary exploration, Proc. 37th ESLAB Symposium, 2004, Nucl. Instr. & Meth., A-522, 62. 2-4 December 2003, ESA SP-543, 23. Scelsi, L., Maggio, A., Peres, G., Gondoin, P., X-ray Brammertz, G., Verhoeve, P., Martin, D., Peacock, A., spectroscopy of the Hertzsprung-gap giant 31 Com, Venn, R., Future optical detectors based on Al observed with XMM-Newton, 2004, A&A, 413, 643. superconducting tunnel junctions, 2004, Proceedings Vaitkus, J., Gostilo, V., Jasinskaite, R., Mekys, A., SPIE, 5499, 269. Owens, A., Tamosiunas, S., Zatoloka, S., Zindulis, A., D’Arcio, L.A., Karlsson, A., Search for Extraterrestrial Investigation of Degradation of Electrical and Planets – The DARWIN Mission, 2004, Proc. 5th Photoelectrical Properties in TlBr Crystals, 2004, International Conference on Space Optics – ICSO Nucl. Instr. & Meth., A531, 192. 2004, ESA SP-554, 213. D’Arcio, L.A., Karlsson, A., Gondoin, P., Use of OPD modulation techniques in stellar interferometry, 2004, Science Payload and Advanced Concepts Office SPIE Proceedings New frontiers in stellar Proceedings and other Publications, 2004 interferometry, 5491, 851. Falkner, P., ESA’s Technology Reference Studies, 2004, Absil, O., Hartog, R. den, Gondoin, P., Fabry, P., 8th ESA Workshop on Advanced Space Technologies D’Arcio, L., Wilhelm, R., Gitton, P., Puech, F., for Robotics and Automation, ‘ASTRA 2004’, 8, 155. Influence of atmospheric turbulence on the Falkner, P., Atzei, A., van den Berg, M., Schiele, A., performance and design of GENIE, 2004, Proc. SPIE Microprobes for in-situ measurements on Planetray Conference 2004 Glasgow, Astronomical Telescopes surfaces and Atmospheres, 2004, Geophysical & Instrumentation, 5491, 1257. Research Abstracts, 6, 5458. Atzei, A.C., Falkner, P., Berg, M.L. van den, Peacock, A., Falkner, P., Erd, C., Kraft, S., Highly Integrated Payload The Jupiter Minisat Explorer – A Technology Suites for Planetary Exploration, 2004, Geophysical Reference Mission, 2004, Proceedings of 37th ESLAB Research Abstracts, 6, 6241. Symposium, ESA SP 543, 17. Falkner, P., Rando, N., Murphy, E., Update on Laser Bavdaz, M., Lumb, D., Peacock, A., Beijersbergen, M., Altimeters for Planetary Exploration, 2004, Kraft, S., Development of X-ray optics for the XEUS Geophysical Research Abstracts, 6, 05450. Mission, 2004, Proceedings SPIE, 5539, 104. Gondoin, P., Absil, O., Hartog, R. den, Wilhelm, R., Bavdaz, M., Lumb, D.H., Peacock, A., XEUS Mission Gitton, P., D’Arcio, L., Fabry, P., Puech, F., Fridlund, Reference Design, 2004, Proceedings SPIE, 5488, M., Schoeller, M., Glindemann, A., Bakker, E., 530. Karlsson, A., Peacock, A., Volonte, S., Paresce, F., Bavdaz, M., Lumb, D.H., Peacock, A., Beijersbergen, Richichi, A., Darwin-GENIE: a nulling instrument at sec4.qxd 7/12/05 9:52 AM Page 146

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the VLTI, 2004, Proc. SPIE Conference 2004 Owens, A., Andersson, H., Campbell, M., Lumb, D., Glasgow, Astronomical Telescopes & Instrumentation, Nenonen, S., Tlustos, L., GaAs arrays for X-ray 5491, 775. spectroscopy, 2004, SPIE, 5501, 241. Hartog, R. den, Absil, O., Gondoin, P., D’Arcio, L., Renton, D.C., Falkner, P., Peacock, A., Deimos Sample Fabry, P., Kaltenegger, L., Wilhelm, R., Gitton, P., Return Technology Reference Mission, 2004, Proc. Puech, F., Fridlund, M., The simulated detection of ‘Tools and Technologies for Future Planetary low-mass companions with GENIE, 2004, Proc. Exploration’, 37th ESLAB Symposium, ESA SP-543, SPIE, New Frontiers in Stellar Interferometry, 5491, 3. 160. Romstedt, J., Torkar, K., Riedler, W., Jeszenszky, H., Hughes, G.W., Macdonald, M., McInnes, C.R., Atzei, A., Arends, H., Butler, B., Biezen, J. van der, Steller, M., Falkner, P., Analysis of a Solar Sail Mercury Sample MIDAS – First Results from Rosetta’s Commiss- Return Mission, 2004, Proceedings IAC, Vancouver ioning Phase, 2004, Geophysical Research Abstracts, 2004, CDROM. 6, EGU04-A-01202. Jones, L.R., Maughan, B.J., Ebeling, H., Scharf, C., Stankov, A., Favata, F., Characterization of the field Perlman, E., Lumb, D., Gondoin, P., Mason, K.O., population in the Pleiades cluster region for Cordova, F., Priedhorsky, W.C., An XMM and EDDINGTON, 2004, Proc. 2nd Eddington workshop: Chandra view of massive clusters of galaxies to z=1, Stellar structure and habitable planet finding, ESA 2004, Clusters of Galaxies: Probes of Cosmological SP-538, 425. Structure and Galaxy Evolution, Carnegie Observa- Verhoeve, P., Martin, D., Brammertz, G., Hijmering, R., tories Astrophysics Series, Pasadena, California, Peacock, A., Photon Counting Cryogenic detectors for USA, 25. Ground-based and Space Telescopes, 2004, Proc. 5th Kaltenegger, L., Karlsson, A., Requirements on the International Conference on Space Optics (ICSO stellar rejection for the DARWIN mission, 2004, 2004), ESA SP-554, 781. Proceedings SPIE, Glasgow, Astronomical Telescopes Wallner, O., Perdigues Armengol, J.M., Karlsson, A., & Instrumentation, 5491, 275. Multi-Axial Single-Mode Beam Combiner, 2004, Karlsson, A., Wallner, O., Perdigues Armengol, J., Absil, SPIE, Glasgow, 2004, 5491, 798. O., Three Telescope Nuller, based on multi beam injection into single mode waveguide, 2004, SPIE – Astronomical Telescopes, Glasgow 2004, 5491, 831. Kilter, M., Micropropulsion Assessment for DARWIN, 2004, Micropropulsion Assessment for DARWIN, 5.2, 145. Kilter, M., Karlsson, A., Micropropulsion Technologies for the European high-precision Formation Flying Interferometer DARWIN, 2004, Proc. 4th International Spacecraft Propulsion Conference, ESA SP-555, 85. Lumb, D.H., Instrumentation Package for ESAs (XEUS) X-ray Early Universe Spectroscopy Mission, 2004, Proceedings SPIE, 5165,1. Lumb, D.H., XEUS Mission – Detector Spacecraft Instrumentation Package, 2004, Proceedings SPIE, 5488, 539. Lyngvi, A., Falkner, P., Atzei, A., Renton, D., van den Berg, M.L., Peacock, A., ESA’s Technology Refer- ence Studies, 2004, Proceedings IAC, Vanouver 2004, IAC, IAC-04-U.1.06. Lyngvi, A., Falkner, P., Peacock, A., The Interstellar Heliopause Probe, 2004, Proceedings of Tools and Technologies for Future Planetary Exploration, 37th ESLAB Symposium, ESA SP-543, 11-17. Lyngvi, A., Falkner, P., Peacock, A., The Interstellar Heliopause Probe, 2004, Proceedings IAC, Vancover 2004, paper number IAC-04-Q.2.A.06. Owens, A., Alha, L., Andersson, H., Bavdaz, M., Brammertz, G., Helariutta, K., Peacock, A., Ldmsd, V., Nenonen, S., The effects of proton induced radiation damage on compound semiconductor X-ray detectors, 2004, SPIE, 5501, 403. sec4.qxd 7/12/05 9:52 AM Page 147

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Stagiaire Research Reports and Theses, 2003 Formation in Low Luminosity Active Galactic Nuclei, 2004, Ph.D. Thesis report, published January 2004, Civeit, T. (Observatoire de Meudon, DESS Outils et defended March 2004. 1999-2003, RSSD supervisor Systemes de l’astronomie et de l’espace), Measure- M.Santos-Lleo, co-supervisor: M. Mas-Hesse at ment of zonal winds velocity in Titan’s stratosphere LAEFF-INTA, Spain. with VLT/UVES observations, RSSD supervisor Jimenez-Esteban, F.M. An Infrared Study of Galactic O. Witasse. OH/IR Stars, Ph.D. Thesis, June 2004, RSSD Coia, D. (Univ. Coll. Dublin), Infrared Observations of supervisor P. Garcia-Lario, co-supervisor D. Engels at Clusters of Galaxies, Ph.D. Thesis, Faculty of Science, Hamburg Observatory. National University of Ireland, RSSD co-supervisor L. Jiménez Luján, F. (U. Complutense de Madrid), Análisis Metcalfe (with Prof. B. McBreen at U.C.D.). de datos de XMM-Newton de galaxias espirales Cordonnier, R. VILSPA RSSD Network Statistics Tool cercanas: Fuentes de rayos X y emisión extensa de Stage Report, RSSD supervisor C. Arviset. M83, September 2004 ‘XMM-Newton data analysis Malloreau, S. (Observatoire de Meudon, DESS Outils et of nearby spiral galaxies: X-ray sources and extended Systemes de l’astronomie et de l’espace), Huygens emission in M83’, Practices at ESAC report, Faculty radar data analysis and test campaign preparation, of Physical Sciences, Astrophysics and Atmosphere RSSD supervisor J.-P. Lebreton. Sciences department, RSSD supervisor M. Ehle, Sierra, M. (Spanish Trainee), Extended Source Analysis co-supervisor J. Zamorano at UCM (Universidad with the RGS aboard XMM-Newton, RSSD Complutense de Madrid). supervisor A. Pollock. Leyder, J.-C. (Université de Liège), Analysis of Sierra, M. (Spanish Trainee), The Use of SNRs as Messenger – The NASA mission to Mercury, May Contamination Monitors for the RGS aboard XMM- 2004, Master Thesis report, Université de Liège, Newton, RSSD supervisor A. Pollock. Faculty of Applied Sciences, supervisors ESTEC J. Romstedt, N. Rando, supervisor Univ. Liège, J.-P. Swings. Stagiaire Research Reports and Theses, 2004 Luna, R. Busqueda de Bandas Difusas en Envolturas Circunestelares, Ph.D. Thesis, November 2004, RSSD Aguardo, D. (U. Complutense Madrid), Refinement of supervisor: P. Garcia-Lario, co-supervisor: M.A. the EPIC count rate estimation in PHS tools, Practices Satorre at U. Alcoy. at ESAC report, Faculty of Mathematics, RSSD Sarmiento Ares, F. (U. Vigo), System Study of a supervisor M. Kirsch, co-supervisor A.I. Gomez de Planetary Data Handling and Archiving System, State Castro at UCM (Universidad Complutense de of the Art and Outlook, July 2004, RSSD supervisor Madrid). J. Zender. Barbarisi, I. VOSpec: a Tool to display and superimpose Schoenherr, G. (U. Bonn), Scientific X-ray data analysis spectra from VO compatible Spectra Server, RSSD of the Crab supernova remnant, RSSD supervisor supervisor C. Arviset. A. Pollock. Brooks Pollock, E. (University College London), Seoane Purrinos, L. (U. Vigo), JMAPPS Client-Server Simultaneous Analysis of Galaxy Clusters with the Interactive Application for browsing the Mars RGS and EPIC Instruments aboard XMM-Newton, Surface, RSSD supervisor J. Zender. RSSD supervisor A. Pollock. Simoes, F. (Portuguese trainee), Subsurface Permittivity Carter, J. (YGT), Review of the XMM-Newton SAS Probe to detect Water/Ice in Planetary Environments, Online Guides and Online Support Structure, RSSD RSSD supervisors R. Trautner, A. Chicarro, R. Grard. supervisor A. Pollock. Stebe, A. ESAC Science Archive Team and Computer Carter, J. (YGT), Order Separation and PI Selection Support Group WebPortal Improvements Stage Regions in the Analysis of XMM-Newton RGS data, Report, RSSD supervisor C. Arviset. RSSD supervisor A. Pollock. Suarez, O. (U. Vigo), Stellar Evolution in the Post-AGB Couturier-Doux, S. (DESS Outils et Systemes de Stage, Ph.D. Thesis, May 2004, RSSD supervisor: l’astronomie et de l’espace, Paris-Meudon), Contribu- P. Garcia-Lario, co-supervisor: M. Manteiga at tion to the operations planning & software tests for the U. Vigo. Camera onboard the SMART-1 Mission, RSSD Vacher, G. VILSPA Science Archive Team and Computer supervisor B.H. Foing. Support Group WebPortal Design and 1st Esquej, M.P. (U. Complutense Madrid), Energy calibra- Implementation Stage Report, RSSD supervisor tion verification of the EPIC cameras with SNR C. Arviset. observations, Practices at ESAC report, Faculty of van Kan, M. (U. Utrecht), Geologic Evolution of the Physical Sciences, Astrophysics and Atmosphere Gusev Crater region on Mars – using Mars Express, Sciences department, RSSD supervisor M. Kirsch, MGS and Mars Odyssey, August 2004, Master Thesis co-supervisor J. Zamorano at UCM (Universidad report, Faculty of Earth Sciences Utrecht, RSSD Complutense de Madrid). supervisors T. Zegers, B.H. Foing, co-supervisor Jimenez-Bailon, E. (U. Autonoma de Madrid), Star C.G. Langereis at Utrecht U. sec4.qxd 7/12/05 9:52 AM Page 149

ANNEX 3 Seminars and Colloquia sec4.qxd 7/12/05 9:52 AM Page 150

150 seminars and colloquia

Seminars held at ESTEC 26 September The Young Earth: A Different Planet 2003 T. Zegers, Planetary Missions Division

17 January 9 October An Observational View on the Variability of Disks ALMA – the Atacama Large Millimetre Array around Pre-Main Sequence Stars W. Wild, SRON C. Eiroa, Astronomy Missions Division 24 October 31 January X-ray Emission and Origin of Runaway Stars NASA’s Far-IR/Submillimeter Roadmap Missions: E. Meurs, Dunsink Observatory SAFIR and SPECS D. Leisawitz, NASA Goddard Space Flight Center 7 November What is XMM Telling us About the Unified Scenario 14 February for Active Galactic Nuclei? Cluster Results and Future Multi-Satellite Mission M. Guinazzi, VILSPA Concepts H. Laakso, Solar and Heliospheric Missions Division 5 December XMM-Newton Observations of Globular Clusters 28 February D. Carrett, CESR Luminosity Functions of Young Stellar Clusters T. Prusti, Astronomy Missions Division 2004 14 March Remote Sensing of Planetary Minerals and Ices by 9 January NIR Imaging Spectroscopy, Objects and Methods Darwin and Exoplanets: Disks, Exoplanets and S. Doute, Laboratoire de Planetologie de Grenoble Darwin M. Fridlund, Astronomy Missions Division 28 March The Transition from AGB Stars to Planetary Nebulae 23 January as seen by ISO Early Mission Highlights from the Spitzer Space P. Garcia, VILSPA Telescope A. Marsdon, Astronomy Missions Division 25 April Measurig the Gas Content of Galaxies: the Effects of 6 February a Higher H2 Formation Rate Dust and Gas Content of Quasars and Galaxies in the P. Papadopolous, University of Leiden Early Universe P. Cox, Université Paris Sud 23 May Optical and Infrared Interferometry 19 February A. Quirrenbach, University of Leiden Imaging and Photometry of Mars: Strategy Toward a Multiscale Understanding of the Optical Properties 19 June P. Pinet, Observatoire Midi-Pyrenées Measurement of Polarisation of the Cosmic Micro- wave Background 19 March L. Piccirillo, Cardiff University Architecture and Concepts for Optical Sensors for Planetary Exploration and Space-Based Astronomy 4 July H. Michaelis, DLR Halo Gas in Spiral Galaxies F. Fraternali, ASTRON 2 April Gas in Elliptical Galaxies and Bulges 11 July S. Peletier, University of Groningen Venus: Mysteries of the ‘Forgotten Planet’ D.V. Titov, Max Planck Inst. für Aeronomie 23 April The Great Observatories Origins Deep Survey: First 12 September Science Results Magellan Mission to Venus: What Did we Learn about B. Mobasher, STScI Venus’ Surface Tectonics and History? P. Rosenblatt, Belgium Royal Observatory sec4.qxd 7/12/05 9:52 AM Page 151

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7 May Colloquia held at ESTEC The Origin of Dust at High Redshift L. Dunne, University of Wales 2003

4 June 9 May On the Cassini-Huygens Mission The Search for the Complete History of the Cosmos J.-P. Lebreton, Planetary Missions Division N. Turok, Cambridge University

2 July 21 November LISA – A Mission to Detect and Observe Gravita- Drilling the Chicxulum Dinosaur Killer Crater – How tional Waves a Meteorite Impact Changed our World O. Jennrich, Fundamental Physics Missions Division J. Smit, Vrije Universitaet

9 July ESO Research Facilities in Chile 2004 C. Alloin, ESO 5 March 10 September The Paradoxes of Evolution: Inevitable Humans but in The Pioneer Anomaly: the Data, its Meaning and a a Lonely Universe Possible Test S. Conway-Morris, Cambridge University M.N. Nieto, Los Alamos 18 June 7 October Archeoastronomy: Stonehenge and Beyond Latest Results from Spitzer – An Infrared View of C. Ruggles, Leicester University Galaxy Evolution H. Dole, Université Paris Sud

22 October Massive Star Nucleosynthesis in Cygnus X J. Knoedlseder, CESR

5 November The High Resolution Stereo Camera Experiment on Mars Express: First Geoscientific Results R. Jaumann, German Aerospace Centre

12 November Dynamics and Instability in Jupiter’s Outer Magneto- sphere D. Southwood, Director of Science

19 November Examples of Studies of the Current Sheet Dynamics by Cluster P. Louarn, CESR

3 December Giant Planets’ Aurora: A Comparative View J.-C. Gerard, Université Liège sec4.qxd 7/12/05 9:52 AM Page 153

ANNEX 4 Acronyms sec4.qxd 7/12/05 9:52 AM Page 154

154 acronyms

AAS American Astronomical Society CNSA Chinese National Space Administration AAT Anglo-Australian Telescope COBE Cosmic Background Explorer (NASA) ACES Atomic Clock Ensemble in Space Co-I Co-Investigator ACS Advanced Camera for Surveys (HST) CONSERT Comet Nucleus Sounding Experiment by ADS Astrophysics Data System (NASA) Radiowave Transmission (Rosetta) AFM Atomic Force Microscope COPUOS Committee for the Peaceful Use of Outer AGB Asymptotic Giant Branch Space (United Nations) AGN Active Galactic Nuclei COROT COnvection, ROtation and planetary Transits AGU American Geophysical Union COS Cosmic Origins Spectrograph (HST) AIV Assembly, Integration & Verification COSAC Comet Sampling and Composition AKR Auroral Kilometric Radiation Experiment (Rosetta) ALICE Rosetta Orbiter UV imaging spectrometer COSIMA Cometary Secondary Ion Mass Analyser ALMA Atacama Large Millimetre Array (Rosetta) AMIE Asteroid Moon micro-Imager Experiment COSPAR Committee on Space Research (SMART-1) COSPIN Cosmic Ray & Solar Charged Particles AO Announcement of Opportunity Investigation (Ulysses) APT Astronomers’ Proposal Tool COSTEP Comprehensive Measurements of the Supra- APXS Alpha-Proton-X-ray Spectrometer (Rosetta) Thermal and Energetic Particles Populations ASCA Advanced Satellite for Cosmology and (SOHO) Astrophysics (Japan) CP Charge Parity ASI Italian Space Agency CPM Chemical Propulsion Module ASIC Application Specific Integrated Circuit (BepiColombo) ASPOC Active Spacecraft Potential Control (Cluster) CR Carrington Rotation ATR Attenuated Total Reflection CS Control Centre AU Astronomical Unit CSA Canadian Space Agency AWG Astronomy Working Group (ESA) CSDS Cluster Science Data System CsI caesium iodide BeppoSAX Satellite per Astronomia in raggi X CSIRO Commonwealth Scientific & Industrial (Italy/The Netherlands) Research Organisation (Australia) BHE banded hiss emission CTIO Cerro Tololo Inter-American Observatory BLR Broad Line Region CTTS Classical T-Tauri Star CV Cataclysmic Variable CAA Cluster Active Archive CVF Circular Variable Filter (ISOCAM) CBRF Cosmic Background Radiation Field CXB Cosmic X-ray Background CCD Charge Coupled Device CDS Coronal Diagnostics Spectrometer (SOHO) D-CIXS Demonstration of a Compact Imaging X-ray CDS Centre de Données astronomiques de Spectrometer (SMART-1) Strasbourg D/HME Directorate of Human Spaceflight, CdTe cadmium telluride Microgravity & Exploration (ESA) CELIAS Charge, Element and Isotope Analysis D/SCI Directorate of Scientific Programmes (ESA) System (SOHO) DEM Digital Elevation Model CEPHAG Centre d’Etude des Phenomenes Aleatoires DESPA Observatoire de Paris, Département Spatial et Geophysiques (France) DIB Diffuse Interstellar Band CERN Centre Européen de Recherches Nucléaires DISR Descent Imager/Spectral Radiometer (France) (Huygens) CESR Centre d’Etude Spatial des Rayonnements DLR Deutsches Zentrum für Luft- und Raumfahrt (France) DPC Data Processing Centre CETP Centre d’Etudes des Environments Terrestres DPU Data Processing Unit et Planetaires (France) DRS Disturbance Reduction System (LISA CFHT Canadian-French-Hawaiian Telescope Pathfinder) CIR Corotating Interaction Region; Composite IR DSDS Double Star Data System Spectrometer (Cassini) DSN Deep Space Network CIS Cluster Ion Spectrometry DSP Digital Signal Processor; Double Star CIVA Comet Infrared and Visible Analyser Programme (China) (Rosetta) DSRI Danish Space Research Institute CMB Cosmic Microwave Background DUO Dark Universe Observatory (NASA) CME Coronal Mass Ejection CMOS Complementary Metal Oxide Semiconductor EAS European Astronomical Society CNES Centre National d’Etudes Spatiales ECF European Coordinating Facility CNR Consiglio Nazionale della Ricercha (Italy) EC European Commission CNRS Centre National de la Recherche Scientifique EDI Electron Drift Instrument (Cluster) (France) EFW Electric Field & Wave experiment (Cluster) sec4.qxd 7/12/05 9:52 AM Page 155

acronyms 155

EGS European Geophysical Society GDASS Gaia Data Access & Analysis Study EGSE Electrical Ground Support Equipment GENIE Ground-based European Nulling EIRO European Intergovernmental Research Interferometer Experiment Organisation GIADA Grain Impact Analyser and Dust EIT Extreme UV Imaging Telescope (SOHO) Accumulator (Rosetta) ELAIS European Large Array ISO Survey GLIMPSE Galactic Legacy IR Mid-Plane Survey ELF Extremely Low Frequency Extraordinaire EM Electrical Model, Engineering Model GMOS Gemini Multi-Object Spectrograph EP Equivalence Principle GMT Greenwich Mean Time EPAC energetic particle instrument (Ulysses) GOLF Global Oscillations at Low Frequency EPDP Electric Propulsion Diagnostic Package (SOHO) (SMART-1) GONG Global Oscillation Network Group EPIC European Photon Imaging Camera GOODS Great Observatories Origins Deep Survey (XMM-Newton) GR General Relativity EPS European Physical Society GRB Gamma Ray Burst EQM Electrical Qualification Model GSE Ground Support Equipment ERNE Energetic and Relativistic Nuclei and GSFC Goddard Space Flight Center (NASA) Electron experiment (SOHO) GSP General Studies Programme (ESA) ESA European Space Agency GSTP General Support & Technology Programme ESAC European Space Astronomy Centre (ESA) (ESA) ESLAB European Space Laboratory (former name of GTO Geostationary Transfer Orbit SSD/RSSD) ESO European Southern Observatory HASI Huygens Atmospheric Structure Instrument ESOC European Space Operations Centre, HCS Heliospheric Current Sheet Darmstadt (Germany) HCSS Herschel Common Science System ESRIN ESA’s Documentation and Information HEB Hot Electron Bolometer Centre (Italy) HEIC Hubble ESA Information Centre ESRO European Space Research Organisation HEMT High Electron Mobility Transistor ESTEC European Space Research and Technology HEW Half Energy Width Centre, Noordwijk HFI High Frequency Instrument (Planck) (The Netherlands) HGA High-Gain Antenna EUSO Extreme Universe Space Observatory HIFI Heterodyne Instrument for Far-IR (Herschel) EUV Extreme Ultra-Violet HIPS Highly Integrated Payload Suite EW equivalent width HPOC Huygens Probe Operations Centre HR Hertzsprung-Russell FEEP Field Emission Electric Propulsion HRC High-Resolution Channel (HST/ACS) FES Fine Error Sensor HRSC High Resolution Stereo Camera (Mars FET field effect transistor Express) FGM Flux Gate Magnetometer HRTS High-Resolution Telescope & Spectrograph FGS Fine Guidance Sensor (HST) HSC Herschel Science Centre FGS-TF Fine Guidance Sensor-Tunable Filter (JWST) HST Hubble Space Telescope FIRST Far Infrared and Submillimetre Space Telescope (now Herschel) IAA Instituto de Astrofísica de Andalucía FM Flight Model IAC Instituto de Astrofisica de Canarias FMI Finnish Meteorological Institute IAU International Astronomical Union FOC Faint Object Camera (HST) IBIS Integral imager FORS2 FOcal Reducer/low dispersion ICC Instrument Control Centre Spectrograph 2 (ESO VLT) IDT Instrument Dedicated Team FOS Faint Object Spectrograph (HST) IFE Instrument Front-End FOV Field of View IFS Integral Field Spectroscopy FP Fabry-Pérot ILEWG International Lunar Exploration Working FPAG Fundamental Physics Advisory Group (ESA) Group FPGA Field Programmable Gate Array ILT Instrument-Level Test FSRQ Flat Spectrum Radio Quasar ILWS International Living With a Star programme FTE Flux Transfer Event IMEWG International Mars Exploration Working FTS Fourier Transform Spectrometer Group FUSE Far-UV Spectroscopic Explorer (NASA) IMF Initial Mass Function; Interplanetary FUV Far-Ultraviolet Magnetic Field FWHM Full Width at Half Maximum IMPACT In-situ Measurements of Particles And CME Transients (STEREO) GaAs Gallium Arsenide INT Isaac Newton Telescope GC Galactic Centre INMS Ion & Neutral Mass Spectrometer (Cassini) sec4.qxd 7/12/05 9:52 AM Page 156

156 acronyms

INTA Instituto Nacional de Técnica Aerospacial LPF LISA Pathfinder (Spain) LPSP Laboratoire de Physique Stellaire et IOA Institute of Astronomy (Cambridge, UK) Planétaire (France) IPAC Infrared Processing Analysis Center LPV Long-Period Variable IR Infrared LTE Local Thermal Equilibrium IRAM Institut de Radioastronomie Millimétrique LTP LISA Technology Package IRAS Infrared Astronomy Satellite LWS Long Wavelength Spectrometer (ISO) IRF-U Institute for Space Physics-Uppsala (Sweden) ISAS Institute of Space and Astronautical Science MAPPS Mapping & Planning for Payload Science (Japan), now part of JAXA (Venus Express) ISDC Integral Science Data Centre MCP Microchannel Plate ISGRI Integral Soft Gamma Ray Imager MDI Michelson Doppler Imager (SOHO) ISM Interstellar Medium MDPU Model Data Processing Unit ISO Infrared Space Observatory (ESA) MECS Medium-Energy Concentrator Spectrometer ISOC Integral Science Operations Centre (BeppoSAX) ISSI International Space Science Institute, Bern MER Mars Exploration Rover (NASA) (Switzerland) MHD Magnetohydrodynamics IST Instrument Science Team Microscope MICROSatellite à traînée Compensée pour ISWT Integral Science Working Team l’Observaton du Principe d’Equivalence ITC International Institute for Geo-Information (CNES) Science and Earth Observation (NL) MIDAS Micro-Imaging Dust Analysing System ITT Invitation to Tender (Rosetta) IUE International Ultraviolet Explorer MIP Mutual Impedance Probe (Rosetta) IUPAP International Union of Pure and Applied MIRI Mid-IR Instrument (JWST) Physics MIRO Microwave Instrument for the Rosetta IWF Space Research Institute Graz (A) Orbiter (Rosetta) MLH Mid-Latitude Hiss JAXA Japan Aerospace & Exploration Agency MLT Magnetic Local Time JCMT James Clerk Maxwell Telescope MMO Mercury Magnetospheric Orbiter JEM-X Integral X-ray monitor (BepiColombo) JIVE Joint Institute for VLBI in Europe MOC Mission Operations Centre JPL Jet Propulsion Laboratory (NASA) MOLA Mars Observer Laser Altimeter JSOC Joint Science Operation Centre (Cluster) MOS-CCD Metal Oxide Semiconductor Charge Coupled JWG Joint Working Group Device JWST James Webb Space Telescope (formerly MoU Memorandum of Understanding NGST) MPAE Max-Planck-Institut für Aeronomie MPE Max-Planck-Institut für Extraterrestrische KATE X/Ka-band Telemetry & Telecommand Physik Experiment (SMART-1) MPI Max-Planck Institut (Germany) KPNO Kitt Peak National Observatory (USA) MPIA Max-Planck-Institut für Astronomie MPIK Max-Planck-Institut für Kernphysik LAEFF Laboratory for Space Astrophysics and MPO Mercury Planetary Orbiter (BepiColombo) Fundamental Physics MRR Mission Risk Review LAP Langmuir Probe (Rosetta) MSE Mercury Surface Element (BepiColombo) LASCO Large Angle Spectroscopic Coronagraph MSSL Mullard Space Science Laboratory (UK) (SOHO) MUPUS Multi-Purpose Sensors for Surface and LBV Luminous Blue Variable Subsurface Science (Rosetta) LDAP Lightweight Directory Access Protocol MUSICOS Multi-Site Continuous Spectroscopy LECS Low Energy Concentrator Spectrometer MXB Medium X-ray Band (BeppoSAX) MXU Mask Exchange Unit LET Low Energy Telescope (Ulysses) LETG Low-Energy Transmission Grating NAC Narrow Angle Camera (OSIRIS) LFI Low Frequency Instrument (Planck) NASA National Aeronautics & Space LIRG Luminous IR Galaxy Administration (USA) LISA Laser Interferometer Space Antenna NED NASA Extragalactic Database LIST LISA International Science Team NFI Narrow Field Instrument (BeppoSAX) LMC Large Magellanic Cloud NGST Next Generation Space Telescope (now LMXB Low Mass X-ray Binary James Webb Space Telescope) LOI Luminosity Oscillation Imager (SOHO) NHSC NASA Herschel Science Center LP LISA Pathfinder NICMOS Near-Infrared Camera and Multi-Object LPCE Laboratoire de Physique et Chemie, de Spectrometer (HST) l’Environnement (France) NIRSpec Near-IR Spectrometer (JWST) sec4.qxd 7/12/05 9:52 AM Page 157

acronyms 157

NIS normal incidence spectrometer RMOC Rosetta Mission Operations Centre NLR Narrow Line Region ROLIS Rosetta Lander Imaging System NOAO National Optical Astronomy Observatories ROMAP RoLand Magnetometer & Plasma Monitor (US) (Rosetta) NOT Nordic Optical Telescope ROSINA Rosetta Orbiter Spectrometer for Ion and NRAO National Radio Astronomy Observatory Neutral Analysis (Rosetta) (USA) ROSITA Roentgen Survey with an Imaging Telescope NSSDC National Space Science Data Center (at Array GSFC, USA) RPC Rosetta Plasma Consortium NSLS National Synchotron Light Source (USA) RSI Radio Science Investigation NTT New Technology Telescope RSOC Rosetta Science Operations Centre NVSS NRAO/VLA Sky Survey RSSD Research and Scientific Support Department (ESA) OAT Osservatorio Astronomico di Trieste RTG Radioisotope Thermoelectric Generator OHP Observatoire de Haute-Provence OM Optical Monitor (XMM-Newton) SAFIR Single Aperture Far-IR (NASA) OMC Optical Monitor Camera (Integral) SAO Smithsonian Astrophysical Observatory OSIRIS Optical and Spectroscopic Remote Imaging (USA) System (Rosetta) SAp/Saclay Service d’Astrophysique (Commissariat à l’Energie Atomique; Saclay, France) PACS Photodetector Array Camera and SAS Scientific Analysis Software (XMM- Spectrometer (Herschel) Newton); Science Analysis Subsystem PAH Polycyclic Aromatic Hydrocarbon (XMM-Newton) pc parsec SAX Satellite per Astronomia in raggi X PCD Photon Counting Detector (Italy/The Netherlands) PDD Payload Definition Document SBC Solar-Blind Channel (ACS/HST) PDFE Particle Detector Front End SCAM Superconducting Camera PDS Phoswich Detector System SciSIM Science Simulator PI Principal Investigator SCOS Spacecraft Operations System PIA (ISO)PHOT Interactive Analysis SCR Software Change Request PICAM Planetary Ion Camera (BepiColombo MPO) SDT Science Definition Team PIPS Passivated Implanted Planar Silicon SED Spectral Energy Distribution PLM Payload Module SEM Scanning Electron Microscope PMS Pre-Main Sequence SEP solar energetic particle; solar electric PN Planetary Nebula (plural: PNe) propulsion; solar electron proton POS Payload Operations Service (Mars Express) SEPM Solar Electric Propulsion Module PP Permittivity Probe (SESAME on Rosetta) (BepiColombo) ppm parts per million SEPP Solar Electric Primary Propulsion PR Public Relations SEPT Solar Energetic Particle Telescope PS Project Scientist (STEREO) PSA Planetary Science Archive SESAME Surface Electric, Seismic and PST Project Scientist Team; Payload Support Team Acoustic Monitoring Experiment (Rosetta) PSF Point Spread Function SEST ESO sub-mm telescope PSO Planck Science Office SETI Search for Extra-Terrestrial Intelligence PWA Permitivity, Waves and Altimetry (part of SFH Star Formation History HASI on Huygens) SFR Star Formation Rate PWG Payload Working Group SIMBA SEST Imaging Bolometer Array SIMBAD Set of Identifications, Measurements and QED Quantum Electrodynamics Bibliography on Astronomical Data QM Qualification Model SIR Stream Interacting Region QPD Quadrant Photodiode SIRTF Space Infrared Telescope Facility (NASA; QPO Quasi Periodic Oscillation now Spitzer) QSO Quasi Stellar Object SIS Superconductor-Insulator-Superconductor SLP Segmented Langmuir Probe R&D Research and Development SM Servicing Mission (Hubble) RAID Redundant Array of Inexpensive Disks SMART Small Mission for Advanced Research in RAL Rutherford Appleton Laboratory (UK) Technology (ESA) RF Radio Frequency SMC Small Magellanic Cloud RGS Reflection Grating Spectrometer (XMM- SMEX Small Explorer (NASA) Newton) SMOG Survey of Molecular Oxygen in the Galaxy RHESSI Reuven Ramaty High Energy Solar (SMART-1) Spectroscopic Imager (NASA) SN Supernova sec4.qxd 7/12/05 9:52 AM Page 158

158 acronyms

SNR Supernova Remnant TRL Technology Readiness Level SOC Science Operations Centre; self-organising TRM Technology Reference Mission criticality TRP Technology Research Programme (ESA) SOHO Solar and Heliospheric Observatory TRS Technology Reference Study SOI Saturn Orbit Insertion TSI Total Solar Irradiance SOS Silicon-on-Sapphire SOT Science Operations Team UCB University of California Berkeley (USA) SOWG Science Operations Working Group UCLA University of California Los Angeles (USA) SPC Science Programme Committee (ESA) ULIRG Ultra-Luminous IR Galaxy SPECS Submillimeter Probe of the Evolution of URSI Union Radio Scientifique Internationale Cosmic Structure (NASA) USNO US Naval Observatory SPEDE Spacecraft Potential, Electron & Dust UT Universal Time Experiment (SMART-1) UV Ultraviolet SPI Integral spectrometer UVCS Ultra-Violet Coronal Spectrometer (SOHO) SPICAM Mars Express UV Spectrometer UVES Ultraviolet-Visual Echelle Spectrograph SPIRE Spectral and Photometric Imaging Receiver (ESO VLT) (Herschel) UVIS UV Imaging Spectrometer (Cassini) SPR Software Problem Report SQUID Superconducting Quantum Interference VILSPA Villafranca Satellite Tracking Station Device VIMOS VLT Visible Multi-Object Spectrograph SRON Space Research Organisation Netherlands (ESO VLT) SRR System Requirement Review VIMS Visual IR Mapping Spectrometer (Cassini) SRV Semi-Regular Variable VIRGO Variability of Irradiance and Gravity SSAC Space Science Advisory Committee (ESA) Oscillations (SOHO) SSC Survey Science Consortium (XMM-Newton) VIRTIS Visible Infra Red Thermal Imaging SSD Space Science Department (ESA), now Spectrometer (Rosetta) RSSD VLA Very Large Array SSP Surface Science Package (Huygens and VLBI Very Long Baseline Interferometry Rosetta) VLF Very Low Frequency SSWG Solar System Working Group (ESA) VLT Very Large Telescope ST Science Team; Space Technology (NASA) VLTI Very Large Telescope Interferometer (ESO ST-ECF Space Telescope European Coordinating VLT) Facility (Germany) VO Virtual Observatory STAFF Spatio-Temporal Analyis of Field VSOC Venus Express Science Operations Centre Fluctuations (Cluster) VTT Vacuum Tower Telescope STEREO Solar-Terrestrial Relations Observatory (NASA) WAC Wide Angle Camera (OSIRIS on Rosetta) STIS Space Telescope Imaging Spectrograph WBD Wide Band Data (Cluster) STJ Superconducting Tunnel Junction WEC Wave Experiment Consortium (Cluster) STOC Science & Technology Operations WFC Wide-Field Camera (HST) Coordination WFPC Wide-Field Planetary Camera (HST) STScI Space Telescope Science Institute WHISPER Waves of High Frequency and Sounder for SUMER Solar UV Measurements of Emitted Probing of Density by Relaxation (Cluster) Radiation (SOHO) WHT William Herschel Telescope SWAN Solar Wind Anisotropies (SOHO) WIYN Wisconsin Indiana Yale NOAO (US) SWAS Submillimeter Wave Astronomy Satellite WMAP Wilkinson Microwave Anisotropy Probe (NASA) (NASA) SWS Short Wavelength Spectrometer (ISO) WWW World Wide Web SWT Science Working Team SVM Service Module XEUS X-ray Evolving Universe Spectroscopy SXB Soft X-ray Band mission (ESA) SXT Soft X-ray Telescope (Yohkoh) XMM X-ray Multi-Mirror Mission (ESA); now SZ Sunyaev-Zeldovich Effect XMM-Newton XSA XMM-Newton Science Archive (ESA) TAC Time Allocation Committee TNG Telescopio Nazionale Galileo YGT Young Graduate Trainee ToO Target of Opportunity YSO Young Stellar Object TPF Terrestrial Planet Finder (NASA) TRACE Transition Region & Coronal Explorer ZAMS Zero Age Main Sequence (NASA) TRIP Technology Readiness and Implementation Plan