SP-1268 SP-1268 R Esearch and Scientific

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SP-1268 SP-1268 R esearch and Scientific

Report on the activities of the Support Department Research and Scientific Support Department 2001 — 2002 Sec1.qxd 3/5/03 3:22 PM Page 1

SP-1268 March 2003

Report on the activities of the Research and Scientific Support Department

2001 – 2002

Scientific Editor K.-P. Wenzel Sec1.qxd 3/5/03 3:22 PM Page 2

ESA SP-1268 Report on the Activities of the Research and Scientific Support Department from 2001 to 2002

ISBN 92-9092-992-8 ISSN 0379-6566

Scientific Editor K.-P. Wenzel

Editor A. Wilson

Published and distributed by ESA Publications Division

Price €30 Sec1.qxd 3/5/03 3:22 PM Page 3

CONTENTS

1. Introduction 5 4. Other Activities 105

1.1 Report Overview 5 4.1 Symposia and Workshops organised 105 1.2 The Role, Structure and Staffing of RSSD 5 by RSSD 1.3 Department Outlook 9 4.2 Science Communications 109 4.3 Other Coordination and Support Activities 110

2. Research Activities 11

2.1 Research Support Division 13 Annex 1: Manpower Deployment 113 2.2 High-energy Astrophysics Research 14 2.3 Optical/UV Astrophysics 19 Annex 2: Publications (separated into 121 refereed and non-refereed literature) 2.4 Infrared/Submillimetre Astrophysics 24 2.5 Exoplanets and Stellar Environments 27 Annex 3: Seminars and Colloquia 153 2.6 Solar Physics and Seismology 28 2.7 Heliospheric Physics 33 Annex 4: Acronyms 157 2.8 Plasma and Gas Environment of 36 Solar System Bodies 2.9 Comparative Planetology and Astrobiology 44 2.10 Cosmic Dust and Comets 49 2.11 Development and Exploitation of Super- 54 conducting Cameras for Astronomy 2.12 Advanced Sensor, Optics and Instrument 60 Development Research

3. Scientific Support Activities 65

3.1 Astrophysics Missions Division 68 3.2 Solar and Solar-Terrestrial 74 Missions Division 3.3 Planetary Missions Division 80 3.4 Fundamental Physics Missions Division 85 3.5 Space Telescope Operations Division 89 3.6 Science Operations and Data Systems 90 Division 3.7 Science Payloads Technologies Division/ 98 Science Payload and Advanced Concepts Office Sec1.qxd 3/5/03 3:22 PM Page 5

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1. INTRODUCTION

1.1 Report Overview ate’s Science Payload and Advanced Concepts Office, are included. Although formally outside the Department This report on the activities of the Research and since late 2002, the close links of this Office with the Scientific Support Department (RSSD, previously the Department for both research and scientific support Space Science Department) covers the 2-year period of activities will be maintained. 2001-2002. It is input to the Department’s Advisory Committee, a group of independent external scientists Finally, Chapter 4 addresses a variety of activities carried invited by the Director of ESA’s Scientific Programme to out by RSSD in its support role to the community. The review the Department’s activities. It forms the basis of Chapter summarises important scientific Symposia and the oral reports made every second year to ESA’s Space Workshops organised by the Department, support to the Science Advisory Committee and Science Programme Directorate’s science communication activities and Committee. Through the publication of the report as an various other activities. ‘SP’ (Special Publication) by the ESA Publications Division, the activities of the Department are brought to While this Biennial Report provides perspective on the the attention of the scientific community and to a broader breadth and quality of the activities of the staff, both in audience. their research and functional work, it is not intended to be comprehensive. Up-to-date information on the Depart- These Biennial Reports have been produced since 1980. ment’s activities can be obtained at http://www. In this edition, a number of changes have been rssd.esa.int introduced to reflect the modified scope of activities and the reorganisation of the Department that occurred The production and content of the report reflects the during the reporting period. The report is divided into efforts of the whole Department. Special acknowledge- four Chapters plus four Annexes. ment for its preparation is due to K.-P. Wenzel, who edited the different contributions. Chapter 1 deals with the Department’s role and organisation. Its mandate and structure both evolved considerably during the reporting period. Based on a 1.2 The Role, Structure and Staffing of RSSD revision of the responsibilities of the Department, the structural changes that began at the end of 2000 were RSSD, one of the two Departments of ESA’s Scientific finalised during the initial year of the present reporting Directorate, provides the direct interface to the scientific period. A reorganisation of the whole Scientific community throughout all mission phases. Following in- Programme Directorate, also affecting the Department, orbit checkout and commissioning, it is also responsible took place in the second year. This led to a further for the management of the missions. In addition, the evolution to its current structure, described below. The Department plays its part in the dissemination of names of staff, their locations, duties and scientific scientific knowledge to the public and for educational research interests are given in Annex 1. purposes.

Chapter 2 addresses the scientific research of the The role and responsibilities of RSSD have evolved Department’s staff, broken down according to considerably during the reporting period. This is clearly ‘discipline’ rather than the divisional structure of expressed through the change of its name. The prime previous reports. A complete listing of the scientific motivation for the reorganisation was to achieve greater papers published in the literature is given in Annex 2. efficiency and effectiveness in the provision of support to Some 380 refereed papers were published during 2001 the scientific community, particularly in the areas of and 2002, and more than 400 conference papers and payload technology, science operations and communica- other publications appeared. tions. Specifically, the departmental organisation has been adapted to respond to the overall strategic Chapter 3 provides a top-level summary of the mission- objectives of the Agency, and be responsive to the needs related activities at Divisional level. For the four of the science community. It was also motivated by the Missions Divisions, the prime contributions to the desire to give more responsibility and authority to the scientific support of the various elements of the Science Department’s scientific staff, and to provide opportuni- Programme are summarised. For the two Operations ties for increased mobility, while maintaining a healthy Support Divisions, special mention is also made of the scientific environment where staff can pursue their own post-operational and archiving phases. The activities of research within a balanced programme. The role of the the Science Payloads Technology Division, which Department’s staff in support of the revised Directorate’s evolved and very recently expanded into the Director- and Agency’s communications activities was also Sec1.qxd 3/5/03 3:22 PM Page 6

6 introduction

Head of Research and Scientific Support Projects Department, the Science Programme Coordina- Department tion and Planning Office and the Science Project SCI-S Management Coordination Office. Science Payload and Advanced Concepts Office Chief Scientist SCI-A SCI-SR In particular, the Department is responsible for providing scientific expertise to studies and projects in all phases, and for ensuring that maximum scientific return within practical technical and budgetary constraints is Astrophysics Missions Scientific Operations and Division Data Systems Division maintained as a target through all phases of a scientific SCI-SD SCI-SA mission. The Department also manages, through its

Planetary Missions Space Telescope Study or Project Scientists, the activities of each mission Division Operations Division SCI-SB SCI-SN science team.

Solar & Solar-Terrestrial RSSD is responsible for all aspects of science operations Missions Division SCI-SH (definition, development, implementation and execution) through all mission phases and manages the operations Fundamental Physics Missions Division phase of missions following in-orbit commissioning, SCI-SP supported, as necessary, by system engineering expertise from the Scientific Projects Department. Figure 1.2/1: Structure of RSSD staff at the end of 2002. The Science Payload and Advanced Concepts In very close coordination with the Science Payload and Office evolved from the Department’s Science Advanced Concepts Office, RSSD provides scientific Payloads Technology Division in late 2002. and payload expertise within the Agency in all phases of scientific missions, including to other directorates of the Agency, such as the Directorate of Human Spaceflight on ISS payloads. RSSD works with external science teams to define the science requirements for studies on future reconsidered. More details about the Department’s tasks payloads and the associated technologies, and passes are given below. these to the Science Payload and Advanced Concepts Office for follow-up. Changes to the structure of the Department were implemented in a three-stage process. The first phase The Department provides input to the Directorate’s began in late 2000/early 2001 with the introduction of the Science Communications Service regarding the scientific Science Payloads Technology Division, the Science aspects of the missions, and ensures that the scientific Operations and Data Systems Division and a Research output of each mission is fully exploited in a timely Division. This phase was essentially completed with the manner for the benefit of public awareness and public arrival of the new Head of Department on 1 July 2001. In communication. a subsequent stage initiated in September 2001, the Planetary Missions Division, the Solar and Solar- It is, of course, very important that members of the RSSD Terrestrial Missions Division, the Space Telescope scientific staff maintain their scientific proficiency by Operations Division and the Fundamental Physics undertaking personal research. Missions Division were created. Further, a reorganisation in July 2002 of the Science Directorate was started that In order to discharge its responsibilities and tasks in an also affected the structure of RSSD. In this third stage efficient manner, the Department is structured into four leading to the current structure, the Department’s Science Missions Divisions: Payloads Technology Division expanded into the Directorate’s Science Payload and Advanced Concepts — the Astrophysics Missions Division; Office. Based on the experience gained in the — the Planetary Missions Division; Department, the organisation of internal research was — the Solar and Solar-Terrestrial Missions Division; recently adjusted. — the Fundamental Physics Missions Division;

In essence, the role of RSSD is to ensure the best possible and two Operations Support Divisions: scientific performance of ESA’s Science Programme missions. To this end, the Department Head, under the — the Science Operations and Data Systems Division; direct authority of the Director of the Scientific — the Space Telescope Operations Division. Programme, is responsible for the implementation of all science management aspects of the missions in the The role and functions of the Chief Scientist, replacing Science Directorate. This responsibility is carried out in those of the previous Research (Support) Division Head, full coordination with the Directorate’s Scientific are described briefly in Section 2.1. Sec1.qxd 3/5/03 3:23 PM Page 7

introduction 7

Table 1: RSSD Staff in Post at end of 2002.

Head of Department: A. Gimenez Admin. Assistant: C. Bingham Project Controller: R. Fontaine Divisional Assistants: S. Ihaddadene, B. Schroeder, C. Villien

Chief Scientist: B.H. Foing

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

Solar and Solar-Terrestrial Missions Division K.P. Wenzel (Head) C.P. Escoubet B.G. Fleck* R.G. Marsden T.R. Sanderson P. Brekke* M. Fehringer S. Haugan* L. Sanchez Duarte*

* located at SOHO/EOF, NASA Goddard Space Flight Center

Planetary Missions Division G. Schwehm (Head) R.J.L. Grard H. Laakso P. Martin R.M. Schulz A. Chicarro D.V. Koschny J.-P. Lebreton A. Ocampo L.H. Svedhem

Fundamental Physics Missions Division R. Reinhard (Head) Y. Jafry O. Jennrich

Space Telescope Operations Division D. Machetto (Head) R.A.E. Fosbury T. Boeker G. Meylan M. Robberto A. Micol A. Clampin-Nota M. Miebach L. Stanghellini ST-ECF (Garching) M.R. Rosa G. De Marchi B. Mobasher T. Wiklind P. Benvenuti (Head) J. Maiz-Apellaniz P. Padovani R. Albrecht STScI (Baltimore) H. Jenkner N. Panagia M. Dolensky S. Arribas

Science Operations and Data Systems Division M.F. Kessler (Head) F. Jansen M.J. Szumlas G. Thoerner W. Wamsteker** C. Arviset** S. Ott D. Texier* A. Toni J.J. Zender K. Bennett J. Riedinger

* located at Integral Science Data Centre Geneva; ** located at Vilspa

Integral Science Operations L. Hansson (Head) P. Barr R. Much A. Orr J. Sternberg

ISO Data Centre (Vilspa) A. Salama (Head) C. Gry R. Lorente S. Peschke E. Verdugo P. Garcia Lario

XMM-Newton Science Operations (Vilspa) B. Altieri J.C. Gabriel M. Kirsch J. Munoz Peiro M. Santos-Lleo M. Arpizou M. Guainazzi L. Metcalfe A. Pollock N. Schartel M. Ehle

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 3/5/03 3:23 PM Page 8

8 introduction

Figure 1.2/2: Distribution of RSSD staff according to Figure 1.2/3: Distribution of RSSD staff according to prime function. Staff from the Science Payload and location. Advanced Concepts Office are included.

The new Office for Science Payload and Advanced close to the Science Directorate’s project teams and the Concepts (having its origin in the previous Science Technical Directorate, but also in Villafranca (ISO and Payloads Technology Division) is under the direct XXM-Newton science operations teams), in Garching authority of the Director of the Scientific Programme. and Baltimore (Space Telescope Operations Division) This Office is responsible for the assessment phase and and Greenbelt (SOHO Project Scientist Team at NASA the strategic approach for future missions, as well for Goddard Space Flight Center). Fig. 1.2/3 shows the distri- new payload technologies in support of the Cosmic bution of RSSD staff according to location. Vision long-term Science Programme. The Office works, in close liaison with the RSSD study scientists and the While not formally on the ESA staff complement, science community, to determine the science and Internal Research Fellows, on contracts of maximum technology needs of this programme. The Office is also 2 years and funded by the Agency’s education budget, responsible for laboratory support throughout the play a major role in the Department’s research activities. Directorate, including those RSSD research activities Typically, some 15 Research Fellows were in post at any requiring such support. one time during the reporting period. The Department also hosted several Young Graduate Trainees on 1-year The current organigram of RSSD is shown in Fig. 1.2/1. contracts, and offered numerous opportunities for The office of the Department Head is supported by a Trainees and Stagiaires. budget controller. The role and functions of the six Divisions and of the Science Payload and Advanced Highlights for the Department in the reporting period Concepts Office are further described in the seven include: sections of Chapter 3. — the successful launch of Integral and the very The staff of the Department (55 at the end of 2002, promising first-light images from all its instruments; including the Science Payload and Advanced Concepts — RSSD’s contributions to the replanning of ESA’s Office) hold posts within the overall ESA staff comple- long-term Science Programme ‘Horizons 2000’ to ment and are funded from the RSSD budget. Staff ‘Cosmic Vision’, required after the Council at associated with the Science Operations Teams hold Ministerial Level in late 2001; supernumerary positions and are funded from the — the completion, testing and delivery of Co- budgets allocated to the Projects. By the end of 2002 Investigator contributions to Rosetta and SMART-1 there was a complement of 69 supernumeraries. It should instruments; be noted that, in these Teams, many contractors and often — the approval of the Eddington and Venus Express staff from Principal Investigator institutes work together missions; in an integrated structure. An overview of the staff in post — the continued excellent science return from HST, at the end of 2002 is given in Table 1. Fig. 1.2/2 gives the Ulysses, SOHO, Cluster and XMM-Newton in orbit; distribution of staff according to functions, integrating — RSSD’s contribution to the implementation of the personnel from RSSD proper and the Science Payload new Huygens mission scenario; and Advanced Concepts Office. — maintaining a high level of research with a significant number of publications in spite of the increasing Staff of the Department are located not only at ESTEC, pressure of the scientific support activities; Sec1.qxd 3/5/03 3:23 PM Page 9

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— the active organisation of a number of Symposia and Scientific support activities to missions under Workshops for the space science community. development or study will require close attention. Continued efforts will be devoted to the preparation of Herschel, Planck and Eddington, as well as to the 1.3 Department Outlook European contribution to JWST and to Gaia. The LISA gravitational wave observatory and its SMART-2 During the past 2 years, time was devoted to the technology mission will require special efforts in this reorganisation of the Department, in line with its new emerging area of space science. In the Solar System role and goals. This also affected its interfaces within the domain, our activities will focus on Double Star, a overall organisation of the Directorate to improve cooperative mission with China, and Venus Express, both efficiency further. Changes were mandated by the need to to be launched in the next 3 years. Equally, the prepara- find new ways to implement the Programme, following tions for BepiColombo, travelling to Mercury, and for the Ministerial Council in 2001. The next 2 years are Solar Orbiter will need to be intensified. expected to see a consolidation of the present structure together with a further refinement of the internal One of the most important responsibilities of RSSD – the workings of the Directorate. science operations of the various scientific missions – continues to require our full attention as well as the The Cosmic Vision 2012 Programme was approved after further development of skills and tools to cope with an a replanning exercise involving the scientific community. increasingly demanding activity. The availability of The challenge was to deliver as much science as possible properly processed scientific data, to the full satisfaction while keeping a realistic plan within the approved budget of the scientific community at large and valid for both boundaries. This implies difficult decisions for institu- observatory-type missions, with its high pressure from tions providing payloads and a more focused role for the scientific community, and for PI-type missions, is a industry. The way to define and implement missions is clear objective and goal for the future. changing considerably. For example, the introduction of production groups relies not only on the reuse of space The need to maintain and improve the links with research platforms, but also on an optimised use of teams and the institutions in Member States through active cooperative tailoring of budgets and schedules to the available programmes remains a prime goal of the Department. resources. Examples are Eddington, incorporated into the Another aim for the future is the support to the existing Herschel/Planck package, and Venus Express, development of science communications and science based on Mars Express and Rosetta. education activities in ESA.

Concerning the research activities in the Department, the coming years are an important challenge. The pressure of Acknowledgements the scientific support activities continues to increase The Scientific Editor acknowledges the invaluable rapidly to the detriment of the time available for research support of C. Bingham, who coordinated multifarious – a dangerous situation that should be avoided. activities and prepared some of the Annexes. Input to Following the streamlining of the internal organisation of Chapter 2 was coordinated and compiled by T. Appour- the research programme at the end of 2002, it is chaux, M. Bavdaz, K. Bennett, F. Favata, B.H. Foing, important to see how these activities develop and M. Fridlund, J.-P. Lebreton, N. Panagia, A. Parmar, whether further adjustments will be necessary in the light A. Peacock, A. Salama, T. Sanderson and G. Schwehm. of experience. Chapter 3 was compiled by the Heads of Division based on the contributions from the Project Scientists. Our opportunities for the analysis of data from missions S. Ihaddadene and M. Riemens compiled the publication in orbit will be improved with the new opportunities list and A. Toni provided technical support. offered by Integral and, soon, by SMART-1 and Mars Express. In astronomy, the data exploitation of successful missions such as XMM-Newton and HST or ground- based observatories continues, as well as that of data archives from previous missions like ISO. 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 for the COROT and STEREO missions. The arrival of Cassini at Saturn in mid-2004 and the entry of the Huygens probe into the atmosphere of Titan in early 2005 will be milestones for our research activities. Finally, we foresee the start of an increased effort in Fundamental Physics research very soon. sec2.qxd 3/5/03 3:37 PM Page 11

2. RESEARCH ACTIVITIES

2.1 Research Support Division 2.7.2 Propagation of solar energetic particles: analysis of the events’ decay phase 2.7.3 3He-rich events 2.2 High-Energy Astrophysics Research 2.7.4 Observations of the Sun’s magnetic field during 2.2.1 X-ray binaries recent solar maximum 2.2.2 X-ray emission from star-forming regions and 2.7.5 The SEPT/IMPACT instrument on the STEREO young stellar objects mission 2.2.3 X-ray background and large-scale structure 2.2.4 Deep XXM-Newton survey of the galaxy M33 2.2.5 The starburst-AGN connection 2.8 Plasma and Gas Environment of Solar 2.2.6 The revival of fossil AGN System Bodies 2.2.7 X-ray spectroscopy of general relativistic effects 2.8.1 Cluster-related research in AGN 2.8.2 Electron density distribution in the Earth’s 2.2.8 Discovery of an ionised Fe K edge in the z = 3.91 magnetosphere quasar APM 08279+5255 2.8.3 Plasma and wave phenomena induced by neutral 2.2.9 The signature of SN ejecta in the X-ray afterglow gas releases in the solar wind of GRB011211 2.8.4 Instrument developments

2.3 Optical/UV Astrophysics 2.9 Comparative Planetology and Astrobiology 2.3.1 Stars and stellar systems 2.9.1 Comparative planetology of Earth-like planets 2.3.2 Galaxies and moons 2.3.3 High-energy activity of radio galaxies and blazars 2.9.2 Lunar research and SMART-1 exploitation 2.3.4 Cosmological Studies 2.9.3 Mars research 2.9.4 Impact cratering processes 2.9.5 Contributions to astrobiology 2.4 Infrared/Submillimetre Astrophysics 2,4.1 ISO data exploitation 2.4.2 Preparations for Planck 2.10 Cosmic Dust and Comets 2.4.3 Sub-mm emission of extra-galactic objects 2.10.1 In situ measurements of cosmic dust 2.10.2 Infrared investigations of interplanetary dust particles 2.5 Exoplanets and Stellar Environments 2.10.3 Ground-based observations of comets 2.5.1 Study of outflows in star-forming regions 2.10.4 Leonid observations 2.5.2 Pulsations of Beta-Pictoris stars 2.10.5 The Rosetta imaging system (OSIRIS) 2.5.3 Exploitation of MUSICOS 2.5.4 Preparations for Eddington 2.11 Development and Exploitation of Super- conducting Cameras for Astronomy 2.6 Solar Physics and Seismology 2.11.1 Overview of activities 2.6.1 The Phoebus Group: the search for g modes 2.11.2 The SCAM-1 programme continues 2.11.3 The SCAM-2 programme 2.6.2 Solar activity and p modes 2.11.4 The SCAM-3 programme 2.6.3 The SUMER spectral atlas of solar disc features 2.11.5 The SCAM-4 programme 2.6.4 Oscillations above sunspots 2.11.6 The SCAM-5 programme 2.6.5 Self-organised criticality and solar flares 2.11.7 The SCAM-6 programme 2.6.6 Magnetic interaction of waves in the chromo- 2.11.8 SCAM programme conclusions sphere 2.6.7 Asteroseismology 2.12 Advanced Sensor, Optics and Instrument Development Research 2.7 Heliospheric Physics 2.12.1 Compound semiconductor photon detectors 2.7.1 Composition measurements of energetic particles 2.12.2 Low-mass X-ray optics above the southern solar pole by the Ulysses COSPIN/LET instrument sec2.qxd 3/5/03 3:37 PM Page 13

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2.1 Research Support Division Stagiaires for up to 6 months, as part of their research or graduate engineering studies, as well as to a few Research at RSSD is an integral part of the activities of externally-supported research students. The scheme of the scientific staff, needed to maintain and develop their Internal Research Fellows, Trainees and Stagiaires, scientific skills, peer recognition and hands-on besides offering training and experience at RSSD, experience in space science. Active involvement in permits a continuous exchange and collaboration with research is necessary for Project Scientists to remain part their institutes of origin or of their future destinations. A of the community when performing their mission-related number of Master or PhD theses were co-supervised by duties. RSSD staff scientists and colleagues from academic institutions. In the new RSSD structure, put in place in early 2001, the Research Division (later renamed the Research Support RSSD scientists managed to maintain a leading role in Division) was formed to facilitate and assist in more than a third of their research papers, despite their coordinating the research activities performed by staff functional workload in scientific support to projects, across the various Mission Divisions, in parallel to their thanks to their commitment, collaborations within main functional activities of scientific support to Research Groups and with the outside community, and projects. The Departmental research programme was the contribution of Research Fellows. The publications in sub-structured into thematic Research Groups. The 2001 and 2002 involving RSSD staff are listed in Research Groups also provided a basis for the integration Annex 2. and regular interaction of Research Fellows and Trainees with staff scientists and support staff. The Head of the RSSD staff organised Symposia and Workshops in Research Support Division was responsible for the support of ESA science missions or in relation to overall supervision of the Research Fellows and scientific themes or collaborative research topics (see Trainees. He also supported the annual assessment of the Section 4.1). They also contributed to science scientific activities and organised annual reviews of the communications and education activities (see Section results and new proposals for these activities. 4.2), as well as to several coordination and supporting tasks (see Section 4.3). The programme of RSSD The research in RSSD reflects the breadth of the Cosmic seminars, arranged by the Research Support Division Vision programme in the different fields related to ESA (and open to other interested scientists), continued with a science missions. The activities have been influenced by mixture of external and internal speakers, presenting opportunities given by the ESA Science Programme, but results or reviews over a wide range of space science also constrained by the limited time available to the topics (see Annex 3). The colloquia programme scientists owing to an increased workload on projects, presenting prestigious speakers to all ESTEC staff studies and other functional activities. RSSD staff continued during the reporting period (see Annex 3). In a conduct research collaborations with institutes from all programme of informal internal seminars, RSSD Member States and with the international community, scientists reported on their research activities or gave mostly in the areas of data exploitation from ESA and tutorials across disciplines. other space science missions and of instrument development. In one or two cases, external researchers Based on the experience gained during the reporting also contribute to the scientific output of the Department period and with the goal of reinforcing and maintaining through extended visits to RSSD. the high standard of the Departmental research programme, the research organisation was recently adjusted. Internal Research Fellows on post-doctoral contracts of At the same time, internal procedures were streamlined. up to 2 years play a major role in the Department’s The Head of the Research Support Division now fulfills research activities. On average, some 15 Research the role of Chief Scientist, advising the Head of Fellows are in post at any one time, covering the large Department on the research activities and their evalua- range of topics in RSSD. They are recruited through the tion, as well as supporting science communications and standard ESA process of interviews, chaired by the Head related activities. Some adjustments to the Research of the Research Support Division. The excellence and Groups, including Lead Scientists coordinating present- publication record of candidates, their research ations and the availability of funds, have also been programme matching RSSD research priorities, and the implemented. training opportunity at RSSD for their career prospects were prime selection criteria. RSSD also hosted a couple The Sections following are arranged according to of post-doctoral researchers funded through EU discipline. They follow in general, but not systematically, European Network collaborations. The Department also the Research Group structure that existed during most of hosted some Young Graduate Trainees on 1-year the reporting period. contracts, as well as Portuguese and Spanish Trainees on 2-year grants funded by their respective nations. The Department also offered opportunities to a number of sec2.qxd 3/5/03 3:37 PM Page 14

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2.2 High-Energy Astrophysics Research

2.2.1 X-ray binaries

In the field of X-ray binary research, the Group has used the outstanding sensitivity and spectral resolution of the XMM-Newton instruments to investigate narrow absorption features in a number of low-mass X-ray binaries (LMXRBs). These features allow the ionisation state, location, abundance and dynamics of the accreting material to be studied. Three systems have been studied in detail: the dipping sources MXB 1659-298 and X 1624-490 and the non-dipping source GX 13+1 (Sidoli et al., 2002). It is likely that the dipping systems are viewed closer to the orbital plane than the non-dipping systems because obscuration by material in an Figure 2.2.1/2: The equivalent widths of the two iron azimuthally-structured accretion disc is thought to be absorption features seen in the EPIC PN spectra of responsible for the dipping activity. MXB 1659-298 as a function of orbital phase. There is no obvious orbital dependence, even during the Sidoli et al. (2001) report the discovery of narrow X-ray dipping activity at around phase 0.8. absorption lines from the low-mass X-ray binary MXB 1659-298 during an XMM-Newton observation in February 2001. MXB 1659-298 is a transient, bursting X-ray source that exhibits 15-min X-ray eclipses every 7.11 h. The eclipses are preceded by intense dipping 2p transitions, together with a broad Fe emission feature activity that lasts for about 2 h. During dips, the amount at 6.47 keV (Fig. 2.2.1/1). The large range of ions of low-energy absorption increases strongly. EPIC and implies either that the absorbing material is present over RGS spectra reveal the presence of narrow resonant a wide range of distances from the central source, or that absorption features identified with O VIII 1s-2p, 1s-3p it has a large range of densities. Strangely, the equivalent and 1s-4p, Ne X 1s-2p, Fe XXV 1s-2p, and Fe XXVI 1s- widths of the Fe absorption features show no obvious dependence on orbital phase, even during dipping intervals (Fig. 2.2.1/2). The equivalent widths of the other features are consistent with having the same values during persistent and dipping intervals. This implies that Figure 2.2.1/1: XMM-Newton RGS spectra in the the material responsible for the narrow absorption regions around some of the narrow absorption features is not the same as that responsible for the dips. features seen from the low-mass X-ray binary Previously, the only X-ray binaries known to exhibit MXB 1659-298. The arrows indicate theoretical narrow X-ray absorption lines were two superluminal jet wavelengths. sources and it had been suggested that these features are related to the jet formation mechanism. This now appears unlikely, and instead their presence may be related to the viewing angle of the system.

An idea of the spectral complexity that XMM-Newton is beginning to see around the iron line from low-mass X-ray binaries can perhaps best be seen in an observation of the dipping source X 1624-490 reported in Parmar et al. (2002). In this source the dips repeat every 21 h and no X-ray eclipses are present. Features identified with the K alpha absorption lines of Fe XXV and Fe XXVI are again present and their properties show no obvious dependence on orbital phase, except during a dip. In addition, faint absorption features tentatively identified with Ni XXVII K alpha and Fe XXVI K beta might be present (Fig. 2.2.1/3). A broad emission feature is also evident. A deep absorption line is present during the dip with an energy consistent with Fe XXV K alpha. This is the second dipping LMXRB source from which narrow Fe absorption features have been observed. sec2.qxd 3/5/03 3:37 PM Page 15

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optical and UV. Favata et al. (2002) for the first time detected X-ray emission from a protostellar jet: HH 154. The jet originated from the highly embedded binary protostar IRS 5 in L1551. The high sensitivity of XMM- Newton allowed the spectrum of the X-ray source to be studied, and its temperature to be determined. At T ~4MK, the plasma responsible for the X-ray emission is hotter than expected from the known characteristics of the jet’s working surface.

Later Chandra observations (Bally et al., 2003) showed that the X-ray emission is not from the working surface, but is displaced by about 7 arcsec. A small knot is present in the jet near this position, which new spectroscopic observations by Fridlund show to have a velocity a factor Figure 2.2.1/3: The 5.5-8.5 keV residuals from the of 2 higher than the working surface. This, together with best-fit continuum model of X 1624-490 observed a lower degree of ionisation, can explain the observed with EPIC. A broad emission feature at 6.58 keV and high temperature. The X-ray luminosity of the jet source two narrow features identified with Fe XXV K alpha is, at Lx ~3x1029 erg s–1, moderate. However, as the and Fe XXVI K alpha absorption at 6.72 keV and X-rays are emitted well above the accretion disc, they 7.00 keV are clearly evident. Fainter features at can illuminate it from above, at a high incidence angle 7.83 keV and 8.28 keV might be present and are (something which the coronal emission from the young tentatively identified with Ni XXVII K alpha and star cannot do), and thus penetrate and ionise the disc Fe XXVI K beta absorption. material at significant distance from the star. If protostellar jet emission turns out to be common, it could have a significant role in determining the accretion disc’s ionisation and thus the accretion rate.

References Marginal detection of some other objects of this class as Parmar, A.N., Oosterbroek, T., Boirin, L., Lumb, D., X-ray sources in the Rosat database has led to a 2002, A&A 386, 910. programme of XMM-Newton and Chandra observations Sidoli, L., Oosterbroek, T., Parmar, A.N. et al., 2001, to search for X-ray emission from other HH objects (PI A&A 379, 540. F. Favata), which has been approved for both missions at Sidoli, L., Parmar, A.N., Oosterbroek, T., Lumb, D., the last AO round. 2002, A&A 385, 940. Whether the presence of dense discs (as in the CTTS) has an influence on the X-ray emission of young stars has 2.2.2 X-ray emission from star-forming regions and been a matter of debate since Einstein observations in young stellar objects 1981. The high XMM-Newton sensitivity has allowed for the first time the X-ray spectral characteristics of X-rays are produced copiously in all stages of star TTauri stars to be studied. Favata et al. (2003) have formation and, thanks to their ability to penetrate the shown that CTTS and WTTS in L1551 have different shrouds of gas and dust that obscure very young stars, X-ray spectral and temporal behaviours, suggesting that they are an ideal tool to study all the stages of star different mechanisms are responsible for the dominant formation. F. Favata and collaborators from Palermo parts of the X-ray emission. CTTS in L1551 have a much Observatory have studied a number of young nearby star- higher temporal variability than do WTTS, and their forming regions using deep XMM-Newton observations. coronal abundances show a large spread of almost three The high sensitivity of XMM-Newton has produced a orders of magnitudes, while the coronal abundances of number of new discoveries, including the detection of WTTS are narrowly clustered around a mean value X-ray emission from protostellar jets (Herbig-Haro Z ~ ZSun (even though the photospheric abundances of objects) and the presence of significant differences in the the two groups are most probably identical). Also, the X-ray spectral characteristics of classical and weak-lined WTTS show a characteristic coronal abundance pattern TTauri stars (CTTS and WTTS). Both results were (with the noble gases, notably Ne, enhanced over Fe) obtained in a deep XMM-Newton observation of the typical of older very active stars, which the CTTS do not nearby L1551 star-forming region in Taurus. share. The X-ray emission mechanism of WTTS appears to be purely coronal in nature, while in CTTS additional Polar jets are a relatively common feature in very young mechanisms are likely to be at play. stars, and jets frequently feature shocked regions, as evidenced by, for example, their emission lines in the A clue to the nature of the X-ray emission from CTTS is sec2.qxd 3/5/03 3:37 PM Page 16

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References Bally, J., Feigelson, E.D., Reipurth, B., 2003, ApJ, in press. Favata, F., Micela, G., Reale, F., 2001, A&A 375, 485. Favata, F., Fridlund, C.V.M., Micela, G., Sciortino, S., Kaas, A.A., 2002, A&A 386, 204. Favata, F., Giardino, G., Micela, G., Sciortino, S., Dami- ani, F., 2003, A&A, in press.

2.2.3 X-ray background and large scale structure

Resulting from calibration work on XMM-Newton, detailed analysis of internal EPIC instrument backgrounds was undertaken, including the effects of magnetospheric soft protons scattered through the mirror system. The Science Operations Centre (SOC) team produced a compilation of ‘blank field’ high galactic latitude pointings that have been widely used in the analysis of extended diffuse objects. The data were also used in their own right to constrain the contribution of the cosmic diffuse X-ray background. The study offered a high-sensitivity measurement which, for the first time, transcended the energy band at ~1 keV where the galactic and extragalactic components cross over in intensity, and concluded that the normalisation is towards the higher end of previously claimed results. This has implications for the necessity of future long-duration exposures of deep XMM-Newton and Chandra fields (Lumb et al., 2002).

Figure 2.2.2: The X-ray light curves of two X-ray D. Lumb is leading the data analysis effort in a long-term bright pre-main sequence stars in the L1551 cloud, as programme with several institutions to determine the Ωm observed by XMM-Newton. The top panel is from the parameter from measurements of a flux-limited sample WTTS V826 Tau, showing little temporal variation. of high-redshift clusters. Data from the first eight clusters The bottom panel is from the young CTTS XZ Tau, (median z = 0.54) have been analysed, and a luminosity- showing the steady increase in X-ray luminosity temperature function established. In comparison with discussed in the text. low redshift samples, the results suggest a mild evolution in cluster parameters, leading to interesting constraints on cosmological parameters and the evolution of intra- cluster gas physics (Lumb et al., 2003). Results on the spectroscopic analysis of XMM-Newton data of the provided by the very peculiar behaviour shown by the central 0.5/h50 Mpc regions of the clusters of galaxies young CTTS XZ Tau, whose X-ray emission increased Coma, A1795 and A3112, were presented in collabora- linearly by a factor of ~ 4 during a 50 ks XMM-Newton tion with the University of Alabama (Nevalainen et al., observation (Fig. 2.2.2). At the same time, the absorbing 2003). A significant warm emission component at a level column density (N(H)) decreases by a comparable factor, above the systematic uncertainties is evident, and the soft pointing to the modulation being dominated by a X-ray (0.2-2.0 keV) luminosity is 10-30% of that of the shadowing effect. The peak N(H) value is compatible hot gas. The best-fit temperatures (0.6-1.3 keV), with the typical optical thickness of the accretion stream, overdensities (200-1000) and metal abundances (0-0.15 suggesting that the X-ray emission is probably being of solar) of the warm component inside the central concentrated at the accretion spot and shadowed by the 0.5/h50 Mpc are consistent with the results of recent accretion stream rotating in and out of the line of sight. cosmological simulations. These results offer observa- This implies that the X-ray source is spatially compact, tional support to the theories that predict a large fraction and it could also imply that a non-negligible fraction of of the current epoch’s baryons are located in a warm-hot the X-ray emission is accretion-dominated. While Favata intergalactic medium. et al. (2001) had shown that the flaring emission of TTauri stars is confined in relatively compact regions, References this is the first evidence that the quiescent emission from Lumb, D.H., Warwick, R.S., Page, M., De Luca, A., CTTS is also confined in small spatial regions. 2002, A&A 389, 93. sec2.qxd 3/5/03 3:37 PM Page 17

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Lumb, D.H., Bartlett, J., Blanchard, A. et al., 2003, A&A, submitted. Nevalainen, J., Lieu, R., Bonamente, M., Lumb, D.H., 2003, ApJ, in press.

2.2.4 Deep XMM-Newton survey of the galaxy M33

XMM-Newton performed raster observations of the bright Local Group spiral galaxy M33 as part of the Telescope Scientist’s guaranteed time and open guest observer’s time. Being a collaboration between scientists at MPE Garching (D), the Osservatorio Astronomico di Brera (I) and M. Ehle, this project had the goal of studying the population of X-ray sources down to a 0.5-10 keV luminosity of 1035 erg s–1, more than a factor of 10 deeper than earlier Rosat observations. EPIC spectra and hardness ratios were used to distinguish between different source classes. Figure 2.2.4: A false-colour image of the XMM- Light curves confirmed the 3.45 d period of the X-ray Newton EPIC raster survey of M33. The optical binary X-7, led to the detection of a transient super-soft extent of M33 is marked by the white ellipse. source (Xn2) and were used to search for short-term Prominent in the soft-energy band (red) are diffuse variability. Diffuse soft X-ray emission due to very hot hot gas, HII regions (NGC 604), foreground stars and gas was detected in the central disc of M33 and from super-soft sources (e.g. Xn2), in the medium band the regions of the optical bright inner spiral arms (yellow) supernova remnants (X-3), and in the hard (Fig. 2.2.4). band (blue and white) the nucleus (X-8), X-ray binaries (X-7, X-2) and background AGN (Xn1).

2.2.5 The starburst-AGN connection

The analysis of Chandra data on the low-luminosity AGN in NGC 4303 gives for the first time hints on the co-existence of an intermediate to high-mass black hole References together with a young super stellar cluster in the three Guainazzi, M., 2002, MNRAS 329, L13. central parsecs of the galaxy. These results are the main Guainazzi, M., Matt, G., Fiore, F., Perola, G.C., 2002, topic of the Ph.D. work of graduate student E. Jimenez- A&A 388, 787. Bailon, supervised by M. Santos-Lleo and M. Mas-Hesse (Laeff, Spain). The study is being complemented with the analysis of XMM-Newton data for a similar AGN, 2.2.7 X-ray spectroscopy of general relativistic NGC 1808. effects in AGN

Reference The unprecedented combination of photon-collecting Jimenez-Bailon, E., Santos-Lleo, M., Mas-Hesse, M., et area and energy resolution allows XMM-Newton to al., 2003, ApJ, submitted. measure directly general relativistic effects in nearby AGN. The emission-line profiles of photons, which are emitted in X-ray-illuminated relativistic accretion discs 2.2.6 The revival of fossil AGN around a super-massive black hole, are distorted by Doppler shift and gravitational redshifts. Guainazzi An XMM-Newton SOC-led group (Guainazzi, 2002; (2003) discovered the typical ‘double-horned’ relativistic Guainazzi et al., 2002) has discovered transitions profile of the iron K-alpha fluorescence line in the between states where the nuclear X-ray emission is brightest Seyfert galaxy so far, ESO198-G24. The visible through a photo-electric screen and states where intensity of the red peak is comparable with the intensity the X-spectrum is dominated by Compton reflection. of the blue peak, almost at odds with standard models. This result suggests that at least 10% of the local AGN The author suggests that this line originates in a single may undergo quiescence phases on timescales of the ‘flare’ above the surface of the disc at about 25 order of several years. This discovery also suggests that Schwarzschild radii from the nuclear engine. X-ray obscuration in type 2 AGN occurs on a wide range of spatial scales, from the innermost parsec to the host Reference galaxy. Guainazzi, M., 2003, A&A, submitted. sec2.qxd 3/5/03 3:37 PM Page 18

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between the supernova and the GRB of about 4 d. The new results add support to one prominent model for the origin of GRBs, that at least some GRBs are associated with very recent supernova. The supernova ejects a substantial quantity of enriched material at high velocity into the surrounding medium, which is subsequently illuminated by the GRB.

Figure 2.2.8: The X-ray spectrum of broad absorption line quasar APM 08279+5255 at a redshift of 3.91 taken with the XMM-Newton pn camera. The fit is with a power-law model absorbed by neutral gas.

2.2.8 Discovery of an ionised Fe K edge in the z = 3.91 quasar APM 08279+5255

XMM-Newton observations of the high-redshift, broad absorption line quasar APM 08279+5255 allowed the detection of a high column density absorber (NH ~ 1023 atom cm–2) in the form of a K-shell absorption edge of significantly ionised iron (Fe XV-Fe XVIII) and corresponding ionised lower energy absorption (Fig. 2.2.8). The findings of Hasinger et al. (2002) confirm a basic prediction of phenomenological geometry models for the broad absorption line outflows and constrain the size of the absorbing region. The Fe/O abundance of the absorbing material is significantly higher than the solar value, giving interesting constraints on the gas enrichment history in the early Universe.

Reference Hasinger, G., Schartel, N., Komossa, S., 2002, ApJ 573, L77.

2.2.9 The signature of SN ejecta in the X-ray afterglow of GRB011211

The XMM-Newton observations of the gamma-ray burst (GRB) afterglow of GRB011211 were analysed by a collaboration of scientists from the University of Leicester (UK), MSSL University College London (UK), M. Ehle and N. Schartel from the XMM-Newton SOC. A mixture of elements including magnesium, silicon, sulphur, argon and calcium was seen as X-ray emission lines. Such elements are typical of a supernova. With a mean outflow velocity of about 0.1 c, the estimated radius of the gas shell illuminated by the GRB and glowing in X-rays of ~1015 cm implies a time delay sec2.qxd 3/5/03 3:37 PM Page 19

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2.3 Optical/UV Astrophysics main-sequence star and a companion that erupts to become a cool supergiant. A remarkably similar event 2.3.1 Stars and stellar systems was seen in the Andromeda Galaxy in the late 1980s.

The mysterious outburst of the star V838 Monocerotis Stellar segregation and the dynamics of stellar clusters The previously unknown variable star V838 Monocerotis erupted in early 2002, brightening suddenly by a factor G. De Marchi has studied how dynamics change the of almost 10 000 at visual wavelengths. An expanding distribution of masses in stellar clusters over time. In light echo appeared around the star shortly afterward, as collaboration with G. Andreuzzi and others, he has illumination from the outburst propagated into a probed the globular cluster NGC 6712 and shown that its surrounding, pre-existing circumstellar dust cloud. This mass function has been severely modified by the tidal is the first light echo seen in the Milky Way since 1936. field of the Galaxy in the course of the cluster’s lifetime, The star and its surrounding medium have been studied to the point that the number of stars presently decreases by N. Panagia and collaborators, obtaining a series of with mass, in marked contrast with any known globular high-resolution images and polarimetry of the light echo clusters. The study of the nucleus of this object, done in with the Hubble Space Telescope and its newly installed collaboration with Paltrinieri et al., has revealed a large Advanced Camera for Surveys (ACS). number of blue straggler stars, suggesting that the cluster was originally much more massive and that most of its The echo exhibits a series of arcs, whose angular stars have been dispersed into the Galactic halo. expansion rates show that the distance is greater than 2 kpc. The polarimetric imaging implies an even greater In collaboration with Albrow et al., G. De Marchi has lower limit to the distance as high as 6 kpc. Both limits used the HST to obtain a detailed and uniform mapping mark the first time that these phenomena have been used of mass segregation in the globular cluster M22. The to constrain an astronomical distance in the Milky Way. degree of mass segregation observed in M22 can be At maximum light, the object was extremely luminous, at accounted for by relaxation processes within the cluster, least as bright as visual absolute magnitude –9.6. The whose global mass function is flatter than the Salpeter spectrum of the star during the outburst remained that of initial mass function and cannot be represented by a a cool stellar photosphere, but a composite spectrum single power law. In collaboration with Sirianni et al. appeared as the outburst subsided. V838 Mon thus (2002), De Marchi found evidence for mass segregation appears to represent a new class of stellar outbursts, in a much younger cluster, NGC 330 in the Small occurring in binary systems containing a relatively hot Magellanic Cloud. While low-mass stars are uniformly

Figure 2.3.1/1: Comparison of ACS images obtained on 20 May 2002 (left) and 28 October 2002 (right). The structure is dominated by a series of near-circular arcs and rings, centred on the variable star, but there are cavities that become progressively asymmetric with time. sec2.qxd 3/5/03 3:37 PM Page 20

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Figure 2.3.1/3: This five-WFPC2-field mosaic of 30 Doradus is the most detailed ever optical image of an starburst region. Three line-subtracted continuum filters (F336W, WFPC2 U; F555W, WFPC2 V; F814W, WFPC2 I) are combined in chromatic order with two narrow-band filters (F673N, [S II] Figure 2.3.1/2: The core of the stellar cluster 6717+6731 in the red and F656N, H-alpha in the NGC 330 in the Small Magellanic Cloud. Massive green channels). The mosaic shows the central stars are found almost exclusively near the centre, 70 x 45 pc of the 30 Doradus nebula at a resolution of where they have probably formed. 0.1 arcsec (0.025 pc).

distributed throughout the cluster, more massive objects References tend to be preferentially located in the central regions. Maíz-Apellániz, J., Cieza, L., McKinty, J.W., 2002, AJ Since the age of NGC 330 is 10 times shorter than the 123, 1307. expected relaxation time, the observed mass segregation must be of a primordial nature rather than dynamical and traces the locations where stars of different mass form. Mayall II = G1 in M31: giant globular cluster or core of a dwarf elliptical galaxy? References Albrow, M., De Marchi, G., Sahu, K., 2002, ApJ 579, Mayall II = G1 is one of the brightest globular clusters 660. belonging to M31, the Andromeda Galaxy. G. Meylan, in Sirianni, M. et al. (incl. G. De Marchi), 2002, ApJ 579, 275. collaboration with Sarajedini (UFL), Jablonka (Obs. Paris), Djorgovski (Caltech), Bridges (AAO) and Rich (UCLA), obtained multicolour photometry with the Wide Massive stars and their environments Field and Planetary camera (WFPC2) of G1 (Meylan et al., 2001). From model fitting, they determined its mean J. Maíz-Apellániz has studied different aspects of metallicity as [Fe/H] = –0.95±0.09, which is rather high massive stars and their interaction with their and is somewhat similar to that of 47 Tucanae. By means environment, ranging from the nearest stars to several of artificial star experiments, they determined that most Mpc away. The most precise measurement to date of the of the observed spread in V-I colour is due to an intrinsic scale height of the early-type stellar component of the metallicity dispersion amongst the stars of G1, possibly Galactic disc and of the relative position of the Sun with as a consequence of self-enrichment during the early respect to its midplane was produced. A new theory for stellar/dynamical evolutionary phases of this cluster. So the origin of the Local Bubble was proposed and far, only Omega Centauri, the giant Galactic globular elaborated for its possible consequences on Earth. The cluster, has been known to exhibit such an intrinsic interaction of two dwarf starbursts, 30 Doradus and NGC metallicity dispersion, a phenomenon certainly related to 4214, with their environment was analysed and the first the deep potential wells of these two star clusters. reliable distance to the latter was provided. Finally, the structural properties of the nearest massive young The total mass of this globular cluster has been estimated clusters was analysed, a new classification scheme for to be about 10 million solar masses or higher, which them provided, and new evidence obtained for their role makes G1 more than twice as massive as Omega as progenitors of globular clusters. Centauri, the most massive Galactic globular cluster. sec2.qxd 3/5/03 3:37 PM Page 21

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Large masses appear to correlate with conspicuous During the last 2 years, they have analysed in detail metallicity spreads, whose origin is still unknown. In the several objects in the sample, such as Arp220 and IRAS diagnostic defined by Kormendy, G1 always falls on the 15206+3342 (Arribas & Colina, 2002). The velocity sequence defined by globular clusters, and definitely field and the velocity dispersion map of the warm away from the sequences defined by elliptical galaxies, (ionised) gas of IRAS 15206+3342 show that the optical bulges and dwarf spheroidal galaxies. The same is true (or infrared) nucleus is clearly offset about 5 kpc relative for Omega Centauri. to the centre of symmetry. This result could be explained in terms of a strong inflow of gas along a tidal tail, which References is feeding the nuclear regions where young stellar Meylan, G. et al., 2003, AJ 122, 830. clusters are forming stars at a rate of about 150 MSun/yr. The two characteristics of strong inflows and massive starbursts are expected during the final coalescence 2.3.2 Galaxies phase of two disc galaxies with bulges.

The nuclei of late-type spiral galaxies References Arribas, S., Colina, L., 2002, ApJ 573, 576. Boeker and collaborators continued an ongoing study of the central morphology of spiral galaxies. Using the WFPC2 camera aboard HST, they completed an imaging 2.3.3 High-energy activity of radio galaxies and survey of a large and unbiased sample of late-type, blazars bulge-less spirals. The survey established that about 75% of the observed galaxies harbour a compact and luminous Studies of radio galaxies star cluster in their nuclei. The formation mechanism of such clusters is unclear, especially in galaxies of late As part of a large research project aimed at investigating Hubble type. In these bulge-less, disc-dominated the nuclear regions of radio galaxies, Chiaberge et al. galaxies, the gravitational potential in the nuclear region (2002) have studied UV-band HST/STIS images of 28 is nearly flat, and gravity is a very inefficient mechanism sources from the 3CR sample. Unresolved nuclei are for gas infall towards the centre. It is therefore puzzling observed in 10 of the 13 low-power sources (belonging how the high star-formation efficiency needed to build to the Fanaroff-Riley I class, FR I), and in five of the 15 such massive clusters can be explained. The team is more powerful Fanaroff-Riley II. Broad-line radio currently deriving stellar population ages and dynamical galaxies are found to have the flattest spectral indices masses for a large number of nuclear clusters in order to similar to those of quasars and are confined within a very better constrain their star-formation history. Early results from this spectroscopic follow-up programme indicate that many clusters are relatively young, i.e. a few 100 Myr. Since this is much shorter than the timescales for dynamical friction processes, this is evidence that the Figure 2.3.3: The central regions of 3C 270 as they clusters have indeed formed where they are observed appear in the UV band HST/STIS MAMA image. today. Note the small (0.3 arcsec) jet-like feature emerging from the nucleus, projected on to the large (~100 pc scale) dusty disc. The most powerful objects in the local Universe

Ultraluminous Infrared Galaxies (ULIRGs), with 12 bolometric luminosities Lbol ~ LIR =10 LSun, are the most luminous objects in the local Universe. ULIRGs show signs of strong interactions and mergers, and they have large amounts of gas and dust that significantly obscure their ionising sources. They might be the precursors of optical quasars, and their properties are believed to be similar to those of high redshift galaxies. The closest ULIRGs offer the possibility of studying in detail how the different physical processes interplay in these spectacular objects. They are indeed exceptional natural laboratories. S. Arribas, in collaboration with L. Colina (CSIC) and STScI colleagues, is carrying out a programme using integral field spectroscopy combined with high-resolution HST imaging to obtain complete data sets for a representative sample of low-redshift ULIRGs. sec2.qxd 3/5/03 3:37 PM Page 22

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narrow range. This is consistent with radiation produced one of the sources, RGB J1629+4008, is dominated by in a geometrically thin, optically thick accretion disc. On synchrotron emission peaking at ~2x1016 Hz, as also the other hand, FR I nuclei show a wide range of spectral shown by its steep (energy index alphax ~ 1.5) spectrum. indices. Also, a clear trend with orientation is found: This makes this object the first known FSRQ whose sources observed almost edge-on, or with clear signs of X-ray emission is not due to inverse Compton radiation. dust absorption, have the steepest spectra. These results Two other sources display a flat BeppoSAX spectrum imply that obscuration in FR I can be present, but the (alphax ~ 0.7) but with indications of steepening at low obscuring material is not in a ‘standard’ geometrically X-ray energies. This is also supported by Rosat and thick torus. The major difference between these multifrequency data and a synchrotron inverse Compton absorbing structures and the classic AGN ‘tori’ resides in model, which suggests synchrotron peak frequencies the lower optical depth of the FR I obscuring material. ~1015 Hz, typical of ‘intermediate’ BL Lacs for which the synchrotron and inverse Compton components overlap in UV observations of the FR I radio galaxy 3C 270 with the BeppoSAX band. HST/STIS permitted Chiaberge et al. (2003) to discover a jet-like structure that is aligned with the jet observed in Reference the radio and X-ray domains. This is the first jet-like Padovani, P. et al., 2003, ApJ, in press. component ever detected in the UV in a radio galaxy with jets lying almost on the plane of the sky. In addition, Chandra X-ray data (image and spectrum) of this source 2.3.4 Cosmological studies have shown the presence of a faint counter-jet. The moderate obscuration inferred from an analysis of the Highest resolution spectroscopy of a distant galaxy HST images and Chandra X-ray spectrum strongly favours the scenario in which a standard geometrically P. Padovani has worked on a high-redshift Lyman Break and optically thick torus is not present in FR I radio galaxy with S. Savaglio (JHU) and N. Panagia galaxies, contrary to the basic expectations from the (ESA/STScI). Very Large Telescope (VLT) high- unification scheme of AGN. resolution observations of MS 1512-cB58 (z = 2.724, V = 20.64) have revealed, with unprecedented detail References along a galaxy sight line, the Ly-alpha forest due to Chiaberge, M., Macchetto, F.D. et al., 2002, ApJ 571, intervening clouds in the intergalactic medium (IGM), 247. with indications of a possible excess of absorption close Chiaberge, M. et al. (incl. Macchetto, F.D.), 2003, ApJ to the galaxy. This high-density region is at least 582 (2), in press. 60/h65 Mpc comoving wide, but the large Ly-alpha absorption of the galaxy itself prevents the detection of a possible structure extending down to the galaxy. This Studies of blazars excess of Ly-alpha clouds is suggestive of two possible

P. Padovani, in collaboration with H. Landt (STScI), E. Perlman (UMBC), P. Giommi (BeppoSAX/ASDC) and others, has continued his work on the Deep X-ray/Radio Blazar Survey (DXRBS). DXRBS is a large Figure 2.3.4: The image of a galaxy acquired by the blazar sample, deeper by a factor ~20 than previously HST/ACS Pure Parallel Ly-alpha Emission Survey available samples. DXRBS is now ~95% identified and (APPLES) (upper right) is shown together with the includes ~350 sources. By sampling for the first time the corresponding extracted and calibrated spectrum. faint end of the radio and X-ray luminosity functions, the DXRBS blazar sample allows us to investigate the blazar phenomenon and the validity of unified schemes down to relatively low powers. Work is in progress on the evolutionary properties of the DXRBS sample. Preliminary results on the luminosity functions show a remarkable agreement with the predictions of unified schemes. Work is on-going on other aspects of the survey, particularly on the definition of a BL Lacertae object.

P. Padovani has also continued his work on BeppoSAX data of blazars. Padovani et al. (2003) presented new BeppoSAX observations of four flat-spectrum radio quasars (FSRQs) having effective spectral indices typical of high-energy peaked BL Lacs. The BeppoSAX band in sec2.qxd 3/5/03 3:38 PM Page 23

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scenarios: the presence of a supercluster of Ly-alpha 2.4 Infrared/Submillimetre Astrophysics clouds not associated with MS 1512-cB58 or a high density of gas associated with the environment of 2.4.1 ISO data exploitation MS 1512-cB58. A. Salama, in collaboration with B. Schulz and S. Ott, in a team led by Coustenis (Observatoire de Paris) Cosmological APPLES: the ACS Pure Parallel Ly- continued the analysis of the ISO Titan data taken by the alpha Emission Survey SWS, ISOPHOT-S and ISOCAM instruments. The combination of these data provides Titan’s spectrum at In collaboration with J. Rhoads (STScI; PI) and others, 2.5-17 µm with resolving powers of up to 3000. The Pasquali, Pirzkal, Walsh and Cristiani have started an authors were able to detect and separate the contributions ambitious survey of high redshift Ly-alpha emitters with of most of the atmospheric gases present on Titan and to the HST-ACS. The project APPLES, the ACS Pure determine disc-average mole fractions. For the first time, Parallel Ly-alpha Emission Survey, is one of the four the ν5 band of HC3N was observed and a tentative approved ACS parallel programmes for Cycle 11 that detection of benzene was obtained (Coutenis et al., directly involves ST-ECF. Its aim is to exploit the 2003). capabilities of the grism coupled with the ACS Wide Field Channel, by acquiring deep spectroscopic In a project led by Mueller (MPE), and involving S. Ott exposures of fields at high Galactic latitude. It also takes and R. Siebenmorgen (ESO), Solar System objects advantage of the spectra extraction software and serendipitously observed in the ISOCAM Parallel Mode wavelength/flux calibrations that have been developed at are being extracted. Many asteroids and comets have ST-ECF for grism slitless spectra. The scientific return of already been found. Publications are in preparation, APPLES (which was granted 173 HST orbits) is to study including the scientific interpretation of the images and galaxy evolution and morphology at low-to-intermediate the photometry. redshifts, and to perform a census of Ly-alpha galaxies, which will be used to constrain hierarchical galaxy formation models at high redshifts. An example of Figure 2.4.1/1: The proposed evolutionary sequence APPLES data being taken is given in Fig 2.3.4. for O-rich AGB stars in their way to become Planetary Nebulae (PN). In the left panel the whole spectral range covered by SWS (2-45 µm) is shown GOODS at ESO/ECF while in the right panel just the short wavelength region is presented, in order to show in detail the most GOODS, the Great Observatories Origins Deep Survey, important features used in the analysis in this spectral is an international project that aims to unite extremely range. deep observations from NASA’s Great Observatories (SIRTF, Hubble, Chandra), XMM-Newton and the most powerful ground-based facilities, to survey the distant Universe to the faintest flux limits across the broadest range of wavelengths. Astronomers at ESO/ECF are putting a major effort into the ground-based optical/near- IR imaging and spectroscopy of the southern GOODS field, the CDF-S. Large programmes have started using the ISAAC, FORS2 and VIMOS instruments on the VLT to obtain deep J, H and Ks images and complete, magnitude limited (R < 25) low-resolution spectroscopy of sources in the field. These data, together with substantial earlier data on the field, are being made publicly available at the ESO GOODS website. sec2.qxd 3/5/03 3:38 PM Page 24

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Figure 2.4.1/2: All-sky view of ISOCAM parallel pointings in galactic coordinates. The different symbols denote different instrumental configurations.

Based on the detailed analysis of more than 300 low- used. Only five stars were found (6%) with excess above resolution IR SWS spectra at 2-45 µm in the ISO Data the photospheric flux attributed to a Vega-like disc. The Archive, P. Garcia-Lario, in collaboration with low fraction and the fact that the discs have already been J.W. Perea Calderon (VILSPA) proposed a classification identified at 60 µm indicate that the bulk emission comes scheme for stars evolving from the Asymptotic Giant from cool dust (Tdust < 120K). The study shows that Branch (AGB) to the Planetary Nebula (PN) stage warm debris discs (warmer than 120K) are relatively (Garcia-Lario & Perea Calderon, 2003). The classifica- rare. Not a single star in our sample older than 400 Myr tion was made on the basis of the detection and analysis has a warm disc, confirming earlier results that debris of: (i) gas phase features in the extended atmospheres of discs are dissipated in the first few hundred million years the AGB stars; (ii) solid-state features in the neutral of the main-sequence. An upper limit of 2 x 10–5 Earth circumstellar shells surrounding the transition objects; masses was derived for the mass of the discs that are not and (iii) nebular emission lines in the ionised PN. This detected. information, combined with the observed overall IR energy distribution in the spectral range covered by ISO R. Siebenmorgen, E. Kruegel and R.J. Laureijs (2001) SWS, was used to determine the evolutionary stage of have analysed photometry, spectro-photometry and each of the sources in the sample. The results obtained polarisation data from ISO of NGC 1808 to understand provide a complete view of the spectroscopic evolution the IR emission of nuclear regions in galaxies. The mid- expected in this short transition phase as a function of the IR polarisation map is the first of its kind of an mass of the progenitor star as the starting point for future extragalactic source. To explain the mid-IR and far-IR spectroscopic research on this field in the IR range. The polarisation synchrotron radiation and scattering from final goal of this research is to determine quantitatively large grains, PAH (Polycyclic Aromatic Hydrocarbon), the effective contribution of low-mass and intermediate- or small grain emission are ruled out. Emission by large mass stars to the chemical enrichment of our Galaxy. (>10 nm), non-spherical grains, aligned on large scales (500 pc) by uniform magnetic fields is proposed as the R.J. Laureijs, in collaboration with scientists from the major mid-IR and far-IR polarisation driver. Mid-IR ISO Data Centre and others, performed a 25 µm spectroscopy revealed a multitude of emission bands. photometric survey with ISO of a sample of 81 nearby PAH features longward of 13 µm are detected for the first main-sequence stars in order to determine the incidence time in a galaxy. The integrated absorption cross sections of ‘warm’ discs (Laureijs et al., 2002). All stars in the of astronomical PAH are derived which can be used for sample were detected by ISO. An empirical relation to future dust studies. The observations are consistently estimate the photospheric flux of the stars at 25 µm was explained by a radiative transfer model which considers sec2.qxd 3/5/03 3:38 PM Page 25

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of the observing instrument is not symmetrical, and will lead to an improvement compared with the results achieved by a classical nearest-neighbour approach.

References Coustenis, A., Salama, A., Schulz, B., Ott, S., Lell- ouch, E., Encrenaz, Th., Gautier, D., Feuchtgruber, H., 2003, Icarus, in press. Derriere, S., Ott, S., Gastaud, R., 2003, A&A submitted. Garcia-Lario, P., Perea Calderon, J.V., 2003, ESA SP-511 in press. Laureijs, R.J., Jourdin de Muizon, M., Leech, K., Sieben- morgen, R., Dominik, C., Habing, H.J., Trams, N., Kessler, M.F., 2002, A&A 387, 285. Siebenmorgen, R., Kruegel, E., Laureijs, R.J., 2001, A&A 377, 735. Figure 2.4.1/3: Cross-correlation of a sub-sample covering 14 square degrees with the 2MASS PSC. The quality enables immediate discrimination of popula- 2.4.2 Preparations for Planck tions. With the support of a small team of in-house contract staff, K. Bennett continued the development of components of the Planck Integrated Data and Informa- tion System (IDIS). This work was carried out in the small localised regions of warm dust in the immediate framework of the Planck LFI and HFI consortia, of vicinity of early-type stars (hot spots). This local heating which the Department is a member represented at Co-I gives rise to a significant contribution to the mid-IR level by Bennett. IDIS is an infrastructure that provides continuum by large grains, whereas the emission of small software components for documentation, software devel- graphites or small silicates is negligible. The model opment, process coordination (or pipeline processing) indicates that NGC 1808 is not a starburst since only (under the responsibility of MPA, Garching) and data 10% of the total luminosity comes from OB stars. This is management and access mechanisms (under the respons- supported by the observation that the optical depth in ibility of OAT, Trieste). These are to be eventually NGC 1808 is more than a factor 5 lower than in genuine federated into a single entry-point system to facilitate starbursts like M82 or NGC 253. processing and analysis of the Planck data (Hazell, Bennett & Williams, 2003). S. Ott, together with N. Schartel and R. Siebenmorgen continued to exploit the ISOCAM Parallel Mode The data analysis of the Planck mission is complicated observations. In this mode, ISOCAM observed the sky by the geographical spread of the analysis teams, which, close to the primary target of one of the three other ISO in combination with the size and the complexity of the instruments, returning one image every 25 s with 1/24th data themselves, pose challenges to the consortia in of the normal telemetry rate. Over 9000 h of such data analysis of the data in a timely manner. The complete were taken, covering 42 square degree of the sky, with up IDIS system will be available by 2004 to support the to 500 times higher sensitivity and up to 50 times higher development of processing software by the Data Pro- spatial resolution than IRAS. Sample themes for cessing Centres (DPCs) located at many sites in Europe. scientific exploitation are: Cosmology (7 µm galaxy counts), starburst and AGN, stellar populations, discs and Prototypes of the major components have been asteroid thermo-physical models. A catalogue of about developed and tested. Several are in daily use and being 16 500 mid-IR objects observed with the broadband filter operated and maintained at RSSD. Additionally, we have LW2 (centred around 6.7 µm) will be published soon. developed several applications to exercise many aspects of the IDIS concept ranging from data storage to In another collaboration, Derriere, Ott and Gastaud (2003) pixelisation methods. Prototyping of methods to use the used a novel approach for cross-identification of ISOCAM IDIS infrastructure is key to the development of IDIS and sources with reference catalogues in the optical and in the several projects have been undertaken to explore and near-IR via a probability pattern was developed. exercise both the algorithms and the IDIS concept. Compared with a classical nearest-neighbour-based cross- identification, the completeness for the selected associa- RSSD has continued to participate in laying the foundations is improved by 4%, while the reliability is boosted by tions leading to the eventual analysis of the Planck data 10%. This method could be applied to all cross- set. For example, J. Tauber and K. Bennett, in collabora- identification problems where the probability distribution tion with G. Giardino, have continued to model the sec2.qxd 3/5/03 3:38 PM Page 26

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galactic synchrotron emission and its polarisation. 2.5 Exoplanets and Stellar Environments Giardino et al. (2002) have analysed the angular power spectra of the Parkes radio continuum and polarisation Several questions related to the existence or formation of survey of the southern galactic plane at 2.4 GHz. They exoplanets have been addressed (see also Section 2.2.2). found that in the multipole range l = 40-250 the angular These include scientific activities in preparation for power spectrum of the polarised intensity is well COROT and Eddington, as well as prepatory studies to described by a power-law spectrum with fitted spectral carry out the required precursor science (e.g. studies of index αE = 2.37±0.21. In the same multipole range the exo-zodiacal dust) for Darwin. Research Group members angular power spectra of the E and B components of the participated in the continued evaluation and development polarised signal are significantly flatter, with fitted of the ground-based high-resolution echelle spectrograph spectral indices respectively of αE = 1.57±0.12 and MUSICOS. They have also continued to plan work on B = 1.45±0.12. Temperature fluctuations in the E and B developing models regarding biomarkers on Earth-like components are mostly determined by variations in planets. A large data set of HST images and spectra polarisation angle. They combined these results with collected from ground exists, covering the objects other data from available radio surveys in order to L1551, M16 (including HH216), S185 and IC1848. A produce a full-sky toy model of galactic synchrotron number of publications are under preparation, but some intensity and linear polarisation at high frequencies data still need to be reduced. (ν ≥ 10 GHz). This can be used not only to study the feasibility of measuring the Cosmic Microwave Background polarisation with forthcoming experiments 2.5.1 Study of outflows in star-forming regions and satellite missions, but it is also an input to the simulations in use by the Planck teams. M. Fridlund continued his work in studying and describing, in as much detail as possible, the energetic G. Franco and J. Tauber, together with P. Fosabla (now at processes taking place in the vicinity of forming stars. IAP, Paris), carried out detailed simulations of the The activity occurring in the close environment of a polarisation response of Planck in order to estimate the young stellar object has consequences for the interaction response to polarised signals (Franco, Fosalba & Tauber, between jets, outflows, small hot dusty discs and larger 2003). These estimates were based on a set of simulation cold (magnetised) molecular discs. This, in turn, has far- using a physical optics code (GRASP8) for linearly reaching implications for the formation of planetary polarised detectors at different frequencies and locations systems, including comets, debris discs and dust in the Planck focal plane. They studied the induced (zodiacal) clouds. A major study of the dynamic aberration on the sky polarisation signals as well as properties of a molecular disc was published during the calculating spurious polarisation introduced by the reporting period (Fridlund et al., 2002). telescope optics. For the Planck example, this was found to be of the order of 0.2%. M. Fridlund continued work together with the Stockholm star formation group. Observations were carried out with References the SEST/SIMBA (1.2 µm continuum) and with the VLT Franco, G., Fosalba, P., Tauber, J.A, 2003, A&A, in press. (UVES), both ESO facilities. The SEST data show a Giardino, G., Banday, A.J., Gorski, K.M., Bennett, K., clear indication of large grains in the disc of Beta- Jonas, J.L., Tauber, J.A., 2002, A&A 387, 82. Pictoris, indicative of large, colliding bodies in the Hazell, A., Bennett, K., Williams, O., 2003, ADASS XI, system. The VLT data are being reduced and the ASP Conference Proceedings Series, in press. interpretation is starting. Atomic gas (resonance lines) have been detected in the whole 400 AU of the Beta- Pictoris disc. The velocity pattern shows considerable 2.4.3 Sub-mm emission of extragalactic objects warping, which could be indicative of planets. This resulted in one publication in conference proceedings so P. Papadopoulos worked on sub-mm emission of far extragalactic objects, specifically on ‘Resolved nuclear CO(1-0) emission in APM 08279+5255: gravitational Reference lensing by a naked cusp?’ (Lewis et al., 2002) and ‘low- Fridlund, C.V.M., Bergman, P., White, G.J., Pilbratt, G.L., excitation gas in HR 10: possible implications for Tauber, J.A., 2002, A&A 382, 573. estimates of metal-rich H2 mass at high redshifts’ (Papadopoulos & Ivison, 2002). This work is in progress. 2.5.2 Pulsations of Beta Cephei stars References Lewis, G.F., Carilli, C., Papadopoulos, P., Ivison, R.J., A. Stankov and M. Fridlund analysed large high- 2002, MNRAS 330, L15. resolution spectroscopic material on BW Vul, the largest Papadopoulos, P.P., Ivison, R.J., 2002, ApJ 564, L9. amplitude Beta Cephei star known. These stars are B- type main sequence stars evolving off the main-sequence sec2.qxd 3/5/03 3:38 PM Page 27

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of the Hertzsprung-Russell diagram. The interesting activity-induced noise can be very effectively filtered thing about the pulsations seen in these stars (radial from the light curves, so that the proposed transit modes) is that, in general and in this case in particular, detection algorithm is quite robust, and stellar activity the atmosphere pulsates with many different velocities does not constitute a significant obstacle to detection of and in dis-equilibrium (the van t’Hooft effect). While habitable planets. As a side product, it has also been part of the atmosphere is falling inwards, new layers are shown (Favata & Aigrain, 2002) that the white-light expanding from below. As the most extreme case, BW curves that Eddington will produce for a large number of Vul shows atmospheric velocities of several hundred stars contain a wealth of information about stellar km/s, an anomalous abundance of several elements activity, so a rich harvest of science will also be produced (possibly indicative of a strong magnetic field). This by Eddington in this field. analysis is the first to include so many spectral lines, also leading to the best determination so far of the stellar References rotational velocity. The resulting paper is being Aigrain, S., Favata, F., 2002, A&A 395, 625. submitted for publication (Stankov et al., 2003), Several Carpano, S., Aigrain, S., Favata, F., 2003, A&A in press. new observing proposals have also been accepted. Favata, F., Aigrain, S., 2002, Astron. Nachr. 323, 283.

References Stankov, A., Fridlund, M., Ilyin, I., 2003, in Astero- seismology across the HR Diagram, in press. Stankov, A., Handler, G., Hempel, M., Mittermayer, P., 2002, MNRAS 336, 189.

2.5.3 Exploitation of MUSICOS

B.H. Foing and colleagues, in collaboration with members of the external community, published the results of the 1998 MUSICOS campaign. For example, the non-radial pulsation, rotation and outburst in the Be star omega Orionis were studied (Neiner et al., 2002). Foing also continued the exploitation and development of the MUSICOS collaboration. Use of the MUSICOS network is foreseen in the areas of stellar activity, circumstellar environments, stellar pulsations and preparatory activities for the COROT and Eddington missions. Upgrading of MUSICOS/Pic du Midi (NARVAL) to same status as MUSICOS/Hawaii (ESPADON) and investigation of the possibility of adding an IR channel to MUSICOS/La Palma (ESA- MUSICOS) are foreseen.

References Neiner, C. et al. (incl. Foing, B., Oliveira, J., Orlando, S.), 2002, A&A 388, 899.

2.5.4 Preparations for Eddington

One of the key goals of the Eddington mission is to detect habitable planets by the transit method. The weak and brief transit signal will be buried in a long-duration light curve with significant noise, including the intrinsic photon noise and astrophysical noise sources, the most prominent being the noise from stellar activity. Aigrain & Favata (2002) developed a novel algorithm for transit detection in light curves, based on a Bayesian approach. The algorithm has been tested (and shown to be effective) using a solar light curve from SOHO. Carpano, Aigrain & Favata (2003) have further shown that the sec2.qxd 3/5/03 3:38 PM Page 28

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2.6 Solar Physics and Seismology quencies is independent of the degree and of the mode frequency, provided that a proper scaling related to the 2.6.1 The Phoebus group: the search for g modes inertia of the mode is performed (Chaplin et al., 2001). continues Solar activity also affects the linewidth and the amplitude of the modes. Using 4 years of SOHO/LOI (Luminosity Solar gravity oscillations (the g modes) provide essential Oscillations Imager) data, Appourchaux et al. (2001) information on the physics of the solar core, where showed that the linewidth increases with solar activity, thermonuclear reactions take place. After the launch of while the mode amplitude decreases (Fig. 2.6.2); the total SOHO in December 1995, it was quickly realised that energy of the modes decreases with solar activity, imply- only a concerted effort of the helioseismic instruments of ing that the energy loss is used for generating magnetic SOHO and of ground-based observatories might enable field in active regions. With a longer data set, Appour- the detection of the elusive g-mode. This consideration chaux et al. (2002) showed that surface magnetic fields has led to the creation of the Phoebus working group could be directly detected in the splitting of the p modes which, coordinated by T. Appourchaux, involves various (modes are split by rotation, advection, magnetic fields institutes from Europe, Japan and the United States (see producing a fine frequency structure in a mode peak). also Section 4.1). The upper limit to g-mode amplitude set in 2000 to 10 mm s–1 has now been lowered using References longer time series and new detection techniques (Chaplin Appourchaux, T. et al., 2001, ESA SP-464, 71. et al., 2002), and also through the formation of a Appourchaux, T., 2002, ESA SP-508, 47. collaboration with the Institut d’Astrophysique Spatiale Chaplin, W. et al. (including T. Appourchaux), 2001, (IAS, F), responsible for the GOLF instrument data MNRAS 324, 910. (Gabriel et al., 2002) that was previously inaccessible to the Phoebus group. Fig. 2.6.1 shows the new limit sets by the Phoebus group, together with the ground-based 2.6.3 The SUMER spectral atlas of solar-disc network BiSON and GOLF (Appourchaux, 2003). This features latter limit of 3 mm s–1 is still somewhat too high for a proper detection of the g modes. A far-UV and extreme-UV (FUV, EUV) spectral atlas of the Sun between 670 Å and 1609 Å has been derived References from observations obtained with the SUMER (Solar Appourchaux, T., 2003, ESA SP-517, in press. Ultraviolet Measurements of Emitted Radiation) Appourchaux, T., Andersen, B., Berthomieu, G. et al., spectrograph aboard SOHO (Curdt et al., 2001). The 2001, ESA SP-464, 467. atlas contains spectra of the average quiet Sun, a coronal Chaplin, W. et al. (incl. T. Appourchaux), 2002, MNRAS hole and a sunspot on the disc. The spectra include 336, 979. emissions from atoms and ions in the temperature range Gabriel, A. et al. (incl. T. Appourchaux), 2002, A&A 6x103K to 2 x 106K, i.e., continua and emission lines 390, 1119. emitted from the lower chromosphere to the corona. The spectral radiances are determined with a relative uncertainty of 0.15-0.30 and the wavelength scale is 2.6.2 Solar activity and p modes accurate to typically 10 mÅ. The atlas is also available electronically. Solar activity is known to affect the frequencies of the p modes. Since this is a surface effect, the impact on the fre- More than 1100 emission lines are available in the

Figure 2.6.1: Current upper limit for GOLF (diamond), BiSON (square) and MDI (upper two curves) derived under the 10% probability limit defined by the Phoebus group in 2000. The GOLF limit is obtained by Gabriel et al. (2002) using almost 6years of data. The BiSON limit is derived for a quadruplet from Chaplin et al. (2002) using 9 years of data. The MDI limit is derived from Appourchaux et al. (2001) for 1 year of data; the upper curve corresponds to the radial displacement and the lower curve to the total displacement (radial and horizontal). The two lines at lower right are two different theoretical estimates of the g-mode amplitudes for l =1. sec2.qxd 3/5/03 3:38 PM Page 29

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Figure 2.6.2: Change of p-mode parameters as a function of mode frequency for various degrees of l obtained during the rising phase of the solar activity cycle (between 1999 and 1996). The parameters are: frequencies (top, left), linewidths (top, right), amplitudes (bottom, left), energy rates (bottom, right).

SUMER spectral range. These include resonance lines as well as previously unobserved faint intersystem lines, which can be detected by SUMER because of its low- noise detectors. Thus, the SUMER spectral atlas provides a rich source of new diagnostic tools for probing essential physical properties of the emitting plasma and studying electron densities, electron temperatures and elemental abundances throughout the solar atmosphere. In particular, the wavelength range below 1100 Å as observed by SUMER represents a significant improvement over the spectra produced in the past.

The atlas also provides an excellent reference for astrophysical applications (Fig 2.6.3). The SUMER spectrograph permits the extensive use of spectroscopic techniques in determining temperatures, pressures, Figure 2.6.3: A close-up of a selected region of the densities and velocities in the upper solar atmosphere. SUMER spectral atlas, compared with the irradiance The atlas also presents a powerful tool for the planning spectrum of Alpha Cen A from Hubble Space of future observations. Telescope (HST-STIS).

References Curdt, W. et al. (incl. P. Brekke), 2001, A&A 375, 591. sec2.qxd 3/5/03 3:38 PM Page 30

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2.6.4 Oscillations above sunspots oscillations they investigated can be seen in Fig. 2.6.4, for a single location in the sunspot umbra. Using cross- E. O’Shea, B. Fleck and co-workers have carried out an spectral analysis of Fourier spectra, time delays were analysis of time-series data obtained in sunspot umbral found between low- and high-temperature emission (e.g. regions. These data were obtained in the context of a between the TRACE 1700 emission and the CDS O V SOHO Joint Observing Program (JOP 97) in September emission). Umbral oscillations were found both inside 2000. This JOP included the Coronal Diagnostic and outside of sunspot plume locations, which indicates Spectrometer (CDS) and the Michelson Doppler Imaging that umbral oscillations can be present irrespective of the (MDI) instrument, both part of SOHO, the TRACE presence of these particular features. From a measure- satellite and various ground-based observatories. The ment of propagation speeds, obtained from the time data were analysed by both Fourier and wavelet time- delay measurements, O’Shea and co-workers proposed series analysis techniques. The CDS lines used covered that the oscillations they observed are due to slow the temperature range between the low transition region magnetoacoustic waves propagating up along the and the upper corona. From TRACE, they obtained data magnetic field lines. from the temperature minimum region to the low chromosphere. MDI was used to give ‘background’ magnetogram and white light context images. O’Shea et al. (2002) found that oscillations were present in the Reference umbra at all temperatures investigated, from the tempera- O’Shea, E., Muglach, K., Fleck, B., 2002, A&A 387, ture minimum up to the upper corona. An example of the 642.

Figure 2.6.4: Time series of TRACE and CDS data. Note that the factors by which each time series has been scaled are shown in the brackets to the right of the line identifications. Thick continuous line: bandpass filtered data (4- 7 mHz); dot-dash line: original (unfiltered) data. The analysis concentrated on two time intervals, A and B. sec2.qxd 3/5/03 3:38 PM Page 31

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2.6.5 Self-organised criticality and solar flares tion of the chromosphere. This can most clearly be seen in Fig. 2.6.6 (p.32) , in about spatial position 80 at the Over the last decade the paradigm of Self-Organised dashed line. Their calculations, based on potential field Criticality (SOC) has been considered a means of extrapolations of the line-of-sight MDI magnetogram, qualitatively understanding the heating of the solar showed that the ‘shadow’ is also co-spatial with a closed corona through the statistics of solar flare occurrence and magnetic field region that can rise to chromospheric released energies (Charbonneau et al., 2001). heights (about 1 Mm and above) and thus appear in the SUMER observations. They hypothesised that the The slope, or index αE, of the flare energy-frequency manifestation of this ‘shadow’ was due to a topological distribution determines the relevance of small and large change in the solar chromosphere and that the magnetic energy events in the overall heating budget of the solar configuration interfered with the signal formation and the corona. Only if its value is greater than 2 are small-scale passage of chromospheric waves. magnetic reconnection events (nanoflares) a viable mechanism to solve the longstanding coronal heating In collaboration with a group from the Institute of problem. Theoretical Astrophysics at the University of Oslo (N), McIntosh and colleagues used multi-dimensional X-ray flare spectra provide values of αE, for spatially magneto-hydrodynamic (MHD) simulations of stimula- unresolved flares of larger energies; they typically lie in ted oscillations in ‘realistic’ solar magnetic field the range ~1.5. Nanoflares are most likely to be observed topologies (Bogdan et al., 2002; Rosenthal et al., 2002). as small, fast brightenings in sequences of UV/EUV They have specifically studied the role played by the images (e.g. with SOHO’s Extreme-ultraviolet Imaging magnetic field on the wave modes present in an effort to Telescope; EIT), and yield αE in the range (1.5-2.3). This quantify the effects of the underlying magnetic topology wide range of values arises from the lack of knowledge on mode conversion and mixing in a stratified atmos- about the emitting volume required to convert the phere like that of the Sun. The ultimate goal of this observed brightening into a measured energy. research is to reproduce, by coupling the multi- dimensional MHD simulations with a detailed descrip- S. McIntosh and collaborators found that the avalanches tion of the radiation field, the spectral signatures in SOC models are fractal in nature with g ~ 1.41 observed by SUMER (or in two-dimensions by TRACE) (McIntosh & Charbonneau, 2001; McIntosh et al., 2002). in order to understand features like the ‘shadow’ of Using this, they computed a correction factor that could McIntosh & Judge (2001). be applied to individual model-dependent observational estimates of αE and found that the published UV/EUV- References determined values of αE could be reconciled using the Bogdan, T.J. et al. (including McIntosh, S.W), 2002, geometric scaling of SOC avalanches as an adjusting Astron. Nach. 323, 196. parameter. They found that the adjusted values of αE lie McIntosh, S.W., Judge, P.G., 2001, Ap.J. 561, 420. below, but close to, 2, in the range 1.70-1.95, and in Rosenthal, C., et al. (including McIntosh, S.W), 2002, better agreement with the spatially unresolved X-ray Ap.J. 564, 508. observations.

References 2.6.7 Asteroseismology Charbonneau, P., McIntosh, S.W., Liu, H., Bogdan, T.J., 2001, Sol. Phys. 203(2), 321. The use of helioseismology for inferring the internal McIntosh, S.W., Charbonneau, P., 2001, Ap. J. Lett. 563, structure of the Sun is soon to be applied to other stars; it 165. is in this case termed asteroseismology. RSSD has been McIntosh, S.W. et al., 2002, Phys. Rev. (E) 65, 46125. involved since the beginning in the definition of the COROT asteroseismology mission. T. Appourchaux and B. Foing are Co-Is of COROT. This CNES-led mission, 2.6.6 Magnetic interaction of waves in the supported in part by ESA for launch in November 2005 chromosphere (see also Section 3.1.6) can be seen as precursor to ESA’s Eddington. The prime scientific objectives of COROT S. McIntosh and collaborators investigated the role are to perform asteroseismology and exoplanet detection. played by the solar magnetic field in the solar For asteroseismology, five stars of magnitude less than 6 chromosphere on wave disturbances propagating through will be continuously observed for 150 d. The spectrum of the atmosphere. Using data from SOHO/SUMER and low-degree stellar p modes will be used for inferring the SOHO/MDI, McIntosh & Judge (2001) studied a feature internal structure and dynamics of these stars. In this dubbed a ‘magnetic shadow’. They demonstrated that the respect, the scientific expertise provided by helio- ‘shadow’ is co-spatial with a significant drop in emitted seismology will be of great help to COROT for reliable continuum intensity (~40%) and an almost complete frequency determination (Appourchaux, 2003). For suppression (~75%) of the characteristic 3-min oscilla- exoplanet search, 5000 stars will be monitored, which sec2.qxd 3/5/03 3:38 PM Page 32

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Figure 2.6.6: The spectroscopic timeseries (space-time) provided by the MDI (panels A & B) and SUMER (panels D-G) instruments on SOHO and TRACE (panel C). These panels are organised by the height at which the signal was formed from top to bottom and from left to right. The location of the ‘shadow’ is shown by the dotted line (originating at spatial position x = 80). The extent of the shadow, and its effect on the signal observed, is seen in panels (C-F) and varies dramatically as function of height in the atmosphere. sec2.qxd 3/5/03 3:38 PM Page 33

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2.7 Heliospheric Physics

2.7.1 Composition measurements of energetic particles above the southern solar pole by the Ulysses COSPIN/LET instrument

In November 2000, during the second southern solar polar pass, the Ulysses spacecraft reached its highest heliographic latitude at 80.2º at a solar radial distance of ~2.27 AU. In the top panel of Fig. 2.7.1, the elemental abundance ratios of carbon, nitrogen, neon and iron with Figure 2.6.7: A COROT MDPU box. Two such boxes respect to oxygen observed during this polar pass, are provide the processing power for the scientific shown. In the bottom panel of the figure, the same payload. The MDPU will be qualified in 2003. elemental abundance ratios are plotted with respect to reference values for solar energetic particles (SEPs). These ratios cluster around 1, i.e. the the majority of the particles observed at high heliographic latitudes had their origin in SEP events, which were found to be coronal may result in the detection of 40 planets in the range of mass ejection (CME)-driven shock accelerated (Hofer et 2-5 times the size of Earth. al., 2001, 2002).

The RSSD contribution to COROT consists of the Model During the current, post-maximum, phase of its mission, Data Processing Unit (MDPU) built in collaboration with Ulysses has encountered the return to more stable solar Observatoire de Meudon (Fig. 2.6.7). The MDPU is the wind stream structures, leading to the formation of central brain of COROT, managing and massaging the Stream and/or Corotating Interaction Regions (SIRs or overall data stream coming from the four CCDs.

Reference Appourchaux, T., 2003, in Asteroseismology across the HR Diagram, in press.

Figure 2.7.1: Daily averaged elemental abundance ratios (C/O, N/O, Ne/O, Fe/O) from day 250 in 2000 to day 14 in 2001 as recorded by the Ulysses COSPIN/LET instrument. Top: Absolute values together with proton intensity profile (1.2-3.0 MeV). Bottom: values with respect to the reference SEP values together with oxygen intensity (4.25- 5.25 MeV/n). The intensity profiles are represented by solid lines. The plotted error bars in the lower panel take the statistical error and the error of the SEP values into account. The triangles at the top of the panels mark the times of the flare identification (upper panel: only X-class flares; lower: X- and M- class flares). The black arrows at the bottom of the panels mark the times of the shock arrival at the Ulysses spacecraft. sec2.qxd 3/5/03 3:38 PM Page 34

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phase and a decay phase. The analysis of Hofer et al. (2003) concentrates on the decay phase. The decay of the maximum amplitude can be described by an exponential decay function The time duration and the slopes of the decay phases of different events and for different energy ranges were derived. In Fig. 2.7.2 the estimated event duration for the selected events recorded at Ulysses are plotted as a function of heliocentric distance. The event duration increases from around 10 d to about 50 d with increasing radial distances. This general trend is confirmed by adding a value averaged over the same events observed with the Uleis instrument on ACE orbiting the L1 point (1 AU).

The authors conclude that events observed father out last longer. Furthermore, higher average energy means a shorter event duration. The slope of the decay phase decreases with heliocentric distance.

The onset time interval of the SEP events, which was Figure 2.7.2: Duration of the MeV particle event usually shorter than the decay phase, has been the object recorded in the lower energy range (1.0-5.0 MeV/n) of another recent joint analysis led by S. Dalla of by Ulysses as a function of solar radial distance. The Imperial College, London (Dalla et al., 2003). average value based on ACE data (0.64-0.91 MeV/n) is added to the plot. Reference Dalla, S., Hofer, M.Y., Marsden, R.G., Sanderson, T.R. et al., 2003, Proc. Solar Wind 10, in press. Hofer, M. et al., 2003, Proc. Solar Wind 10, in press.

CIRs), in addition to the CME-associated transients. During a few occasions the composition data show 2.7.3 3He-rich events clearly the reoccurrence of compression regions, i.e. SIRs, which seem to accelerate interplanetary material A systematic survey of Ulysses COSPIN/LET pulse and do not reaccelerate the SEP particles present. A height data has identified 12 3He-rich events since the closer analysis shows that some SIRs occur within the start of the mission. These events have been defined by characteristic time delay of 26 d. These are therefore periods during which the ratio of 3He to 4He is recurrent SIRs, i.e. a CIR reappears around mid-2002. significantly greater than the Solar System value of 0.0004. The spatial distribution of the events span Reference heliocentric distances to 5 AU and helio-latitudes up to Hofer M. et al., 2001, Proc.27th Int. Cosmic Ray Conf., 50º, providing the first in situ observations of non- 8, 3116. ecliptic energetic 3He populations. Hofer M. et al., 2002, Geophys. Res. Lett. 29(16), 10.1029/2002GL014944. Figure 2.7.3 shows the Ulysses trajectory plotted as a function of heliocentric distance and helio-latitude from launch to May 2002. The second orbit is slightly 2.7.2 Propagation of solar energetic particles; displaced from the true orbit in order to separate it from analysis of the events’ decay phase the first pair of polar passages for clarity. Colour-coded along the Ulysses trajectory is the pulse height derived 4- The conditions in the interplanetary medium in the 6 MeV/n helium intensity measured by COSPIN/LET. heliosphere change on large scales with the solar cycle The 12 periods of 3He enrichments identified are labelled and on small scales with the passage of transient as events A to L. Events A-G took place during the in- phenomena, e.g. outward propagating modulation ecliptic transfer to Jupiter (launch to February 1992), and barriers, and also with heliospheric distance. In order to the remaining events (H-L) were seen during the high- achieve an insight in the changes in the interplanetary latitude phase of the mission. medium, M. Hofer and colleagues analysed the variation of the decay phases of large SEP events that are directly The 3He rich events are seen only during the active phase influenced by the conditions in space. of the solar cycle but are not associated with periods of the highest SEP intensities. There appears to be no direct The intensity-time profile of an SEP event has an onset correlation between the occurrence of these events with sec2.qxd 3/5/03 3:38 PM Page 35

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influences the location of the current sheet, how the structure of the current sheet changes with time, and how all of this propagates into the heliosphere have important implications for the propagation and acceleration of energetic particles.

Reference Sanderson, T.R., Appourchaux, T., Hoeksema, J.T., Harvey, K.L., 2003, J. Geophys. Res. in press.

2.7.5 The SEPT/IMPACT instrument on the STEREO mission

The IMPACT (In-situ Measurements of Particles And CME Transients) investigation forms part of the payload of the two STEREO spacecraft. STEREO is a NASA mission of considerable interest to European scientists. Its prime science goals address the 3D corona and solar wind structure, CME origins, CME interplanetary Figure 2.7.3: He intensity measured by COSPIN/LET evolution, solar-terrestrial coupling, solar energetic along the Ulysses trajectory. particle acceleration and the solar magnetic flux cycle.

The IMPACT investigation will perform comprehensive in situ measurements to complement the remote-sensing measurements. It will be provided by a large transatlantic any salient features in the magnetic field or solar wind, international consortium under the leadership of which (if present) might indicate particle confinement or J. Luhman (UCB, US). The Solar Energetic Particle an association with interplanetary travelling shocks. Telescope (SEPT) is being developed by RSSD in close Association of the events with solar X-rays and radio cooperation with the University of Kiel (D). emissions may provide direct evidence for a coronal origin for the 3He ions. SEPT consists of two identical units (SEPT-NS and

2.7.4 Observations of the Sun’s magnetic field during the recent solar maximum Figure 2.7.5/1: The SEPT Engineering Model. The analogue board with two PDFE ASICs is shown at T.R. Sanderson, T. Appourchaux and US colleagues have upper left. The board carries two additional ASICs on analysed a comprehensive set of solar data to show how the backside. The digital board with the FPGA (Actel the magnetic field of the Sun and the associated coronal 54SX32) on its frontside is shown at lower right. The holes varied through the last two solar cycles, and in two RAMs placed on the backside are not visible. particular the recent solar maximum (Sanderson et al., 2003).

The behaviour of the dipole term and the quadrupole term were analysed, and a new way of visualising them was developed. This shows the manner in which the dipole rotates once every 22-year cycle, and also how the quadrupole varies around solar maximum.

Combining coronal hole outline data with the magnetic field data reveals that the sites of the coronal holes move across the Sun’s disc in sympathy with the motion of the poles of the dipole, and also that when the poles of the quadrupole become apparent, the coronal holes break up into smaller, like-polarity groups of holes.

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2.8 Plasma and Gas Environment of Solar System Bodies

The structure and dynamics of the plasma environments of various bodies in the Solar System were investigated by analysing measurements collected by instruments developed with RSSD’s involvement. One of the main research activities was related to Cluster data analysis and maintaining the ESA Cluster Data Centre. The structure and dynamics of atmospheres were also investigated, including the ionospheres of Earth, Mars, Venus, Titan and comets as well as electrical properties of planetary body surfaces and their coupling with the atmosphere (Mars, Titan, comets) or with the solar wind (Mercury, Moon). In the near future, we will look to participation in the challenging BepiColombo mission. Figure 2.7.5/2: Calibration spectra obtained with the SEPT breadboard model, using the electron On the application side, the Group was concerned about conversion lines of a Bismuth 207 source. At top right, interactions between space vehicles and their environ- the position of the source with respect to the detectors ments. The main issues studied were spacecraft-plasma is represented. The green curve is related to CS1, the interaction and spacecraft charging; atmospheric centre segment of D1. The red curve shows the count electricity, winds and interaction with descent probes; rate observed in CS2, the centre segment of D2. The surface electrical properties, lander charging and lander/ blue curve is related to XT1, the cross-talk ring of D1. surface electrical interaction; effects of solar electric The K conversion lines are nicely resolved (FWHM propulsion. ~27 keV). The different lines are also visible in CS2, shifted by ~110 keV, the average energy deposited by electrons that traverse D1. 2.8.1 Cluster-related research

Observations in the mid-altitude cusp

SEPT-E). Four detectors are used in two opposite P. Escoubet, M. Fehringer, H. Laakso, A. Masson and oriented telescopes, either in north-south (NS) or ecliptic external collaborators worked on Cluster observations in (E) orientation. SEPT uses a miniaturised electronics the polar cusp. The polar cusp is a huge funnel in the based on a Mixed Analogue/Digital Application Specific Earth’s magnetic field where particles from the Sun can Integrated Circuit (ASIC) which has been developed enter directly and reach the atmosphere. There is under the ESA General Support Technology Programme. typically one cusp in each hemisphere. Some theoretical Each telescope is made up of 300 µm-thick PIPS studies predicted a few years ago that the polar cusp detectors (D1 and D2 provided by the University of Kiel could sometimes split, giving rise to a double cusp. Such as well as the housing) with guard rings and cross-talk an example was found and analysed by P. Escoubet and rings. One Particle Detector Front-End (PDFE) collaborators. integrated circuit is used to analyse the signal from D1, using the guard ring in anti-coincidence. A second PDFE When the Cluster orbit has its apogee on the nightside, is used to analyse the signal from D2 in anti-coincidence the spacecraft cross the mid-altitude polar cusp with its guard ring. Furthermore, anti-coincidence successively as a ‘string of pearls’ (left panel of signals between D1 and D2 ensure that an exclusive Fig. 2.8.1/1) and therefore temporal changes can be ‘OR’ function is performed, i. e. only stopping particles measured, for the first time observed by spacecraft. are analysed. In a special calibration mode, this exclusive During this cusp crossing three spacecraft (SC1, SC2, ‘OR’ is inhibited in order to use minimum ionising SC4) were a few minutes apart, while SC3 lagged by particles for on-station calibration. The resolution on the about 45 min. The right panel of Fig. 2.8.1/1 shows the full range of energy (2.2 MeV for protons) is 8 bits, ion precipitation in the cusp observed by three spacecraft limited on board to 5 bits, logarithmically scaled for at altitudes of 4-6 RE. The polar cusp is characterised by telemetry reasons. the decrease of the energy of the ions as the spacecraft moved poleward (typical for IMF Bz negative). SC4 and The development of the instrument is well underway SC1 observed approximately the same ion dispersion, (Figs. 2.7.5). The Critical Design Review was recently although it was seen longer by SC1, whereas SC3 held; the Engineering Model is being assembled in observed a double dispersion. First there was a decrease house. The critical ASIC has now been evaluated and in energy of the ions for about 30 min and then a second shown to be capable of reaching the required noise level. decrease (starting around 1645 UT) lasting about 45 min. sec2.qxd 3/5/03 3:38 PM Page 37

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Figure 2.8.1/1: Crossing of the mid-altitude cusp (around 5 RE altitude) successively by the Cluster spacecraft on 30 August 2001. The positions of the spacecraft are shown in the left panel and the ion precipitation measured by CIS on SC4, SC1 and SC3 are shown in the right panel.

Since the four spacecraft were almost at the same local plasmasphere, the plasma drift changes from co-rotation time, this observation is clearly a temporal effect. into convection. The geomagnetic-field-aligned outer Something changed around 1645 UT that reconfigured boundary of the plasmasphere, which separates these two the polar cusp and moved it poleward. The IMF had a plasma regimes, is usually called the plasmapause. negative Bz component during the interval with a strong By component. However, an excursion to Bz positive was Various Very Low Frequency (VLF, 3.0-30 kHz) and observed around 1645 UT, which most likely produced Extremely Low Frequency (ELF, 0.3-3.0 kHz) waves the motion of the cusp. propagate in the vicinity of the plasmapause, and in particular near the geomagnetic equator, in a mode of A simulation of the magnetosphere by a magneto- propagation called the whistler mode (whistlers, hiss, hydrodynamic code will be compared to the data to better chorus). These waves, through wave-particle inter- understand these temporal events in the cusp. This actions, can scatter radiation belt electrons from their example clearly demonstrates the Cluster capabilities to orbits. These electrons may precipitate in the upper observe how the polar cusp is moving and changing atmosphere and create auroras. As a consequence, the according to external solar wind changes. localisation of their source regions, their propagation, occurrence and dependence upon the geomagnetic activity are fundamental issues. Moreover, these waves VLF and ELF waves near the plasmasphere are also observed in the plasmaspheric region of other planets of the Solar System (e.g. Jupiter, Saturn, The Earth’s plasmasphere is an inner magnetospheric Neptune). region located above the ionosphere, which typically extends out to L = 3-6, depending on the magnetospheric The Cluster mission provides excellent opportunities to activity. Its topology can be seen as a toroidal belt around study whistler mode waves as the spacefleet crosses the the Earth where the density is relatively high equatorial plane, in the vicinity of the plasmapause, at (>100 cm–3), compared to the outer tenuous magneto- each perigee pass. Both the WBD and WHISPER spheric plasma (few cm–3). Near the outer region of the experiments show a variety of structured ELF and VLF sec2.qxd 3/5/03 3:39 PM Page 38

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Figure 2.8.1/2: Top panel: plasma frequency deduced from WHISPER below 80 kHz and from the EFW spacecraft potential measurements above 80 kHz on 5 June 2001 between 2145 UT and 2335 UT. Middle panel: WHISPER electric field spectrogram. The hiss-like emissions are well ducted inside the electron cavities (see dotted lines). Bottom panel: high-resolution WBD data corresponding to a shorter time interval. sec2.qxd 3/5/03 3:39 PM Page 39

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emissions in this region. Research conducted at RSSD by O. Moullard, H. Laakso and A. Masson in collaboration with external colleagues, allowed the identification of a new whistler mode wave called banded-hiss emission (BHE) at frequencies below the electron cyclotron frequency but above the lower hybrid resonance frequency (Moullard et al., 2002). The new method employed in this case study allows extraction of the electron density from the spacecraft potential, measured by the electric field instrument EFW, and the active measurement of the density by the WHISPER relaxation sounder. Results from this case study are displayed in Figure 2.8.1/2.

A statistical survey has since been conducted and identified around 30 cases in Cluster data. This survey showed that 1) the location of these waves is strongly correlated with the position of the plasmapause, 2) their central frequency varies from 2 kHz to 10 kHz, with a 1- 2 kHz bandwidth, depending on the geomagnetic activity (Kp), (3) their magnetic latitude is included in the [–20°, 20°] range and 4) these waves are sometimes guided in Figure 2.8.1/3: Electron density measured by large detached density structures. The unique Cluster WHISPER given as a function of the spacecraft to facility of multi-point measurements has been probe potential difference, Vs-Vp, derived from EFW systematically used to estimate the spatial extent and the observations. A similar relationship is shown for temporal behaviour of these waves. Moreover, when comparison, from the Polar satellite (Pedersen et al., these waves reach frequencies below 4 kHz, the analysis 2001). of the STAFF experiment data reveals that they are of the whistler mode type, escaping from the geomagnetic equator.

Reference before. Preliminary calibrations against other density Moullard, O. et al., 2002, Geophys. Res. Lett. 29(20), measurements on Cluster has been done and more 1975. detailed investigations will be performed in the future.

Figure 2.8.1/3 presents Cluster measurements for the High time resolution measurements of electron density electron density vs. spacecraft potential relationship. The by the EFW experiment data are collected in various magnetospheric regions, and a good relationship appears between these two For accurate measurements of electric fields, the Cluster- parameters. EFW spherical double probes are electronically controlled to be set at a positive potential of Reference approximately 1 V relative to the ambient magneto- Pedersen, A. et al. (incl. Escoubet, C.P., Laakso, H.), spheric plasma. The spacecraft itself acquires a potential 2001, Ann. Geophys. 19, 1483. that balances photoelectrons escaping to the plasma and the electron flux collected from the plasma. Spacecraft potential control with ASPOC The probe-to-spacecraft potential difference can be measured with a time resolution of a fraction of a second. M. Fehringer and P. Escoubet were involved in the It provides information on the electron density over a operations of the ASPOC instrument on Cluster. The wide range from the lobes (~0.01 cm–3) to the objective of this instrument is to move the spacecraft magnetosheath (>10 cm–3) and the plasmasphere potential near the plasma potential in order to perform (>100 cm–3). low-energy ion and electron measurements. The Cluster spacecraft potential varies from a few volts positive in This technique has been calibrated against other density the magnetosheath to 50-60 V in the tenuous magneto- measurements on GEOS, ISEE-1, CRRES, Geotail and spheric lobes. When the potential reaches high values, Polar. The Cluster spacecraft potential measurements, the ions below that energy can no longer be measured open for new approaches, particularly near boundaries and the low-energy electrons are accelerated to the value and gradients, provide information never obtained of the spacecraft potential. ASPOC can reduce the sec2.qxd 3/5/03 3:39 PM Page 40

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concerning Earth’s space environment and how it responds to energy and momentum transfer, both in response to the solar wind, as well as to internal sources, such as the ionosphere.

Although the electron density in the magnetosphere is known in a general sense from case studies, large-scale, systematic studies of the electron density distribution in the magnetosphere have been performed only a few times in the past. Consequently, the models of the magnetospheric plasma density are much poorer than those for the magnetic field. The latter have been under development for many decades and have benefited from the fact that almost every scientific satellite in the magnetosphere has carried a magnetometer. Figure 2.8.1/4: X component of the electric field, measured by the EFW (red) and EDI (black) Plasma density measurements are more difficult to obtain instruments on Cluster 1 and 3 (courtesy M. Andre in a systematic sense from a single instrument, since the and G. Paschmann). plasma density and temperature might typically vary over several orders of magnitude. There are a number of techniques for measuring the total plasma number density, but each technique has its own limitations. spacecraft potential typically to around 8 V or lower by Spacecraft charging seriously limits the direct detection emitting a beam of indium ions. of low-energy charged particles and must be taken into account for a variety of instruments. Furthermore, Under certain conditions, such as intense cold photoelectrons and secondary electrons can cause a ionospheric outflow events in the polar cap, a wake significant increase. parallel to the magnetic field can appear due to high spacecraft potential, which can perturb electric field Using spacecraft potential measurements of the Polar measurements with wire booms. Fig. 2.8.1/4 shows the electric field experiment, H. Laakso and colleagues have electric field measurements by two complementary investigated electron density variations of key plasma methods: with wire booms (EFW) and an electron gun regions within the magnetosphere, including the polar (EDI). The electron gun is not influenced by the cap, cusp, trough, plasmapause and auroral zone, spacecraft potential since electrons have a much higher attempting to model how the electron density varies in energy (1.5 keV) than the spacecraft potential, and the space under various conditions. The research in this area wake cannot affect the motion of the energetic electrons. has been very active, which is reflected in a series of It is clearly seen that the two methods agree very well publications. when ASPOC is turned on (after 04:23 UT on Cluster 3). The agreement is not good on Cluster 1, where ASPOC References is not operated. In most regions, however, the agreement Janhunen, P. et al., 2001, Adv. Space Res. 28 (11), 1575. between the two methods is good even when ASPOC is Janhunen, P. et al., 2002, Ann. Geophys. 20, 1743. off. Further work is therefore needed to better understand Laakso, H., 2002, J. Atmos. Sol. Terr. Phys. 64, 1735. the situations where the wire boom measurements may Laakso, H. et al., 2001, J. Atmos. Sol. Terr. Phys. 63, not be applicable. 1171. Laakso, H., Grard, R., 2002, Space Weather Study Using Reference Multi-Point Techniques, COSPAR Coll. Ser., p.193. Torkar, K. et al. (incl. Escoubet, C.P., Fehringer, M.), Laakso, H. et al., 2002a, Ann. Geophys. 20, 1711. 2001, Ann. Geophys. 19, 1289. Laakso, H. et al., 2002b, Ann. Geophys. 20, 1725. Palmroth, M. et al., 2001, J. Geophys. Res. 110, 21109.

2.8.2 Electron density distribution in the Earth’s magnetosphere 2.8.3 Plasma and wave phenomena induced by neutral gas releases in the solar wind The total electron number density is a key parameter needed for both characterising and understanding the H. Laakso and colleagues have investigated plasma and structure and dynamics of the magnetosphere. The wave disturbances generated by nitrogen (N2) gas spatial variation of the electron density and its temporal releases from the cooling system of an IR-camera of the evolution during different geomagnetic conditions and Vega 1 and Vega 2 spacecraft, during their flybys of seasons reveal numerous fundamental processes Comet Halley in March 1986. N2 molecules were ionised sec2.qxd 3/5/03 3:39 PM Page 41

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sensor mounted on a short boom. The comparison between the model and observations suggests that the gas expanded as an exhaust plume, and approximately only 1% of the ions could escape the beam within the first few metres. The releases were also associated with significant increases in wave electric field emission (8 Hz - 300 kHz); this phenomenon lasted for more than 1h after the end of the release, which was most likely due to the temporary contamination of the spacecraft surface by nitrogen gas. DC electric fields associated with the events were complex. No magnetic field perturbations were detected, suggesting that no significant diamagnetic effect (i.e. magnetic cavity) were associated with these events.

Similar measurements will be performed by the SPEDE experiment on the SMART-1 satellite during the operations of the solar electric propulsion thrusters (see Section 2.8.5).

Reference Laakso, H. et al., 2002, Ann. Geophys. 20, 1.

2.8.4 Instrument developments

Rosetta Mutual Impedance Probe (MIP) and Langmuir Probe (LAP)

The scientific payload of the Rosetta Orbiter includes an integrated plasma package (RPC) of six instruments. RSSD is collaborating on two of these instruments: the Mutual Impedance Probe (hardware development, mission operations and data analysis), and the Langmuir Figure 2.8.3: Summary of the plasma and wave Probe (data analysis). The performance of MIP and its disturbances observed during the gas releases by preamplifiers was characterised over the whole opera- Vega 1. The quantities are, from top to bottom, signals tional expected temperature range (–120ºC to +120ºC) as measured with the electric antenna in the frequency part of the calibration activities. range 8 Hz - 300 kHz, the square of the electric field integrated over the whole frequency range, the The objectives of MIP and LAP are to study the plasma electron current collected by a Langmuir probe, DC environment of the diamagnetic cavity surrounding the electric field, and potential difference between a comet nucleus. Both instruments will cover, in a biased electric field probe and the spacecraft (Laakso complementary way, the variation of the cold plasma et al., 2002). population in equilibrium with the neutrals.

MIP is a collaboration with LPCE, Orleans (PI: J.- G. Trotignon; RSSD Co-Is: J.-P. Lebreton, R. Grard, by solar UV radiation at a rate of ~7 x 10–7 s–1 and gave H. Laakso; technical support was provided by rise to a plasma cloud expanding around the spacecraft. U. Telljohann and B. Johlander). LAP is a collaboration Strong disturbances owing to the interaction of the solar with IRF, Uppsala (PI: A. Eriksson; RSSD Co-Is: + wind with the N2 ion cloud were observed with the J.-P. Lebreton and R. Grard). plasma and wave experiment (APV-V instrument). Fig. 2.8.3 summaries the plasma and wave phenomena observed by the Vega 1 spacecraft. The SESAME Permittivity Probe on the Rosetta Lander

Three gas releases studied are accompanied by increases The Permittivity Probe (PP) is part of the Surface Elec- in cold electron density and simultaneous decreases of trical, Seismic and Acoustic Experiment (SESAME). the spacecraft potential. This study shows that the This experiment consists of a variety of sensors to spacecraft potential can be monitored with a reference monitor electric, acoustic and seismic properties of the sec2.qxd 3/5/03 3:39 PM Page 42

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subsurface layers of Rosetta’s target comet nucleus in situ as well as the dust flux falling back to the surface. The PP instrument consists of six sensors. Five are dedicated to measuring the permittivity properties: two are receivers and three transmitters. Three sensors are placed under the three Lander feet and the other two on the MUPUS and APX sensors. The PP measurements will be used to monitor the water-ice content and temperature of the surface layer.

The sixth PP sensor is a simple Langmuir probe that monitors the electron flux variations just above the comet’s surface. This measurement can be used to monitor the level of nucleus activity. Similarly, the plasma wave activity can be observed with the two receivers placed on the Lander feet.

The responsibility of RSSD was to develop the sensors Figure 2.8.4/1: The ASPOC emitter on Double Star. for the PP instrument as well to participate in the determination of the instrument specifications and the calibration of the permittivity measurements. The PP hardware was delivered in the summer of 2002. ASPOC on Double Star

PP is a collaboration with the Finnish Meteorological RSSD contributes mechanisms, the box, harness and Institute (FMI; PI: W. Schmidt). RSSD Co-Is are expertise in ion emitter development and in-flight R. Grard, H. Laakso and R. Trautner; engineering operations to ASPOC on the equatorial satellite of the support was provided by B. Johlander. Chinese Double Star mission for launch in December 2003. Triggered by the experience gained during almost 2 years of operating ASPOC on Cluster, the ion emitter The Spacecraft Potential, Electron Flux and Dust module was modified to improve protection against (SPEDE) experiment on SMART-1 emitter cross-contamination. The cover opening mechanism had to be redesigned to fit the change to a The SPEDE experiment consists of two Langmuir probes European-supplied pyro-actuator. Fig. 2.8.4/1 shows a and an electronics unit. The experiment is designed to computer-generated illustration of the ASPOC emitter on monitor in real-time large ion flux variations expected Double Star. during the operations of the solar electric propulsion thrusters on the SMART-1 spacecraft. In addition to ion ASPOC is a collaboration with the Space Research and electron measurements, the experiment can also Institute of the Austrian Academy of Sciences, Graz (PI: monitor low-frequency (10-1000 Hz) plasma waves first K. Torkar; RSSD Co-Is: M. Fehringer and P. Escoubet). around the Earth and later around the Moon, the final target of the SMART-1 mission. Segmented Langmuir Probe on Demeter The main responsibility of RSSD was to develop two lightweight carbon fibre booms for the experiment. The RSSD has developed a multi-collector Segmented electric sensors are placed at the end of these 60 cm Langmuir Probe (SLP). This sensor will be flown for the stationary (i.e. no deployment mechanism) booms. first time in early 2004 on the French Demeter mission, RSSD also participated in the calibration of the the first in the CNES microsatellite programme. experiment by running several tests in its plasma Demeter’s scientific objectives are to study the electro- chamber. The SPEDE hardware was delivered in the magnetic emissions and the ionospheric perturbations autumn of 2002. associated earthquakes and volcanic activity. The mission is developed under the PI M. Parrot, CNRS/ SPEDE is a collaboration with the Finnish Meteor- LPCE (Orleans, F). ological Institute (FMI; PI: A. Mälkki). RSSD Co-Is are R. Grard and H. Laakso; engineering support was The Demeter Langmuir Probe (ISL: Instrument Sonde de provided by B. Johlander. Langmuir) is a miniaturised 8-channel instrument consisting of a classical cylindrical Probe and a small References spherical Langmuir Probe (Fig. 2.8.5/3). Demeter will Laakso, H., Foing, B., 2001, ESA SP-476, 601. provide an excellent opportunity to demonstrate the SLP Tajmar, M. et al., 2002, Planet. Space Sci. 50, 1355. concept. The instrument was delivered for integration in sec2.qxd 3/5/03 3:39 PM Page 43

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equipment responds to real targets, even if at a different composition and a lower temperature than on Titan. A. Piot, H. Svedhem and J.-P. Lebreton are taking part in these activities.

Quadrupolar Probe development

The measurement of the electric properties of surface materials is an important issue for planetary space missions. RSSD has contributed to Quadrupolar Probes (QPs), which are part of the Huygens HASI instrument and the Rosetta Lander PP instrument. The RSSD group (R. Grard, R. Trautner, F. Simões) is also investigating further development of this sensor that may become ubiquitous on future planetary lander/surface missions. New QP architectures may include subsurface instru- Figure 2.8.4/2: Demeter ISL in flight configuration ments and the employment of mobile platforms, allowing with the connector saver. new applications such as the investigation of buried structures and the detection of subsurface water (Trautner & Simões, 2002). In order to meet the requirements of future missions, RSSD is supporting prototype the payload in May 2002. A preliminary version of the developments and computer modelling of new QP data analysis software was delivered from IAP to RSSD architectures. in November 2002. Reference ISL is one of the five instruments of the scientific Trautner, R., Simões, F., (2002), ESA-SP 518, 319-322. payload. ISL is developed under RSSD responsibility (J.-P. Lebreton, Co-I; D. Klinge, Instrument Manager) in collaboration with the Institute of Atmospheric Physics (IAP of Prague, Czech Republic), LPCE (F) and the Observatoire de Paris (Meudon, F).

The Huygens radar altimeter

The radar altimeter on Huygens has a dual function. Firstly, it provides the instantaneous distance to the Titan surface during the descent, information used by several instruments to change modes during descent and as post flight reference for the data analysis. Secondly, its RF return signal from the surface contains scientific information on the topography and the permittivity of the surface. This information is extracted by dedicated electronics, developed by RSSD, within the Permittivity, Wave and Altimetry (PWA) unit of the HASI instrument. To further enhance the confidence in the operation of the radar and to improve the understanding of the scientific applications, preparations for further testing started during 2002. This will include the use of the SM2 Huygens probe mock-up with the flight spare models of the radar altimeters for sky tests and interference checks. During 2003 and 2004, helicopter and/or a stratospheric balloon test may be carried out on the same combination. A previous balloon flight in Spain in 1995 and a helicopter flight in Tucson in 1996 showed the great potential of these field tests. The results obtained led to significant improvements to the flight hardware. With the new tests we want to study how the new flight-identical sec2.qxd 3/5/03 3:39 PM Page 44

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2.9 Comparative Planetology and Astrobiology

2.9.1 Comparative planetology of Earth-like planets and moons

Comparative planetology is a core study area and is part of the preparations for scientific exploitation of ESA’s upcoming planetary missions. More fundamentally, comparative studies are key to the continuing advance of our scientific knowledge of the Earth and Solar System. Studies of the Moon, Mars, Venus and Mercury provide unique opportunities to understand the processes and factors that have shaped our own planet. Similarly, the processes involved in geological and climatic evolution on a planetary scale can only be understood through comparisons of these features on all of the inner planets. SMART-1, Mars Express, Venus Express and Bepi- Colombo offer research opportunities for comparative planetology. This motivated the Department to organise in 2002 the 36th ESLAB Symposium on Earth-like Planets and Moons (see Section 4.1). RSSD staff presented review papers on the missions to different planetary targets and on scientific thematic topics. Figure 2.9.1: Earth-like planets and moons, targets References for comparative planetology (Chicarro, 2002). Chicarro, A., 2002, ESA SP-514, 21. Foing, B.H., Battrick, B. (eds), 2002, ESA SP-514. Foing, B.H., ILEWG, 2002, ESA SP-514, 3. Foing, B.H. et al., 2002, ESA SP-514, 345. lunar volcanism related to the thermal and physical Grard, R., Laakso, H., Svedhem, H., 2002, ESA SP-514, evolution of the Moon, and the detailed geological study 25. of large impact craters and crustal stratigraphy. Both Koschny, D., Marini, A., Hoofs, R., Almeida, M., 2002, applications use the mineralogical and chemical data sets ESA SP-514, 89. provided by the Clementine and Lunar Prospector missions.

2.9.2 Lunar research and SMART-1 exploitation For volcanic studies, large-scale mapping of the southern Oceanus Procellarum region was completed (Heather & The Moon bears the scars of countless impact craters and Dunkin, 2002a). In this work, techniques have been holds the only accessible record of the conditions in the developed from which spectrally distinct mare basalts Earth-Moon system over the past 4.5 billion years. The can be mapped, and estimates of basalt thickness active geology and climate have long since destroyed the obtained. A total of 13 basalts was recognised in the early record of these events on the Earth, so the Moon is region, 10 of which are spectrally distinct, and three of critical to our understanding of the early history of our which represent previously unrecognised members of the planet. The recent Clementine and Lunar Prospector Oceanus Procellarum stratigraphic group. The average missions to the Moon provided the first views of global thickness of the basalts is between 160 m and 625 m, geochemistry. The SMART-1 mission will add our first ranging from tens to hundreds of metres near the global IR dataset on minerals olivine and pyroxenes mare/highland boundaries and consistently greater than across the surface, and the first global measurements in several hundred metres closer to the centre of the mare. X-ray fluorescence, which will allow for the mapping of This represents 8-32% of the total volume of basalts in elemental Mg. These are critical to our understanding of Oceanus Procellarum (Fig. 2.9.2/1). the Moon’s crustal evolution and origin, which is intrinsically linked to the early evolution of the Earth (Foing et al., 2001). In addition to the large-scale study, special focus has been applied to the Marius Hills region, for which spectrally distinct flows have been mapped for the first Analysis of Clementine data time using photographic and Clementine multispectral data (Heather et al., 2003). The basalts on the plateau are The lunar research performed by D. Heather and varied in age and composition, but are dominated by a collaborators had two primary applications: the study of young high-titanium basalt. sec2.qxd 3/5/03 3:40 PM Page 45

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The Asteroid Moon micro-Imager Experiment (AMIE) on SMART-1

AMIE, the imaging experiment of SMART-1, is built around a very compact camera cube featuring a 1024 x 1024-pixel CCD, read out with 10-bit dynamical range. The camera has an f/10 objective lens with a focal length of 140 mm. A set of colour filters is hard-mounted directly to the CCD for mineralogical imaging. D. Kos- chny is Co-I of the investigation, led by J.L. Josset, Neuchatel (CH). RSSD was responsible for the environmental testing and the optical calibration of the camera.

A thorough optical calibration of the Flight Model was performed before delivery in the beginning of 2002. This calibration included dark-current measurements, flat- fielding, geometrical distortion and straylight tests. The camera performs well. Absolute calibration is planned during the cruise phase using standard stars.

Following completion of the calibration report and of the input to the PI team for the in-flight calibration, a set of routines using the software tool IDL will be provided to the AMIE science team. The help of M. Almeida is greatly acknowledged. The support of J. Zender, the Planetary Data Archiving Manager, was essential to ensure that the image format is compatible with the Figure 2.9.2: A TiO2 map of the southern Oceanus standard of the Planetary Data System. Procellarum, constructed using multi-colour Clemen- tine data (Heather & Dunkin, 2002a). 2.9.3 Mars research

Mars Express exploitation

Impact crater studies have focused on King, a large A. Chicarro, B.H. Foing, P. Martin and H. Svedhem are impact structure on the lunar farside (120ºE, 5.5ºN). Both preparing for the participation in scientific exploitation Clementine multispectral and photographic data sets of Mars Express. Much remains to be understood about have been used to investigate the crustal stratigraphy and the precise identity and form of the surface constituents geology in the region (Heather & Dunkin, 2003). The and to constrain physical, weathering/alteration and surrounding area of the lunar crust was also studied for a climatic processes on Mars. Analysis of data from the more regional perspective, including the Al-Khawrizmi- High Resolution Stereo Camera (HRSC) will allow for King/Tsiolkovsky-Stark region of the farside (Heather & comprehensive investigations of geological, atmospheric Dunkin, 2002b). The Clementine data show a varied and topographic features on Mars. The analysis of radar surface composition between the two sites, highlighted data will allow for subsurface sounding and the detection by the FeO content of the highland soils, which contain a of liquid or water ice. relatively high iron abundance at King in comparison to Tsiolkovsky. Conversely, on a vertical scale, the highland Martin et al. (2002) have prepared for this a programme crust appears to show a matching trend of increasing that will use data from the HRSC and from the OMEGA feldspar content with depth. imaging spectrometer. This programme is to characterise the full range of spectral, compositional and mineral- References ogical diversity of Mars; to correlate mineralogical, Foing, B.H. et al., 2001, Earth Moon & Planets 85, 523. compositional and geomorphological information; to Heather, D.J., Dunkin, S.K., 2002a, Planet Space Sci. define the roles played by weathering, mixing and 50(14-15), 1299. alteration of the soils; and to determine the implications Heather, D.J., Dunkin, S.K., 2002b, Planet. Space Sci. for future missions an landing sites. 50(14-15), 1311. Heather, D.J., Dunkin, S.K., 2003, Icarus in press. Maps for the Beagle-2 Isidis landing site were produced Heather, D.J., Dunkin, S.K., Wilson, L., 2003, J. Geo- from a compilation of existing scientific datasets phys. Res., in preparation. (Fig. 2.9.3/1). sec2.qxd 3/5/03 3:40 PM Page 46

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Figure 2.9.3/1: Topography of eastern Isidis Planitia highlighting the low relief features of the region. Beagle-2 landing ellipse shown in white (MOLA data, detrended over 1°; G. Michael, private communication).

Figure 2.9.3/2: Modelling results of the composition of the lower ionosphere of Mars (Witasse et al., 2001).

attenuation of HF radio waves has been evaluated. The model predicts a layer of metallic ions and electrons at around 80 km height. Typical densities are 104 cm–3 during the daytime (Molina-Cuberos et al., 2003). The one-way attenuation can reach 50 dB for a 5 MHz radio wave (Witasse et al., 2001). Our work will be applied to the interpretation of the Mars Express ionosphere measurements. Fig. 2.9.3/2 shows an example of modelling results of the composition of the lower ionosphere of Mars.

References Molina-Cuberos, G.N. et al. (incl. O. Witasse, J.-P. Le- breton), 2003, Planet. Space Sci. submitted. References Witasse, O. et al., 2001, Geophys. Res. Lett. 28, 3039. Chicarro, A., 2001, LPI 32, 1044. Martin, P. et al., 2001, LPI 32, 1575. Martin, P., Chicarro, A., 2002, LPI 33, 1495. 2.9.4 Impact cratering processes Martin, P. et al., 2002, ESA SP-514, 73. A most common geological process in the Solar System is impact cratering. Greater understanding of the impact Mars meteoritic layer modelling process and the resulting crater’s morphology and geological nature will enhance the science that can be The meteoric influx into a planetary atmosphere deposits derived from remote-sensing data on the depths, diameters a metallic ion layer. In the context of the future Mars and stratigraphy exposed by impact craters on other missions, the influence of such a layer at Mars on the terrestrial planets. A. Chicarro and collaborators (2003) sec2.qxd 3/5/03 3:40 PM Page 47

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have investigated statistics of Earth impact craters, and Search for large organics in space and diffuse inter- have started using Envisat and other satellite data to look stellar bands for new and catalogue known impact craters on preserved paleo-surfaces on Earth. G. Michael (2003) has developed Polycyclic aromatic hydrocarbons (PAHs) are believed algorithms to recognise crater structures on Mars within to be the most abundant free organic molecules and the Mars Global Surveyor MOLA altimetry data. remarkably stable in space. PAH molecules are produced partly in the outer atmospheres of carbon stars, or formed The Chicxulub crater in the Yucatan Peninsula, Mexico is by shock fragmentation of carbonaceous solid material. among the largest impact craters on our planet, with a PAHs are also identified in meteorites and interplanetary diameter greater than 200 km. Owing to the pristine state dust particles (IDPs). The polyhedral geometry of C60 of its ejecta blanket, it presents a unique opportunity to fullerene was discovered in 1985. The presence of soot study large impact craters processes in situ. A. Ocampo material in carbon-rich stars, the spontaneous formation and collaborators have examined the evidence for fluid- and the remarkable stability of the fullerene cage ised ejecta emplacement by the Chicxulub impact (Pope suggested the presence of fullerene compounds in et al., 2003). The Yucatan Peninsula was rich in volatiles interstellar space. In the 1990s fingerprints of the C60+ at the time of impact (65 Myr ago). Models predict that ion were confirmed in the near-IR which indicates that about 2-4% of the impact vapour plume was composed fullerenes can play an important role in interstellar of CO2, SO2, and H2O produced from the carbonate, chemistry. B.H. Foing, N. Boudin and collaborators have sulphate and water in the target rocks. The impact searched for other diagnostics of fullerenes or PAH occurred in a shallow sea, hence there was abundant molecules (Ruiterkamp et al., 2002; Boudin, 2002). It is surface water that may have mixed with the ejecta. Since now crucial to understand the formation, evolution of the Earth has a thick atmosphere, ejecta emplacement, organics and their transport to planetary surfaces as especially in the outer parts of the ejecta blanket and ingredients for prebiotic chemistry (Ehrenfreund et al., beyond, was no doubt affected by atmospheric drag. 2001).

References The problem of Diffuse Interstellar Bands (DIBs) is one Chicarro, A., Michael, G. et al., 2003, ESA Bulletin, of the oldest unsolved of modern astronomy. Following submitted. their very successful work in the 1990s, B. Foing and Michael, G., 2003, Planet. Space Sci., submitted. collaborators have looked with an ESO-VLT observing Pope, K.O. et al. (incl. A. Ocampo), 2003, Science, run (four nights in September 2001) at the Magellanic submitted. clouds (Fig. 2.9.5/1) to see the effect of low metallicity in

2.9.5 Contributions to astrobiology Figure 2.9.5/1: Discovery of Diffuse Interstellar Dense interstellar clouds are the birth-sites of solar-mass Bands in the Magellanic clouds (ESO-VLT data). stars and their planetary systems. Interstellar molecules and dust become the building blocks for protostellar discs, from which planets, comets, asteroids and other macroscopic bodies eventually form. Observations at IR, radio, mm and sub-mm ranges show that a large variety of gas-phase organic molecules are present in the dense interstellar medium. Organic molecules evolve from their formation in molecular clouds to their incorporation into the early Solar System. Large carbon-bearing species, such as polycyclic aromatic hydrocarbons (PAHs) and fullerenes as well as carbonaceous solids have been identified in the interstellar medium, in comets, meteorites and planetary environments. Current and future ESA space missions can make a key contribution to astrobiology (Foing, 2002). The knowledge of organic chemistry in molecular clouds, comets, meteorites and planets and their common link provides constraints for the processes that lead to the origin, evolution and distribution of life in the Galaxy.

Reference Foing, B.H., 2002, in Astrobiology. The Quest for the Conditions of Life, Springer, p.389 sec2.qxd 3/5/03 3:40 PM Page 48

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the formation of complex organic compounds References (Ehrenfreund et al., 2002). They are continuing the Ruiterkamp, R., Ehrenfreund, P., Foing, B.H., Salama, F., analyses of the VLT data, and of the WHT, CFHT and 2001, ESA SP-496, 137. ISO spectroscopic data of PAH features. They have Ruiterkamp, R. et al. (incl. B.H. Foing), 2002, NASA reviewed reasons why fullerenes could be detected, Laboratory Astrophysics Workshop, 77. while PAH electronic absorption signatures in the DIB spectra have remained elusive. Exobiology preparation for Mars Express: Mars References simulation chamber studies Boudin, N., 2002, ESA SP-518, 37. Ehrenfreund, P., O’Tuairisg, S., Foing, B.H. et al., 2001, B.H Foing and collaborators from Leiden Univ. (NL), in in The Bridge between Big-Bang & Biology, 150. preparation for the exploitation of data from the Mars Ehrenfreund, P. et al. (incl. B.H. Foing), 2002, ApJ Letts. Express Beagle-2 exobiology lander and future 576, L117. exobiology multi-user facilities on future Mars landers, Ruiterkamp, R. et al. (incl. B.H. Foing), 2002, A&A 390, were selected for an investigation to expose different 1153. organics, embedded in martian soil analogues, to simulated martian atmospheres, UV radiation and oxidising agents in order to study the stability and Survival and evolution of organics in space evolution of organic molecules on the martian surface and their implications for extinct and extant life on Mars B.H. Foing, in a collaboration led by Leiden Univ. (NL), (ten Kate et al., 2003). will study the survival and evolution of large organic molecules under space UV exposure within the EXPOSE An atmospheric simulation chamber in combination with experiment on the International Space Station (ISS) with a UV lamp is being set up to obtain data on the combined a 1-year exposure in 2005. A set of large organic effects of UV photo-processing, atmospheric conditions molecules has been defined: a) aliphatic and aromatic and the presence/absence of oxidising agents on organic hydrocarbons (5-20 carbon atoms per molecule) b) molecules. The organic compounds represent analogues nitriles, ketones, aldehydes, organic acids; c) amino for abundant meteoritic and cometary molecules and acids; d) large PAHs; e) fullerenes C60, C70, C84 and entail aliphatic and aromatic hydrocarbons, fullerenes, their hydrogenated or exohedral compounds; f) kerogens amino acids and nuclear bases, carbonaceous solids and and complex organic mixtures of 3-D networks of terrestrial analogues (i.e. kerogens). The simulation aromatic and aliphatic structure, including a variety of chamber is a refurbished vacuum chamber of 1 m heteroatoms (also a reference material for meteorites); g) diameter and 1.2 m length. It offers thermal and pressure spores and living organisms. Before and after space control. A window allows the attachment of UV lamps exposure, the samples will be subjected in the different and appropriate filters to simulate the variation of the Co-I institutes to various analysis methods, such as high- solar UV flux at 190-280 nm according to the O3 content performance liquid chromatography, IR spectroscopy, in the martian atmosphere. Compact martian soil gas chromatography, laser desorption mass spectrometry analogues (representing the sedimentary deposits) will and secondary ion mass spectrometry . allow less oxidation penetration and be representative of material present at the recommended landing sites. As a precursor to the ISS-EXPOSE experiment, a space Among the oxidising agents, we intend to use mainly UV exposure experiment of a sample tray filled with 16 H2O2 and O2. The chamber can be filled with gases samples of different organics was selected for a simulating the evolution of the martian atmosphere (CO2, Biopan/Foton flight with a planned 1-week exposure (Ruiterkamp et al., 2001; 2002). The experiment sample- tray was integrated at ESTEC and launched from Plesetsk aboard the Foton-M1 spacecraft on 15 October 2002. Unfortunately, the Soyuz rocket failed 15 s after lift-off and the experiment was lost in the explosion.

Figure 2.9.5/2: The Mars simulation chamber equipment, with controlled temperature and environment, solar radiation lamp, UV lamps, sample trays with martian analogue soil, and gas chromatograph mass spectrometer and other instruments to monitor the evolution of organics. sec2.qxd 3/5/03 3:40 PM Page 49

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N2 and Ar and traces of O2 and CO). H2O2 and O3 can be 2.10 Cosmic Dust and Comets added as gases in the chamber in order to study oxidation effects. We shall reproduce the thermal (e.g. 180-280K) This research theme encompasses a wide range of cycling and measure the evolution and thermal activities performed by members of RSSD, mostly in degradation products of embedded organics, and the international collaborations. Activities range from sublimation of the more volatile compounds. First opera- analysing data from dust detectors flown on spacecraft, tions after the build-up phase will include: procurement ground-based observations of comets and interplanetary and processing of Mars-like soils; simulations on surface dust particles, preparations of flight instruments to the water; experiments related to biological activity and dark development of generic elements for future dust spots; simulations of survival organics; and tests of instruments. sensors for organics and life.

The research activities on large organics, and especially 2.10.1 In situ measurements of cosmic dust the simulations in the Mars chamber, will contribute to the interpretation of measurements obtained by Beagle-2. From April 1997 to July 2002 the impact detector We shall therefore focus our experiments on the most GORID on the Russian Express-II satellite collected data abundant organic molecules identified in Solar System on cosmic dust and space debris from its location in bodies and beyond, which may have been exogenously geostationary orbit. The spacecraft was positioned at delivered to the martian surface. 80°E until July 2000, after which it was moved to 103°E.

Reference H. Svedhem and colleagues analysed the impact events Ten Kate, I. et al. (incl. B.H. Foing), 2002, ESA SP-518, to study the relation to interplanetary and interstellar dust 81. and to the space debris population, taking into account Ten Kate, I. et al. (incl. B.H. Foing), 2003, Int. Astro- geometrical and seasonal effects. Dust and debris biology J., in press. particles can, in a first approximation, be separated by evaluating the velocity: particles in Earth orbit are related to space debris and particles with velocities above the Earth-escape velocity are cosmic dust. Data sets from one or several full years are required to suppress possible biases that can result from spatial, temporal and directional variations in the flux and to reduce the statistical errors. The results have been compared with and match well existing models of the interplanetary dust flux.

On a few occasions a flux increase has been observed during the major known meteor showers. A number of occasions with clustered events that are very likely real particle impacts have also been identified. Many of these occur at n:m resonance, where n ≥ 1 is the number of full orbits of the satellite and m is the number of orbits of the clustered particles. This indicates that the clusters or clouds are fairly recent. A likely origin of these particle clouds is orbit circularisation burns from apogee boost motors of geostationary spacecraft. Indeed, simulations of the propagation of the dust clouds from a few known rocket firings have shown that the particles should be present at the observed positions at the observed times. At other times/positions events are registered in every orbit (n = 1). These events could be related to particle clouds that have been orbiting the Earth for a longer time.

The GORID detector has two different concentric fields of view, a narrow FOV with high sensitivity and a wide (almost 2π sr) FOV with lower sensitivity. Recent recalibration of a spare model of the detector have enabled a better separation of the two ranges and has also shown that the difference in sensitivity between the two ranges is less than has been previously thought. sec2.qxd 3/5/03 3:40 PM Page 50

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The instrument was built by MPI-K in Heidelberg (D) as an engineering model for the Ulysses Dust Experiment. It was subsequently refurbished by RSSD to suit the new environment in geostationary orbit.

The routine analysis of data from the Galileo, Ulysses and Cassini dust detectors also continued in close collaboration with the dust group at MPI-K.

To prepare for future mission opportunities, studies were performed to simulate the ion trajectories for a novel dust mass spectrometer design. To verify the simulation results, a test set-up was prepared to study the ion Figure 2.10.2/1: AFM image of IDP L2036 V25. The response to hypervelocity impacts simulated by laser image size is 10x10 µm; maximum height difference is pulses. 3µm.

2.10.2 Infrared investigations of interplanetary dust particles at NSLS: one covering the 2.5-28 µm range and the other Interplanetary dust particles (IDPs, < 50 µm diameter) the 22-60 µm range. The spectral overlap between the from comets and asteroids are collected in the two measurements is such that only a very slight stratosphere. Some of them are among the most multiplication factor was necessary to splice the two chemically and isotopically primitive meteoritic regions together (Fig. 2.10.2/2). Beyond 50 µm, the materials available for laboratory investigation. Studies signal-to-noise becomes too low. of IDPs provide insight about grain dynamics in the early Solar System and presolar interstellar and circumstellar The absorption spectrum of L2036-V25 is similar to the environments. Processes like grain condensation, emission spectrum of Comet Hale-Bopp obtained by ISO chemical and physical evolution, and grain density (Fig. 2.10.2/ 2). The similarity is not unexpected since distribution in the protoplanetary disc can be investigated highly porous, fragile IDPs like L2036-V25 are through studies of IDPs. It is now also possible to suspected to be from comets or comet-like outer compare the properties of IDPs directly with those of asteroids. dust around other young stars using their spectral properties in the IR, where most of the translational and The strongest features in the spectrum of IDP L2036- vibrational bands are also found.

In order to compare the spacecraft IR data with laboratory IR data from IDPs, it is highly desirable to obtain the data over a similar spectral range. Essentially Figure 2.10.2/2: The IR absorption of IDP L2036-V25 all of the existing IR spectroscopic data on IDPs has been (black line) compared with the absorption profile of collected over the 2-25 µm wavelength range, in contrast forsterite (green line) and enstatite (blue line). Also to the ISO data that covers 2.4-200 µm. So far, two plotted is the emission spectrum of Comet Hale-Bopp problems have hindered acquisition of spectral data (red line) taken with ISO (Crovisier et al., 1997, beyond 25 µm from IDPs: the small size of individual Science 275, 1904). IDPs relative to the wavelength of the incident radiation, and the lack of detectors sensitive beyond ~25 µm. The recent upgrade of the National Synchrotron Light Source (NSLS) at Brookhaven National Laboratory (US) allowed us for the first time to take spectra of an IDP over the important ‘mineral fingerprint’ region of 2.5- 50 µm.

Figure 2.10.2/1 shows an atomic force microscope (AFM) image of an IDP (diameter ~10 µm) pressed onto a CsI window. The high IR transparency of CsI allows us to measure the IR absorption properties of L2036-V25 out to extended wavelengths, but the small size of the IDP demands the use of a high-brightness synchrotron light source. We acquired two IR spectra of L2036-V25 sec2.qxd 3/5/03 3:40 PM Page 51

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V25 are due to olivine, while some weaker features of of the comet’s debris on 5/6 August 2000 revealed that pyroxene are also detected. The peak positions of the apart from the bright dust tail dominating its visual features, especially the ones at the longer wavelengths appearance, more than a dozen individual fragments (>20 µm), provide information about the Mg/Fe ratio of were spread around the predicted position of the original the minerals. The features suggest an Mg/Fe ratio of nucleus. All these fragments faded rapidly and were no about 3:1 for both the olivines and pyroxenes. Note that longer detected in any of the subsequent observations. It the peak positions in the IR spectra of Hale-Bopp are became clear rather soon that the time of the outburst consistent with pure Mg-olivine and pyroxene, i.e. (22 July 2000) that produced the dust tail and resulted in forsterite and enstatite. This difference gives some very the complete disintegration of the comet did not coincide important clues about the formation history of the with the separation times of some individual fragments. different components. These fragments must have separated some time between late June and mid-July, hence the true splitting event F. Molster and colleagues have demonstrated that it is must have occurred some time before the final now possible to obtain IR spectra of individual IDPs over disintegration started. Indeed the analysis of imaging a spectral range extending out to ~50 µm. Silicate observations of Comet C/1999 S4 (LINEAR) obtained minerals like olivine and pyroxene can be between 28 June and 1 July 2000 (Fig. 2.10.3) confirmed unambiguously distinguished and their Mg/Fe contents that a splitting of the nucleus occurred on 28 June 2000, can be estimated. The above results are encouraging which produced at least one major fragment and a because IDP L2036-V25 was prepared as a calibration number of small fragments drifting in the tail direction standard for the AFM Micro Imaging Dust Analysing (Schulz & Stuewe, 2002). The fragments remained active System (MIDAS) onboard Rosetta and not as a sample at least until 1 July 2000, producing further disintegra- optimised for IR spectroscopy. ting dust particles.

2.10.3 Ground-based observations of comets Comet C/1996 Q1 (Tabur)

Comet C/1999 S4 (LINEAR) The spectrophotometric CCD observations of Comet C/1996 Q1 (Tabur) (Lara et al., 2001) allowed for the One of the most spectacular cometary splitting events first time detailed multi-colour photometry of cometary ever observed was the complete disruption of the nucleus continuum in the near-nucleus region to be extracted. of Comet C/1999 S4 (LINEAR). HST/VLT observations The change of the spectral properties of the cometary dust as a function of distance to the nucleus was theoretically modelled to separate the influence of particle size and composition on the colour of cometary dust. The calculations provided important characteristics Figure 2.10.3: Comet C/1999 S4 (LINEAR) imaged in of the dust in the coma of Comet Tabur as a function of blue continuum (BC) and red continuum (RC). On nucleus distance. These are the power of the power-law 1July 2000, the coma is much more elongated than on size distribution and the radius of the smallest particles in 28 June 2000. The Sun is to the left in all images. the dust distribution (Kolokolova et al., 2001).

Comet 46P/Wirtanen

The observations of the nucleus of Comet 46P/Wirtanen obtained at the VLT were analysed. No coma was detected in May 1999 when the comet was at a heliocentric distance of 4.98 AU. The mean nucleus radius was confirmed to be 555±40 m (albedo 4%). The measured light curve was in agreement with a rotation period of 5-7.5 h and a ratio of the main nucleus axes of at least 1.4. The non-detection of a coma allows us to approximate the upper limit on the dust production rate to be 0.05 kg s–1. A weak and condensed coma appears to be present in the seeing disc of the comet at 2.9 AU inbound (December 2001), causing a higher brightness than expected from previous size estimates of the nucleus. The comet was very red (V-R spectral gradient ~47%/100 nm) and the dust production rate was determined to be 1 kg s–1 (Boehnhardt et al., 2002). sec2.qxd 3/5/03 3:40 PM Page 52

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References an inhomogeneous comet nucleus, where there are areas Boehnhardt, H. et al. (incl. Schulz, R. & Schwehm, G.), of higher and of lower strength. Large particles from the 2002, A& A 387, 1107. low-strength areas will break apart immediately at Kolokolova, L., Lara, L., Schulz, R. et al., 2001, Icarus ejection and never make it away from the comet. This 153, 197. assumption needs to be confirmed by further modelling. Lara, L., Schulz, R. et al., 2001, Icarus 150, 124. Schulz, R., Stuewe, J.A., 2002, Earth, Moon and Planets As part of the Leonid campaigns of 2001 and 2002, the 90, 195. terrestrial electric field was monitored by an electric field sensor derived from the Rosetta SESAME Quadrupolar Probe sensors (Trautner et al., 2002). The electric field 2.10.4 Leonid observations sensor showed a significant increase in the field fluctuations during the 2001 Leonid storm. The curve As for 1999, theoreticians had predicated a meteor storm matches the activity profile of the Leonids very well generated by the Leonid meteor stream in November (Fig. 2.10.4/1). The experiment was repeated during the 2001 and 2002. The storm of 2001 was observable only 2002 Leonids shower using a modified sensor setup and from Asia and Australia, with a second peak in the US, improved recording equipment. The data analysis is in the 2002 storm from Europe, and again a second peak in progress. It is expected that the measurement data will the US. provide important information on the link between electric field fluctuations and meteor impacts in the In 2001, D. Koschny, J. Zender and R. Trautner success- terrestrial atmosphere. The experiments in our terrestrial fully observed the storm peak from Western Australia. environment are also a preparation for future missions to A. Knöfel from the International Meteor Organisation Mars. (D) accompanied them. A number of image-intensified video cameras and a special sensor to record the electric For the Leonid storm in 2002, the same team repeated the field changes in the atmosphere were operated. Meteor measurements from Southern Spain in a collaboration spectra together with precise altitude information were with the Instituto Astrofisica de Andalucia (IAA) in obtained. Zender et al. (2002) have prepared a first Granada (E), from two stations close to Granada. There analysis. The observers have also analysed the light was clear sky for only half of the time. As in 1999, we curves of the meteors and compared them to a also had one camera flying aboard a DC-8 aircraft as part fragmentation model developed at RSSD (Koschny et al., of a campaign organised by the NASA SETI institute. It 2002). Indications for an inhomogeneous comet nucleus recorded the very bright fireball shown in Fig. 2.10.4/2. have been found: bright meteors appear to be from A total of about 1000 meteors were recorded with this material with higher strength. This can be explained by system alone in about 3 h around the peak. The analysis of the 2002 data has just started.

Figure 2.10.4/1: Comparison between the vertical electric field in arbitrary units and the Zenithal Hourly Rate (ZHR) of the Leonid meteors as Figure 2.10.4/2: A very bright fireball recorded by the recorded by the International Meteor Organisation, airborne camera operated by R. Jehn (ESOC). It versus time on 18 November 2001. appeared at 05:10:38 UT on 19 November 2002. Clouds are visible in the lower part of the image. sec2.qxd 3/5/03 3:40 PM Page 53

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References D. Koschny participated in the optical calibration at Koschny, D., Reissaus, P., Knöfel, A, Trautner, R., MPAe. A complete calibration including absolute Zender, J., 2002, ESA SP-500, 157. responsivity measurements was performed. Trautner, R., Koschny, D. Witasse, O., Zender, J., Knöfel, A., 2002, ESA SP-500, 161. D. Koschny and K.-P. Wenzel are OSIRIS Co-Is, Zender, J., Witasse, O., Koschny, D, Trautner, R., U. Telljohann is Project Engineer and B. Johlander was Knöfel, A., 2002, ESA SP-500, 121. responsible for parts procurement.

Reference 2.10.5 The Rosetta Imaging System (OSIRIS) Keller, H.U., et al. (incl. Koschny, D.V., Telljohann, U., Wenzel, K.-P.), 2003, ESA SP-1165, in preparation. OSIRIS is the scientific imaging system of the Rosetta mission (Keller et al., 2003). It will address key problems in understanding the properties and behaviour of comets by investigating the physical and chemical processes that occur on the nucleus and in the coma. OSIRIS consists of two cameras: a narrow-angle camera (NAC) with a 2.4 x 2.4° FOV and a wide-angle camera (WAC) with a 12 x 12° FOV. Two identical full-frame CCDs with 2048 x 2048 pixels are used in the cameras.

OSIRIS is provided by a European consortium under the leadership of H.U. Keller (MPAe Lindau, D). RSSD is part of this consortium and responsible for the Data Processing Unit (DPU; Fig. 2.10.5). It consists of two Digital Signal Processor (DSP) boards, a mass memory board and the relevant interfaces.

The Flight Model was delivered to MPAe and integrated with the Electronics Box in the first half of 2001. After some required rework, it passed all environmental tests. The complete OSIRIS Flight Model was delivered to the Rosetta Project in summer 2001 and mounted on the spacecraft on 11 December 2001. OSIRIS participated in the extensive spacecraft-level test campaign and the operational interface with ESOC was refined.

Figure 2.10.5: The DPU Interface Board of the OSIRIS Flight Model DPU. sec2.qxd 3/5/03 3:40 PM Page 54

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2.11 Development and Exploitation of Super- conducting Cameras for Astronomy

2.11.1 Overview of activities

The development and exploitation of superconducting cameras has concentrated on the application of Superconducting Tunnel Junctions (STJs) to the optical part of the spectrum. This region provides opportunities to develop the basic technology coupled to practical field-testing with rapid technical and scientific feedback from ground-based optical telescopes – specifically the William Herschel Telescope (WHT) in La Palmas (E). Such an approach also allows for parallel spin-off developments at X-ray wavelengths for future high- Figure 2.11.1/2: A cross-section showing the basic energy astrophysics missions such as XEUS. This optical characteristics of an STJ sensitive to optical photons. program, known as the Superconducting Camera Programme (SCAM), is broken into six phases, of which two were completed between 1999 and 2001. Fig. 2.11.1/1 summarises the overall programme in terms of a provisional time-line and the key objectives. essential result of this cascade is that the photon’s energy is converted into a population of free charge carriers The basic superconducting detector used within the (quasiparticles) in excess of any thermal population. For SCAM programme is an STJ. Fig. 2.11.1/2 shows typical transition metals, this conversion process ranges essentially the key characteristics of such a device. from nanoseconds (niobium) to microseconds (hafnium). Incident photons break Cooper pairs responsible for the At sufficiently low temperatures (typically about an superconducting state. Since the energy gap between the order of magnitude lower than the superconductors ground state and the excited state is only a few meV, each critical temperature Tc), the number density of thermal photon creates a large number of free electrons in carriers is very small while the average number of excess proportion to its energy. Examining the photoabsorption carriers No created as a result of the photoabsorption 5 process in detail at optical wavelengths has been a key process can be written as No(λ)~7x10/λ∆(T/Tc). theoretical effort in collaboration with the School of Here, the wavelength is expressed in nm and the Physics and Chemistry at Lancaster Univ. (UK). The temperature-dependent energy gap ∆(T/Tc) is in meV. absorption of a photon of a wavelength λ (nm) in a Thus, in a superconductor such as tantalum, with T << Tc superconductor is followed by a series of fast processes (4.5K), the initial mean number of free charge carriers 6 3 which involve the breaking of Cooper pairs by energetic created No(λ) is ~ 10 (10 /eV). phonons created by the hot electrons produced as the atom relaxes after the initial photoabsorption. The The variance of No(λ) depends on the variance in the partition of the photon’s energy between productive phonons (phonons with an energy Ω >2∆ which can break Cooper pairs) and phonons which are essentially Figure 2.11.1/1: The overall Superconducting lost from the system (Ω <2∆). The population of Ω <2∆ Camera Programme (SCAM) for ground-based phonons evolves with time as the average energy of the optical astronomy. increasing quasiparticle population relaxes, through quasiparticle phonon emission, towards the bandgap. The variance depends on the superconductors bandgap ∆ and its Fano factor F such that –4 ~7x10 F/[λ(nm) ∆(T/Tc)]. Expressing this variance in terms of the wavelength resolution, we have dλF (nm) ~ –3 3/2 1/2 2.8x10 λ [F ∆(T/Tc)] . It has been shown that F ~ 0.2 for elemental superconductors such as niobium and tin (Kurakado, 1982; Rando et al., 1992). This therefore represents the fundamental Fano limited resolution of any superconductor. Thus a superconductor such as tantalum, with T<

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STJs under development (those based on Nb,Ta, Al, Mo or Hf ) could achieve such a resolving power. In fact, a superconducting critical temperature Tc << 100 mK is implied to achieve a resolving power of 104 leading to the development of STJs based on such elemental superconductors as rhodium. Of course, things are not quite this simple with the temporal characteristics associated with the production of the free excess charge carriers being a function of the critical temperature, while the phonons with Ω >2∆ have wavelengths significantly larger than the thickness of the film. Thus such low temperature superconductors may well be significantly slower in their overall response. Figure 2.11.1/3: The tunnel-limited resolution of some types of STJs under development as a function of Given that the resolution of a typical STJ based on wavelength. tantalum is not appropriate for high- or even medium- resolution spectroscopy, what are the alternative key attributes that such a device can bring to the field of optical/UV astronomy? Two features are important: (a) the timing characteristics (≤ 10 µs) coupled to the The quasiparticles produced through photoabsorption broadband spectral capability may make this the ideal can be detected by applying a DC potential across two spectrophotometer. Objects such as pulsars and flare such films separated by a thin insulating barrier, forming stars may be important objects with which to observe an STJ (c.f. Fig. 2.11.1/2). The bias favours the transfer with narrow field small arrays; (b) the efficiency at UV of quasiparticles from one film to the other through wavelengths which, if coupled to a large-format array (a quantum mechanical tunnelling across the barrier. The panoramic detector), may allow for the development of current developed by this tunnel process therefore an efficient broadband imaging spectrometer with which represents the detector signal. After initial tunnelling, a to determine the low-resolution spectra of very faint quasiparticle can tunnel back, therefore contributing objects, allowing very deep-field surveys. Such surveys many times to the overall signal (Grey, 1978). On could allow the determination in a single exposure of the average, each quasiparticle will contribute times to broadband spectra and possibly therefore the redshift z the signal through an average of tunnels before it is (and therefore age) of all objects in the field through the lost from the system through traps etc. Hence the mean measurement of the Lyman edge and the Lyman emission number of effective charge carriers N = nNo. The lines (the Lyman forest). Note that the observed multiple tunnel process leading to n, the average number wavelength λo = λR (z+1), where λR is the rest wave- of tunnels per quasiparticle, is of course subject also to length. Thus the classical Lyman edge would appear at statistical fluctuation (Goldie et al., 1994). The ~ 400 nm at z ~ 3. This is close to the optimum fluctuations due to the Fano process and that arising performance for a tantalum-based STJ, where it has an from the tunnel process can be added in quadrature such intrinsic efficiency of ~70% and a resolution of ~20 nm. that the overall limiting resolution for a perfectly It is, however, clear that STJ devices based on lower symmetrical superconducting tunnel junction can be temperature superconductors such as hafnium would –3 3/2 1/2 written as: dλT (nm) ~ 2.8 x 10 λ ∆(T/Tc) allow the clear evaluation of redshift. This, therefore, is [F+1+1/n]1/2. Fig. 2.12.1/3 illustrates this tunnel one of the key goals of the SCAM programme: to junction-limited resolution for a number of elemental develop a large-format (FOV ~1 arcmin), high- superconductors for the case when n ≥ 2. Note this resolution, multi-object imaging instrument capable of expression for the tunnel-limited resolution dλT can be measuring with reasonable resolution (~1 nm) the further generalised to any superconductor compound or spectra of deep field extragalactic objects so as to proximised bilayer through the use of the approximate determine their redshift. BCS relation in the weak coupling limit of 2∆ = 3.5 k Tc, where k is Boltzmann’s constant. References Deviations from this relation are small even for strongly Goldie, D., et. al., 1994, Appl. Phys. Lett. 64, 3169. coupled superconductors such as niobium. Thus in terms Grey, K., 1978, Appl. Phys. Lett. 32, 392. of the critical temperature we can write dλT (nm) Kurakado, M., 1982, Nucl. Instr. & Meth. 196, 275. –3 3/2 1/2 1/2 ~1.1x10 λ Tc [F+1+1/n] (n ≥ 2). Typically, n is Rando, N., et al., 1992, Nucl. Instr. & Meth. A313, of order 10-100 and depends on the size and nature of 173. the STJ. Of course, in optical and UV spectroscopy, high Peacock, A., et. al., 1997, Astron. & Astrophys. Sup. 123, resolution normally implies a resolving power 581. λ/δλ >104. From Fig. 2.11.1/3 it is clear that none of the Peacock, A., et. al., 1998, Astron. & Astrophys. Sup., classical superconductors forming the basis of current 127, 497. sec2.qxd 3/5/03 3:40 PM Page 56

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2.11.2 The SCAM-1 programme

The SCAM-1 instrument represented the first demonstration of a superconducting camera developed specifically for integration onto the WHT telescope. In this technology programme, all the basic key elements of such an instrument were brought together into a single instrument:

—STJ array; — STJ multi-pixel bias system; — STJ readout electronics; — cryogenic system; — diagnostic test software; — real-time quick-look analysis.

SCAM-1 can therefore be considered as a technology Figure 2.11.2/2: Pulse profile of the Crab pulsar as demonstrator rather than a scientific astronomical observed by SCAM-1 in February 1999. instrument. Fig. 2.11.2/1 shows the basic 6 x 6-pixel STJ array prior to its integration into the cryogenic cooling system. The array fabricated in tantalum with each pixel 25 µm square covered a FOV of only 3.6 arcsec. This FOV is a critical issue since it only allows for effective photons from the 33 ms Crab pulsar. Here we demon- single-object studies when the telescope ‘seeing’ is strate with this single observation the power of the new reasonable (typically < 2 arcsec). instrument allowing for detailed pulse phase spectroscopy at high temporal resolution (Perryman et al., Each device had its own bias, amplification and signal 1999). This celestial clock’s speed is so well established processing circuitry outside of the cryostat and operated that we can literally calibrate the complete system – end at room temperature. The cryostat was a pumped He4 to end. Fig. 2.11.2/2 shoes the observed pulse profile as a system with an internal closed-cycle He3 sorption pump function of pulse phase. which brought the base temperature from ~1K to ~300mK, the operating temperature of the tantalum Reference array. The instrument was integrated onto the Nasmyth Perryman, M.A.C., Favata, F., Peacock et al., 1999, A&A focus of the WHT in February 1999 and after system 346, L30. testing was able to record individual photons from specific targets with a temporal accuracy of 5 µs while measuring the photon colour over the wavelength range 2.11.3 The SCAM-2 programme 310-610 nm with a resolution of 100 nm at 500 nm. SCAM-2 covered a series of three campaigns at the A crucial technical demonstration of the system WHT over the period December 1999 until October performance was the detection and measurement of 2000. A significant number of improvements on the SCAM-1 design were introduced to ensure this programme was orientated to astronomical exploitation even if still centred on the 6 x 6 pixel tantalum array. In Figure 2.11.2/1: The original SCAM-1 6 x 6 array. particular, the resolving power and photon event rate were improved. The campaigns highlighted three areas where the SCAM can make a serious astronomical contribution:

— spectro-photometry of variable stars; — stellar temperature measurements; — quasar redshifts.

Fig. 2.11.3/1-3 show data referring to all three types of astronomical observations.

References de Bruijn, J.H.J. et al., 2002, A&A 381, 57. Reynolds, A.P., de Bruijne, J.H.J., Perryman, M.A.C., sec2.qxd 3/5/03 3:41 PM Page 57

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Figure 2.11.3/1: The light curve of the eclipsing AM Her system V2301 Ophiuchi during the eclipse ingress. Spectra, with high time resolution through the eclipse, allow the separation of the accretion stream component from the white dwarf, thereby constraining the system geometry. Figure 2.11.3/3: The redshift of a number of quasars as measured by SCAM-2 versus the actual known literature redshift as determined through high- resolution spectroscopy (de Bruijn et al., 2002).

Figure 2.11.3/2: The observed stellar temperature Figure 2.11.4: The SCAM-3 array prior to instrument versus the literature temperatures for eight stellar system tests. Each device is still biased and read out objects in the SCAM-2 sample (Reynolds et al., 2002). individually.

Ramsay, G., Cropper, M., Bridge, C.M., 2002, A&A in provided weaker areas can be further developed. In press. particular these weaker areas are considered to be:

— the field coverage (field of view); 2.11.4 The SCAM-3 programme — the long wavelength limit; — the resolving power; It is clear from these results that the SCAM instrument — the count rate limits. can be a powerful tool for observational astronomy sec2.qxd 3/5/03 3:41 PM Page 58

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Figure 2.11.5/2: The field coverage envisaged in the SCAM-4 programme. A deep field exposure from a Figure 2.11.5/1: The basic concept of the DROID. CCD camera at the WHT prime focus is used as background.

The SCAM-3 programme is based on the SCAM-2 been introduced is the Distributed Readout Optical campaigns. SCAM-3 is therefore built around a 10 x 12- Imaging Detector (DROID). Fig. 2.12.5/1 shows the pixel array of tantalum-based STJs each 33 µm square basic principle of the DROID. (c.f. Fig. 2.11.4) covering a field of ~10 x 12 arcsec. Essentially, photons are not absorbed directly in the STJ The IR rejection has also been improved with the but in a superconducting absorber strip. The resultant introduction of new filters allowing an increase in charge carriers diffuse along the strip until they reach efficiency and resolving power to 34% and 13 each end, where they are trapped by a lower bandgap respectively, compared with 22% and 8 at 500 nm for material and enter the STJs. The sum of the two STJ SCAM-2. In addition, the red response has been signals provides the energy of the photon, while their extended to 750 nm compared with 650 nm. Finally, the ratio is a measure of the position in one-dimension, the electronics have been dramatically improved, with second dimension being simply the width of the strip. modules operating in banks of 32 pixels. With such an Such systems have been tested successfully at optical and approach, single pixel rates of 8 kHz and 250 kHz per X-ray wavelengths. Clearly packaging such individual bank (i.e. a MHz for the whole array) has been achieved. detectors into arrays as shown in Fig. 2.11.5/2 will allow This will allow SCAM-3 to take real advantage of the large field coverage. 5µs intrinsic timing ability to study short timescale phenomena. 2.11.6 The SCAM-5 programme

2.11.5 The SCAM-4 programme For observing at very remote sites, the general use of a SCAM instrument will be limited by the requirement to While the SCAM-3 programme, about to enter its cool a tantalum detector to ~300mK by liquid helium. operational phase, will increase the field coverage so that The availability of helium, coupled with complex filling single objects can be observed in reasonable or even poor and cool-down procedure, could possibly preclude ‘seeing’, while still being able to observe the surrounding SCAM-type cameras becoming available as general user sky background, the single-pixel approach will be always instruments. Therefore it is the aim of the SCAM-5 limited. Clearly with each pixel requiring its own wiring technology demonstration programme to provide a and readout electronics, an expanded array can never tantalum-based SCAM camera cooled to 300mK by a hope to be able to cover a significant field fully closed-cycle refrigeration system. This is achieved (~1 x 1 arcmin). In addition, larger pixels introduce through the use of a Pulse Tube Refrigerator (PTR) serious degradation in performance. The solution that has coupled to a He4 sorption pump, which is then coupled to sec2.qxd 3/5/03 3:41 PM Page 59

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Figure 2.11.7/2: A 32 x 10-pixel molybdenum test Figure 2.11.7/1: The optical spectrum from 500 nm array prior to such Mo-based devices undergoing photons recorded by a pure aluminium-based STJ testing at 40mK in a cryostat. operated at 40mK.

a second He3 sorption pump. The PTR provides a base 2.11.8 SCAM programme conclusion temperature of 4K from which the closed-cycle He4 pump takes the temperature to ~1K, from which the He3 The SCAM programme seeks to develop a new class of pump provides the final base temperature of 300mK. instrument for use by general astronomers, both for Currently the system is under test and has achieved the ground-based and space-based platforms. The heart of required base temperature. EMC and acoustic issues are the programme is the material science associated with now being addressed prior to the start of device testing. superconductors. These materials offer for the first time the technique of single photon counting coupled to medium-resolution imaging-spectroscopy (Peacock et 2.11.7 The SCAM-6 programme al., 1996). Design issues derived from the SCAM ground-based observing runs will feed into future space- From Fig. 2.11.1/3 it is clear that STJs or DROIDS based based spectrometers for applications in wavelength from on tantalum will be limited in their resolving power to at the near-IR to the soft X-ray. best ~25 at 500 nm. The purpose of the SCAM-6 programme is to develop STJs and DROIDs based on Reference lower bandgap materials. Two materials are currently in Peacock, A. et al., 1996, Nature 381,135. development at the device level for the STJ” molybdenum and aluminium. Since aluminium (Tc ~ 1K, compared with 4.5K for Ta) is a basic building block of Ta-based STJs, it is natural to develop devices based on this material as a precursor to developments in other lower Tc materials. Aluminium devices, which theoretically should have a resolving power twice as good as tantalum, have been developed to a level where they are now sensitive to optical photons. Fig. 2.11.7/1 shows the spectrum from such a single STJ device illuminated by monochromatic 500 nm light.

In parallel with the developments in aluminium, devices in Mo-Al have also been fabricated. Fig. 2.11.7/2 shows a large-format array of Mo prior to such STJs undergoing basic junction tests such as current leakage and Josephson current suppression. sec2.qxd 3/5/03 3:41 PM Page 60

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2.12 Advanced sensor, optics and instrument development research

X-ray optics and detectors are being developed for space- based astrophysics observatories and planetary missions. In the area of semiconductor-based photon detectors, compounds like gallium arsenide (GaAs), thallium bromide (TlBr), indium phosphide (InP) and narrow bandgap materials are the focus of the research.

2.12.1 Compound semiconductor photon detectors Figure 2.12.1/2. A surface plot of the spatial variation of the gain (i.e., the fitted centroid position) across the GaAs has attracted considerable interest as a viable 4x4 GaAs array measured at HASYLAB using a alternative to Si or Ge for the detection of X-rays above 15 keV, 20 x 20 µm pencil beam. The spatial sampling a few keV. It has a simple cubic lattice structure and is in X and Y was 10 µm. one of the high group compound semiconductors with a bandgap sufficiently wide (1.42 eV) to permit room- temperature operation but small enough so that its Fano- limited spectroscopic resolution is close to that of Si. temperature operation, with typical FWHM energy A small GaAs array was produced by growing an ultra- resolutions of 600 eV at 5.9 keV and 0.7 keV at pure 325 µm epitaxial layer onto an n+ semi-insulating 59.54 keV (pulse width 550 eV). substrate using chemical vapour phase deposition techniques. To reduce leakage currents, a 10 µm thick p+ The spatial uniformity of the array was evaluated on layer was then deposited onto the epi-layer, forming a p- beamline X1 using a 15 keV pencil beam of size i-n structure. This layer was then patterned by etching, to 20 x 20 µm, normally incident on the pixels. The create a 4 x 4-pixel structure surrounded by a guard ring detector is very uniform over the surface of each pixel (Fig. 2.12.1/1). The pixel sizes are 350 x 350 µm with an and the array, as shown in Fig. 2.12.1/2. inter-pixel gap of 50 µm. Contact with the pixels is achieved by wire bonding. In this configuration, biasing Wide-gap compound semiconductors offer the the n+ side and collecting off the p+ side utilises hole possibility of room-temperature operation, while charge collection, preamplified by low capacitance FETs. maintaining sub-keV spectral resolution at hard X-ray The array uses resistive feedback preamplifiers in the wavelengths. The ability to mix and match available form of hybrids, also mounted directly on the substrate. band-gaps and stopping powers is commercially The leakage currents were low enough to permit room- attractive, since it suggests that materials can be tailored

Figure 2.12.1/1: Left: photomicrograph of the 4 x 4 GaAs detector assembly used in the present study. The device is die-attached to the substrate, which in turn is mounted on a 2-stage Peltier cooler. Right: the completed GaAs array/hybrid/substrate assembly. sec2.qxd 3/5/03 3:41 PM Page 61

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Figure 2.12.1/3: Left: the world’s first 3 x 3, 1 mm thick TlBr array. The array has a pixel size of 350 x 350 µm with an interpixel gap of 100 µm. Right: spatial response of the array to a 15 keV, 20 x 20 µm X-ray pencil beam.

Figure 2.12.1/4: Top: the first prototype 3.14 mm2 180 µm-thick InP detector. Centre: the detector’s response to a 40 keV, 20 x 20 µm X-ray beam. Bottom: a composite of energy-loss spectra recorded at HASYLAB.

for specific applications and wavelengths. Of available materials, TlBr and InP are two of the least studied.

TlBr has emerged as a particularly interesting material for room-temperature hard X-rays and gamma-ray applications, in view of its wide band-gap (2.5 times that of Si) and high atomic numbers (Tl = 81, Br = 35) of its constituent atoms. In fact, its density (7.5 g cm–3) is comparable to bismuth germanate and thus it has excellent stopping power for hard X-rays and gamma- rays. Prototype detectors have been fabricated from a thermally grown mono-crystal, produced by the Bridgeman-Stockbarger technique and tested on the X-1 beamline at HASYLAB. Measurements were carried out over the energy range 10.5-100 keV. We have produced a third generation of detectors making several modifications in material production and detector design. Several new devices have been fabricated, including a prototype 3 x 3 array, shown in Fig. 2.12.1/3.

InP is a group III-V direct band-gap material whose resistivity and mobilities are intermediate between Si and GaAs. While the rest of its properties are similar to GaAs, it is potentially a more attractive material because of its larger stopping power (2-3 times that of GaAs), and higher drift velocities (again, 2-3 times that of GaAs).

thickness of 180 µm. A p+ layer was then deposited on InP was synthesised from solution and purified by one side of the plate by vapour-phase epitaxy using Zn as vacuum distillation. Semi-insulating material was a dopant. Circular Au/Ti contacts of diameter 2 mm were produced by doping with Fe and a monocrystal grown by deposited on the top and the bottom of the plate. The liquid-encapsulated Czochralski. Wafers were sliced completed detector and its response is shown in from the boule along the <100> direction and detector Fig. 2.12/.14. The device is clearly spectroscopic and, in platelets diced from the wafer. These were lapped and fact, these data represent the best spectroscopic polished by chemical and mechanical processing to a performance yet reported for an InP detector. sec2.qxd 3/5/03 3:41 PM Page 62

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2.12.2 Low-mass X-ray optics

ESA, together with European industry, is exploring the X-ray optics technologies for the next generation of space astrophysics and planetary missions currently under design. A number of technologies are under study, ranging from low-mass replication processes built around conventional Wolter-I nested geometries as well as radically different approaches. In the later case, e.g. the technology used to produce glass micro-channel plates (MCPs) is used to produce X-ray optics with very thin reflecting surfaces, of the order of only a few micrometers. Figure 2.12.2/2: SEM micrograph of the hierarchical structure of the prototype MCP X-ray ‘lens’. Note that a Wolter-1 configuration comprises, as a basic element, a paraboloid (P) coupled to a hyperboloid (H) and is shown schematically in the left side of Fig. 2.12.2/1. To achieve a reasonably large collecting area, pairs of shells (P+H) are stacked inside each other. The conical approximation to the Wolter-1 geometry is To ensure an adequate imaging resolution, these shells acceptable, if the length of the reflecting surfaces must be stiff and well aligned, leading to bulky and (indicated as ‘L’ in Fig. 2.12.2/1) is small compared with heavy optics. On the right side of Fig. 2.12.2/1 the the focal length of the system (‘F’ in the figure). implementation of a conical approximation to a Wolter- 1 system based on MCPs is shown. Such a system Such a compact and light lens has been made for the first allows the substantial reduction of the mirror wall time in a geometry that produces true X-ray imaging. thickness, due to an additional radial structure. Such a This lens has been manufactures under ESA contract by system can therefore be made very much lighter than Photonis (F) with support from Leicester University current state-of-the art optics, maintaining the required Space Centre (UK). Testing has been performed by ESA mechanical stiffness of the reflecting surfaces. The staff in collaboration with the Bessy PTB synchrotron mirror plate thickness can be reduced by a factor of a facility in Berlin (D) and at the European Synchrotron few 100. Radiation Facility in Grenoble (F), with support provided by personnel of the the Univ. of Leicester.

MCPs have been developed for image intensifiers and photon-counting detectors, and their mass production has Figure 2.12.2/1: A Wolter-1 X-ray telescope showing reached a high level of optimisation. Inherent to the the key parameters, left. Only grazing incidence production process, which involves severe stretching of reflections are used. Concentric stacking is essential the glass fibres, very smooth walls are obtained, which for achieving a practical effective area for the system. are arranged in a regular geometry. Starting with a slab of By implementing the concentric mirrors in two material, the glass is drawn into long and thin fibres, MCPs, as shown on the right side, the packing density which are then grouped into multi-fibres and drawn increases and the mirror thickness can be again. Finally the multi-fibres are stacked to the desired substantially reduced owing to the radial walls geometry, and then fused to form a monolithic block. The stabilising the optics. block is then cut into slices, which are then slumped to the required radius and finally etched to form pores by removing the core glass. To adapt the MCPs for use as X-ray optics, it was necessary to change and improve the micro-fibre geometry and reduce the surface roughness. The resulting optics are, however, very rigid and extremely light. In fact, the optics are also very robust, since the specific mass and the corresponding forces during vibration are low.

A prototype X-ray optics consisting of two circular plates of 60 mm diameter, each plate being 5 mm thick, was produced, and is shown in the left part of Fig. 2.12.2/2. Each plate contains 20 million almost perfectly square holes, each 10 µm in diameter with a wall thickness of a micron (right part of Fig. 2.12.2/2). The MCP plates are sec2.qxd 3/5/03 3:41 PM Page 63

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Figure 2.12.2/3: Mass density comparison of the nickel-based XMM optics and a glass-based MCP optics prototype. The angular resolution of the XMM Figure 2.12.2/4: Si MCP optics architecture. The optics is only a factor of 4 better than that of this first X-ray optics are composed of strips of Si grids radially-packed doublet MCP X-ray optics prototype (MCPs) of width W, arranged concentrically around ever produced. the optical axis. The strips are deformed elastically in their mounting structure, which, for thermal reasons, is also Si.

made of glass with a high bismuth content, to increase the X-ray reflectivity and improve the processing of the glass. To achieve the conical approximation to a Wolter-1 — good stiffness; geometry, one plate is slumped to a spherical profile with — low specific mass; a radius of curvature of 20 m, the other to a radius of — high uniformity (monocrystalinity). curvature of 6.7 m. In combination, this doublet has a focal length of 5 m, which was chosen to facilitate X-ray The main advantage of this approach is, next to the testing. Fig. 2.12.2/2 shows the hierarchical structure of superior material qualities of silicon over glass, the the radially packed square micro-fibres in the MCPs of intrinsically excellent alignment of the individual pore these optics. The RMS surface roughness is 10 Å walls owing to the crystalline structure of the material. (measured 20-2000 mm–1), which is sufficiently smooth By using lithographic techniques to pattern the surface of to reflect medium-energy X-rays. silicon wafers and applying standard industrial processes, very accurate geometries can be realised with This X-ray optic behaves in the same way as a normal a significant freedom in the design. biconvex lens in the visible range. It is effectively an X-ray lens. The mass of the 60 mm diameter prototype is The main development is concentrated on the processes 28.5 g (10 kg m–2, in comparison with ~900 kg m–2 for necessary to produce deep structures in the Si wafers, XMM-Newton). Half the focused radiation of these with very smooth surfaces. The later is difficult, without optics falls within a circle with a diameter of 1.0 arcmin. destroying the general surface geometry or figure. This is only a factor of 4 larger than the imaging resolution of XMM-Newton, with a much larger specific The crystalline structure of Si and the associated etching mass (with 350 kg at a diameter of 700 mm, i.e. processes permit only the fabrication of square 910 kg m–2). If this imaging quality were to be further structures, but not radial ones, which are in principle improved, it might be possible to build a comparable required for the X-ray optics. The solution to this mirror system for under 10 kg with accompanying problem is the division of the optics into narrow strips, savings on mission costs, as illustrated in Fig. 2.12.2/3. arranged in concentric circles and covering the complete aperture. The individual strips are limited in width by the An alternative technology to produce MCPs is size of the angular resolution element in the focal plane micromachining of silicon. Silicon of very high quality is (e.g. in the case of XEUS the plate scale is 250 µm per available on the market today, and the methods and arcsec, and therefore the angular resolution element is processes to structure it have been developed in recent about 1 mm in the focal plane, corresponding to 4 arcsec, decades with enormous efforts by the electronics and therefore the silicon strips would be limited in their industry. Silicon also very good thermal and mechanical width to about 1 mm). The length of the strips would be properties: limited by the size of available silicon wafers used as starting material, nowadays 300 mm in diameter. In — good thermal conductivity; practice, the MCP strips would therefore be about 1 mm sec2.qxd 3/5/03 3:41 PM Page 64

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wide and 200 mm long, slightly trapezoidal to better cover the aperture in the radial arrangement, as schematically shown in Fig. 2.12.2/4. Note that the effective area of each strip is highly comparable to the area covered by each shell in a traditional nested system based on electroformed nickel or bent aluminium foils.

The MCP strips are assembled into the X-ray optics using very stiff support structures, made also of Si and produced by either traditional and/or micromachining techniques. The geometry of the support structure is chosen to produce a rigid body and at the same time minimise the projected area in the optical axis. The MCP strips are elastically formed into the required figure. sec3.qxd 3/5/03 3:46 PM Page 65

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3.1 Astrophysics Missions Division 3.5 Space Telescope Operations Division 3.1.1 Herschel 3.1.2 Planck 3.1.3 Eddington 3.6 Science Operations and Data Systems 3.1.4 James Webb Space Telescope Division 3.1.5 Gaia 3.6.1 Overview and general activities 3.1.6 COROT 3.6.2 ISO 3.1.7 Darwin 3.6.3 XMM-Newton 3.1.8 DTP on SMART-2-Plus 3.6.4 Integral 3.1.9 XEUS 3.6.5 Astro-F 3.1.9 ISS payloads: Lobster-ISS, EUSO, ROSITA 3.6.6 Herschel science operations development

3.2 Solar and Solar-Terrestrial Missions Division 3.7 Science Payloads Technology Division / 3.2.1 Introduction and overview Science Payload and Advanced Concepts 3.2.2 Ulysses Office 3.2.3 SOHO 3.7.1 Overview of activities 3.2.4 Cluster 3.7.2 Assessment phase of future missions 3.2.5 Double Star BepiColombo 3.2.6 Solar Orbiter Solar Orbiter 3.2.7 Solar-B Darwin/SMART-3 XEUS International Space Station (ISS) payloads 3.3 Planetary Missions Division 3.7.3 Towards a strategic approach to future mission 3.3.1 Introduction and overview development 3.3.2 Cassini/Huygens 3.7.4 Coordination and development of new payload 3.3.3 Rosetta technologies 3.3.4 Mars Express 3.7.5 Payload support to ESA science projects 3.3.5 SMART-1 3.7.6 Technical infrastructure support to RSSD 3.3.6 BepiColombo research programme 3.3.7 Venus Express 3.3.8 The Cosmic DUNE mission definition study

3.4 Fundamental Physics Missions Division 3.4.1 Introduction 3.4.2 LISA 3.4.3 SMART-2 3.4.4 STEP 3.4.5 Hyper 3.4.6 Microscope sec3.qxd 3/5/03 3:46 PM Page 67

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Chapter 3 addresses the contributions of RSSD Project and Study Scientist support until in-orbit commissioning. Scientists and covers the mission–related activities of the Responsibility for the development and execution of Department. These encompass ESA’s science missions in science operations and, after completion of the in-orbit their orbital and post-operations phases, the approved commissioning phase, for the mission management rests missions under or awaiting development, and missions with the Science Operations and Data Systems Division. under study. ‘Europeanised’ missions led by a national The Space Telescope Operations Divisions hosts the agency and potential International Space Station (ISS) ESA staff supporting the Hubble Space Telescope payload elements are included. Science Institute (STScI) in Baltimore (US) and the European Coordinating Facility (ST-ECF) in Garching The chapter is structured by Division, reflecting the (D). RSSD organisation at the end of the reporting period (see Table 3). As stated in Chapter 1, RSSD has four Missions For the sake of brevity, the instruments, Principal Divisions (Sections 3.1 to 3.4) and two Operations Investigators, mission or interdisciplinary scientists, Divisions (Sections 3.5 and 3.6). The responsibilities and science team members etc. of the missions described are activities of the former Science Payloads Technology not tabulated here. Such information may be found in Division (now the Science Payload and Advanced ESA’s report to COSPAR, the most recent being being Concepts Office) are summarised in Section 3.7. ESA SP-1259 (August 2002), produced by the RSSD Project Scientists, and in the relevant Web pages (the For astronomy missions (excluding HST), the Astro- addresses are included here as footnotes with each physics Missions Division has responsibility for Project mission description).

Table 2: Research and Scientific Support Department 2002 – Projects and Studies.

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

Missions in Ulysses Cassini/ HST ISO Operation or SOHO Huygens XMM Post-Operation/ Cluster -Newton Archive Phase Integral

Missions in or Herschel Double Star Rosetta LISA Astro-F awaiting Planck Solar Orbiter Mars Express Microscope Herschel development Eddington SMART-1 science ops. JWST Venus Express Gaia BepiColombo COROT

Mission and Darwin ILWS SMART-2 ISS Payload XEUS Solar-B Hyper Studies ISS*

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3.1 Astrophysics Missions Division — the extended payload module with a superfluid helium cryostat housing the instrument focal plane 3.1.1 Herschel units, and supporting the telescope, the sun- G. Pilbratt shield/shade and payload-associated equipment; — the service module, providing the infrastructure and The ‘Herschel Space Observatory’ (formerly known as resources such as power, attitude and orbit control, the ‘Far InfraRed and Submillimetre Telescope’, or onboard data handling and command execution, FIRST) is a multi-user observatory-type mission that communications, and safety. targets approximately the 57-670 µm wavelength range in the far-IR and submillimetre spectrum, providing Herschel will be launched by an Ariane-5 shared with observation opportunities for the entire astronomical Planck (see 3.1.2), and will operate from the vicinity of community. Herschel is now being implemented as an L2, 1.5 million km away from the Earth in the anti- element of the next major astronomy mission set in sunward direction. L2 offers a stable thermal ‘Cosmic Vision’, the new ESA Space Science environment with good sky visibility. Commissioning Programme, with a planned launch in 2007. and performance verification will take place enroute Herschel is designed to address the ‘cool’ Universe. It towards L2. Once these crucial mission phases are has the potential of discovering the earliest epoch proto- completed, Herschel will go into routine science galaxies, revealing the cosmologically evolving AGN- operations for a minimum duration of 3 years. starburst symbiosis, and unravelling the mechanisms involved in the formation of stars and planetary system The scientific operations will be conducted in a novel bodies. decentralised manner. The operational ground segment comprises six elements: Herschel will complement other facilities by offering space observatory capabilities in the far-IR and sub- — the Herschel Science Centre (HSC), provided by millimetre for the first time, extending the wavelength ESA; coverage longwards from that of, for example, IRAS, — three dedicated Instrument Control Centres (ICCs), ISO, SIRTF and Astro-F, and shortwards of SWAS and one for each instrument, provided by their PIs; Odin. A major strength of Herschel is its photometric — the Mission Operations Centre (MOC), provided by mapping capability for performing unbiased surveys ESA; related to galaxy and star formation. Redshifted — the NASA Herschel Science Center (NHSC), ultraluminous IRAS galaxies peak in their spectral provided by NASA. energy distributions (SEDs) around 50-100 µm (in their rest frames). Similarly, class 0 proto-star and pre-stellar The HSC acts as the interface to the science community objects also have SEDs that peak in the Herschel prime and outside world in general, supported by NHSC for the band. Herschel is also well equipped to perform US science community. The HSC/NHSC provides spectroscopic follow-up observations to further charac- information and user support related to the entire life- terise particularly interesting individual objects. cycle of an observation, from calls for observing time, to data processing, archiving and distribution to their In order to fully exploit the favourable conditions offered owners. The Science Operations and Data Systems by being in space, Herschel needs a precise, stable and Division is responsible for the implementation of the very low-background telescope and a complement of science operations (Section 3.6.6). very sensitive scientific instruments. The Herschel telescope will be be passively cooled (to maximise size) while the instruments will be housed inside a superfluid 3.1.2 Planck helium cryostat, on top of which the telescope is J. Tauber mounted. The three instruments, provided by consortia led by PIs in return for guaranteed observing time, are: The Planck mission is designed to image the anisotropies of the Cosmic Background Radiation Field (CBRF) over — the Photodetector Array Camera and Spectrometer the whole sky, with unprecedented sensitivity (PACS) is a camera and low- to medium-resolution (∆T/T ~2x10–6) and angular resolution (better than spectrometer for wavelengths up to 210 µm; 10 arcmin). Planck will allow the testing of current — the Spectral and Photometric Imaging REceiver theories of the early Universe and of the origin of cosmic (SPIRE) is a camera and low- to medium-resolution structure. spectrometer for wavelengths longer than 200 µm; — the Heterodyne Instrument for the Far Infrared The ability to measure the angular power spectrum of the (HIFI) is a heterodyne spectrometer. It offers very CBRF fluctuations to high accuracy will allow the high velocity resolution for a single pixel on the sky. determination of fundamental cosmological parameters such as the density parameter and the Hubble constant, The spacecraft has a modular design: with a few percent uncertainty. In addition to the main

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and operated as a PI mission. The instruments are being provided by two PI teams, who will also man and operate two Data Processing Centres responsible for the processing of all Planck data. All-sky maps in 10 frequency bands will be made publicly available a year after completion of the mission, as well as a first generation set of maps of the CBRF, Sunyaev-Zeldovich effect, dust, free-free and synchrotron emission. The time series of observations (after calibration and position reconstruction) will also be made available on-line.

In early 1999, ESA selected two Consortia of scientific institutes to provide the two Planck instruments. LFI is being developed by a Consortium led by R. Mandolesi of the Istituto TeSRE (CNR) in Bologna (I). HFI is being developed by a Consortium led by J.-L. Puget of the Institut d’Astrophysique Spatiale (CNRS) in Orsay (F). In total, more than 40 European and US institutes are collaborating on the development, testing and operation of the Planck instruments and the final data analysis.

In early 2000, ESA and the Danish Space Research Figure 3.1.2: Planck in orbit. (Alcatel Space) Institute (DSRI, Copenhagen) signed an Agreement for the provision of the two reflectors that constitute the Planck telescope. DSRI leads a Consortium of Danish institutes. In late 2000, it issued an Invitation to Tender (ITT) to industry for the development of the Planck cosmological goals of the mission, the Planck sky survey reflectors. The winning bid was by Astrium GmbH will produce a wealth of information on the properties of (Friedrichshafen, D), who will manufacture the reflectors extragalactic sources, and on the dust and gas in our using state-of-the-art carbon fibre technology. At the end Galaxy. For instance, Planck will measure the Sunyaev- of 2002, the design of the reflectors was finished, the Zeldovich effect in many thousands of Galaxy clusters. moulds needed for the layout of the facesheets were advanced, and all was proceeding according to plan. Planck comprises three basic components: In early 1999, ESA selected Alcatel Space (F) to carry —a telescope and baffle system, providing the angular out a detailed study of the architecture of the Planck resolution and rejection of straylight; payload. This study was completed in early 2000, and —a Low Frequency Instrument (LFI), an array of tuned laid the basis for the issue in September 2000 of an ITT radio receivers, based on HEMT amplifiers, to industry for the procurement of the Herschel and covering the frequency range 30-100 GHz and Planck spacecraft. From the submitted proposals, a single operated at 20K; prime contractor, Alcatel Space, was selected in early —a High Frequency Instrument ( HFI), consisting of an 2001. Alcatel Space is supported by two major array of bolometers operated at 0.1K and covering subcontractors: Alenia Spazio (Torino, I) for the Service 100-857 GHz. Module, and Astrium GmbH (Friedrichshafen, D) for the Herschel Payload Module; and by many other industrial Planck will be launched together with the Herschel subcontractors from all ESA member states. The detailed observatory (see 3.1.1). It will be placed into a Lissajous definition work (Phase-B) began in June 2001, and is orbit around the L2 Lagrange point of the Earth-Sun well advanced. The Preliminary Design Review was system. At this location, the payload can be continuously completed in December 2002. The current design of pointed in the anti-Sun direction, thus minimising Planck is shown in Fig. 3.1.2. parasitic signals induced by thermal fluctuations and straylight entering the detectors through far sidelobe. The In parallel, instrument development is proceeding largely spacecraft is spin-stabilised at 1 rpm and the viewing according to schedule, in spite of a number of financial direction of the telescope is offset by 85º from the spin difficulties during 2002. Some hardware subsystems are axis, so that the observed sky patch traces a great circle already being manufactured and tested. The first on the sky. Planck will carry out two complete surveys of deliveries of instrument qualification models are the full sky in about 15 months. expected in late 2003, with the flight models due in early 2005. The development of the spacecraft and payload is Planck is a survey-type project which is being developed on track for a launch in February 2007. sec3.qxd 3/5/03 3:46 PM Page 70

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3.1.3 Eddington telescope and a FOV 5º in diameter. The payload will be F. Favata mounted on top of a copy of the platform used for the Herschel mission. Eddington will be placed into an L2 The two key science goals of the Eddington mission are: orbit by a Soyuz-Fregat vehicle, for 5 years of operations. For 3 years, planet finding will be the primary — to map the interior structure of stars spanning a range science goals, while 2 years will be dedicated to astero- of mass, age and chemical composition; seismologic observations of typically 1-2 months — to detect a significant number of planetary systems duration. The planet-finding programme will consist of spanning a range of planetary sizes and orbital a single, 3-year observation of the same field, allowing periods, with an emphasis on the detection of the detection of repeated transits of planets with periods habitable planets. up to a year.

While the stellar structure will be investigated by means Eddington will be implemented as a facility-type of asteroseismology, planetary systems will be detected mission, fostering a wide involvement of the scientific through the transit method, looking for the minute dips in community. The observing programme will be subject to the starlight caused by a transiting planetary body. Both a broad community consultation. The area to be searched goals require high-precision, wide-field, long-duration for habitable planets will be selected during an open optical photometry, and therefore can be effectively workshop to be held in Palermo (I) in April 2003. The implemented in a single space observatory. pointing directions for the asteroseismic observations will be subject to an AO. All Eddington data will be made The accurate asteroseismic investigations performed by immediately accessible to the entire European scientific Eddington will bring stellar astrophysics to new, community, without any proprietary period. Eddington’s quantitative grounds, allowing, for example, the accurate scientific operations will be carried out by the Eddington dating of individual stars and stellar populations. Open Science Centre (ESC), provided by ESA under the clusters are expected to be among Eddington’s key responsibility of RSSD. The ESC will be the interface to targets, as are old, Population-II stars. Nucleosynthesis the external scientific community, and will ensure that will be studied in detail by mapping the interior structure Eddington data are properly calibrated before being of massive stars, which are the precursors of type-II distributed. supernovae.

Eddington’s goal of finding habitable planets (planets 3.1.4 James Webb Space Telescope with a rocky surface, sufficient gravity to hold an P. Jakobsen atmosphere and a temperature compatible with the presence of liquid water) will have a clear impact on the NASA, ESA and the Canadian Space Agency (CSA) public at large. At the same time, Eddington will provide have since 1996 collaborated on a worthy successor to a large, statistically significant database on the the Hubble Space Telescope, the so-called Next characteristics of planetary systems spanning a broad Generation Space Telescope. The observatory, which is range of parameters (e.g. mass, orbital period, scheduled for launch in the 2010-2012 time frame, was eccentricity), supplying the data needed for a in 2002 renamed the James Webb Space Telescope comprehensive theory of the formation and evolution of (JWST; Fig. 3.1.4), in honour of NASA’s second planetary systems. administrator. ESA’s participation in the mission was formally approved as a Flexi-mission by the Science Long-duration, accurate space-based photometry will Programme Committee in October 2000. also permit a number of additional scientific investigations to be carried out, including the study of JWST is to consist of a passively cooled, 6 m-class long-term variability from, for example, AGN and telescope, optimised for diffraction-limited performance compact binaries, or the detection of transient in the near-IR (1-5 µm) region, but with extensions to phenomena, such as novae and supernovae. either side into the visible (0.6-1 µm) and mid-IR (5- 28 µm) regions. Eddington was originally proposed to ESA in 2000 in the framework of the ‘F2/F3’ call for proposals, and it The large aperture and shift to the IR embodied by JWST was then selected with a ‘reserve’ status. In May 2002, is, first and foremost, driven scientifically by the desire the SPC formally approved it for implementation in the to follow the contents of the faint extragalactic Universe context of the Herschel/Planck project. The target back in time and redshift to the epoch of ‘First Light’ and launch date is 2007. The baseline configuration for the ignition of the first stars. Nonetheless, like its Eddington (subject to confirmation from the ongoing predecessor, JWST will be a general-purpose observa- final study) is a split-aperture four-telescope system tory capable of addressing a very broad spectrum of with a mosaic of CCD camera (six chips per camera), a outstanding problems in galactic and extragalactic collecting area equivalent to that of a 1.2 m monolithic astronomy.

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states, Europe will provide the Optics Module for the Mid-IR Camera/Spectrograph to be developed jointly by NASA and ESA. Both instruments are presently undergoing definition studies in industry and the scientific community; — Non-instrument flight hardware. ESA’s non- instrument contribution to JWST is being negotiated. The possibility of ESA providing the launcher for JWST is being explored; — Contributions to operations. ESA will participate in JWST operations in a similar manner as on HST.

Through its contributions, ESA will gain a ~15% partnership in JWST and secure for astronomers from its member states full access to the observatory on identical terms to those enjoyed today on HST. They will have representation on all advisory bodies of the project and will win observing time through a joint peer-review Figure 3.1.4: JWST concept. (TRW/Ball) process, backed by a guarantee of a minimum ESA share of 15%.

3.1.5 Gaia JWST will carry the following complement of three M. Perryman instruments: By extending the successful Hipparcos concept to fainter — Near-IR Wide Field Camera covering 0.6-5 µm; magnitudes and higher accuracies, Gaia will provide — Near-IR Multi Object Spectrograph covering 1- unprecedented positional and radial velocity measure- 5µm; ments with the precision needed to produce a stereo- — Mid-IR combined Camera/Spectrograph covering 5- scopic and kinematic census of about a billion stars in 28 µm. our Galaxy and throughout the local group. Combined with on-board multicolour photometry, these data will In contrast to HST, JWST will be placed into a Sun-Earth allow us to quantify the early formation and subsequent L2 halo orbit and will not be serviceable after launch. It dynamical, chemical evolution of the Milky Way. will therefore not be possible to repair or replace these Additional scientific output includes the detection and instruments over the lifetime of the observatory. orbital classification of tens of thousands of extra-solar planetary systems, a comprehensive survey of many The JWST telescope proper and its three instruments are different astrophysical sources, from huge numbers of to be cooled in bulk to < 50K, a temperature determined minor Solar System bodies to some 500 000 distant by the operating temperature of the (InSb and HgCdTe) quasars. Gaia will also provide a number of stringent detector arrays covering the prime near-IR 1-5 µm range. new tests of general relativity and cosmology. Cooling is passive by placing the observatory at L2 and keeping the telescope and its instrumentation in perpetual Approval of a Concept and Technology Study for Gaia shadow by means of a large deployable sunshade. was given in 1996. A 1-year industrial study took place between mid-1997 and mid-1998, with the support of an In order to fit into the shrouds of suitable launchers, it is ad hoc scientific advisory group. The resulting report, necessary to fold the primary mirror during launch. The ESA-SCI(2000)4, July 2000, presented the scientific fine pointing required to exploit the telescope spatial case, a technical design, the mission performance resolution will be achieved by deflecting the telescope assessment and a description of the proposed approach to image by means of a fast steering mirror controlled by a the data analysis and mission management. On the basis fine guidance sensor located in the telescope focal plane. of this study, Gaia was selected as one of the next Cornerstone missions of the ESA science programme by ESA’s participation in JWST will follow closely the the SPC in September 2000. The design included two successful HST model, and consist of three main separate astrometric telescopes (viewing directions) each elements: with its own focal plane, and a dedicated telescope for radial velocity and medium-band photometry. Launch — Scientific instrumentation. ESA will provide the was foreseen by Ariane-5, with operation at the L2 Near-IR Multi-Object Spectrograph. In addition, Lagrange point. Through on-board object detection, all through special contributions from its member billion objects down to 20 mag would be observed, with

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resulting astrometric accuracies of about 10 microarcsec a 2.8 x 2.8º FOV at its focal plane. The polar orbit of at 15 mag. COROT allows it to observe two sky directions for 6 months at a time. The long observations imply that At the end of 2001, as a result of the Council Meeting at very high precision will be reached on the oscillation Ministerial Level, the revised ESA science programme frequencies, allowing, for example, the mapping of the funding suggested that the high costs of the major interior rotation of the target stars. Cornerstone missions could not be supported, and a major review of the overall ESA science programme was COROT will be the first space-based search for extra- undertaken by the agency’s advisory bodies, with a target solar planets using the transit method. Its performance date for completion of the review of June 2002. The Gaia will allow it to find large rocky planets in near orbits. project initiated a rapid technical reassessment study, While limited to planets significantly larger than the starting in December 2001 and with a duration of Earth, COROT is thus well-placed to discover the first 6 months. The constraints on the launch vehicle were extra-solar planets around normal stars that are not gas relaxed, and the detailed industrial reassessment study, giants (like all those discovered to date via the radial again supported by the Gaia Science Team, identified a velocity method). In addition, the COROT data will payload design compatible with the smaller and cheaper allow us to study a number of additional science topics, Soyuz launch vehicle, but otherwise maintaining all of including stellar activity and surface rotation. the primary scientific goals. Gaia was confirmed within the ESA programme by the SPC in June 2002, with a Originally proposed in 1996 as a CNES-only mission, a target launch date in mid-2010. number of European partners joined the programme in the course of 1999 and 2000. In particular, the COROT The redesigned mission is now being subjected to project applied for ESA support in 2000 in the context of intensive technical and scientific optimisation and the F2/F3 call for proposals. As a result, a €2million investigation, in which the Gaia Science Team is contribution was approved by ESA’s advisory bodies. supported by 15 scientific working groups focused on Under this scheme, ESA is contributing the telescope particular aspects of the overall design and optimisation. optics and the payload environmental tests. In return, On the technical side, all of the major industrial scientists in ESA member countries will have access to development activities related to the advanced technical COROT data. The satellite is planned for launch at the activities (focal plane, on-board data handling, silicon end of 2005. carbide mirror manufacture, etc), including two major industrial technical assistance contracts, started during 2002. On the scientific side, working groups devoted to 3.1.7 Darwin the satellite design (accuracy, on-board detection, M. Fridlund calibration, etc), to the treatment of specific objects (double stars, variable stars, Solar System objects, etc), Darwin is ESA’s mission to search for terrestrial and to the data analysis activities have made considerable exoplanets, i.e. worlds like our own orbiting other stars, progress. A highlight has been the completion of the first with the explicit purpose of determining their ability to prototype of the data analysis environment for Gaia, host life as we know it. Darwin is baselined as a space- which is successfully handling the ingestion of simulated deployed interferometer, operating in the mid-IR and satellite telemetry, and which will form the basis for consisting of six free-flying telescope units and a more extensive development of the data analysis system separate beam-combiner unit and a communications and over the coming years. control spacecraft. Planned for a launch after 2013, and possibly in a joint mission with NASA, the European The immediate goal is to complete all technical roadmap leading to a Darwin mission is following three development activities, and the associated scientific parallel paths: design, by the end of 2004, allowing for the detailed definition and Phase-C/D of the mission to begin in —a phase of intensive technology development, 2005, consistent with a launch date in early 2010. mainly through Technology Research Programme (TRP) activities with industry and laboratories; — the definition of a ground-based precursor instru- 3.1.6 COROT ment (GENIE: Ground-based European Nulling F. Favata Interferometer Experiment), in close collaboration with ESO. This instrument is being developed with a COROT (COnvection, ROtation and planetary Transits) two-fold purpose. It is primarily to gain the is a CNES-led mission that will perform astero- experience in building and operating such an seismology and planet-finding using the transit method. instrument, including the development of the The mission will be based on a Proteus platform. The required technology. Secondly, it will carry out the payload of COROT consists of a 27 cm-diameter required precursor science. A major disturbing factor telescope and a mosaic CCD camera (of four chips) with in obtaining exoplanetary data in the mid-IR will be

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the large amount of zodiacal dust in the target used by XMM-Newton. Narrow- and wide-field imagers systems, the so-called exo-zodi emission. All Darwin will provide energy resolutions of 500-1000 and 20 at targets will have to be screened in advance in order 1 keV, respectively. The detector spacecraft will to select only those where a planetary signal can be manoeuvre to remain at the focus of the optics. After obtained in a reasonable time. This will be done with using most of its propellant, the detector spacecraft will GENIE; dock with the mirror spacecraft and the pair will transfer — the third avenue is the definition of ways of to the same orbit as the ISS. The mirror spacecraft will cooperation between Darwin and its NASA then dock with the ISS and additional mirror segments counterpart, the Terrestrial Planet Finder (TPF). An will be attached around the outside of the spacecraft. This agreement has been made with NASA for a first increases the mirror diameter to 10 m and the effective 3-year phase of scientific cooperation and area at 1 keV from 6 m2 to 30 m2. An 18-month System technological coordination. The study scientists and Study addressing the critical issues identified in an managers on both sides participate in both studies. earlier feasibility study is imminent. ESA is also represented in the TPF team by two external scientists, while two US scientists are members of the Darwin study team. The aim of this 3.1.10 ISS payloads: Lobster-ISS, EUSO, ROSITA first phase of collaboration is for ESA and NASA to A. Parmar define, by 2007, the final architecture of a joint mission. Lobster-ISS

A new X-ray source may suddenly appear, shine brightly, 3.1.8 DTP on SMART-2-Plus and then disappear a few days later. A highly sensitive M. Fridlund X-ray mission such as XMM-Newton observes only a small region of sky at any one time and could easily miss For SMART-2 (see 3.4.3), the option of including a such unpredictable events. This is where an all-sky X-ray Darwin Technology Package (DTP) to verify the monitor, such as Lobster-ISS, can play a vital role. By technology required for formation flying, was also alerting astronomers to important events occurring actively studied. This necessitated two spacecraft and anywhere in the sky, powerful observatories can be was referred to as ‘SMART-2-Plus’.The DTP package rapidly repointed to take advantage of new opportunities. consisted of the following elements: Formation Flying (deployment, collision avoidance and RF metrology with Lobster-ISS is a proposal to fly an extremely sensitive a precision of about 1 cm), Precision Formation Flying all-sky monitor on the International Space Station (ISS) along one axis (High Precision Optical Metrology with around 2009. It was submitted to ESA in response to the an accuracy of about 1 µm), and verifying the need for an ‘F2/F3’ call for proposals, issued in October 1999. optical delay line in the Guidance, Navigation and Lobster-ISS will use a novel form of micro-channel plate Control (GNC) system. The actual hardware consisted of X-ray optics. It will be the first true imaging X-ray all- a set of RF antennas, an optical metrology bench, a sky monitor and will be able to locate X-ray sources to lateral sensor, a fine longitudinal sensor and an optical within 1 arcmin. Lobster-ISS will produce a catalogue of delay line. All components were to be interfaced into the 200 000 X-ray sources every 2 months which will be GNC. made available via the Internet. As well as providing an alert facility, the high sensitivity will allow many topics to be studied using Lobster-ISS data alone. A 12-month 3.1.9 XEUS Phase-A study started in 2002 is progressing smoothly. A. Parmar

The X-ray Evolving Universe Spectroscopy mission EUSO (XEUS) has been under study as part of ESA’s long-term Horizons 2000 science programme. The key goal is the The Earth is being continuously bombarded by high- X-ray spectroscopic study of the first massive black energy cosmic rays. While those with energies up to holes. By studying how black hole masses and spin rates 1015 eV almost certainly originate from well-understood evolve with cosmic time, astronomers will be able to objects, understanding the origin of cosmic rays with investigate how they grow and the role they play in the energies >5 x 1019 eV is one of the current challenges in evolution of the galaxies. astrophysics. At such extreme energies, cosmic rays interact with the cosmic microwave background and the XEUS will consist of separate detector and mirror distance that a cosmic ray can travel is limited to our spacecraft flying in formation, 50 m apart. XEUS will be galactic neighbourhood. Intriguingly, all the astro- launched by an Ariane-5 rocket after 2012 and have an nomical objects that could produce such cosmic rays lie initial mirror diameter of 4.5 m. XEUS requires a much further away than this. Using double Fresnel lens revolutionary extension of the X-ray mirror technology optics, EUSO will observe the flash of UV fluorescence

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light and the reflected Cerenkov light produced when 3.2 Solar and Solar-Terrestrial Missions Division such a cosmic ray interacts with Earth’s atmosphere. By looking down from the ISS with a 60º FOV, EUSO will 3.2.1 Introduction and overview detect around 1000 events per year, compared to the handful seen so far with ground-based experiments. The Solar and Solar-Terrestrial Mission Division emerged in February 2002 as one of two branches of the The EUSO proposal was submitted to ESA in response to previous Solar System Division. It provides scientific the F2/F3 call for proposals. Following an initial support for all ESA missions in solar, heliospheric and feasibility study, the best way of accommodating such a solar-terrestrial science. This encompasses Ulysses, large (2.5 m-diameter) and heavy (1.4 t) payload on the SOHO and Cluster in their operational phases, Double ISS around 2009 is one of the key topics of the 12-month Star under development and Solar Orbiter in the Phase-A study that began in March 2002. assessment phase. The Division also has responsibility for the management of the missions in the exploitation phase. ROSITA Divisional staff is located at ESTEC, Noordwijk (NL) ROSITA (ROentgen Survey with an Imaging Telescope and at the SOHO Experiment Operations Facility at the Array) is a proposal received by ESA to perform the first NASA Goddard Space Flight Center, Greenbelt (USA), imaging all-sky survey in the medium-energy X-ray where the SOHO Project Scientist Team resides. range using an array of telescopes aboard the ISS. The main scientific goals are to detect all obscured accreting Ulysses has completed its 12th year in orbit and has black holes in nearby galaxies and many new, distant, continued to unveil striking differences in high-latitude active galactic nuclei, to detect the hot intergalactic heliosphere during its second solar maximum orbit in medium in many galaxy clusters and groups and the hot comparison to the data from its first, solar minimum gas in filaments between clusters, to find massive distant orbit. In 2001, NASA approved funding for Ulysses clusters of galaxies and to study the physics of galactic operations until September 2004, in line with the earlier X-ray source populations, such as pre-main sequence SPC decision. As in the past, Ulysses results featured stars, supernova remnants and X-ray binaries. Above prominently at international meetings and in the 2 keV, the proposed ROSITA survey will have 100 times scientific literature. In addition, two books focusing on the sensitivity and better angular resolution than the last the science output of Ulysses, co-edited by the Project all-sky survey in this band, which was performed about Scientist, were published in 2001. 25 years ago. In the 0.5-2 keV, band the ROSITA survey will be more sensitive and have substantially better The SOHO scientific operations, conducted at the energy and angular resolutions than the previous (Rosat) Experiment Operations Facility at GSFC, continued all-sky survey. An initial feasibility study using ESA’s smoothly throughout 2001 and 2002. SOHO remained at Concurrent Design Facility did not reveal any world centre stage in solar physics, with numerous showstoppers and preparations are underway for a coordinated observations with ground observations and Phase-A study. other spacecraft. Science communications and outreach activities were given specific attention by the SOHO Project Scientist Team, contributing to a high visibility of this mission with its spectacular images of the dynamic Sun at solar maximum and with its unique discoveries of processes in the solar interior. A particular milestone was reached in February 2002 when the SPC approved extension of the mission to March 2007. This will ensure observations of the Sun’s evolution over a full solar activity cycle.

A wealth of new scientific results on small-scale structures of magnetospheric boundaries in 3-D is emerging from the Cluster mission. The operations of the spacecraft quartet in its first 2 years in orbit went smoothly and as planned. The scientific value of being able to adjust the spacecraft separation to the appropriate structure size of the region to be studied was clearly proved. A major milestone was reached in February 2002 when the SPC approved both the extension of the mission until December 2005 and the full data coverage along the Cluster orbit. sec3.qxd 3/5/03 3:46 PM Page 75

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ESA’s collaboration with China on the two-spacecraft 3.2.2 Ulysses magnetospheric Double Star Programme was approved R.G. Marsden in mid-2001. The activities mostly related to the support of European space-plasma scientists with Cluster-type Ulysses is an exploratory mission carried out jointly by instruments on the Chinese spacecraft had a slower start ESA and NASA to study the properties of the inter- than expected, but are now progressing well. Delivery of planetary medium and solar wind in the inner heliosphere most of the European instrument flight models to China as a function of heliographic latitude and solar activity. for the first (equatorial) spacecraft is planned for mid- The mission also focuses on the dust and gas components 2003 for launch in December 2003. of the local interstellar medium that gain access to the heliosphere inside the orbit of Jupiter. The European- Following confirmation the Solar Orbiter mission as part built Ulysses spacecraft was launched by the Space of the ‘Cosmic Vision’ programme, activities have Shuttle on 6 October 1990 and a Jupiter gravity-assist focused on the detailed definition of the model payload. manoeuvre, executed in February 1992, deflected the A Payload Working Group comprising experts of the probe into its final high-inclination heliocentric orbit. scientific community, was established in 2002. It has Major milestones of the mission to date include the solar worked closely with the Divisional Study Scientists and minimum traversal of the polar regions in September members of the Directorate’s Science Payload and 1994 (south) and July/August 1995 (north), and the Advanced Concept Office to provide input to a Payload return to high heliographic latitudes, this time near solar Definition Document and to define potential payload maximum, in 2000 and 2001. Ulysses is presently technology developments. engaged in the exploration of the high-latitude heliosphere in the declining phase of solar cycle 23, It is very rewarding to note the continued good focusing in particular on the effects of the polarity performance in-orbit of several instruments built in reversal of the large-scale solar magnetic field. previous years by members of the Solar System Division, including the COSPIN investigation on Ulysses, the LOI Scientific highlights during the reporting period included instruments on SOHO, the GORID dust instrument in the first complete characterisation of the high-latitude geostationary orbit on the Russian Express-II spacecraft, solar wind at solar maximum, the first in situ the MDC dust instrument on the Japanese Nozomi observations of CMEs over the solar poles, the first spacecraft, as well as the electric field (EFW) and observations of solar energetic particle events at high potential control (ASPOC) instruments on Cluster. heliographic latitudes, and the first definitive in situ measurement of the flow direction, speed and tempera- Divisional staff also continued to undertake scientific ture of interstellar neutral helium in the heliosphere. research. This encompasses, in line with the previous activities of the Solar System Division, both the A joint ESA-NASA Mission Operations Team located at development of scientific instrumentation and analysis of the Jet Propulsion Laboratory in Pasadena conducts scientific data, mostly from instrumentation previously spacecraft operations. The spacecraft and its scientific built. payload encountered very few problems during the period covered by this report, and remain in excellent In line with the modified role of the Department, health. As predicted, December 2000 saw the return of hardware development concentrated on the completion the nutation-like disturbance to the spacecraft motion of commitments; no new hardware commitments were that is caused by non-symmetric heating of the axial taken on during the reporting period. The development of boom by incident sunlight. Operational procedures all flight instrumentation for Rosetta (now under the developed prior to the 1994/95 build-up proved highly responsibility of the Planetary Missions Division) was effective in once again controlling the level of nutation to completed. A prototype of the SEPT/IMPACT instrument a point that scientific operations were generally was successfully tested, being developed for flight on unaffected. In recognition of the excellent job done in NASA’s STEREO mission. The SEPT instrument is the controlling nutation throughout the period, the members most recent link in the very successful series of energetic of the Mission Operations Team were awarded both a particle instrumentation built for previous missions. NASA Group Achievement Award, and a special ESA Certificate. On the data analysis side, Divisional staff were involved in work on solar physics (see Section 2.6), heliospheric On the programmatic side, the outcome of the 2001 physics (2.7) and space plasma physics (2.8). The NASA Sun-Earth Connection Missions Senior Review, continued presence of Research Fellows has been an held in July 2001, was generally positive for Ulysses. important prerequisite for maintaining these research NASA approved funding for Ulysses operations until activities. 2004, in line with the earlier SPC decision.

During the reporting period, the ESA Project Scientist, together with his JPL counterpart, E. Smith, provided

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Figure 3.2.2: A comparison of solar wind observations during the pole-to-pole transits near solar minimum (left panel) and around solar maximum (right panel). (Courtesy D.J. McComas, SWRI, San Antonio, US).

scientific advice to the operations team on all mission co-edited by the Project Scientist, were published in aspects, and co-chaired the Science Working Team 2001. (SWT) meetings. Four SWT meetings were held in 2001/2002, two at ESA establishments (ESOC in The ESA Ulysses Data Archive is maintained at ESTEC 2001 and ESTEC in 2002) and two in the USA. In and is mirrored at JPL. Ulysses data are also archived by July 2002, the responsibilities for all aspects of the NASA at the National Space Science Data Center ESA project, including those that were formerly (NSSDC), and form part of the Planetary Data System handled by K.-P. Wenzel, were transferred to the (PDS) archive. The Ulysses Science Working Team, at its Project Scientist. meeting in October 2002, agreed to waive the proprietary 1-year period for exclusive rights to analyse and publish As in the past, the Project Scientist was involved in the their measurements. The most recent Ulysses data (in the organisation of a number of special sessions at interna- majority of cases to mid-2002) are therefore now tional scientific meetings that focused on Ulysses results available in the public domain from dedicated mission and the study of the heliosphere. In keeping with archives. Efforts have also focused on securing new data Ulysses’ key role as a member of the international flotilla submissions, where appropriate, to bring the most of solar and heliospheric missions currently in operation, complete and highest time resolution data into the the project was the focal point of a very successful Ulysses data archives. The CD-ROM archive of the Solar Ulysses-ACE-Voyager joint workshop held in Oxnard, Wind Ion Composition experiment (SWICS) that CA (USA), in October 2001. Ulysses investigators have provides all the instrument matrix rates at the highest continued to publish prolifically, with more than 140 time resolution available is a good example of this. All papers appearing in 2001-2002. In addition, two major Ulysses data can be accessed at http://helio.estec.esa.nl/ books focusing on the science output of Ulysses, ulysses/archive sec3.qxd 3/5/03 3:46 PM Page 77

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3.2.3 SOHO B. Fleck

Since its launch on 2 December 1995, SOHO has provided a wealth of information about the Sun, from the interior, through the atmosphere, and out to the solar wind. Helioseismology data from SOHO have shed new light on a number of structural and dynamic phenomena in the solar interior. The imagers and spectrometers have revealed an extremely dynamic solar surface and atmosphere. Together with the in situ particle experiments and sky mappers, they have greatly expanded our knowledge of conditions in the interplanetary space and how it is affected by the Sun.

At its meeting in February 2002, the SPC approved another mission extension of 4 years through March 2007, allowing SOHO to cover a full 11-year solar cycle.

SOHO remains a busy observatory, with a high number of coordinated observations involving different Figure 3.2.3: SOHO has provided an unparalleled instruments as well as ground-based observatories and breadth and depth of information about the Sun. other spacecraft, mostly with TRACE, RHESSI and Ulysses. The coordinated observing time has increased slightly, and is now at over 12 h per day.

Science operations coordination focuses on maximising was the replacement of NASA’s SOHO Command and the science output of the mission on both short- and long- Data Handling Facility with a highly automated system time scales. Current interests in joint observations are developed by the ESA SOHO Science Data Coordinator. served by facilitating requested joint observing The new service, using primary and backup servers campaigns; possibilities for future analysis is further provided by NASA, has taken over the following enhanced by initiating ad hoc collaborations based on functions: individual instrument plans. —level-0 telemetry processing. Reception of level-0 Science operations coordination also involves telemetry from the NASA ground segment, identifying and resolving technical conflicts between automated distribution of telemetry to the PI teams different instruments and between instrument and with standing requests, and archiving of telemetry spacecraft operations. During exceptional operations, for on-demand retrieval at a later time; such as Emergency Sun Reacquisition and spacecraft — ancillary data processing: Processing of telemetry manoeuvres, instrument activities are scheduled in close and flight dynamics orbit inputs to create and contact with the Flight Operations Team. In particular, distribute the SOHO ancillary data sets. two offpoint manoeuvres and a 360º +90º roll manoeuvre for instrument calibration and special science Thanks to special efforts and a network of personal observations were planned and executed. media contacts, SOHO keeps a high profile in the media. For instance, SOHO observations were featured in 18 The Internet-based approach to science operations stories on CNN.com and five stories on BBCi in the coordination and data dissemination that SOHO reporting period. On 27/28 April 2001 we celebrated pioneered since 1994 is still the cornerstone of the SOHO Sun-Earth Day and SOHO’s 5th anniversary with special information and data system, and continues to grow. An events in 47 cities in 14 European countries, and 12 average of almost 7 million requests were received, and events in the US and Canada. Building on the success more than 950 GB of data were transferred from the from the 5-year celebrations, we supported the EU SOHO servers every month during the last 2 years (up initiative ‘Space Weather and Europe’, part of the from 3.3 million requests and 287 GB during the European Science and Technology Week (4-10 previous period). The increase is in large part due to a November 2002). revamping of the SOHO web pages, and new features such as the ‘SOHO Hot Shots’ and ‘SOHO Weekly We have established an active dialogue with the ESA Picks’. Education Office, providing support for various initiatives (e.g. the Nuna solar car tour, screenings of the Another key development during the reporting period IMAX movie SolarMax, Space Weather and Europe).

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3.2.4 Cluster C.P. Escoubet and M. Fehringer

The aim of the Cluster mission is to study small-scale structures of the magnetosphere and its environment in three dimensions. To achieve this, Cluster comprises four identical spacecraft flying in a tetrahedral formation. The separation distances vary between 600 km and 20 000 km, according to the scientific objectives.

During the reporting period, the Project Scientist and his deputy have devoted a large part of their time to the scientific operations of the Cluster mission. These started, after a 5-month commissioning and verification phase, on 1 February 2001. The excellent status of the spacecraft and instruments soon suggested a mission extension beyond the planned 2 years. It was also quickly realised that the data coverage of about 50% of the time was not fully satisfactory. Abrupt events like solar storms or geomagnetic substorms were missed or not fully recorded. Large regions of the magnetosphere such as the Figure 3.2.4: Cluster orbit (upper) and electric plasmasheet could not be fully covered. Thus, the SPC current in the FTE (lower panel). In red is the current agreed in February 2002 both to extend the mission parallel to the magnetic field and in green operations for three more years up to December 2005 and perpendicular to the magnetic field. (Courtesy of to acquire data over 100% of each orbit. This increase Robert & Roux, CETP, F) could be implemented as early as June 2002 by adding a second ground station and with the very good support from ESOC, the Joint Science Operation Centre (JSOC) and the PI teams.

The Cluster Science Data System (CSDS), which was JSOC, located at Rutherford Appleton Laboratory (UK), specially developed to allow for an easy and fast access was established to support the Cluster Project Scientist in to the Cluster physical parameters measured by the coordinating the complex science operations of the instruments, has been running smoothly since February Cluster mission. Its five main tasks are payload 2001. All instruments are routinely providing data and commanding, payload health monitoring, planning and the PI teams verify and validate them before making information dissemination, delivery and maintenance of them available to the community. Nine national data the command data management system and of the centres from Austria, China, France, Germany, Hungary, CSDSweb. JSOC has operated successfully for 1.5 years. Netherlands, Sweden, United Kingdom and the United States constitute the CSDS. These national data centres Cluster, with four identical spacecraft, can for the first are funded by their national agencies. ESA coordinates time measure physical quantities that cannot be measured the system and provides the user interface to allow a with single- or double-spacecraft missions. For instance, scientific user to query, retrieve and manipulate the data the electric current, which is a source of energy that coming from all instruments. User access to the data deforms the Earth’s magnetic field, can be measured for system is gradually increasing every month. The average the first time with Cluster without any assumptions. By download by scientific users over the last 3 months of combining the measurements of the magnetic field at the 2002 was above 3.5 GB/month. The physical parameters four spacecraft and using Ampere’s law, we obtain the database contains about 14 GB at the end of 2002. current flowing through the volume of space enclosed by the four spacecraft. Fig. 3.2.4 shows the current The CSDS parameters take a few weeks to be generated measured in a flux transfer event (FTE) formed by the after data acquisition owing to the distribution of data on reconnection of a flux tube from the Sun and from the CD-Roms and to the time needed by the PIs to validate Earth. The direction (away from Earth) as well as the the data. For faster access to data, the CSDSweb was value (50 mA km–2 maximum) are obtained without any created. These web pages show data from one spacecraft assumptions. It is also seen that the maximum current is and are produced as soon as the data arrive at ESOC, observed on the edge of the flux tube and mainly parallel which may vary from a few hours to a few days, to the magnetic field (J// dominates). This new finding depending on the ground station visibility, and are then has important implications for modelling these structures made available to the public. CSDSweb software is and, furthermore, our understanding of energy transfer under the responsibility of JSOC. from the solar wind to the magnetosphere.

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3.2.5 Double Star 3.2.6 Solar Orbiter C.P. Escoubet and M. Fehringer R.G. Marsden and B. Fleck

The Chinese Double Star Programme of two satellites The key mission objectives of the Solar Orbiter are: to will study the effect of the Sun on the Earth’s study the Sun from close up (45 solar radii, or 0.21 AU), environment. The equatorial spacecraft (DSP-1) will permitting investigation of the solar surface at high investigate substorm processes as well as the entry of spatial resolution; to study the links between the solar solar particles on the front-side of the magnetosphere. surface, the corona and inner heliosphere during The polar spacecraft (DSP-2) will monitor the energy perihelion passes that are matched to the Sun’s rotation input from the solar wind into the polar ionosphere. The speed; to provide images of the Sun’s polar regions from two spacecraft will be launched in December 2003 and heliographic latitudes in excess of 30º. The mission was June 2004, respectively, into orbits to maximise the originally approved for implementation as a Flexi- conjunctions with Cluster. Half of the payload consists of mission by the SPC in October 2000. Following the European instruments (spares or duplicates of the Cluster reevaluation of the Science Programme in the aftermath instruments); the other half are built by the Chinese. of the November 2001 Council Meeting at Ministerial level, Solar Orbiter will now be implemented together In July 2001, ESA and the Chinese National Space with the BepiColombo mission as a common project. Administration (CNSA) signed the DSP cooperation Launch of all elements of the two missions is foreseen agreement. ESA’s goal in this first collaboration with for 2010-2012. China is to provide unique opportunities for European space plasma scientists. To this end, ESA has been Solar Orbiter’s model payload currently comprises two supporting the refurbishment/rebuilding of the European sophisticated instrument packages: Heliospheric in situ instruments, helped in the pre-integration of the instruments: solar wind analyser, radio and plasma wave European instruments in Europe, will advise China on analyser, magnetometer, energetic particle detector, dust building magnetically clean spacecraft, will increase the detector, neutral particle detector, gamma-ray detector, scientific return of DSP by acquiring 4 h of data per day solar neutron detector. Solar remote-sensing instruments with a European ground station and will coordinate the are: EUV imager, EUV spectrometer, visible-light scientific operations of the European instruments. imager and magnetograph, EUV and visible-light coronagraph, radiometer, X-ray imager and heliospheric In the last 2 years, the Project Scientist and his deputy, in imager. addition to their prime duties on Cluster, have devoted a large part of their time, first in preparing the approval of Activities during the reporting period focused on the the collaboration agreement with China by SPC in May detailed definition of the above model payload 2001 and by Council in June 2001 and then in the instruments. To this end, a Payload Working Group implementation of several of the ESA responsibilities. (PWG) was established in 2002, comprising members of the scientific community with expertise in instrument- Regular meetings with the Chinese and the European PIs ation of the kind envisaged for the Solar Orbiter. The have been arranged and supported to define the interfaces PWG, which has sub-groups for the In-Situ and Remote- and to verify that the Cluster spare models can be Sensing packages, has worked closely with the Study integrated on the spacecraft. In order to keep the European cost to a minimum, the Chinese partners built a special data handling system to match the ‘Cluster interfaces’. This system was successfully tested with all European instruments in September 2002. Figure 3.2.6: Artist’s view of the Solar Orbiter, showing the operational orbit with its progressively It was also decided to reuse as much as possible the increasing inclination. ground data system developed for Cluster. The European Payload Operation Centre (adapted from Cluster’s JSOC) will coordinate the commanding of the European payload and update the Data Management System for Double Star. Similarly the Double Star Data System (DSDS), a subset of the Cluster data system, will be used to distribute the data to the user community.

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Scientists and members of the SCI-A Office to provide 3.3 Planetary Missions Division input to the Payload Definition Document, and to define potential payload technology developments. Another 3.3.1 Introduction and overview PWG task has been the identification of problems to be expected as a result of the extreme thermal and radiation The Planetary Missions Division is the second branch that environment to which the Orbiter will be exposed. emerged from the Solar System Division after the Meetings of the PWG were held in ESTEC in May and reorganisation of the Department in February 2002. The November 2002. In addition to supporting the PWG, the Division provides scientific support for all ESA missions Study Scientists have presented the mission at a number in planetary science: Huygens, the Titan Probe contributed of international meetings addressing the future of solar by ESA to the joint NASA/ESA Cassini/Huygens mission and heliospheric physics. In this regard, Solar Orbiter on course to the Saturnian System; three missions in their enjoys broad international support, and is seen as a key final stages of implementation for launch in 2003-2004, contribution to the International Living With a Star Rosetta, the comet rendezvous mission, SMART-1 and (ILWS) programme. Mars Express. Venus Express was approved in late 2002 with a very ambitious schedule to be launched by end- 2005. The mission to Mercury, BepiColombo, is under 3.2.7 Solar-B reassessment. Huygens is the first mission for which the B. Fleck Division took over responsibility for the mission management in its exploitation phase. Solar-B is an ISAS-led solar physics mission planned as the follow-on to the highly successful Yohkoh (Solar-A). Cassini/Huygens completed its 6-month Jupiter flyby The Solar-B payload consists of a coordinated set of campaign very successfully, providing unique science optical, EUV and X-ray instruments to investigate the observations.It is now en route for Saturn arrival in late interaction between the Sun’s magnetic field and corona. June 2004. The Huygens mission trajectory was changed The result will be an improved understanding of the in 2001 to accommodate a new geometry requirement mechanisms that give rise to solar magnetic variability during the Probe relay phase that will reduce the Doppler and how this variability modulates the total solar output shift received by the Orbiter. This change was necessary and creates the driving force behind space weather. to cope with a design flaw of the Huygens radio receiver Solar-B is scheduled for launch in August 2005. discovered during inflight testing in 2000. In this new scenario, the Probe will be released in late December ESA has been invited to collaborate on Solar-B, 2004 to enter Titan’s atmosphere on 14 January 2005. particularly in data analysis systems and operational ground support from a polar station. ESA will seek SPC For both Rosetta and Mars Express, the reporting period approval to accept this invitation. If endorsed, ESA was very busy, with the flight payloads being completed would provide funds for the use of a Norwegian ground and delivered for integration into the spacecraft and the station, which, owing to its high-latitude location, can extensive environmental test programmes. The activities provide downlink on all passes of Solar-B in its Sun- of the Project Scientist Teams focused on monitoring of synchronous polar orbit. This collaboration would the instrument development, supporting the regular provide the European solar physics community with progress meetings with the experiment teams and the rapid access to the Solar-B data. ESA review cycle, e.g. Experiment Flight Operations Review, Flight Acceptance Review, and Flight and ESA envisages its involvement in Solar-B as an element Mission Readiness Reviews. In addition, the of its contribution to the International Living with a Star development for both the Rosetta and the Mars Express/ (ILWS) programme. The ultimate goal of this Beagle-2 Landers required dedicated coordination programme is to increase our understanding of how the support. It was rewarding to see that the payloads for variability of the Sun affects the terrestrial and other both missions was delivered on time and met the planetary environments, both in the short- and long- specified performance criteria. Specific efforts were also terms, and in particular how mankind and society may be deployed towards the preparations for the science affected by the solar variability and its consequences. operations of these missions.

B. Fleck acted as the prime ESA contact person with SMART-1, the first in the SMART (Small Missions for ISAS. R. Marsden was recently appointed as ESA Advanced Research In Technology) series, will prepare representative on the ILWS Steering Committee. the use of Solar Electric Primary Propulsion for future deep-space missions. SMART-1 hosts seven instruments, some with novel technologies that will be tested during the mission. All instruments were delivered at the end of 2002. In close collaboration with the Projects Department, the Division prepared the science operations activities for the cruise and lunar orbit phase. sec3.qxd 3/5/03 3:47 PM Page 81

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The activities for BepiColombo focused on the detailed 3.3.2 Cassini/Huygens definition of a baseline mission scenario. Two J.-P. Lebreton competitive industrial definition studies were carried out, based on the separate launches of the Mercury Planetary The Cassini/Huygens mission carried out jointly by Orbiter (MPO), to be provided by ESA, and the Mercury NASA and ESA is designed to explore the Saturnian Magnetospheric Orbiter (MMO), to be provided by system and all its elements: the planet and its Japan, with two Soyuz-Fregat launchers in 2011-2012. atmosphere, rings and magnetosphere, and a large Extensive efforts were mounted to include a Mercury number of its moons, particular Titan and the icy Surface Element (MSE) in the mission scenario through satellites. The Cassini/Huygens spacecraft was launched an enlarged international cooperative approach. The in October 1997. The interplanetary voyage of about 6.7 Directorate’s Science Payload and Advanced Concept years included gravity-assist manoeuvres at Venus (April Office, supported by the Project Scientist Team from the 1998 and June 1999), at Earth (August 1999) and at Division, is reassessing the mission scenario and the Jupiter (December 2000) (Fig. 3.3.2/1). After completion model payload in order to optimise the mission and to of the scientifically successful Jupiter 6-month flyby enable the implementation of all three elements, MPO, campaign, the spacecraft is now on a direct trajectory to MMO and MSE, within the programmatic constraints Saturn, where it will arrive in late June 2004. The Saturn (see Section 3.7.2). Orbit Insertion manoeuvre will be executed while the spacecraft is crossing the ring plane on 1 July 2004. This Flight instruments involving Division hardware manoeuvre will place the spacecraft in a 90-day orbit, contributions continued to provide excellent data, which includes the first targeted Titan flyby. The second especially the MDC dust detector on the Japanese (48-day) orbit, which also includes a targeted Titan flyby, Nozomi spacecraft and the GORID dust instrument in will shape the trajectory so that the Huygens mission can geostationary orbit on the Russian Express-II spacecraft. be carried out on the third (32-day) orbit using an Orbiter The GORID instrument was eventually switched off in flyby altitude of 60 000 km (Fig. 3.3.2/2). The Probe will mid-2002, after it had worked well for many years. be released on 24 December 2004, 22 days before Titan encounter. Five days after the release, the Orbiter will Research in the Division concentrated on the analysis of perform a deflection manoeuvre to avoid impacting data from flight instruments where either hardware had Titan. This manoeuvre will also set up the Probe-Orbiter been provided or members of the Division participated as radio communication geometry for the Probe descent Co-investigators based on their expertise in specific areas phase. Huygens’ entry into Titan’s atmosphere is planned of planetary research. A number of activities have been for 14 January 2005. directly related to supporting the implementation of specific missions. During the reporting period, the Project Scientist had to invest a major effort to coordinate and support the Flight hardware development concentrated on the activities to recover the Huygens scientific mission. This completion of the instrumentation for Rosetta, a was done in close collaboration with the Directorate’s responsibility taken over from the former Solar System Division, and on support to instrument development for SMART-1. In expectation of the AO for BepiColombo, no new commitments were taken on in the reporting Figure 3.3.2/1: The Cassini/Huygens trajectory upon period. Instrument pre-development concentrated on the arrival at Saturn. The Huygens mission trajectory study of key elements for a generic dust detector and the was changed in 2001 to accommodate a new geometry support to feasibility studies for miniaturised in situ requirement during the Probe relay phase that composition analysers for planetary landers. reduces the Doppler shift of the radio signal received by the Orbiter. With regard to data analysis, Divisional staff were involved in cometary physics and studies of the properties of interplanetary and interstellar dust grains, comparative planetology and exobiology, the study of terrestrial impact craters, and the study of meteor streams. The excellent work of the Research Fellows in the Division must be acknowledged as a key factor for maintaining these research activities at a high standard.

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3.3.3 Rosetta G. Schwehm

The main goal of the Rosetta mission was a rendezvous with Comet 46P/Wirtanen and included the study of two asteroids during close flybys en route to the comet. Launch was set for 13 January 2003. Following the failure of the new Ariane-5 ECA version during its first launch in December 2002, the vheicle was grounded and the Rosetta launch had to be postponed. Studies have been initiated to work out in detail alternative mission scenarios that will preserve the scientific objectives of the mission and minimise technical risks and the financial impact on the overall Science Programme.

Figure 3.3.2/2: The revised approach strategy for Rosetta will rendezvous with a comet, follow it along its Huygens at Titan. orbit and study the nucleus and its environment in great detail over a heliocentric distance between 4.5 AU and the perihelion passage of the comet. A Lander will be deployed on to the nucleus early in the near-nucleus observation phase. Projects Department, the Huygens Operations Team at ESOC, the Huygens team collocated at JPL in 2002, and The Project Scientist and his team closely monitored the the JPL Cassini Project. The Project Scientist chaired the flight hardware development by supporting regular Huygens Science Working Team meetings and co- Progress Meetings and the Project Reviews. During the chaired with his JPL counterpart the Cassini/Huygens extensive environmental test period at ESTEC they Project Science Group meetings. In late 2002 the Project participated in the flight instrument check-out to fill Scientist took on the additional responsibility of Mission manpower gaps in some Experiment Teams. Manager when the responsibility for the overall management of the mission was transferred from the The team will be responsible for the Rosetta Science Projects Department to RSSD. Operations Centre (RSOC), especially for the consoli-

Figure 3.3.3: The elements of the Rosetta ground system.

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dation of the command sequences for the operation of the The Project Scientist Team (PST) organised a series of science payload. These command files will be submitted meetings with the Mars Express PI teams at ESTEC and to the Rosetta Mission Operations Centre (RMOC) at ESOC throughout the reporting period, under the ESOC (Fig. 3.3.3). The development of the tools for umbrella of the Mars Express Science Working Team. payload operations planning progressed well in the This included two working groups on Science Operations reporting period. In close cooperation with the Mission and Data Archiving. The PST has monitored the Operations Team at ESOC, the RSOC interfaces with the scientific performance of the instruments during their RMOC were tested. The RSOC was ready to support the development phase. It has responsibility for planning the in-orbit payload commissioning phase. scientific operations, including commissioning, in coordination with the Mars Express Payload Operations In parallel, the preparatory work for the Rosetta Science Service (POS), located at the Rutherford Appleton Data Archive was initiated as part of a general ESA Laboratory (UK). Science Data Archive in close collaboration with RSSD’s Science Operations and Data Handling Division. The long mission duration of Rosetta with the prime science 3.3.5 SMART- 1 phase starting only long after launch, makes it mandatory B.H. Foing that a complete, easily accessible database and documentation for both spacecraft and the payload is SMART-1 is the first of the SMART mission series established. Knowledge management and its practical introduced in the ESA Scientific Programme to prepare implementation was therefore brought up as a major new the technology for future major missions. SMART-1 will topic for the Project Scientist Team. In close cooperation demonstrate the use of Solar Electric Primary Propulsion with the Experimenter Teams, a prototype of a (SEPP) for future deep-space missions like Bepi- knowledge database, including documentation, daily Colombo and Solar Orbiter. The SMART-1 scenario aims correspondence and video-taped interviews with team at a transfer of the spacecraft to the Moon. It will members involved in instrument design, manufacturing demonstrate the use and navigation of SEPP with a and calibration has been produced. Stationary Plasma Thruster throughout the cruise phase from geostationary transfer orbit into lunar orbit. SMART-1 will reach the Moon in 15-17 months, entering 3.3.4 Mars Express a polar orbit of 300 x 10 000 km for lunar observations. A. Chicarro Science operations in lunar orbit are baselined for 6 months, with a possible extension. The mission was to The Mars Express mission will be launched in May 2003 be launched nominally in March 2003 as an Ariane-5 from Baikonur aboard a Russian Soyuz-Fregat launcher. piggyback payload into geostationary transfer orbit. The mission comprises an Orbiter to be placed in a quasi- polar martian orbit, with closest approach at 250 km and During the reporting period, the Project Scientist devoted a mission lifetime of one martian year (687 days), and the a large fraction of his time to monitoring the small Beagle-2 probe. Beagle-2 will land at Isidis development of the payload, which includes seven highly Planitia in December 2003 and operate on the martian minaturised instruments incorporating a number of novel surface for about 6 months. In addition to studying the technologies. He organised the preparation of the science surface, subsurface and atmosphere of Mars, the main operations activity in close cooperation with the Project themes of the mission are the search for water at present Team and members of the Rosetta Science Operations and the search for possible signs of life in the history of Centre. He also initated and carried out a very broad the planet. The specific scientific objectives of the orbiter range outreach programme to promote lunar science with are: global high-resolution imaging and imaging of a number of symposia and student workshops. selected areas with super-resolution, global IR mineralogical mapping, sounding of the subsurface structure down to a few km, global atmospheric 3.3.6 BepiColombo circulation study and mapping of the atmospheric R. Grard and H. Laakso composition, study of the interaction of the interplanetary medium with the upper atmosphere, as well as The BepiColombo mission to Mercury was selected as an radio science. The goals of the Beagle-2 lander are: interdisciplinary mission in October 2000. The proposed geology, geochemistry, meteorology and exobiology of space segment consists of three components: a Mercury the landing site. Beagle-2 will use a suite of imagers, Planetary Orbiter (MPO) mostly dedicated to remote organic and mineral chemistry analysers, environmental sensing, a Mercury Magnetospheric Orbiter (MMO) sensors and robotic devices to sample soil and rocks on accommodating field and particle instruments, and a and below the surface. Collaboration with the Japanese Mercury Surface Element (MSE) for in situ observa- Nozomi mission will diversify the scope and enhance the tions. MPO is a nadir-pointing platform that orbits the scientific return of both missions, as they are planet at 400 x 1500 km, whereas MMO is a spinner on complementary in terms of orbits and science goals. an eccentric orbit (400 x 12 000 km) (Fig. 3.3.6). The

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definition studies; interfacing with technological studies and developments, and development of science operation tools.

3.3.7 Venus Express H. Svedhem

Venus Express was proposed to ESA in response to the March 2001 Call for Ideas for reuse of the Mars Express platform. The mission was approved by the SPC in Figure 3.3.6: The BepiColombo MPO orbiter (left) November 2002 for a launch on Soyuz in November and MMO magnetospheric orbiter (right). 2005, thereby making it the fastest-ever developed ESA scientific project. This will be possible due to the rebuild, with only minor modifications, of the Mars Express spacecraft, the availability of scientific instruments and the use of experienced teams from industry and ESA. interplanetary transfer is to be performed with a Solar The scientific payload includes three original Mars Electric Propulsion Module (SEPM) and gravity assist; Express instruments and two original Rosetta the orbit insertion and landing are ensured with a instruments. During the definition study it was found to Chemical Propulsion Module (CPM). The MPO, MSE, be scientifically valuable and technically feasible to SEPM, CPM, launch service segment and cruise replace the standard Mars Express engineering Video operations are to be provided by ESA, the MMO element Monitoring Camera by a scientific instrument, the Venus being contributed by Japan’s Institute of Space and Monitoring Camera (VMC). A magnetometer was added Astronautical Science (ISAS). Launch is foreseen in the to further enhance the payload. 20011/2012 time frame. The Venus Express mission will study the atmosphere Two competing industrial definition studies were and plasma environment of Venus on global and detailed conducted from May 2001 to early 2003. A single launch regional levels. Venus orbit insertion will take place in of the three scientific modules, MPO, MMO and MSE April 2006, followed by a nominal operational phase of with an Ariane-5 was used as the initial baseline. two Venus days (~500 Earth days) and a possible Budgetary constraints imposed on the ESA Scientific extension of another two Venus days. The highly Programme at the November 2001 ESA Council at elliptical polar orbit will have a pericentre altitude of Ministerial Level dictated a redirection to a split launch about 250 km and an apocentre altitude of 66 000 km. on two smaller Soyuz-Fregat rockets. In order to The pericentre will be located at about 70ºN latitude. maintain the full scientific goals of BepiColombo, This orbit is well-suited to remote observations at a including the MSE segment, additional partners willing to join in this international cooperative effort are being identified. In September 2002 the mission moved into reassessment phase, where the payload design and mission implementation profile are being reevaluated for Figure 3.3.7: Venus Express in orbit at its target technical and financial feasibility (see Section 3.7.2). planet. This phase is expected to end in July 2003.

In the reporting period, the Division’s involvement in BepiColombo was primarily in support of a variety of scientific and payload issues. This included participation in the definition of an overall strategy for the mission; definition of the model payload, based on the scientific objectives and together with the external Science Advisory Group; preparation of a draft science management plan; preparation of the Payload Definition Document, and contributions to the Payload Interface Document.

Additional activities included scientific assessment of the synergies and complementarity of BepiColombo and NASA’s Messenger mission; support to Mercury surface and environment modelling; follow-up of the industrial

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global level from high altitude, for detailed studies of the 3.4 Fundamental Physics Missions Division northern hemisphere from low altitude and for in situ measurements covering a large range of distances from 3.4.1 Introduction the planet, at varying solar aspect angles. The selected payload will allow studies of the physics and chemistry In September 2001, the Fundamental Physics Office, of the atmosphere and clouds and the related circulation which had been set up in 1997 following a recommen- at an unprecedented level. In particular, the poorly dation by the SSD Advisory Committee, became the studied lower atmosphere will be probed through the Fundamental Physics Missions Division. Unlike the ‘windows’ in the near-IR wavelengths. The interaction of other divisions in RSSD, this change had no conse- the upper atmosphere with the solar wind will be quences for the functional tasks, manpower allocation investigated by dedicated instruments. and assignment of staff in the Division. During the 2001- 2002 reporting period, the Office/Division supported the The tasks of the Project Scientist, who took over activities described below. responsibilities from the Study Scientist in October 2002, include the coordination of all scientific aspects of the For the ESA/NASA collaborative LISA mission, a study mission and the harmonisation of the requirements of the on laser ranging with centimetre precision, a study on the different experiments, in order to maximise the scientific initial acquisition procedure, the LISA Observatory output from the mission under the given constraints. The Architecture Team (co-chaired by the Project Scientist) preparation for the mission science operations will be an as a scientific advisory group to the Joint System important part of the activities taking into consideration Engineering Board (since October 2002), organising a the very short preparation time until launch. workshop on Time-Delayed Interferometry for LISA, organising the 5th Science & Engineering Workshop and supporting the compilation of the Technology Readiness 3.3.8 The Cosmic DUNE mission definition study and Implementation Plan (TRIP) for NASA. H. Svedhem For the SMART-2 mission, two parallel industrial The Cosmic DUNE (Cosmic Dust Near Earth) mission system-level studies (September 2001 to July 2002), two was submitted to ESA in March 2001 in response to the parallel industrial studies in an extended definition phase Call for Ideas for a low-cost mission based on the reflight (activities started in October 2002 and will continue until of the Mars Express platform. It was proposed as an the foreseen start of the implementation phase in July observatory for the investigation of interstellar dust, an 2003) and the activities of the LTP (LISA Technology important but little-studied component of the interstellar Package) Architect, particularly the design of the inter- medium. It also addressed many questions concerning ferometer for the LTP. the interplanetary dust complex that has only been partially studied. Galactic interstellar dust constitutes the For the NASA/ESA collaborative STEP mission, a solid phase of matter from which stars and planetary pre-Phase-B study (January to October 2002) of the systems form. Interplanetary dust from comets and STEP Service Module, an industrial study on the drag- asteroids represents remnant material from bodies of free control subsystem (April 2001 to October 2002), different stages of early Solar System formation. Data various technical development studies of European from this mission would enable comparison between the payload elements, preparation of the Science Manage- composition of the interstellar medium and primitive ment Plan, and a Phase-A Concept Study in NASA’s planetary objects and so provide insights into the Small Explorer (SMEX) programme (October 2001 to physical conditions during the planetary system April 2002). Unfortunately, NASA’s Office of Space formation. Science in July 2002 announced the non-selection of STEP; all STEP-related activities in ESA were brought to The proposed payload consisted of four co-aligned a close shortly thereafter. instruments for in situ measurements, addressing different aspects of the dust particles encountered, such For the CNES/ESA collaborative Microscope mission, a as composition, mass and dynamical properties. The Phase-A study (mid-2001 to January 2003), preparation Mars Express spacecraft was found to be very well- of the Letter of Agreement between CNES and ESA, and suited for the payload and for the desired position for preparation of the AO and subsequent selection of operation, the Lagrangian L2 point. experiments.

Cosmic DUNE received a ‘high’ scientific rating and was For the Hyper mission, an industrial system-level Phase-A found to be both technically and programmatically study (June 2002 to February 2003) and preparation for feasible, but was not included in the Agency’s Science payload development in ESA’s Technological Research Programme. The RSSD Study Scientist coordinated the Programme in the 2004-2006 time frame. work of the Cosmic DUNE definition study team in 2001. The Division provided the Study Scientists for these sec3.qxd 3/5/03 3:48 PM Page 86

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studies and the Study Manager for the STEP industrial design for the mission and oversee the definition and studies. A senior LISA Mission Scientist from the development, helping to make trade-offs and mission scientific community has been associated with the design choices, NASA and ESA formed a LISA Division since August 2001. A LISA Project Scientist in International Science Team (LIST) in early 2001. LIST RSSD, who also serves as SMART-2 Study Scientist, has has 11 US and 11 European members, including the US been in post since May 2002. A Microscope Project and European Mission and Project Scientists. The day- Scientist, with prime duties in another Division, was to-day scientific work is organised in six working groups. appointed in October 2001. In October 2002, a meeting of the Interferometry Working Group was held at ESTEC to discuss Time With the recruitment of a new staff member (the LISA Delay Interferometry. To employ this technique, the Project Scientist) the Office/Division is now for the first distance between the spacecraft has to be known to better time in the position to start up a research programme in than 30 m. Recent studies supported by the LISA Project fundamental physics. However, it is too early to report Scientist showed laser ranging to be suitable. any results. The last two meetings of LIST (in July 2002 at Penn. State University and in December 2002 at the AEI in 3.4.2 LISA Hannover) brought forward the potential change of the O. Jennrich launcher from the Delta-II 7925H to the more powerful Delta-IV, an identification of items to be included in an The objective of the Laser Interferometer Space Antenna industrial rider study, and a preliminary concept for a (LISA) mission is the detection and observation of ‘minimum mission’. gravitational waves from massive black holes and galactic binaries in the low-frequency range 10–4-10–1 Hz, As LISA presents new challenges to scientists and inaccessible to ground-based interferometers. The LISA engineers alike, regular meetings between both groups are mission comprises three identical spacecraft, located at taking place. The 5th Science & Engineering Workshop the vertices of an equilateral triangle with a baseline of was held at ESTEC in October 2002, supported by the 5million km. The centre of the triangular formation is in Project Scientist. The meeting dealt in large parts with the the plane of the ecliptic, 1 AU from the Sun and trailing preparation of the Technology Readiness and the Earth by approximately 20º (Fig. 3.4.2/1). LISA’s Implementation Plan (TRIP) report, requested by NASA working principle is that of a Michelson interferometer, Headquarters. This report will be reviewed in February obtaining information about amplitude, direction and and March 2003 and is supposed to support NASA’s polarisation of gravitational waves and providing some decision in prioritising either LISA or Constellation-X in redundancy via the third arm. the proposed ‘Beyond Einstein’ theme of NASA.

LISA is an ESA/NASA collaborative mission with a Every 2 years, typically in July, the LISA Team organises nominal launch in 2011. To develop the requirements and a major LISA Symposium, with the venue alternating between the US and Europe. The 4th Int. LISA Symposium was held on 20-24 July 2002 at Penn. State University. The fifth will be held on 12-16 July 2004 at Figure 3.4.2/1: Orbital configuration of the three ESTEC, to be organised by the Project Scientist. LISA spacecraft.

3.4.3 SMART-2 O. Jennrich

SMART-2 is primarily intended to demonstrate the key technologies for the LISA mission. To this end, SMART-2 will accommodate a LISA Technology Package (LTP), provided 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. The LTP and the DRS can be accommodated on a single spacecraft. 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 will be to demonstrate the drag-free system with a

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performance on the order of 10–14 ms–2 Hz–1/2 in the Service Module and a Rockot launch vehicle, while bandwidth 10–3-10–1 Hz. The LISA requirement in the NASA would procure the dewar and the ground segment same band is 10–15 ms–2 Hz–1/2; and be responsible for overall project management, — demonstrating the feasibility of performing laser integration, testing and pre-launch, mission and science interferometry in the required low-frequency regime operations. The payload sharing ratio is 50/50. The with a performance as close as possible to European payload elements are assumed to be nationally 10–12 mHz–1/2in the frequency band of 10–3-10–1 Hz, as funded. STEP was planned for launch in February 2006 required for the LISA mission; into a Sun-synchronous, circular orbit at 550 km altitude. — assessing the longevity and reliability of the capacitive sensors, thrusters, lasers and optics in the From July 1999 to April 2000, ESA carried out an space environment. industrial study of the Service Module at Phase-A level. This was followed by a pre-Phase-B study from January As the environment on the SMART-2 spacecraft will be 2002 to October 2002. An industrial study on drag-free comparatively noisy (in terms of temperature control and algorithm design was started in April 2001 fluctuations and residual forces), the technology and ended in October 2002. On the US side, STEP was demonstrator is aimed at meeting specifications that are selected for a Phase-A Concept Study in NASA’s Small about a factor 10 more relaxed than necessary for LISA. Explorer (SMEX) programme. This study was carried out from May to November 2001. ESA’s share in the The LTP represents one arm of the LISA interferometer; project (Service Module, launch vehicle) was provision- the distance between the two proof masses is reduced ally approved by the SPC in December 2001, subject to from 5 million km to 20 cm. As in LISA, the proof later approval by NASA of its share. masses fulfil a double role: they serve as optical references (‘mirrors’) for the interferometer and as On 2 July 2002, NASA announced the non-selection of inertial references for the drag-free control system. The STEP as a SMEX. It is clear that the continued technical drag-free control system onboard the LTP consists of an problems and consequent delay of Gravity Probe-B had a accelerometer (or inertial sensor), a propulsion system negative influence on the STEP non-selection. If GP-B is (Field Emission Electric Propulsion) and a control loop launched successfully in 2003 and the experiment works using capacitive sensing in three dimensions. The properly in orbit, STEP would have a better chance if distance between the proof masses is obtained by an reproposed to NASA. interferometric measurement system. The various ESA industrial studies were carried out Two parallel industrial system-level studies were carried under the technical, programmatic and budgetary out from September 2001 to July 2002. These definition responsibility of the STEP Study Manager in the studies investigated several mission scenarios involving Division. He worked closely with the US Study Manager one or two spacecraft. In December 2002, it was decided at JPL and with the Science Team at Stanford and that SMART-2 will consist of only one spacecraft supported the SMEX review at Stanford by a NASA housing the LTP and the DRS. The mission is currently Review Committee with a presentation on ESA’s undergoing an extended definition phase that allows us to contributions. He was supported in these activities by the reinvestigate issues specific to the one-spacecraft Study Scientist in the Division. The Study Scientist also scenario. This phase will run from October 2002 until the initiated and monitored various technical development start of the Implementation Phase in July 2003. Advice studies of European payload elements (completed in on the LTP requirements and specifications is provided October 2002), prepared the Science Management Plan by the Project Scientist. and organised a Working Group on test mass material selection, design, fabrication, metrology and verification The SMART-2 launch is currently scheduled for August in the first half of 2002. 2006. Following the commissioning phase, the in-flight demonstration of the LISA technology will take place in the second half of 2006, providing timely feedback for the 3.4.5 Hyper development of the LISA mission to be launched in 2011. R. Reinhard

Hyper (hyper-precision cold atom interferometry in 3.4.4 STEP space) carries four cold-atom interferometers that can be R. Reinhard operated either in the Mach-Zehnder mode to measure rotations and accelerations or in the Ramsey-Bordé mode The Satellite Test of the Equivalence Principle (STEP) is to measure frequencies. The primary scientific objectives a NASA/ESA collaborative project to test the of the Hyper mission are: Equivalence Principle to a precision of 1 part in 1018, an improvement of five orders of magnitude over present — to test General Relativity by mapping for the first knowledge. In this collaboration, ESA would procure the time the spatial (latitudinal) structure (magnitude sec3.qxd 3/5/03 3:48 PM Page 88

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and sign) of the gravitomagnetic (frame-dragging or ESA as the FEEP technology is currently foreseen to fly Lense-Thirring) effect of the Earth with about 10% later on the SMART-2, LISA, Gaia, Darwin, Hyper and precision; GOCE missions. — to determine independently from Quantum Electrodynamics (QED) theories the fine structure A joint CNES/ESA AO was prepared by the Project constant α by measuring the ratio of Planck’s Scientist and released in December 2001 with the aim of constant to the atomic mass one to two orders of Europeanising the payload. Two proposals were received magnitude more precise than present knowledge; from European institutes and, after careful review by — as a secondary objective, to investigate matter-wave ESA’s advisory bodies and the Microscope Project Team, decoherence to set an upper bound for quantum accepted by the SPC in May 2002. ZARM (Bremen, D) gravity models. proposes to perform free-fall tests of the Microscope accelerometers and to do end-to-end simulations of the Atom interferometry also allows us to test the EP measurement. The second proposal was submitted by Equivalence Principle with quantum particles by the ESA Project Scientist and deals with extended FEEP comparing the free fall of two distinct atomic species testing in orbit in view of the importance of FEEPs for (rubidium and caesium). This measurement is comple- ESA’s space science programme. mentary to the Microscope and STEP missions, which investigate the free fall of macroscopic objects. Hyper’s CNES is currently performing the Phase-A study of the atom interferometer should reach an accuracy of about mission; the Phase-A review will be held in May 2003. one part in 1016. The constraints in mass and power The payload has already passed this review and is now in imposed by the satellite make it difficult to pursue both its detailed design phase. A contract for the procurement the measurement of the Lense-Thirring effect and the EP of the complete FEEP micropropulsion system has been test. The EP test is therefore considered as an alternative awarded to Alta (Pisa, I). The Project Scientist has been objective. For the measurement of the gravitomagnetic nominated as ESA’s Directorate of Science represent- effect of the Earth, the four atom interferometers are ative for the FEEP development and is monitoring this operated in the Mach-Zehnder mode; for the measure- contract in close coordination with ESA’s Directorate of ment of the fine structure constant, they are operated in Technical and Operational Support. During the the Ramsey-Bordé mode. development phase, a 1-year endurance test of a flight- representative thruster will be carried out. The date for Hyper was proposed to ESA in January 2000 in response the delivery of the flight propulsion system is set for late to ESA’s Call for Mission Proposals for the second and 2005; launch is planned for late 2006. third Flexi-missions (F2/F3). It was selected for a study at assessment level, which was carried out from March to July 2000 by the Concurrent Design Facility Team at ESTEC. This was followed by a system-level industrial study with Astrium (D) as prime contractor. The study was kicked-off in June 2002 and is expected to finish in March 2003.

A Hyper Symposium was held on 4-6 November 2002 at CNES HQ, Paris. The Study Scientist supported the industrial study and the preparation of the Symposium. He was also actively involved in the discussions on Hyper’s scientific objectives.

3.4.6 Microscope M. Fehringer

Microscope (MICROSatellite à traînée Compensée pour l’Observation du Principe d’Equivalence) is a CNES/ESA collaborative mission to test the Equivalence Principle in space to a precision of 1 part in 1015. It is a low-cost, room-temperature experiment in low-Earth orbit with a total mission cost to CNES of about €15 million. ESA’s share in this collaboration is the provision of the Field Emission Electric Propulsion (FEEP) thrusters for drag-free and fine attitude control of the satellite. This contribution is of particular interest to sec3.qxd 3/5/03 3:48 PM Page 89

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3.5 Space Telescope Operations Division despite the downtime associated with servicing. The net efficiency for HST from 3 July 2001 to 2 July 2002 was The Hubble Space Telescope (HST) programme is the 43.6% for prime observations and 51.0% for prime plus envy of every science facility in the world: it has one of snap exposures. The science data rate increased by more the most recognised names, it is considered as one of the than a factor of two following the installation of the new most effective science mission ever as rated by citations instruments, and the Institute supported this increases. in the science news media, and it is routinely cited as a major reason for increased world-wide interest in HST is also becoming easier to use, thanks to the new astronomy. The demand for telescope time is at a record tools produced at the Institute. Migration of the archive high: more than eight times as much time was requested data to magneto-optical media was completed last in Cycle 11 than was available. autumn. Several new software tools in support of HST operations were released: the Astronomer’s Proposal The Space Telescope Science Institute (STScI) is Tool (APT), StarView and the Space Telescope Grant responsible for all aspects of HST operations and in Management System (STGMS). particular for its scientific productivity. ESA contributes to this effort with the assignment of 15 scientists and The Institute, and in particular the ESA staff, has provided engineers who are fully integrated into the organisational leadership in several important science policy issues. Two structure of the Institute. Some of the senior staff new programmes, the Treasury and Theory programmes, members have achieved significant leadership roles added to the opportunities for scientists to do research within the Institute’s structure and are influential in key with Hubble and its data archives. With Cycle 11 we have areas of the decision-making process. started the Hubble Treasury Program, which had been recommended by the Hubble Second Decade Committee Highlights of the HST programme include notable to stimulate science that might not naturally be enhancements in Hubble’s ability to produce world-class encouraged by the existing process, and, in particular, to science, along with several achievements that gained promote the creation of important data sets that one would worldwide attention. By every measure, HST has more regret not having obtained when Hubble is ultimately science capability now than at any time in its lifetime. It decommissioned. Treasury programmes address multiple has achieved a discovery power 10 times greater than at scientific problems with a single, coherent data set. The the beginning of the reporting period. Institute staff data sets carry no proprietary rights. contributed to all phases of this improvement. There were other novelties in Cycle 11. Given the rate of Some of the most important achievements were the increase in the size of the Hubble data archive and the support for a highly successful SM-3B servicing mission, value of large, homogeneous data sets, we wished to with the installation of a new camera, the Advanced stimulate more ambitious Archival Research (AR) by Camera for Surveys (ACS), and the revival of NICMOS creating the new AR Legacy Programme. Selected through the installation of the NICMOS Cooling System Legacy programmes will perform a homogeneous (NCS). Institute personnel provided key support for this analysis of a well-defined data set in the Hubble archive mission at the technical, scientific and programmatic and will generate data products of use to the scientific levels. The Institute carried out the Servicing Mission community (catalogues, software tools, web interfaces, Orbital Verification flawlessly despite having to modify etc.), which will allow a variety of new investigations. the work plan when it became apparent that the NCS cooling was proceeding much slower than expected. Another important change in Cycle 11 was the start of the Hubble Theory Programme, funded as part of the Hubble Following the SM-3B mission, Early Release AR programme. The Theory Programme stressed the Observations were obtained with the new instruments. importance of promoting theoretical research in ACS produced some spectacular images, both of nearby conjunction with major observing facilities, in order to objects (e.g. the Cone Nebula) and of the distant improve the interpretation and understanding of the data Universe (e.g. in the background of the Tadpole from these facilities. interacting galaxies, where some 6000 galaxies can be seen). These observations were presented in a press Another policy-related topic has been the conference on 30 April 2002, and resulted in an implementation of the project to trade observing time unprecedented worldwide media coverage. The Early between Chandra and HST. This initiative came to Release Observations of the resurrected NICMOS fruition in Cycle 10 and was also advertised in Cycle 11. camera (e.g. of the dusty disc of the galaxy NGC 4013) Both the HST and Chandra Time Allocation Committees demonstrated the camera’s power to peer through the (TACs) and users are very supportive of the concept and dust all the way into the galaxy’s core. The results were we expect that we will soon see the published results presented at a press conference on 5 June 2002. from these joint efforts.

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Cycle 11 was the most oversubscribed Cycle yet, by a 3.6 Science Operations and Data Systems Division factor of 8.5! As judged by an external review committee of the TAC process, the STScI ran the Cycle 11 time 3.6.1 Overview and general activities allocation process ‘in an exemplary fashion’. The Science Operations and Data Systems Division was The On-The-Fly Recalibration (OTFR) capability for formed in early 2001 as part of the reorganisation of the WFPC-2 and STIS was implemented in 2001. This work Department into a more matrix-based structure. It is was originally pioneered by the European Coordination responsible for the development and execution of science Facility (ECF) staff in Garching and later adopted at the operations for astronomy missions and, after completion STScI. Implementation of this capability enables STScI of the in-orbit commissioning phase, takes over overall to provide better service to the user community by project management responsibility. Currently, for Solar providing science data products using the latest System missions, the Division provides support and calibration reference files. With OTFR implementation, plays an oversight role. The Division also provides we are now only storing the raw science data. By support in data systems to the entire Department. The eliminating the archiving of calibrated data sets, we have staff of the Division are located in VILSPA (Villafranca, reduced the media requirements and since August 2001 near Madrid, E), in ESTEC and currently also has one we are able to provide on-line access to the entire Hubble staff member collocated with the Integral Science Data archive. New agreements with the ST-ECF were Centre in Versoix (near Geneva, CH). negotiated to implement the changes arising from OTFR operations. The migration of the HST archive from Sony The key goals of the Division are to: platters to magneto-optical media was completed ahead of schedule, before the end of 2001. — improve the efficiency with which payload operations are prepared, executed and the resulting In summary, these have been two highly productive years data captured, distributed and archived; for the Institute and the Hubble programme. — provide (and ensure) continuity of expertise not only from concept to conclusion but also from mission to mission’ — streamline RSSD-internal information technology support and usage.

To achieve these goals, the approach includes starting work on defining science operations requirements and their associated costs as early as possible in the mission, looking for maximum commonality between in-orbit operations and pre-launch testing and calibration, maximising the reuse of experience, techniques and (if possible) tools between projects, and designing and developing the system in very close contact with the eventual users. The Herschel development (see Section 3.6.6) embodies these principles. Support has been given to early definition of Eddington science operations to help establish realistic costs. The Division has also organised reviews of the science operations of Herschel, Planck, Integral, Rosetta and SMART-1 and supported reviews of Mars Express; these not only establish the current status of the individual project but also help in the transfer of experience.

Archives provide a good current example of cross- project developments reducing costs and reusing expertise and code. A small archive-development group has been set up at VILSPA to provide horizontal support to various missions’ archive projects. A flexible multi- tier architecture and modern technology (Java, XML) is being used to enable reuse of design and code from earlier projects, thereby bringing down both development and maintenance costs, while speeding up development timescales. The modular approach facilitates evolution and port of subsystems without sec3.qxd 3/5/03 3:48 PM Page 91

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affecting other systems, thus assisting in preserving 3.6.2 ISO efficient long-term access to the data from ESA’s science A. Salama missions. Furthermore, the openness of this model allows ESA science archives to interface easily with external The Infrared Space Observatory was the world’s first true archives and applications, thus ensuring their early and orbiting IR observatory. With a pointing accuracy at the full integration in the Virtual Observatory initiatives arcsec level and four highly-sophisticated scientific worldwide. instruments, ISO provided a facility of unprecedented sensitivity and capabilities for exploring the Universe at People in this archive team developed the ISO Data 2.5-240 µm. During its highly-successful in-orbit opera- Archive (first public release in December 1998, tional phase from November 1995 to April 1998, ISO www.iso.vilspa.esa.es/ida) and then reengineered the made some 30 000 individual scientific observations of system to produce the XMM-Newton Science Archive all types of astronomical objects. All the data are (April 2002, xmm.vilspa.esa.es/xsa) in about half the available to the community via the ISO Data Archive time and at one-third the cost. Current activities include (follow the links from the ISO home page at maintenance of the ISO and XMM-Newton archives as www.iso.vilspa.esa.es). well as the development of a general ESA Planetary Science Archive and a browser for the Integral archive. The ISO project is now in its Active Archive Phase, The Planetary Archive is being designed for general- which will run until December 2006. This final phase is purpose use (International Halley Watch campaign, Mars designed to maximise the scientific exploitation of ISO’s Express, Rosetta, SMART-1, etc); the first release with extensive IR database and to leave behind a IHW Giotto data is planned for mid-2003. homogeneous archive with refined data products, as a legacy to future generations of astronomers. During the reporting period, the Division has managed all of RSSD’s computer systems. The work has been For ISO, RSSD has the cradle-to-grave responsibility for organised by platform, namely: the Unix environment ISO’s scientific operations and, from the end of the (mainly Solaris but also LINUX and some Mac OS X commissioning phase, overall responsibility for the systems), primarily orientated towards science project. Currently, the Division has a team of staff and operations and data analysis; the Windows environment, contractors, led by the Project Scientist, in Villafranca, including laboratory control, data analysis and office comprising the ISO Data Centre, whose activities include automation systems; and a small VMS environment for maintaining the central data archive and providing expert data analysis. In addition to maintaining and whenever support to the community across all instruments. The possible improving services for users (such as ISO Data Centre collaborates with National Data Centres availability, reliability, connectivity, back-up, e-mail, at MPIA (Heidelberg, D), SRON (Groningen, NL), MPE WWW, print-sharing, file-sharing, licence serving, etc), a (Garching, D) and RAL (Chilton, UK). Until the end of focus has been placed on merging and streamlining the 2001, there was also a formal involvement of centres in originally separate systems that were a legacy from the Saclay/Orsay (F) and IPAC (USA). long-standing two-division structure of the Department. Significant progress has been made in 2001-2002 and the During 2001, the automatic processing pipeline and merger is expected to be completed during 2003. associated calibration (used to generate the products for the archive) continued to be refined. Then, all data were Other information technology services provided by the reprocessed with the final version of the pipeline to Division include a document management system produce the Legacy Archive. This was released at the end (Livelink), a hierarchical storage management system of February 2002 and represents the best set of products (presently scalable up to 38 TB), the Departmental that can be generated by automatic processing. The ISO WWW site, development of a publications-tracking Data Centre is now stimulating and coordinating database, maintenance of a personnel database and activities to reduce selected data sets systematically by associated mailing lists, various database services hand so as to obtain the ultimate quality data products (LDAP), helpdesk applications and various major and to capture these into the archive (the Expert-Reduced software packages (including user support) such as the Data). Oracle database and the Concurrent Versioning System for software development. Additionally, the Division Regular archive maintenance and improvement activities manages the human resources needed to provide data have continued. Refereed ISO publications have been processing support to the various research topics. tracked and the resulting information incorporated. New ISO catalogues and atlases have been ingested. First sets of expert-reduced data were captured. In addition to previously-existing links to SIMBAD, NED, IPAC/IRAS and ADS, the ISO archive now interacts with CDS/Vizier, HEASARC, ADS and IRSA for display and direct retrieval of ISO data products.

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The ISO archive remains intensively used by the 3.6.3 XMM-Newton astronomical community. There are now over 1300 F.A. Jansen registered users, who in the first 4 years of use have downloaded the equivalent of seven times the total The XMM-Newton X-ray astrophysics observatory number of scientific observations in the archive, a enables astronomers to conduct sensitive X-ray spectro- monthly retrieval rate of around 15%. scopic observations (with simultaneous monitoring at optical wavelengths) of a wide variety of cosmic sources. A major element of the ISO Data Centre’s activities is It was launched in December 1999 and has an expected providing support to the general community on all lifetime of over 10 years. Full information is available via matters regarding ISO data. The deep expertise of the the WWW at http://xmm.vilspa.esa.es/. staff across all four instruments is used in a variety of ways: answering questions sent to the helpdesk facility Its three telescopes and suite of complementary (one per day on average); assisting visitors (28 visits in instruments (EPIC, RGS and OM, used simultaneously) the reporting period); and organising dedicated meetings. are designed to investigate in detail the spectra of cosmic During 2001/2, two large conferences were organised. X-ray sources down to a limiting flux of 10–15 erg cm–2 s–1. These were ‘ISO’s Calibration Legacy’ in February 2001 Sources down to a few times 10–16 erg cm–2 s–1 can be and ‘Exploiting the ISO Data Archive’ in June 2002 (see detected; however, at these low flux levels, source Section 4.1). Each attracted about 100 participants. Also, confusion starts to play a role. The principal character- three small workshops (each with about a dozen people) istics of XMM-Newton are: were held; these gave an intensive 1-week course on a specific aspects of ISO data processing, namely PHT32 —effective aperture of 4500 cm2 at 1 keV (12.4 Å) and Oversampled Mapping. The proceedings are published in 1000 cm2 at 10 keV (1.24 Å); the ESA SP series. — almost constant angular resolution of ~15 arcsec HEW across the full waveband; Another major activity is documentation. Various — X-ray FOV ~30 arcmin; releases of a 5-volume ISO Handbook were made. This — capability of performing sensitive medium-resolution is the definitive standalone guide to the ISO mission and spectroscopy with resolving powers between 100 and to its data products. Volume I gives an overview of the 700 over the wavelength band 5-35 Å (350-2500 eV); mission and the spacecraft and volumes II-V cover the — broadband imaging spectroscopy from 100 eV to four instruments. The legacy version is under preparation 15 keV (0.8-120 Å); and will be released in early 2003. Regular summary — simultaneous sensitive coverage of 1600-6000 Å reports on the recent advances in ISO calibration were (~17 arcmin FOV) through a dedicated optical released. These summarised the activities of all monitor, co-aligned with the X-ray telescopes; participants, including various working groups and the — continuous coverage of a source for up to 42 h. national ISO centres, and made the results easily accessible to the community. The WWW continues to be The Division has overall management responsibility for widely used to disseminate information, with an average the project and is directly responsible for the execution of of three postings per month being made on the ISO the science operations. server, with about one every 2 months being dedicated to outreach. Mission operations for XMM-Newton are conducted from ESOC (Darmstadt, D), while science operations are ISO’s scientific results, impacting astronomical research conducted from VILSPA (Villafranca del Castillo, E). The fields from comets to cosmology, continue to consolidate main tasks of the Science Operations Centre are: the earlier technical and operational success of the mission. In the 2001-2002 period, around 300 papers — monitoring payload operations in real time; appeared in the major refereed journals and many more — performing mission planning and maintaining all in the conference literature. With the ISO data archive contacts with the observers necessary to construct an having establishing itself as a general astronomical optimally efficient schedule. This includes issuing research resource and also as an important tool for and processing announcements of opportunity, as planning future missions, with activities continuing on well as handling Targets of Opportunity; enhancing its contents and functionality, many more — maintaining a variety of XMM-Newton handbooks, astronomical surprises and discoveries from ISO are still including the XMM-Newton users handbook, the expected. users guide to the interactive analysis software, etc; — tracking the maintenance of and implementation of change requests to its operations subsystems by external contractors; — providing the archive containing all science data; — defining, implementing and tracking procedures for operating the scientific instruments;

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— implementing instrument calibration observations, coordinating and participating in their analysis, and delivering finalised calibration files to the community; — pre-release checking of scientific validity of the Science Analysis Software (SAS) and the associated data products.

During the first half of 2001, the emphasis was on ensuring smooth and fast data delivery to the end-users. The mission met with considerable problems in this area, which resulted in unacceptable delays in data delivery. Numerous changes were implemented and additional processing power was made available to the Survey Science Consortium (SSC, PI: M. Watson, Leicester Univ., UK) to cope with the backlog. One of the remaining problems, the generation of science data files for all observations performed before end-2000, was solved by the installation of a separate processing chain, which could regenerate these data by bulk reprocessing of the raw telemetry stream. By August 2001, most of the backlog processing had been executed and a more routine way of working could be adopted. The time between execution of an observation and delivery of the data is now the nominal 3 weeks. Figure 3.6.3: These pictures illustrate the enormous Work continued at ESTEC on developing and enhancing effect that detector cooling has on the amelioration of the SciSIM (Science SIMulator) and the Science radiation induced damage. Panel (a) with detectors at Analysis Software (SAS). Robustness of the SAS, a –80ºC clearly shows many ‘hot pixels’ as artefacts, collaborative development between ESA and the SSC, is whereas they are completely absent at –110ºC (panel a crucial factor in the success of any XMM-Newton data (b). processing. The latest SAS release is capable of routinely processing >98% of all data. SAS and SciSIM work will be transferred to VILSPA by mid-2003. ment by energetic particles, which causes degradation in In close collaboration with a considerable number of performance. Measured in-orbit results match pre-launch independent external advisers, requirements were predictions quite well. In order to ameliorate most of the defined for the XMM-Newton Science Archive. This is degradation incurred to date, it was agreed with the EPIC the final, public repository of all XMM-Newton data. and RGS PIs to cool the detectors by an additional 20- Following the definition of these user requirements, an 30ºC to around –120ºC. This action began in November implementation study concluded that the best option for 2002 and will be completed in early 2003. An indication implementing the archive would be reuse of the highly- of the effect of cooling the XMM-Newton detectors can successful ISO Data Archive software and expertise. be seen in Fig. 3.6.3. This was done and resulted in a well-received first release of the XMM-Newton Science Archive (XSA) in The second Call for Observing Proposals (AO-2) was March 2002, with additional functionality added in a issued in August 2001 and some 860 proposals were second release in November 2002. received. The selection of the AO-2 observing programme met with some delays and was finally ESA took a more active role in defining changes to announced in July 2002. Priority was given to onboard software in response to two anomalies. An completion of the guaranteed time programme so the autonomous switch-off of the EPIC PN thermal controller AO-2 observations started in September 2002. led to the definition and implementation of new software onboard XMM-Newton that will ensure proper remedial In November 2001 a highly successful meeting, ‘New action should such an event ever occur again. The EPIC Visions of the X-Ray Universe in the XMM-Newton and onboard software was modified to ensure filter wheel Chandra Era’, attended by over 300 participants, was closure of the instruments should ground contact be lost held at ESTEC. The proceedings are being issued as an shortly before entering the radiation belts. ESA SP publication.

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Scientist on all matters relevant to optimising the science output of the mission, was appointed. The chairman is Prof. J. Schmitt (Hamburger Sternwarte, Hamburg, D). The group met in March and September 2002 in VILSPA.

Despite its 10-year potential lifetime, only 2 years of operations were initially included in the overall cost. In December 2001, the SPC unanimously approved a 4-year extension until March 2006 and agreed the budget for the first two of those years. Future extension requests will also be based on this rolling 4-year horizon, which enables making longer-term investments aimed at reducing future costs for mission operations, such as porting the operations systems from SCOS-1b to SCOS- 2000.

With a very strong demand for observing time and a rapidly increasing number of XMM-Newton papers appearing in the refereed literature, it is evident that the observatory is fulfilling the scientific expectations of the Figure 3.6.4/1: A first light ISGRI image of Cyg X-1 community. Results from XMM-Newton have already (centre) and Cyg X-3 (upper right) from 16 Novem- challenged and invalidated some hitherto broadly- ber 2002. Energy range 14-60 keV, exposure 4 h. accepted theories and and have provided the basis for (Courtesy IBIS team). new and refined models. Further exciting science is confidently expected.

3.6.4 Integral each fitted with coded masks, and a Spanish-led CCD C. Winkler, A. Parmar and L. Hanson imager (OMC) operating in the Johnson V-band. Figs. 3.6.4/1 and /2 show first-light images from IBIS Integral is dedicated to the fine spectroscopy and fine and SPI. imaging of celestial gamma-ray sources in the energy range from 15 keV to 10 Mev, with concurrent source The Division provides the Project Scientist, who chairs monitoring in the X-ray and optical bands. It was the Integral Science Working Team. It has direct launched on 17 October 2002 from the Baikonur responsibility for the development, operations and Cosmodrome by a Russian Proton. The Launch and Early maintenance of the Integral Science Operations Centre Operations Phase was completed 2 weeks after launch, (ISOC) as well as for coordination of the overall Science with all nominal spacecraft functions having been Ground Segment. As of the formal end of the commiss- verified, and with all subsystems working nominally. ioning phase on 13 December 2002, the Division has Further information is available via the WWW at taken over the overall management responsibility for the http://astro.estec.esa.nl/Integral/isoc/. project.

Integral has two main gamma-ray instruments: a During 2001-2002, the main activities of the Integral spectrometer (SPI) and an imager (IBIS). Both use coded Science Working Team focused on finalisation of the aperture masks for gamma-ray imaging. Developed by a Core Programme observation planning, reviewing the Franco-German-led team, SPI is performing spectral pre-launch calibration results, participating in major ESA investigations of point-like and extended gamma-ray programme reviews (flight acceptance, ground segment sources with unprecedented energy resolution readiness) and scientific support for the planning of the (E/∆E = 500) and sensitivity using Ge detectors cooled performance and verification phase that was conducted to 85K. SPI provides images of the gamma-ray sky with during the 2-month commissioning phase after launch. 2.5º FWHM spatial resolution. IBIS, designed by an Further activities concentrated on the preparation of the Italian-French-led team, is the perfect partner for SPI. It next (5th) Integral scientific workshop. has lower energy resolution (E/∆E = 10) but is able to produce the finest images ever of the gamma-ray sky The Integral Science Ground Segment (SGS) formally owing to its good sensitivity and unprecedented spatial consists of the ESA-provided ISOC, located at ESTEC resolution of 12 arcmin FWHM. To supplement the during the nominal mission phase (until December observations by SPI and IBIS, Integral also carries a 2004), and the nationally-funded Integral Science Data Danish-led X-ray imager (JEM-X) with two detectors Centre (ISDC), located in Versoix (CH). The main inter-

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Figure 3.6.4/2: A SPI spectrum obtained during the solar flare of 10 November 2002 showing gamma-ray lines from activation of local detector material due to solar flare protons and demonstrating the spectroscopic quality of SPI. (Courtesy SPI team).

Figure 3.6.4/3: The blue boxes show the two parts of the Integral science ground segment (ISOC and ISDC) together with the main interfaces and information flows to ESOC.s Mission Operations Centre (MOC), the scientific community and the satellite.

faces and information flows are shown schematically in issued by ISOC in November 2000 with proposals due Fig. 3.6.4/3. The instrument teams also contribute to the from the scientific community by 16 February 2001. The SGS. To support the community, ISOC and ISDC jointly response was overwhelming, with 291 proposals operate a web-based helpdesk system. requesting more than 19 times the open observing time available. This remarkable over-subscription is testament The first Call for Observation Proposals (AO-1) was to the scientific capabilities of the mission and to the sec3.qxd 3/5/03 3:48 PM Page 96

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interest of the astronomical community in the topics that — supporting the instrument teams in instrument Integral addresses. configuration and operations (e.g. telemetry allocation). All proposals were scientifically assessed by an independent Time Allocation Committee (TAC), chaired On the technical side, 2001-2002 marked the coming by Prof. E. van den Heuvel (Univ. Amsterdam, NL). together of all the ISOC software systems shown in the Based on scientific merit, the proposals selected by the left-hand side of Fig. 3.6.4/3. A first release of the TAC still oversubscribe the available time for 1 year by a operational system was available for AO-1 and the factor of ~2. ISOC checked for targets close together in subsequent TAC process. It included a proposal the sky that can be observed in a single pointing, so generation tool (PGT) plus proposal handling software saving observing time through the amalgamation of running in ISOC. The PGT is a Java application that is several independent research proposals. This is downloaded via the Web by a proposer and run locally at particularly important for Integral where the his premises. In addition to capturing the incoming observations are generally long and the fields of view of proposals, the proposal handling system also includes the gamma-ray instruments are very large – the fully capabilities for printing, sorting, viewing and amalga- coded fields of view are 16º (SPI) and 9 x 9º (IBIS). Any mating proposals. After the proposal process was over, scientifically outstanding proposals (grade A) that cannot the observation scheduling system was brought on line. be scheduled during the first year will be carried over to ISOC’s system is largely implemented in Java and an the AO-2 cycle. ORACLE database. The majority of the code was developed in-house but it includes pieces of software The accepted proposals were processed at ISOC into an from ESOC/Flight Dynamics and software from the optimised observing plan consisting of a timeline of OMC PI. The complete ISOC system was used to support target positions, together with the corresponding instru- interface tests and end-to-end tests with the entire ground ment configurations. Optimised observing plans are then segment and the satellite or an overall simulator. Before forwarded to the ESOC MOC for the creation of the launch, the system was also used to support activities like corresponding commands to be sent to the spacecraft fuel budget assessment and long-term planning. It has, of which is, routinely, commanded using a pre-planned course, also been used extensively to support the automatic command sequence. preparation and execution of the PV phase as well as lately the routine phase mission planning. The gamma-ray sky is very variable and interesting new targets may appear unexpectedly anywhere in the sky. With the start of the routine operations phase in late The Integral ground segment is designed to react rapidly December 2002, the community is looking forward to a to these Targets of Opportunity. Observations with new view on the variable gamma-ray sky. Integral may be requested via the ISOC WWW pages. Following a positive decision by the Project Scientist, ISOC will generate a new observing programme, forward 3.6.5 Astro-F it to the MOC, and make it available on the WWW so that M.F. Kessler other coordinated observations can be planned. Astro-F is a Japanese mission with the prime goal of Related to the core tasks of ISOC of processing making a second-generation IR all-sky survey with higher observing proposals and creating observing schedules, sensitivity and longer wavelength coverage than IRAS. ISOC staff, in close collaboration with the Integral Launch is scheduled for 2004. ESA is collaborating with science working team, were involved in a number of ISAS to provide tracking support (use of a second ground activities including: station) and assistance with the survey data reduction (pointing reconstruction) in return for 10% of the — finalising the Core Programme of guaranteed time observing opportunities during the non-survey parts of the observations; mission, to distribute to the ESA community. The SPC — preparation and management of the initial in-flight approved this collaboration in autumn 2000. calibration for the instruments during the Performance and Verification Phase; Regarding tracking support, ESOC, in cooperation with — various case studies to assess in-orbit performance. ISAS and with support from the Division, has drafted the An example is the prediction that the IBIS detector ‘Mission Implementation Requirements Document’ and plane is sensitive to gamma-ray radiation passing ‘Mission Implementation Plan’. For the pointing through the SPI coded mask at ~45º off-axis. This reconstruction and community support activities, which effect can be used to localise strong sources (e.g. will be carried out in VILSPA sharing staff with the ISO GRBs) outside IBIS’ FOV but also imposes Data Centre, a plan has been made covering details of the constraints on the scheduling of some observations necessary software development. so as to minimise the contribution from the few strong ‘contaminating’ sources like the Crab Nebula; In August 2001, the community in Europe was contacted sec3.qxd 3/5/03 3:48 PM Page 97

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to find research groups interested in participating in, and greatly increased interactions between end users and contributing their own resources to, the catalogue system implementers and reduction of the problems production in return for scientific access prior to public inherent in bulk integration of a software system of data release. Some dozen responses were received which significant size. were processed with ISAS. As a result, ISAS are entering into collaborations with a few European institutes. Previously, the development of systems for operations has been separated from facilities developed and used for In summary, activities during the reporting period have, instrument development, test and integration on the in general, been preparatory awaiting completion of the ground. To overcome this, the HSC development formal agreement between ESA and Japan for the supports the concept of ‘smooth transition’. A kernel collaboration. This was achieved in December 2002, so system is rolled out to the instrument teams early the pace of activities will sharply increase. (5 years before launch) for use in tests at instrument level. Then, in parallel with instrument and satellite development, this kernel system is expanded in 3.6.6 Herschel science operations development functionality, used at system level and carried forward to J.R. Riedinger operations. The possible disadvantage of continually expanding a system while it is already in use to archive The Herschel Space Observatory is scheduled for launch and analyse vital data is believed to be more than offset in 2007 (see Section 3.1.1). Its science ground segment is by the advantages of this approach. Benefits of this being implemented in a distributed architecture with the extensive pre-launch use include much more thorough science community being supported by an ESA-provided validation of the flight software, essential for a time- Herschel Science Centre (HSC) located at VILSPA, limited mission, and early detection of inconsistencies Spain (US astronomers supported by the NASA Herschel between different parts of the overall space-ground Science Center at IPAC at CalTech) and instrument system. operations being carried out from three Instrument Control Centres at MPE (Garching, D), RAL (Chilton, Almost from the beginning of this development, ESA UK) and SRON (Groningen, NL). and the PI Teams have made a conscious decision to develop the Herschel Science System as a joint effort. All Within RSSD, the Astrophysics Missions Division has believe that this is the best way of producing a system overall responsibility for the scientific integrity of the that best meets the needs of its end users, despite the fact mission and for providing many of the requirements for that it cannot be completely specified at the start of science operations. The Science Operations and Data development. Systems Division is responsible for implementing the science operations, in close collaboration with the Two years into this development, very significant instrument teams, and will take over overall project progress has been made: management responsibility from the end of the in-orbit commissioning phase. — the user requirements have been consolidated; — the system has passed a System Requirements HSC development started in February 2000. This Review, a Preliminary Design Review, and a Critical development will reuse many of the key operational Design Review for the kernel system that is to be concepts from previous, successful ESA astrophysics delivered to the instrument teams for the start of their missions (ISO, XMM-Newton, Integral). However, instrument-level tests at the beginning of 2003; based not only on progress in software technology and — the kernel system has been integrated and is being computer hardware but also on lessons learned from prepared for System and Acceptance Tests; previous missions, several changes in ESA’s approach to — the infrastructure to further control and coordinate such a Science Centre development are being made. this development is in place, and it seems that the development of Herschel science operations is well As part of the increasing acceptance of object-oriented on track. software development, the HSC software is being developed in Java. For HSC, this gives the advantages of a large degree of platform independence and increases the possibility of reusing software components from one project to another.

The traditional single ‘waterfall’ development (with all components coming together only at the end ) has been replaced by an incremental development with frequent intermediate releases that can be used, and commented on, by end users. The benefits of this approach include

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3.7 Science Payloads Technology Division / Science BepiColombo Payload and Advanced Concepts Office The scientific objectives of the BepiColombo mission 3.7.1 Overview of activities (see also Section 3.3.6) to Mercury are summarised in Fig. 3.7.2/1, while the specific aims of the reassessment The overall responsibilities of the Science Payloads phase can be summarised as follows: Technology Division, which in July 2002 evolved and expanded into the Directorate’s Science Payload and — to reassess in detail the payload design; Advanced Concepts Office (hereafter ‘the Office’) can — to examine the potential for new technology to be be summarised as follows: applied to individual instruments. Optimisation of payload resources through the introduction of — support and manage the assessment phase of future advanced technologies and levels of integration; missions; —to reassess a range of mission implementation — develop a strategic approach to future mission profiles with a view to maximising the scientific development; return, within the associated technical and fiscal — coordinate and develop new payload technologies in constraints; support of the longer-term ESA science programme; — to provide a basic mission design that can achieve — provide scientific and technical support to ESA the scientific objects and is technically and science mission payloads and to the ESA science financially feasible for all the parties involved. project teams; — provide the technical infrastructure in support of the There are three core elements to the mission, which are RSSD research programme. shown schematically in Fig. 3.7.2/2: Mercury Polar Orbiter (MPO), Mercury Magnetospheric Orbiter (MMO), provided by ISAS/Japan, Mercury Surface 3.7.2 Assessment phase of future missions Element (MSE), essentially the lander spacecraft.

The new Science Payload and Advanced Technologies The reassessment has been restricted to MPO and MSE Concepts Office has taken over responsibilities for and, in particular, the optimisation of the payload performing the assessment phase of future missions prior through the use of advanced technologies to improve to a mission entering the definition and development scientific performance while reducing resource phases. The current missions under assessment are: requirements (mass, volume, power etc.). With such an BepiColombo, Solar Orbiter, Darwin/SMART-3, XEUS approach, the mission profile can be modified in such a and ISS payloads. manner as to provide an improved performance and technical feasibility while reducing overall costs. The

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BepiColombo mission should enter the definition/ development phase after the completion of this reassessment, which is envisaged to be completed in July 2003.

Solar Orbiter

The scientific objectives of the Solar Orbiter mission (see also Section 3.2.6) are summarised in Fig. 3.7.2/3. It will form part of the BepiColombo mission group from the Figure 3.7.2/4: The Solar Orbiter near-term schedule. development phase onwards since many of the PDD: Payload Definition Document. technologies required for both missions are common. Technologies such as high temperature solar-arrays, antennae and Solar Electric Propulsion (SEP) are possibly common to both missions so close to the Sun (~ 0.2 AU). The Science Payload and Advanced Concepts Office has, and will continue, this mission assessment, through the conduct of the following key activities:

— detailed evaluation of the proposed model payload in close cooperation with an external Payload Working Group (PWG); — optimisation of payload resources through the introduction of advanced technologies and levels of integration; — development and implementation of a payload technology plan; Figure 3.7.2/5: The Solar Orbiter overall configura- — industrial study of the mission profile options and tion and current characteristics. spacecraft design, making full use of the heritage and technologies of the BepiColombo mission.

The overall schedule related to the assessment activities is summarised in Fig. 3.7.2/4. Solar Orbiter would be ready to enter its development phase by March 2004. The basic configuration is illustrated in Fig. 3.7.2/5 together with the mission’s currently established characteristics.

Figure 3.7.2/3: The basic scientific objectives of the Solar Orbiter mission. Darwin/SMART-3

The scientific objectives of the Darwin mission (see also Section 3.1.7) are summarised in Fig. 3.7.2/6. Darwin has four core building blocks, which the Office is developing so as to be able to move the mission eventually into its definition/development phase. These can be summarised as follows:

— development and implementation of a payload technology plan; — study and implementation of a ground-based nulling interferometer at the ESO-VLTI in collaboration with ESO. This is a key project teaming with the community and is known as GENIE; — study and assessment through the SMART-3 programme of the required in-orbit demonstration technologies such as formation flying; — industrial study of the mission profile options and spacecraft design, making full use of the heritage from SMART-3. sec3.qxd 3/5/03 3:48 PM Page 100

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Original Science Case • to detect the Earth orbiting a G2V star at 1 AU at r = 10 pc in a reasonable time Darwin Mission Development Science Case • to detect the Earth in the habitable zone around a large enough (>500) sample of F, G, K & M-type stars Secondary Scientific Objective • astrophysical interferometry imaging in the near-IR

Figure 3.7.2/6: The basic scientific objectives of the Darwin mission.

Figure 3.7.2/8: The XEUS science objectives.

Figure 3.7.2/7: In-orbit configuration of Darwin.

Figure 3.7.2/9: XEUS docked at the ISS undergoing Darwin is a very complex and technically demanding expansion of the mirror from the initial 4.5 m to 10 m mission that needs to be developed in a careful and step- diameter. wise manner on a number of fronts. Only with this approach can a technically feasible and financially well- bounded mission be able to enter the development phase. The current configuration featuring six spacecraft containing 1.5 m-diameter telescopes covering 5-20 µm as to be able to move the mission into the development and a seventh acting as the beam combiner form the full phase. These are: nulling interferometer operated at 40K is illustrated in Fig. 3.7.2/7. An eighth spacecraft handling communica- — development of a large-aperture segmented high- tions and data processing is also shown. resolution X-ray mirror; — integration and expansion of the mirror system using GENIE represents the demonstration in the near-IR of the International Space Station in-orbit infra- the basic nulling interferometer concept using some of structure. the telescopes at the ESO VLTI. The technology developments focus on many of the technical problems The key technology is, of course, the mirror and its associated with combining the light with the appropriate requirement to provide high resolution (~2 arcsec) with a delays and phase-shifts from the various apertures. large aperture (>10 m2). In addition, it needs to be modular, segmented and low-mass, all of which challenge the basic heritage associated with X-ray mirror tech- XEUS nology. The problems – difficult but not insurmountable – are being handled in the Office through a number of The scientific objectives of the XEUS mission (see also industrial technology development contracts to demon- Section 3.1.9) are summarised in Fig. 3.7.2/8. XEUS has strate at breadboard level the required characteristics and two key building blocks, which the Office is engaged so performance needed in the flight model. sec3.qxd 3/5/03 3:48 PM Page 101

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A single Ariane-5 launch could not lift and deploy in 3.7.3 Towards a strategic approach to future mission orbit a mirror of diameter ~10 m. XEUS overcomes this development limitation by making use of the in-orbit infrastructure currently being developed in low Earth orbit, namely the Future missions proposed through the normal Call for ISS. This requires not only XEUS to be launched into a Ideas and selected for assessment through the fellow-traveller Orbit to the ISS but it must also be able consultative process with the appropriate working groups to dock with the ISS so as to grow the mirror from an and advisory committees need to be strengthened initial 4.5 m diameter to the final 10 m. Fig. 3.7.2/9 through active preparatory work by ESA. To this end, the illustrates XEUS docked to the ISS undergoing the Office has embarked on the study of a number of mirror expansion through the use of ISS robots. Technology Reference Missions (TRMs) with the aim of:

— studying potential future mission profiles; International Space Station (ISS) payloads — identifying key technology areas needing development in a longer-term strategic technology plan; Three science payloads are being studied within the Office — providing early mission support to the scientific at Phase-A level towards a possible phased integration on community to help in developing ‘new ideas’. to the ISS (see also Section 3.1.10). These studies are being conducted in close cooperation with external science A number of TRMs are under study of which a subset, teams as well as the Directorate of Human Spaceflight, providing the overall flavour, is: responsible for ESA’s ISS development. These three payloads are: EUSO (a high-energy cosmic ray observa- —a sample and return mission from a low-gravity tory); Lobster (a medium-energy X-ray transient monitor environment, specifically the martian moon Deimos; using novel X-ray optics); ROSITA (a medium-energy X- —a number of jovian system explorer missions to a ray all-sky survey, essentially a replacement for the failed number of Jupiter’s moons, in particular Europa; Abrixas German national mission). —Venus Aerobot explorers; — gamma-ray astrophysics imaging telescope. While the scientific community would develop the payloads, the uplift, integration and operation would be Such missions should allow mission drivers, mission part of ESA’s responsibility. Figure 3.7.2/10 summarises feasibility and technological developments to be identi- the overall objectives and characteristics of these three fied and provided as input into the wider deliberations of significant astrophysics ISS payloads. the scientific community.

It is clear that as the ISS infrastructure capabilities develop and mature in-orbit the demand in particular 3.7.4 Coordination and development of new payload areas such as astrophysics and solar physics will technologies increase. Additionally, the modalities of studying future payloads and the clarification of responsibilities between The TRMs described above allow for the longer-term the various partners will also need to develop. planning of strategic technologies at both payload and

Figure 3.7.4: The overall flow of the technology plan- Figure 3.7.2/10: The ISS payload objectives and ning and implementation process. characteristics.

ISS Science Payload Objectives EUSO • space-based detection of extremely energetic cosmic rays and neutrinos (> 5x1019 ev) •what are the limits to high-energy cosmic-ray processes, how do they propagate, where do they come from? • open up new channels such as high-energy neutrino astronomy • uses Earth’s atmosphere as a fluorescent detector of cosmic-ray showers Lobster • continual all-sky coverage in the energy band 0.2-3 keV, with new Lobster- eye optics •order-of-magnitude increase in sensitivity cf. previous missions allows first opportunity to achieve long-term coverage of AGN light curves •breakthrough capability in monitoring energetic events such as X-ray bursters, relationships to gamma-ray bursts, supernova shock breakouts, super transients, etc. ROSITA •all-sky survey in energy band 2-10 keV, extending the sensitivity of Rosat to higher energies and bringing higher angular resolution than previous missions at high energies • discover the rare brightest QSO type-2 objects, determine the obscuration budget to black holes in the Universe, and map structure in the Universe sec3.qxd 3/5/03 3:48 PM Page 102

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spacecraft level. This allows therefore long-term needs to 3.7.6 Technical infrastructure support to RSSD be built into overall Science Directorate and Agency- research programme wide technology plans. In addition, the assessment phases of missions described in Section 3.7.2 allow for a The Office also provides the technical infrastructure in detailed assessment of the instruments forming the model support of RSSD’s research programme. In this regard, payload. This assessment not only allows the develop- the Department’s laboratories, test facilities and technical ment of a Payload Definition Document (PDD), which support fall within the responsibility of the Office of forms the backbone of any industrial assessment study, Science Payload and Advanced Concepts. The Office but is the basis for the payload technology plan. The supports the development both of flight instrumentation, Science Payload and Advanced Concepts Office, generally in collaboration with external institutes, as well supported by other parts of the Science Directorate and as applied physics/technology development for longer- ESA, particularly the Directorate of Technology and term potential ESA science missions. The core support Operations Support, has tried to bring together these provided can be summarised as follows: many strands of the long-term and medium-term technologies necessary for ESA’s future science — maintenance of the laboratory infrastructure; missions. This whole process involves identification, — planning of the laboratories’ evolution in terms of management, coordination and finally implementation, internal test facilities, support skills; which are summarised in Fig. 3.7.4. — provision of technical and scientific support to research projects involving flight and technology development hardware; 3.7.5 Payload support to ESA science projects — management of all flight hardware and technology development projects. The Office provides support to ESA science missions, specifically payload support for missions in-orbit and Some of the key flight programme instrument payloads for missions under development. developments underway or nearing completion are:

In the first case there are several areas where effort is — the MIDAS Atomic Force Microscope for Rosetta provided: (Fig. 3.7.6/1). This extremely challenging dust- analysis instrument is now integrated on the — instruments undergoing problems where instrument spacecraft. A spare unit will soon be integrated physics and engineering expertise can be utilised within the laboratory to support calibration, data often in support of a PI team; analysis and cruise phase diagnostics; — instrument performance monitoring to develop a — the impedance probes for the Rosetta Lander; database of instrument heritage and problems, which — the Data Processing Unit for the Rosetta OSIRIS may be useful in the design of future instruments; camera, which is now integrated and fully tested on — collation of instrument development costs including the spacecraft (see Section 2.10.5); in-orbit support in order to mature the instrument — the SPEDE instrument on SMART-1, which development cost models. monitors the electromagnetic environment around the spacecraft resulting from the Solar Electric In the case of missions under development the following Propulsion Module (see Section 2.8.4); additional activities are undertaken: — the detector electronics for the electron and proton telescopes on-board the NASA STEREO spacecraft — reviews of instruments during the development cycle (see Section 2.7.5); in support of the ESA project team as well as the PI- — the Data Processing Unit for the CNES/ESA team; COROT mission (see Section 2.6.7). COROT is an — support to PI-teams in problem-solving and testing. important precursor mission to ESA’s Eddington An example here would be the extensive support mission now entering development as part of the given to the Rosetta COSIMA instrument; Herschel-Planck-Eddington mission group, based — specific payload technology development such as around the common Herschel spacecraft bus. those required for Eddington and Gaia. In the case of Eddington, both the telescope design and the CCD In addition to these flight instrument units, a significant design and procurement for the focal plane cameras effort is underway in support of the research and are technically coordinated through the Office in technology development in the following (non- support of the project and project scientist. For Gaia, exhaustive) areas: the Office experts also support the focal plane technology in cooperation with the Project Scientist; — semiconductor sensors from the UV to the gamma- — cost analysis of payloads under development, both at ray part of the spectrum; the start and end of the cycle, followed by the — superconducting sensors from the near-IR to the soft maturing of instrument cost models. X-ray part of the spectrum; sec3.qxd 3/5/03 3:49 PM Page 103

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— low-mass X-ray optics for planetary exploration and astrophysics; — in situ planetary instrumentation; — gamma-ray astrophysics developments in the field of optics and sensors; — highly integrated analogue and digital electronics; — integrated payload suites for planetary orbiters; — biosensors.

Many of these laboratory developments are carried out in close collaboration with industry and the scientific community. In particular they are generally orientated to the establishment of enabling technologies for the scientific community as building blocks for instruments expected to be required in the long-term on future science missions. Figure 3.7.6/1: The Rosetta MIDAS Atomic Force Microscope. The overall infrastructure support is summarised in Fig. 3.7.6/2. Note that both technical and scientific manpower support (technicians, engineers and applied physicists) are involved. In conclusion, the Office of Science Payload and Advanced Concepts provides broad technical support to the Science Directorate’s instrument and payload developments while assisting in the planning, moulding and assessment of future missions.

Figure 3.7.6/2: The overall infrastructure support provided by the Science Payload and Advanced Concepts Office. sec3.qxd 3/5/03 3:49 PM Page 105

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4. OTHER ACTIVITIES

4.1 Symposia and Workshops organised by RSSD to discuss the mission science and implementation, following the decision, in September 2000, to include ‘The Calibration Legacy of the ISO Mission’, ISO Data Eddington in the scientific programme of ESA (although, Centre, ESA-VILSPA, Spain, 5-9 February 2001 at the time, with a ‘reserve’ status). About 100 participants discussed the scientific goals of Eddington This conference, organised by the ISO Data Centre, took and the various options for the mission’s payload. The place shortly after the ISO Calibration Working Groups workshop attracted a broad variety of scientists, had completed their synthesis of the results of ISO reflecting Eddington’s broad scientific goals. Experts in instrument calibration work. The meeting’s aim was to extrasolar planetary astronomy and in stellar structure focus the memory of the community of involved and and evolution featured prominently, reflecting the two interested experts and to gather in one place the legacy of key scientific goals of the mission. In addition, scientists the ISO calibration work, with emphasis on clear and whose main field is galactic structure, supernovae and thorough exposition of the experience gained and of the gamma-ray bursts, were present. Scientists active in the lessons learned. Particular emphasis was placed on the other high-accuracy space photometry missions relevance of the ISO experience to the calibration of (COROT, MOST, MONS and Kepler), played a very future space missions. important role at the workshop.

The conference attracted almost 100 participants from The Scientific Organising Committee was co-chaired by institutes all over the world involved in a wide range of I.W. Roxburgh of Queen Mary & Westfield College, current and planned Earth- and space-based astronomy University of London (UK) and by F. Favata. The local projects. The participants shared their extensive organisation was performed by colleagues at the Instituto experience of calibration through 65 oral and 33 poster de Astrophysics de Andalucia and Cordoba University. presentations that captured the full range of calibration experience, and much of the mission operational The proceedings of the workshop were published as ESA experience, gained through the decades of the ISO SP-485. mission. Topics addressed included instrument pre- launch and in-flight calibration, the challenges posed by the space environment, detector physics, optical design, 35th ESLAB Symposium, ‘Stellar Coronae in the the establishment of reference source databases, and data Chandra and XMM Era’, ESTEC, 25-29 June 2001 processing, and concluded with a session gathering together lessons of importance for future missions. The symposium covered all aspects of high-energy phenomena in normal stars, ranging from the solar The proceedings were published as ESA SP-481. corona to the coronae of active stars to the role of X-rays in star formation. More than 100 participants from Europe, US and Japan attended the event. ‘The Dark Universe: Matter, Energy, and Gravity’, STScI, Baltimore, Maryland, USA, 2-5 April 2001 Recent observational results from both Chandra and XMM-Newton obviously featured prominently among The goal of this symposium was to bring together the presentations at the meeting, as did solar results physicists and astronomers working on all aspects of based on SOHO and TRACE. These were complemented dark matter and theories of gravity. The topics covered with a number of presentations about key (and yet include: nucleosynthesis, hot gas in clusters, MACHOs, unsolved) theoretical issues, such as the coronal heating WIMPs, rotation curves, gravitational lensing neutrinos, mechanism, the physics of flares, the spatial distribution large-scale flows, dwarf spheroidals, cosmological of stellar coronal plasma, and the nature and presence of parameters from supernovae, the cosmic microwave elemental fractionation and abundance anomalies. background, the cosmological constant and theories of Observational results from previous missions, such as gravity. EUVE, Rosat and SAX were also presented, showing the lasting legacy of these past observatories. The symposium was organised by S. Casertano and M. Stiavelli, together with other colleagues from STScI. The Scientific Organising Committee was co-chaired by F. Favata (who was also responsible for the local organisation) and by J. Drake from the Harvard- The First Eddington Workshop, ‘Stellar Structure and Habi- Smithsonian Center from Astrophysics in Cambridge table Planet Finding’, Cordoba, Spain, 11-15 June 2001 (Massachussets, USA). The 600-pp proceedings of the Symposium (edited by F. Favata and J. Drake) were The first Eddington workshop was the first occasion for published in the Astronomical Society of the Pacific the wide community interested in the Eddington mission Conference Series, as Volume 27. sec3.qxd 3/5/03 3:49 PM Page 106

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‘New Visions of the X-ray Universe in the XMM-Newton the support of the scientific community. Three and Chandra Era’, ESTEC, 26-30 November 2001 workshops, each attended by more than 120 scientists, were conducted with two or three parallel sessions, This symposium focused on those areas in astrophysics chaired by scientists from RSSD and the community. where the results obtained by XMM-Newton and/or Each session concentrated on a theme or a scientific Chandra invalidated current models and allowed the region. The chairmen had pre-selected a list of events creation of much more detailed ones. Examples were the for discussion. At the end of each workshop, the most Log N -Log S in deep fields at high energies (6-10 keV), promising events were selected for further study, with which now largely explains the X-ray background at an assigned coordinator to lead the preparation of a those energies, and the cooling flow model for AGN, publication. which was invalidated by the new observations. The highly successful meeting was attended by over 300 The first workshop covered Cluster observations in the registered participants, who were very enthusiastic about dayside of the magnetosphere, made about 6 months the meeting and the results presented. earlier. Specific attention was given to the bow shock, magnetopause, polar cusp, auroral region and plasma- The proceedings were published as ESA SP-488. sphere. One of the main results of the workshop was the publication of a paper on the black aurora in Nature a few months later. Phoebus Workshops on ‘g-mode Detection Techniques’, ESTEC, May 2001 and June 2002 The second workshop emphasised the magnetotail and mid-altitude polar cusp. It was also the first workshop In 1997, the Phoebus group was formed on the initiative initiating a collaboration with the NASA IMAGE team. of T. Appourchaux. The aim is to detect low-frequency, Both the IMAGE PI and several Co-Is participated. Two low-degree g modes. The group is composed of highlights were the results on thinning and oscillation of B. Andersen (Norwegian Space Center); G. Berthomieu, the plasma sheet and the observation of double cusps. J. Provost and T. Toutain (Observatoire de Nice); W. Chaplin, Y. Elsworth and G. Isaak (University of The third workshop concentrated again on the dayside Birmingham); C. Fröhlich and R. Wachter (World magnetosphere and inner magnetosphere. This time, Radiation Center); D.O. Gough (University of however, the discussions focused on the small spacecraft Cambridge); T. Sekii (National Astronomical Observa- separations (100 km) that were achieved at the beginning tory of Japan); T. Hoeksema, A. Kosovichev and of 2002. Highlights of this workshop were the first P. Scherrer (Stanford University); A .Jiménez (Instituto identification of the various waves present in the de Astrofisica de Canarias) and T. Appourchaux. magnetosheath, using the k-filtering method, and the first multi-point observations of the magnetic reconnection in The 4th and 5th workshops were held in May 2001 and the magnetotail. June 2002, leading to the production of three papers related to g-mode detection (Chaplin et al., 2002, MNRS, More information about the workshops can be found at 324, 910; Gabriel et al., 2002, A&A, 390, 1119; Wachter http://solarsystem.estec.esa.nl/~hlaakso/Cluster/ et al., 2003, ApJ). These workshops focused on using additional information on the internal structure of the Sun (rotational splitting) and on novel statistical IAU Colloquium 186, ‘Cometary Science after Hale- techniques for lowering the upper limit set by the Bopp’, Puerto de la Cruz, Tenerife, Spain, 21-25 January Phoebus group in 2000. These new findings led to a 2002 review talk presented by T. Appourchaux on behalf of the group at the 12th SOHO workshop. A new research The Colloquium, dedicated to the memory of the late direction has been set that may lead the group to propose Prof. Mayo Greenberg, was a follow-up of ‘The First new instrumentation and/or new space missions. International Conference on Comet Hale-Bopp’ held in 1998. Its aim was to cover the progress in cometary science made since 1998. The scientific sessions covered ‘Cluster Workshops’, ESTEC, 3-5 October 2001; the following topics: ESTEC, 5-8 March 2002; RAL, 18-20 September 2002 — Hale-Bopp, what makes a big comet different; The Cluster mission has now been operating for almost — split comets; 2 years. An efficient data analysis phase requires — physical properties of cometary nuclei; exchange of data among the 11 instrument teams as — the relationship between coma abundances and well as discussions on the scientific topics. To this end, nuclear composition; Cluster workshops have been organised by RSSD staff — dust observations and models; (specifically C.P. Escoubet, H. Laakso and A. Masson) — what we can learn from space missions; once every 6 months since the start of operations with — origin and dynamical evolution of comets; sec3.qxd 3/5/03 3:49 PM Page 107

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—a roundtable discussion on how to benefit optimally considerations. The aim was to lay the astrophysical from the new 8-10 m telescopes and space groundwork for locating habitable places in the observations. Universe. New astronomical mission concepts were also an important element of the conference. About 100 participants from 22 countries took part, presenting a total of 111 papers (18 invited and 93 This symposium was organised by A. Clampin-Nota and contributed oral and poster presentations). colleagues.

The colloquium also looked into the relationship between comets and the interstellar medium, where comparison 36th ESLAB Symposium, ‘Earth-Like Planets and between the chemical compositions of the gas and dust of Moons’, ESTEC, 3-8 June 2002 both was a key issue. The 36th ESLAB Symposium covered comparative R. Schulz chaired the Scientific Organising Committee studies of the Earth, Mercury, Venus, Mars, Moon, and is Co-Editor of the proceedings, which will be Galilean moons, Titan and terrestrial exoplanets. The published as a special issue of Earth, Moon and Planets. goal was to review the understanding of their observed similarities and differences, and to give both an Earth- oriented and a cosmic perspective. 11th SOHO Workshop, ‘From Solar Min to Max: Half a Solar Cycle with SOHO’, Davos, Switzerland, 11-15 The Symposium had the following sessions: March 2002 —a family portrait of Earth-like planets and moons; The 11th SOHO Workshop, dedicated to Roger M. — the contribution of space missions for understanding Bonnet, covered the whole field of SOHO science, from Earth-like planets and moons; the deep solar interior out to the solar wind and — Earth as a planet; heliosphere, with special emphasis on solar cycle — methods for comparative planetology; variations. More than 160 participants from all over the — interiors, surfaces, exospheres and impact processes; world discussed the current knowledge about our varying — comparing atmospheres and fluids (with emphasis star in over 180 papers. It was organised around eight on Earth, Mars, Venus, Titan, Europa); sessions: — Earth-like planets and moons in the Galaxy; — habitable Earth-like planets and moons; — Solar Interior and Dynamo Theories; — perspectives for future robotic and human exploration; — Subsurface/Surface Dynamics and Magnetic Fields; —Young Planetary Explorers Special Session. —Total and Spectral Irradiance; — Magnetic Coupling and Dynamics of the Transition The programme was based on comprehensive invited Region and Corona; reviews, supported by interdisciplinary contributed — Coronal Holes and Large-Scale Structures; papers and a large body of posters on specific results, —Transient Events: CMEs, Flares, Energetic Particles; methods and planetary objects. Lectures by J. Head and — Solar Wind and Heliosphere; Apollo 17 astronaut H.H. Schmitt, open to all ESTEC — Is Cycle 23 Normal, Abnormal or a Sign of Long- staff, were well attended. Term Changes? The organisation of the Symposium was led by B. Fleck was a member of the Scientific Organisation B.H. Foing, supported by several other RSSD staff. The Committee, chaired by C. Froehlich. The proceedings proceedings were published as ESA SP-514. More were published as ESA SP-508. information can be found at http://www.rssd.esa.int/ Resources/conferences/eslab36/index.htm

‘Astrophysics of Life’, STScI, Baltimore, Maryland, USA, 6-9 May 2002 ‘Exploiting the ISO Data Archive – Infrared Astronomy in the Internet Age’, Parador of Siguenza, Spain, 24-27 The aim of this symposium was to understand the astro- June 2002 nomical and astrophysical foundations upon which searches for life in the Universe must be based, and The symposium, organised by the ISO Data Centre, which bear on the nature and origin of life. Topics VILSPA (SOC Chair: C. Gry; LOC Chair: P. Garcia- included extrasolar planet searches and properties, the Lario), had a number of objectives, including offering the history of the Solar System, emergence, dust discs, star opportunity to present new results obtained with ISO, and planet formation, interstellar and Solar System with special emphasis given to the generation of chemistry, the habitability of planets, satellites and the catalogues, to projects involving large datasets or Galaxy, strategies for searches, and cosmological systematic data reduction, or any project making use of sec3.qxd 3/5/03 3:49 PM Page 108

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the data with a different purpose to that planned in the to foster the sharing of information and techniques original proposal, as well as offering new ideas and between observers, instrument developers, and collaborations for such projects. Another objective was instrument support teams. About 130 astronomers to encourage new projects by providing inventories of attended the workshop, which included approximately 30 the scientific content of the archive and to advertise the invited talks, 40 posters and time for demonstrations and relevance of the ISO Data Archive for the use of future splinter groups on various topics. infrared science facilities (Herschel, SIRTF, Astro-F, SOFIA, etc.) and solicit suggestions to make the archive The proceedings will be published by the US more useful in this respect. A final objective was to Government Printing Office, NASA and STScI in 2003 facilitate the use of the archive by offering information (Eds. S. Arribas et al.). on the different tools available to work with ISO data and by addressing the relationship of the archive to other databases and virtual observatories. 12th SOHO Workshop, ‘Local and Global Helio- seismology: The Present and Future’, Big Bear Lake, All these points were covered by the active participation CA, USA, 27 October - 1 November 2002 of close to 100 scientists from 13 countries, who gave an equal number of contributions and data-handling The 12th SOHO Workshop was held jointly with the demonstrations. The presentations revealed the existence annual meeting of the Global Oscillation Network Group of many systematic data-reduction projects and (GONG). It focused on the study of the interior of the highlighted the interest of the participants for the Sun from a seismic perspective and the prospects for ingestion of expert-reduced data into the archive as one similar study of Sun-like stars. The workshop provided of the main goals of the ISO Active Archive Phase an excellent opportunity for the scientific community to (running until 2006). The high scientific quality of the pause and reflect on the status of this fertile field, with presentations emphasised the continuing avid interest of more than half a solar cycle of SOHO and GONG the community in ISO data and in mining the wealth of observations. More than 120 participants discussed over its archive in particular. 100 papers addressing a wide variety of topics, including the observational status of low-, medium- and high- The proceedings were published as ESA SP-511. degree p-mode characterisation, low-frequency g-mode detection, solar structure and dynamics, mode excitation and damping, and advances in local helioseismology. ‘Astronomical Data Analysis Software & Systems XII’, There were seven sessions: STScI, Baltimore, Maryland, USA, 13-16 October 2002 — Local and Global Helioseismology; The ADASS conferences provide a forum for scientists — Helioseismic Imaging; and programmers concerned with algorithms, software —Temporal Variations in the Solar Interior; and software systems employed in the reduction and — Irradiance and Helioseismology; analysis of astronomical data. An important element of — From Solar to Stellar Seismology; the programme is to foster communication between — Structure of the Solar Interior; developers and users with a range of expertise in the — Prospects for the Future. production and use of software and systems. The programme consisted of invited talks, contributed papers The proceedings will be published as ESA SP-517. and poster sessions. A number of user group meetings and special interest group meetings were also held during the conference.

The proceedings will be published by ASP. The editors are H. Payne, R. Jedrzejewski and R. Hook.

The 2002 HST Calibration Workshop’, STScI, Baltimore, Maryland, USA, 17-18 October 2002

The workshop featured reports from the commissioning of ACS and the recommissioning of NICMOS. New calibrations and advances in the understanding of STIS, WFPC2, FOS and FGSs were also presented, as well as previews of calibration plans for COS and WFC3, which are planned to be launched during HST Servicing Mission 4 in 2004 or 2005. The workshop was designed sec3.qxd 3/5/03 3:49 PM Page 109

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4.2 Science Communications placed on spacecraft ground tests as well as on the planned science (origins of Solar System; Rosetta – a The prime responsibility for disseminating knowledge comet ride to solve planetary mysteries; life ingredients and information about the goals and achievements of the from comets), and on the technological challenge of ESA Science Programme to the general public rests with long-duration survival. The Project Scientist participated the Science Communications Service. However, RSSD in a press event at Kourou after the Mission Flight Project Scientists and staff provide scientific expertise Readiness Review Board on 13 November 2002. RSSD specifically related to their project or discipline in staff also supported national media events in Munich, support of this responsibility. In the reporting period, this Berlin and London. included providing text and images for leaflets, posters, brochures, press releases and media interviews, as well Both Mars Express and science from Mars attracted as validated background information on ESA science major media attention in 2002. They were the subject of missions, space topics and special features for the ESA 11 web stories, building on the Mars Odyssey science Science public website (http://sci.esa.int). For the latter results on Mars water ice and weather, and the purpose, RSSD staff contributed to 187 web stories in perspective of the ESA Mars Express mission. RSSD 2001 and to 115 stories in 2002. staff also supported the ‘Red Encounter’ initiative of the Science Communications Service. Of the 90 and 93 ESA press releases issued in 2001 and 2002, respectively, 10 and 16 were related to science Communication activities in the reporting period (somewhat less than 27 and 17 in 1999 and 2000). In included the promotion of lunar and planetary science, addition, there were more than 10 press releases issued new technologies, ESA horizons and new methods for by the STScI over the 2 years. ESA staff of the SOHO small space missions and international space exploration. Project Scientist Team also made major contributions, Project Scientists gave interviews to various media together with their NASA colleagues, to keep the high representatives on ESA planetary missions. On the profile of solar science in the media. occasion of the ESLAB Symposium on ‘Earth-like Planets and Moons’ in June 2002, several outreach events were organised. For example, the SMART-1 Project Supporting the Science Communications Service towards Scientist supported interviews on lunar exploration and the general public filming of the spacecraft. A Lunar Base Design Workshop, attended by young scientists, engineers and RSSD staff supported a Science Media day on 18 June architects, held after the Symposium, attracted the 2002 at ESTEC, when the Integral and Rosetta spacecraft interest of the public and media. The Apollo 17 Astronaut were being prepared for shipping to their launch sites. H.H. Schmitt served as a lecturer. RSSD Project Scientists, together with ESA project managers and industry representatives, gave present- The Lunar Explorers Society (LUNEX), created in 2000, ations and interviews. Visits to the spacecraft in their test is a bridge between space agencies and the public inter- environment were included. ested in lunar, planetary and space exploration, empha- sising public outreach and education aspects. At its First The highlight for ESA science in 2002 was the successful Lunar Explorers Convention at Palais de la Découverte, launch of Integral on 17 October. The mission was a Paris in March 2001, the SMART-1 mission and other prime topic for ESA public relations and science ESA planetary missions were highlighted by present- communication activities, with seven ESA press releases ations, models, computer simulations, leaflets, posters and and 10 web stories in 2002. Emphasis was placed on the information for the public. A press conference attracted 70 preparations of the spacecraft and the Proton launch journalists and resulted in good media coverage. campaign from August to October, on the launch and, finally, on the first light from the different instruments at The often spectacular observations and discoveries made the end of 2002. The public appeal of Integral was with SOHO continued to make news headlines, often concentrated along the following lines: it will give new triggered by CNN news stories. Articles about SOHO views of the most extreme environments and from the appeared in several popular magazines. Several film and most violent events far away in the Universe, and will TV crews visited the SOHO Experiment Operations detect radiation from processes that created heavy Facility and SOHO has featured in a number of science chemical elements necessary for life. Media represent- TV stories. SOHO observations and images also play a atives in Europe could follow the video transmission of prominent role in the 40-min giant-screen IMAX the launch at ESOC (the main European press centre), documentary ‘SOLARMAX’ (see www.solarmovie.com). ESTEC, ESRIN and VILSPA. RSSD experts were available at each site for interviews. The international Sun-Earth Day on 27-28 April 2001 provided an exciting opportunity to ponder our links with There was also a high level of public-relations activities our nearest star and to celebrate the discoveries of ESA’s in 2002 on Rosetta (18 web stories). Emphasis was SOHO, Cluster and Ulysses solar observatories. This sec3.qxd 3/5/03 3:49 PM Page 110

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event, held on the 5th anniversary of the SOHO mission, — lectures and tutoring in support of the ESA/IAF was an opportunity to promote public awareness of the initiative, arranging the participation of about 200 dynamics of our Sun and its influence on the Earth. It European students at IAF Toulouse in October 2001, was shown how solar physics research, both from space and at the World Space Congress Houston in October and from the ground, contributes valuable information 2002; that can affect our daily lives. RSSD staff supported — reviews for the SSETI workshop project, where events (in local languages) at more than 40 locations student teams all over Europe built a satellite via the throughout Europe. Web.

RSSD scientists also supported a large number of other ESA Space Science public web site (missions and news): communication activities in 2001-2002, including the Paris Salon at Le Bourget in June 2001, which included a http://sci.esa.int realtime broadcast of the 21 June total solar eclipse from SOHO site: http://sohowww.estec.esa.nl/ Africa, in coordination with SOHO coronal observations. Lunar Explorers Society: http://www.lunarexplorer.org Animations included presentations on space science and Life in the Universe: http://www.lifeinuniverse.org/ technology for the press and public, and a simulated martian landscape featuring a Beagle2 lander.

RSSD support to ESA corporate public relations activities

RSSD staff supported the ESA TV Service in the production of material related to ESA science missions, in a variety of formats covering missions such as Integral, Mars Express and HST.

Support to other outreach initiatives

RSSD staff supported science communications events for the science community at large. These took place, for example, during sessions at IAF, COSPAR and EGS assemblies, where a network of space science communications partners was further developed.

Collaborative science communications events with museums, planetaria and educational institutions in different Member States were supported. Assistance was given in organising exhibition events co-sponsored by ESA featuring ESA space science missions.

Public outreach activities were conducted during the Leonid meteor campaigns in 2001 (from Australia) and 2002 (from Calar Alto observatory, Spain). RSSD staff also served as experts for the ‘Life in the Universe‘ programme, when secondary school students prepared projects on science and art. National winners were presented at a central event at CERN, Geneva in November 2001. The EU Commission programme Netdays to promote the use of new media in education and culture was also supported.

Finally, RSSD staff also served as lecturers or expert reviewers in projects coordinated by the ESA Outreach and Education Office, such as:

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4.3 Other Coordination and Support Activities Telescopes. The proposals are selected by a peer-review process on a yearly basis. The programme started in 2000 EIROFORUM and will finish at the end of 2003. During the three Cycles, some 15 proposals were supported at various Since the early 1950s, a number of powerful research levels. The outcome of the Astrovirtel programme has infrastructures and laboratories used by an extensive been very positive because it not only produced novel network of scientists have been developed and deployed scientific results, such as discovering new asteroids and within Europe by the European Intergovernmental studying supernovae progenitors, but also stimulated the Research Organisation (EIRO). These organisations attention of the community on the huge scientific (including CERN, EMBL, ESA and ESO) have set up a potential of digital on-line archives. Astrovirtel was also coordination and collaboration group (EIROFORUM), instrumental in providing actual science requirements for with their Directors General or equivalent as members. A the design and implementation of a fully-fledged primary goal of EIROFORUM is to play an active role in Astrophysical Virtual Observatory (AVO). promoting the quality and impact of European research through effective high-level inter-organisational interaction and coordination. This is possible by exploiting Opticon the existing intimate links between the member organisations and their respective European research The ST-ECF, on behalf of ESA/RSSD, participated in the communities. EIROFORUM encourages and facilitates Opticon Network, an EC-supported forum for the discussion on issues of common interest, relevant to discussion of initiatives in optical and infrared European research and development, to maximise the scientific astronomy. The ST-ECF completed a feasibility study return and optimise use of resources and facilities by (fully funded by the EC) on the possible implementation sharing developments and results whenever feasible. It in Europe of an ‘Elite Fellowship Programme’, similar to coordinates the outreach activities, including technology the Hubble Fellowship Program in the US. The study was transfer and public education, and simplifies high-level well received by the EC and will be considered for interactions with the European Commission and other implementation in the 7th Framework Plan. organs of the European Union (EU).

A. Gimenez is a member of the ESA EIROFORUM External Research Fellows delegation. During the reporting period, a number of joint projects have been presented to the EC for funding In addition to the internal Research Fellowship including, for example, the European Excellence Fellow- Programme, there are about 20 External Research ship Programme (EEFP) and the European Science Fellows, funded to work 1 or 2 years in ESA Member Teachers Initiative (ESTI). A number of Thematic State institutions outside of their own countries. These Working Groups have also been set up, including those Fellows contribute to research networking in support of on Instrumentation and Grid. ESA missions. Research Fellows working with the ESA SOHO team at NASA/GSFC or at the STScI are also recruited via this scheme. During the reporting period, Astrovirtel/AVO both R. Grard and B.H. Foing were members of the ESA inter-Directorate selection board. The ST-ECF, on behalf of ESA/RSSD, is involved in two Programmes, co-funded by the EC, that aim to implement in two steps a European Astrophysical General Scientific Support Virtual Observatory. The Virtual Observatory is an international astronomical community-based initiative. The existence of an RSSD laboratory with experience in Its goal is to allow global electronic access to the the construction of flight instrumentation (now part of available astronomical data archives of space- and the Science Payload and Advanced Concepts Office) ground-based observatories and sky survey databases. It proved valuable for several external groups. Several also aims to enable data analysis techniques through a Rosetta and SMART-1 experiments that required in- coordinating entity that provides common standards, house support during test programmes conducted at wide-network bandwidth and state-of-the-art analysis ESTEC could be supported on short notice. tools. RSSD staff provided scientific advice and support to and In this context, the ST-ECF is responsible for the participated in committee and working groups not precursor Astrovirtel programme, which provides directly within the purview of the Scientific Directorate specific scientific and technical support to selected and of ESA. These included: proposals based on the exploitation of existing digital archives of astronomical data, in particular those —G.Schwehm continued to provide support to the obtained with the Hubble Space Telescope and the ESO Agency’s Space Debris Working Group. He was also sec3.qxd 3/5/03 3:49 PM Page 112

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nominated as coordinator for all Planetary Protection — RSSD staff also taught space sciences and related activities in the Agency. He represents ESA in the topics in Member State universities and in several COSPAR Planetary Protection Panel and is an instances were also appointed as jury members for observer on NASA’s Planetary Protection Advisory Ph.D. theses. The direct contact between ESA staff Committee. In April 2002, G. Schwehm participated and students and staff at the universities continues to in the COSPAR/IAU Workshop on Planetary be mutually rewarding; Protection in Williamsburg, Virginia, USA, which — M.F. Kessler and K.P. Wenzel were invited to co- was convened to organise, update and consolidate author review papers in fields of their scientific COSPAR’s Planetary Protection Policy; expertise for the book The Century of Space Science, —W.Wamsteker and the Department’s Operations which appeared in 2002. staff at VILSPA, in coordination with ESA's Inter- national Affairs Department, have continued to provide support to the organisation and programme development of the UN/ESA Workshops. This series of workshops has found a special niche in identifying opportunities to use space science in the developing world. Special support was given to the 2001 Workshop in Reduit, Mauritius, where a full session was dedicated to the possibilities for the utilisation of data from SOHO. Also, at a workshop on Space Data Utilization, the possibilities of using the archival data of the ISO and IUE missions were explained. The 10th UN/ESA workshop was held in Cordoba, Argentina. One of the concepts that has arisen out of the deliberations of these workshops is the general model of a World Space Observatory as an effective means of stimulating space science in developing countries, and to generate better opportunities for participation of scientists from developing countries in space science and education. The implementation of this is being studied by an International Committee, the World Space Observ- atory Implementation Committee (WIC), with a membership of scientists from 20 countries; —B.H. Foing supported, as ESA representative, activities of the International Lunar Exploration Working Group (ILEWG), a body charged with developing an international strategy for the exploration of the Moon. He also assisted as an expert the United Nations Space Generation Advisory Council (UNSGAC), in particular for the Space Generation Summit held at the World Space Congress 2002 in Houston; — RSSD staff were active in numerous scientific societies (EAS, EGS, EPS) and some of the Scientific Unions (COSPAR, IAU, URSI, IUPAP), where they contributed to scientific meetings (e.g. EGS, COSPAR) by organising special sessions and discussions, and, in some cases, holding elective offices. For example, W. Wamsteker is a member of the Executive Working Group of the IAU for Future Large Scale Facilities, and K.-P. Wenzel is Chairman of COSPAR Scientific Commission D on Space Plasmas in the Solar System, and Chairman of IUPAP Commission C4 on Cosmic Rays; sp1247s4.qxd 3/5/03 3:58 PM Page 113

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ANNEX 1: MANPOWER DEPLOYMENT

Department Office, ESTEC Giardino, G. (to January 2001), Cosmology studies. Jansen, R. (to December 2001), Optical/UV astronomy. Head of Department Katz, D. (to Septermber 2001), Optical astronomy. Gimenez, A. (from July 2001). Nevalainen, J. (to August 2001), X-ray astronomy. Papadopolous, P., Interstellar medium. Chief Scientist Sidoli, L. (to June 2001), X-ray astronomy. Foing, B.H., SMART-1 Project Scientist, comparative Stankov, A. (from February 2002), Analysis of stellar planetary and astrobiology, solar-stellar physics. seismology.

Administrative staff Young Graduate Trainees Bingham, C., Departmental Administrative Assistant. Aigrain, S. (to September 2001), Algorithm for exo- Fontaine, R., RSSD Project Controller. planet transit detection. Ihaddadene, S., Divisional Secretary and Administrative Carpano, S. (to September 2002), Exoplanet transits with Assistant. Eddington. Nilsson, C. (to July 2002), Divisional Secretary and Administrative Assistant. Stagiaires Schroeder, B., Divisional Secretary and Administrative Chico, A. (March-August 2001), GENIE configuration. Assistant. Drummond, R. (July-September 2002), Spacecraft jitter Villien, C. (from November 2002), Divisional Secretary simulations for Eddington. and Administrative Assistant. Hijmering, R. (May-September 2002), Quicklook data analysis software for STJs.

Astrophysics Missions Division Portuguese/Spanish Trainees Franco, G. (to October 2002), Planck/XMM. Clavel, J., Head of Division (from April 2002), Perez Ramirez, D. (from May 2002), XMM data Multiwavelength Observational Astronomy. analysis. De Bruin, J., (from October 2002), Support Scientist on Silva, B. (from November 2002), Eddington data Gaia. analysis. Favata, F., Eddington Study Scientist, COROT Project Scientist, support to GAIA studies, cool stars and Contractor Staff (full- or part-time during the reporting stellar activity, X-ray astronomy. period) Fridlund, M., IRSI/Darwin Study Scientist, astrophysics Bremer, M., Planck ground segment system engineering of star formation. and web support. Heras, A., Herschel scientist, infrared astronomy. Jakobsen, P., JWST Study Scientist, optical/UV astronomy with HST and ground-based astronomy. Solar and Solar-Terrestrial Missions Division Laureijs, R.J. (from December 2001), Planck Deputy Project Scientist, interstellar medium, dust properties. Wenzel, K-P., Head of Division, Deputy Head of Parmar, A., Acting Integral Project Scientist, XEUS, Department, energetic particles studies. Lobster, ROSITA and EUSO Study Scientist, Leader Brekke, P., Support to SOHO Project Scientist, solar for SAX LEGSPC, X-ray astronomy (X-ray binaries physics, science communications. and AGN). Escoubet, C.P., Cluster and Double Star Project Scientist, Perryman, M.A.C., Hipparcos Project Scientist, Gaia magnetospheric physics. Project Scientist, exploitation of Hipparcos data. Fehringer, M., Support to Cluster and Double Star Pilbratt, G.L., Herschel Project Scientist, IR and sub-mm Project Scientist, Microscope Study Scientist (since astronomy. September 2001, 25% under the Fundamental Physics Prusti, T., Herschel Scientist, infrared astronomy. Missions Division). Tauber, J., Planck Project Scientist, sub-mm astronomy. Fleck, B., SOHO Project Scientist, Solar Orbiter Study Scientist, solar physics. ESA Research Fellows Haugan, S., SOHO Science Operations Coordinator, Bocchino, F. (to September 2001), X-ray astronomy. solar physics. Boirin, L. (from October 2001), X-ray astronomy. Marsden, R.G., Ulysses Project Scientist and Project Del Burgo, C. (from October 2002), Modelling of sky as Manager, Solar Orbiter Study Scientist, ILWS seen by Planck. support, energetic particle data interpretation. Dupac, X. (from October 2002), Planck-related science Sanchez, L., SOHO Science Data Ordinator, SOHO on cosmic background and interstellar dust. archive. sp1247s4.qxd 3/5/03 3:58 PM Page 115

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Sanderson, T.R., Cluster Archive Scientist, energetic Research Fellows particle instrument development and data Boudin, N. (from March 2002), Astrochemistry (for B.H. interpretation. Foing). Heather, D. (to June 2002), Lunar studies. ESA Research Fellows Michael, G. (from March 2002), Comparative Berghmans, D. (to June 2002), develop image recognition planetology. software tools for detection of major solar events in Piot, A. (from March 2002), Exploitation of Huygens test SOHO data. balloon data. Fierry-Fraillon, D. (to January 2002), Helioseismology. Witasse, O. (to September 2002), Planetary atmospheres. Hofer, M. (to December 2002), Energetic particle data analysis. Young Gradutate Trainees Masson, A. (to October 2002), Cluster data analysis. Hoofs, R. (to June 2001), Science operations planning Moullard, O. (to January 2002), Plasma and particles tool development. studies. Kazeminejad, B. (to June 2002), Huygens mission O’Shea, E. (to September 2002), Solar magnetic field analysis studies. studies, ESMN Fellowship. O’Sullivan, J. (to September 2002), Development of Trautner, R. (to October 2001), Instrument development. Dust Mass Spectrometer for BepiColombo.

ESA External Fellow Stagiaires McIntosh, S. (from February 2001), Criticality of solar Almeida, M. (February-June/August-September 2002), flares and chromospheric dynamics. SMART-1 AMIE calibration, science operations support. Trainees Diaz, J. (March-July 2002), Meteor research. Winston, E. (June-August 2001), Solar events. Dages, O. (March-August 2001), SMART-1 risk analysis. Firre, D. (March-May 2001), Huygens mission scenario. Contract staff Larfors, K. (April-July 2002), Instrumentation develop- Mann, I. (to August 2002), Cosmic dust studies and ment on dust spectrometer. IRSI/Darwin support. Lefevre, F. (March-August 2001), Payload operations. Masson, A. (from November 2002), Cluster data Manaud, N. (March-August 2002), Planetary operations. analysis. Martinez, S. (October 2001-January 2002), Rosetta Tranquille, C., Ulysses data archive. science operations. Riesen, T. (March-May 2002), Rosetta science archive. Reissaus, P. (to December 2001), Meteor simulations. Planetary Missions Division Samaine, T. (March-August 2002), Laboratory testing of multi-channel I-V converter ASIC chip. Schwehm, G., Head of Division (from February 2002), Uberia, M. (March-June 2002), Rosetta knowledge Rosetta Project Scientist. management. Chicarro, A., Mars Express Project Scientist, planetary Vasquez, B. (October 2001-January 2002), Planetary geology. science data archives. Grard, R.J.L., BepiColombo Project Scientist, modelling Vilar, E. (April-August 2002), SMART-1 and Rosetta and instrument development. operations and data simulation. Koschny, D.V., Support to Rosetta Project Scientist, Science operations planning, meteor research, PhD/MS Students planetary cameras. Ruiterkamp, R. (from 2001), BioPAN and organics in Laakso, H., Support to BepiColombo, magnetospheric space. plasma research. Ten Kate, I. (from 2002), Mars simulations chamber. Lebreton, J.-P., Huygens Project Scientist and Mission Zijlstra, A. (September-December 2002), Lunar lander Manager, Solar System technology support, plasma design thesis (MS). physics instrument development. Martin, P., Mars Express Operations Scientist. Spanish/Portuguese Trainees Ocampo, A. (from February 2002), Support to Mars Perez Ayucar, M. (from June 2002), Huygens telecomm- Express and BepiColombo. unications engineering (E) Schulz, R.M., Support to Rosetta Project Scientist, Simoes, F., (from April 2002), Water on Mars (PT). Rosetta Lander, cometary studies. Vazquez Garcia, J. (June 2002), SMART-1 telecommuni- Svedhem, L.H., Venus Express Project Scientist, cations engineering (E). development of planetary instrumentation, cosmic dust studies. Contractors Heather, D. (from July 2002), Support to planetary data analysis. sp1247s4.qxd 3/5/03 3:58 PM Page 116

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Hoofs, R. (from July 2001), Rosetta science operations ESO staff under ESA contract engineer. Alexov, A., Post-operation instrument scientific Trautner, R. (from November 2002), Mars Express programmer. engineer. Bristow, P., Post-operation instrument scientific programmer. Christensen, L., HST Outreach Astronomer. Fundamental Physics Missions Division Fourniol, N., Archive operator. Kerber, F., Post-operation Instrument Scientist, early- Reinhard, R., Head of Division, Study Scientist for LISA type stars. (until April 2002), STEP, Hyper and Microscope (until Kornmesser, M., HST Outreach Technical Editor. September 2001). Pasquali, A., Instrument Scientist, stellar winds, nebulae. Jafry, Y., STEPStudy Manager (until October 2002), drag- free control expert for fundamental physics missions. Contract staff Jennrich, O. (from May 2002), LISA and SMART-2 Pettefar, N. (from August 2002), ST-ECF systems Study Scientist. administrator.

Space Telescope Operations Division STScI, Baltimore Arribas, S., NICMOS Instrument Scientist, AGN, high- Macchetto, D., Head of Division, AGN, elliptical redshift galaxies, cosmology. galaxies, gamma ray bursts. Boeker, T., NICMOS Instrument Scientist, galaxy formation and evolution, in particular gas dynamics in ST-ECF, Garching the central regions. ESA scientific staff Clampin-Nota, A., Deputy Head, Science Division, Benvenuti, P., Head of ECF, HST Project Scientist, massive stars, late stages of stellar evolution, IMF extragalactic HII regions, SNRs. studies. Albrecht, R., Deputy Head ECF, Head of Science Data De Marchi, G., ACS Instrument Scientist, initial mass and Software Group, minor bodies of the Solar function, globular clusters, dark matter haloes. System, computer science. Espey, B. (to April 2002), STIS Instrument Scientist, Dolensky, M., Science archive and WWW software emission line diagnostics, symbiotic binary stars, specialist. QSO emission and absorption lines, HDF South. Fosbury, R.A.E., Head of HST User Support Group, Goudfrooij, P. (to October 2002), STIS Instrument galaxies and AGN. Scientist, interstellar matter and stellar populations in Micol, A., Science archive software specialist, image early-type galaxies. processing techniques and information systems. Jenkner, H., HST Mission Deputy, Guide Star Catalog II, Rosa, M.R., Head Post-operational Archive Group, HII microvariability studies using FGS photometry. regions, star formation, supernovae, evolution of Mais-Appellaniz, J. (from July 2002), Spectrographs galaxies. Instrument Scientist, HII regions, young clusters. Meylan, G., Proposal Scientist, gravitational lensing and ESO staff (included here to give the full picture of ST- cosmology, stellar dynamics, photometry. ECF team staffing) Miebach, M., Lead Engineer for scientific instruments. Cristiani, S. (to July 2002), Instrument Scientist, obser- Mobasher, B. (from April 2000), STIS Instrument vational cosmology, galaxy evolution. Scientist, Galaxy surveys, dwarf galaxies, elliptical Freudling, W., Instrument Scientist, observational cos- galaxies. mology, peculiar motion of galaxies. Padovani, P., Multi-Mission Archive Scientist, AGN: Haase, J. (from June 2002), Astronomical data archive unified schemes, evolution, X-ray spectra, blazars. and pipeline software specialist. Panagia, N., NGST Science Lead, stars, interstellar Hook, R.N., HST Data Analysis Scientist, scientific medium, supernovae, galaxies, cosmology. software support, image restoration applications. Robberto, M., WFC3 Instrument Scientist, star forma- Kuntschner, H. (from November 2002), Instrument tion, massive stars, IR instrumentation. Scientist, galaxy formation and evolution. Stanghellini, L., Proposal Scientist, planetary nebulae Pierfederici, F., Astrovirtel support scientist. and their central stars, extragalactic distance scale. Pirenne, B., HST Archive Scientist, data storage tech- Stiavelli, M. (to September 2001), ACS Instrument nology, gravitational lenses. Scientist and Integrated Product Team Member for Pirzkal, N., Scientific analyst/programmer, pre-main- WFC3, formation and evolution of galaxies. sequence stars. Wiklund, T. (from September 2002), NICMOS Sjöberg, B., ST-ECF administrative assistant/secretary. Instrument Scientist, AGN, starburst galaxies. Walsh, J.R., Instrument Scientist, planetary nebulae, HII regions. sp1247s4.qxd 3/5/03 3:58 PM Page 117

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ESA External Research Fellows Ott, S. (from July 2002), System analyst, interactive Chiaberge, M. (from 2001), AGN, FRI and FRII analysis coordinator. unification, BL Lacs. Prades-Valls, R., Quality assurance (part-time, TOS support). Veillat, S. (to June 2002), System engineer (integrated Science Operations and Data Systems Division TOS support). Contractor Staff (full- or part-time during the reporting Kessler, M.F., Head of Division (from April 2001), period) Infrared Astronomy. Bakker, J. (from September 2002, shared with XMM), Bennett, K., Gamma-ray astronomy, Planck (Co-I). interactive analysis. Jansen, F., XMM-Newton Project Scientist, X-ray Bonfield, A. (from September 2002), Proposal handling, astronomy. (integrated TOS support). Szumlas, M., Technical coordination, data bank Brumfitt, J., System architect, core classes, scientific maintenance. mission planning. Thoerner, G., Divisional system analyst/computer Candussio, N. de (from July 2002), Interactive analysis, manager, SAX data analysis and cosmology studies. (integrated TOS support). Toni, A., Computer administration. Galloway, K., System engineer, telemetry ingestion, Winkler, C., Integral Project Scientist, gamma-ray documentation. astronomy data analysis. Porrett, C. (from June 2001), Calibration uplink system, Wamsteker, W., Multi-disciplinary scientist, active testing, build scripts. galaxies, abundances at high redshifts (at VILSPA). Siddiqui, H., MIB interface, interactive analysis, SPR Zender, J.J., Data handling/archiving management for system. planetary science operations. Zondag, R. (from June 2001), Configuration control, system builds, testing, installation, web. Contractor Staff (full- or part-time during the reporting period: ESTEC) Bowen, A., Data librarian. Integral Science Operations Centre (ISOC), ESTEC Bowen, H. (from December 2002), Solaris system Hansson, L., Integral Science Operations Manager. administration. Barr, P., Operations scientist, mission planning. Buggy, O. (from February 2001), Solaris system Breneol, C. (to July 2001), Computer software admininstration plus HSM M&O. development manager. Cappa, F. (to October 2002), Computer system Much, R., Operations scientist and Deputy Project administration. Scientist, observational astronomy. Esson, S., VMS system administration, Oracle and Orr, A. (from June 2002), Operations scientist, JEM-X Livelink support. and OMC expert, helpdesk. Giardino, G., Planck IDIS Development: data layer. Sternberg, J., System engineering, ISDC liaison. Hansen, J. (to December 2002), Solaris system Trams, N. (to July 2001), Operations scientist. administration. Hazell, A., Planck IDIS Federation and system Contractor staff (full- or part-time during the reporting engineering. period) Hulsbosch, A. (to December 2002), Ulysses research Cruse, B. (to April 2001), Software engineer, PHS support, Rosetta SOC development. development. Moser, F., Windows system administration. Dean, N., Testing, OSS maintenance, backup software Phipps, K. (from March 2002), Planck IDIS develop- librarian. ment: software repository, LDAP support. Jacobs, F. (from January 2001), PHS maintenance Planje, K., Graphics and printers support. (JAVA), DB administrator. Riemens, M., Administrative support and database Jeanes, A. (25% since mid 2002), OSS development/ maintenance. maintenance (JAVA). Williams, O.R. (to July 2002), COMPTEL/Planck data- Greenwood, S. (from January to August 2002), OSS base management and scientific operations. development. Kuulkers, E. (from June 2002), Operations scientist, backup mission planner, IBIS expert. Herschel Science Centre, ESTEC Nolan, J., ISOC procedures, instrument and spacecraft Riedinger, J., Herschel Science Centre Development operations expert. Manager. Oosterbroek, T. (from August 2002), Operations Claes, P. (to February 2001), Herschel software engineer. scientist, SPI expertise, local science analysis Mathieu, J-J., Interactive analsysis (part-time, TOS software expertise. support). Orr, A. (to May 2002), Operations scientist. sp1247s4.qxd 3/5/03 3:58 PM Page 118

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Treloar, J., Software librarian, PGT and associated Research Fellows software maintenance. Sanchez Fernandez, C. (from April 2002), ISO and Williams, O.R. (from August 2002), Integral Science XMM-Newton data analysis. Data Archive installation and maintenance. Zondag, R. (to June 2001), Archive engineer, system Contractor staff (full- or part-time during the reporting administration. period) Martin, S. (from September 2001 to January 2002), Integral Science Data Centre (Geneva) secretarial and administrative support. Texier, D. (from June 2002), Resident engineer. Matagne, J., ISO WWW master. Salomone, M. (to January 2002), Science journalist. Willis, A., Secretarial and administrative support. XMM-Newton Science Operations (ESTEC) Contractor staff (full- or part-time during the reporting period) XMM-Newton SOC (VILSPA) Bakker, J., SAS/SciSIM GUI/cross platform develop- Clavel, J. (to March 2002), XMM-Newton Science ment. Operations Manager. Lammers, U., CAL software/Event selection. Altieri, B., Software and payload support, observational astronomy. Arpizou, M., Secretarial and administrative support. ISO Data Centre (IDC), (VILSPA) Ehle, M., XMM-Newton user support, observational Blommaert, J. (to October 2001), ISO Resident astronomy. Astronomer, ISOCAM expert, ISOCAM Handbook, Gabriel, C., XMM-Newton instrument support, super- Handbook co-editor, AGB evolution and galactic nova remnants, cosmology. structure. Guainazzi, M., XMM-Newton user support, observa- Burgdorf, M. (to November 2001), ISO Resident tional astronomy. Astronomer, LWS expert, Solar System, stellar Kirsch, M. (from February 2002), EPIC calibration statistics. scientist. Garcia-Lario, P., ISO Resident Astronomer, cross- Metcalfe, L. (from July 2002), XMM-Newton Science calibration expert, Handbook co-editor, late stages of Support Manager. stellar evolution. Munoz Peiro, J. (from May 2002), Instrument Operations Gry, C., ISO Resident Astronomer, LWS expert, LWS Manager. Handbook, interstellar medium. Pollock, M. (from February 2002), RGS calibration Kessler, M.F. (to March 2001), ISO Project Scientist. scientist. Laureijs, R.J. (to December 2001), ISO Resident Santos-Lleo, M., XMM-Newton user support, observa- Astronomer, PHT expert, ISM and dust. tional astronomy. Leech, K. (to December 2001) ISO Resident Astron- Schartel, N., XMM-Newton User Support and Mission omer, SWS expert, SWS Handbook, infrared Planning Group Team Leader, observational astronomy, brown dwarfs, Hale-Bopp. astronomy. Lorente, R. (from October 2002), ISO Resident Texier, D. (to March 2002), XMM-Newton Instrument Astronomer, ISOCAM expert. Support Group Team Leader. Metcalfe, L. (to July 2002), ISO Project Scientist, gravitational lensing. Contractor staff (full- and part-time during the reporting Müller, T. (to December 2001) ISO Resident period) Astronomer, Handbook co-editor, Solar System Alonso Martinez, E. (from July 2001), Computer studies, asteroids. operator. Ott, S. (to June 2002), ISOCAM expert, ISOCAM Alvarez, R., Analyst. interactive analysis lead, ISOCAM parallel mode. Bailey, R. (from September 2001), WWW creation/ Peschke, S., ISO Resident Astronomer, ISOPHOT maintenance and proposal handling tools. expert, comets. Breitfellner, M., Enhancement/mission/planning/ToO Salama, A., ISO Project Scientist (from May 2002), on-call. SWS expert, Titan, novae and symbiotic stars. Brenchley, M., Software engineer. Schulz, B. (to January 2002), ISO Resident Astronomer, Buenadicha, G., Instrument on-board software main- ISOPHOT expert, AGN. tenance. Verdugo, E. (from November 2002), Resident Astron- Calderon Riano, P, Inscon. omer, ISOPHOT expert, ISO Data Archive products Cheek, N., Operations analyst, Operations database. quality. Chen, B., OM calibration scientist. Delgado Rioja, J., Software maintenance: SGS/QLA. Diaz Rodriguez, D. (from March 2002), Software maintenance: PHS-RPS. sp1247s4.qxd 3/5/03 3:58 PM Page 119

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Djavidnia, S., Operations analyst. Science Payload and Advanced Concepts Office Fauste, J., Operations engineer. (formerly Science Payloads Technology Division) Fuente, A. de la, Analyst. Garcia Beteta, J.J., Software maintenance: ODS/PMS. Peacock, A., Head of Office, STJ Research Team Leader. Garcia Mandillo, A., Computer operator. Andersson, S., Electronics engineering for advanced Gilolmo Lobo, M. (from November 2001), Inscon. technologies for semiconductors sensors. Gonzalez Garcia, B., Inscon. Appourchaux, T., Solar Orbiter payload support, solar Gonzales Riestra, R., RGS calibration/community research, COROT instrument Research Team Leader. support. Adriaens, M. (to June 2002), Mechnical engineer. Hoar, J. (to August 2002), Software engineer. Arends, H., Mechanical engineer and mechanical Juarez Blanca, B., Inscon. laboratory coordinator. Loiseau, N. (from March 2001), Inscon. Bavdaz, M., Advanced technologies sensors and optics, Lorente, R. (to September 2002), Inscon. Sensors and Optics Research Team Leader, Head of Martin, T., Analyst. Advanced Technology Section (p.i.). Martos, A., Inscon. Beaufort, T., Electronics engineer for COROT PDU. Ojero, E., Analyst. Biezen, J.F. van der, Electronics and laboratory Olabarri, B., Operations engineer. metrology support to advanced technology Perea Calderon, P., Computer operator. programme. Perez Martinez, R. (from June 2001), Inscon. Butler, B.A.C., Instrument development engineer. Rives, S., Operations engineer. Dordrecht, A. van., Advanced Sensors electronics Rodriguez Duran, F. (from July, 2001), Computer engineer. operator. Erd, C., Sensor research and development, ESA missions Rodriguez Pascual, P., Community support scientist. support. Salgado, J. (to August 2002), Instrument controller. Falkner, P., Electronics research and development, Head Sanchez-Beato, R., Software maintenance: PMS/ODS. of Planetary Exploration Section (p.i.). Smith, M., EPIC calibration. Gondoin, Ph., Darwin-Genie instrument manager, XMM Soriano Borrull, R., Software maintenance: AMS. observational research. Talavera, A., OM calibration scientist. Heida, J., Instrument support engineer. Tomas, L., Mission planning. Johlander, B., Head of Instrument Support Group, Vallejo, J.C., Managing software support team. instrument development engineer. Verdugo, E. (to December 2002), OM calibration/ Klinge, D., Instrument development engineer. community support. Lumb, D., Advanced sensor research, XEUS an ISS payload and mission support, XMM observational research. Science Archives Group (VILSPA) Martin, D., SCAM3 instrument manager, Head of Staff Infrastructure Section (p.i.). Arviset, C., System engineering, archive group leader. Rando, N., Payload support and development engineer, Head of Missions Section (p.i.). Stagiaires Romstedt, J., In-situ planetary instrument development, Meddour, R. (from August 2002 to January 2003). Rosetta-MIDAS (AFM) Lead Scientist. Rodriguez, E. (from April to August 2001). Smit, L.C., Instrument development support engineer. Sunter, W., Mechanical design engineer (seconded from Contractor staff (full- and part-time during the reporting D/TOS). period) Telljohann, U., Instrument electronics engineer. Dowson, J., Archives: database expert. Verveer, J., Laboratory cryogenic systems support. Hernandez, J., Archives: JAVA/GUI expert. Ortiz, I. (from October 2002), Archives: database expert. Research Fellows Osuna, P., Archives: data distribution/virtual observatory. Molster, F., Rosetta-MIDAS AFM. Salgado, J. (from August 2002), Archives: data distribution/virtual observatory. Stagiaires San Miguel, G. (from October 2002), Archives: Bonal, L., Scientific Evaluation of MIDAS (April-July JAVA/GUI expert. 2002). Venet, A. (from November 2001), Archives: database expert. Trainees Moreira, O. (Portuguese Trainee from April 2002), Helioseismology. Pitcher, K. (June to August 2001), International law. sp1247s4.qxd 3/5/03 3:58 PM Page 120

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Contractor staff (full- or part-time during the reporting period) Beijersbergen, M. (to December 2001), X-ray optics. Brammertz, G., Laboratory Cryogenic and solid-state test support. Den Hartog, R., Cryogenic Optics and solid-state test support. Duvet, L. (from July 2002), COROT and STEREO flight instrument technical support. Hijmering, R. (from November 2002), Croygenic camera sensor test data analysis. Jeanes, A., Payload databases and payload cost analysis support. Kraft, S., Payload minaturisation technical support. Owens, A., Solid-state support and optics technical support. Page, J. (to April 2002), Cryogenic engineering support. Reynolds, A., Laboratory data processing and test analysis. Sirbi, G. (from October 2002), Laboratory cryogenic technical support. Smit, H. (from January 2002), STEREO flight instrument technical support. Verhoeve, P., Laboratory cryogenic and solid-state test support. sp1247s4.qxd 3/5/03 3:58 PM Page 121

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ANNEX 2: PUBLICATIONS and J.-E. Wahlund, First Results of Electric Field and Density Observations by Cluster EFW Based on Initial Months of Operation, Densitites, Ann. Solar & Solar-Terrestrial Missions Division Geophys., 19, 1219-1240, 2001. and Planetary Missions Division Heber, B. and R.G. Marsden, Cosmic Ray Modulation Refereed Journals, 2001 Over the Poles at Solar Maximum: Observations, Space Sci. Rev., 97(1-4), 309-319, 2001. Banerjee, D., E. O’Shea, J.G. Doyle and M. Goossens, Heber, B., E. Keppler, R.G. Marsden, C. Tranquille, The Nature of Network Oscillations, Astron. B. Blake and M. Fraenz, The Evolution of the Astrophys., 371, 1137-1149, 2001. Anomalous Cosmic Ray Oxygen Spectra from 1995 Banerjee, D., E. O’Shea, J.G. Doyle and M. Goossens, to 1998: Ulysses Observations, Space Sci. Rev., 97(1- Long Period Oscillations in the Inter-Plume Regions 4), 363-366, 2001. of the Sun, Astron. Astrophys., 377, 691-700, 2001. Houdek, G., W.J. Chaplin, T. Appourchaux, J. Christ- Banerjee, D., E. O’Shea, J.G. Doyle and M. Goossens, ensen-Dalsgaard, J.W. Däppen, Y. Elsworth, D.O. Signatures of Very Long Period Waves in the Polar Gough, G. Isaak, R. New and M.C. Rabello-Soares, Coronal Holes, Astron. Astrophys., 380, L39-L42, Changes in Convective Properties over the Solar 2001. Cycle: Effect on p-Mode Damping Rate, MNRAS, Bosqued, J.M., T.D. Phan, I. Dandouras, C.P. Escoubet, 327, 483, 2001. H. Reme et al., Cluster Observations of the High- Janhunen, P., A. Olsson, W.K. Peterson, H. Laakso, J.S. Latitude Magnetopause and Cusp: Initial Results from Pickett, T.I. Pulkkinen and C.T. Russell, A Study of the CIS Ion Instruments, Ann. Geophys., 19, 1545- Inverted-V Auroral Acceleration Mechanisms Using 1566, 2001. Polar/Fast Auroral Snapshot Conjunctions, J. Geo- Chaplin, W. J., T. Appourchaux, Y. Elsworth, G. R. Isaak, phys. Res., 106, 18995-19012, 2001. and R. New, The Phenomenology of Solar Cycle- Keller, H.U., H. Hartwig, R. Kramm, D. Koschny, W.J. Induced Acoustic Eigenfrequency Variations: A Markiewicz, N. Thomas, M. Fernandez, P.H. Smith, Comparative and Complementary analysis of GONG, R.M.T. Reynolds, J. Weinberg, R. Marcialis, BISON and IRGO/:LOI data, MNRAS, 324, 910, R. Tanner, B. J. Boss and C. Oquest, The MVACS 2001. Robotic Arm Camera, J. Geophys. Res., 106, 17609- Charbonneau, P., S.W. McIntosh, H.-L. Liu and T.J. 17622, 2001. Bogdan, Avalanche Models for Solar Flares (Invited Kolesnikova, E., C. Beghin, R. Grard and C.P. Escoubet, Review), Sol. Phys., 203 (2), 321-353, 2001. The Electrical Stability of the Electric Field Antennas Curdt, W., P. Brekke, U. Feldman, K. Wilhelm, B.N. in the Plasmasphere, J. of Atm. Sol. Terr. Phys., 63(11), Dwivedi, U. Schühle and P. Lemaire, The SUMER 1217-1224, 2001. Spectral Atlas of Solar-Disk Features, A & A, 375, Kolokova, L., L.M. Lara, R. Schulz, J.A. Stuewe and 591-613, 2001. G.P. Tozzi, Properties and Evolution of Dust in Comet Drolshagen, G., H. Svedhem, E. Gruen, K.D. Bunte, Tabur (C/1996Q1) from the Color Maps, Icarus, 153, Measurements of Cosmic Dust and Micro-Debris in 197-207, 2001. Geostationary Orbit, Adv. Space Res. 28(9), 1325- Koschny, D. and E. Gruen, Impacts into Ice-Silicate 1333, 2001. Mixtures: Crater Morphologies, Volumes, Depth-to- Escoubet, C.P., M. Fehringer and M. Goldstein, Intro- Diameter Ratios, and Yield, Icarus, 154, 391-401, duction: The Cluster Mission, Ann. Geophys., 19, 2001. 1197-1200, 2001. Koschny, D., G. Kargl and M. Rott, Experimental Fierry-Fraillon, D. and T. Appourchaux, The Effects of a Studies of the Cratering Process in Porous Ice Targets, Gap-Filling Method on P-Mode Parameters, MNRAS, Adv. Space Res., 28(10), 1533-1537, 2001. 324, 1159, 2001. Koschny, D.V. and E. Gruen, Impacts into Ice-Silicate Gloeckler, G. and K.-P. Wenzel, Acceleration Processes Mixtures: Ejecta Mass and Size Distributions, Icarus, of Heliospheric Particle Populations, In Century of 154, 402-411, 2001. Space Science, J.A.M. Bleeker, J. Geiss, M.C.E. Krueger, H., E. Gruen, A. Graps, D. Bindschadler, Huber (eds), Kluwer Academic Publ., 963-1005, S. Dermott, H. Fechtig, B.A. Gustafsson, D.P. 2001. Hamilton, M.S. Hanner, M. Hoanyi, J. Kissel, B.A. Grard, R. and A. Balogh, Returns to Mercury: Science Lindblad, D. linkert, G. Linkert, I. Mann, J.A.M. and Mission Objectives, Planet. & Space Sci., 49(14- McDonnell, G.E. Morfill, C. Polanskey, G. Schwehm, 15), 1395-1407, 2001. R. Srama and H.A. Zook, One Year of Galileo Dust Gustafsson, G., M. André, T. Carozzi, A.I. Eriksson, Data From the Jovian System: 1996, Planet. Space C.-G. Fälthammar, R. Grard, G. Holmgren, J.A. Sci., 49, 1285-1301, 2001. Holtet, N. Ivchenko, T. Karlsson, Y. Khotyaintsev, Krueger, H., E. Gruen, M. Landgraf, M. Baguhl, S. Klimov, H. Laakso, P.-A. Lindqvist, B. Lybekk, S. Dermott, H. Fechtig, B.A. Gustafson, D.P. G. Marklund, F. Mozer, K. Mursula, A. Pedersen, Hamilton, M.S. Hanner, M. Horanyi, J. Kissel, B.A. B. Popielawska, S. Savin, K. Stasiewicz, P. Tanskanen Lindblad, D. Linkert, I. Mann, J.A.M. McDonnell, sp1247s4.qxd 3/5/03 3:58 PM Page 123

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G.E. Morfill, C. Polanskey, G. Schwehm, R. Srama Pedersen, A., P. Decreau, C.P. Escoubet, G. Gustafsson, and H.A. Zook, Four Years of Ulysses Dust Data: H. Laakso, P.A. Lindqvist, B. Lybekk, F. Mozer and 1996-1999, Planet. Space Sci., 49, 1303-1324, 2001. A. Vaivads, Four-Point High Time Resolution Laakso, H. and M. Jarva, Evolution of the Plasmapause Information on Electron Densities by the Electricity Position, J. of Atm. Sol. Terr. Phys., 63, 1171-1178, Field Experiments (EFW) on Cluster, Ann. Geophys., 2001. 19, 1483-1489, 2001. Lara, L.M., R. Schulz, J.A. Stuwe, and G.P. Tozzi, Reme, H., C. Aoustin, J.M. Bosqued, I. Dandouras, Activity of Comet Tabur (C/1996 Q1) During Sept. B. Lavraud, J.A. Savaud, A. Barthe, J. Bouyssou, 12-17, 1996, Icarus, 150, 124-139, 2001. T. Camus et al. (incl. C.P. Escoubet), First Mann, I. and H. Kimura, Dust Properties in the Local Multispacecraft Ion Measurements In and Near the Interstellar Medium, Space Sci. Rev., 97, 389-392, Earth’s Magnetosphere with the Identical Cluster Ion 2001. Spectrometry (CIS) Experiment, Ann. Geophys., 19, Marsden, R.G., The Heliosphere after Ulysses, 1303-1354, 2001. Astrophys. & Space Sci., 277, 337-347, 2001. Sanderson, T.R., R.G. Marsden, C. Tranquille, Marsden, R.G., Highlight Results from Ulysses: In A. Balogh, R.J. Forsyth, B.E. Goldstein, J.T. Gosling Recent Insights into the Physics of the Sun and and K.L. Harvey, The Influence of the Sun’s Magnetic Heliosphere : Highlights from SOHO and Other Space Field and the Heliosphere on Energetic Particles at Missions, IAU Symposium 203, P. Brekke, B. Fleck, High Heliospheric Latitudes, Geophys. Res. Lett., and J.B. Gurman (Eds), 525-532, 2001. 28(24), 4525-4528, 2001. Masson, A., B.B. Shishkov and F. Lefeuvre, Use of Torkar, K., W. Riedler, C.P. Escoubet, M. Fehringer et al., Higher-Order Statistical Tests in the Analysis of Time Active Spacecraft Potential Control for Cluster – Series Associated with Space Data, Signal Processing, Implementation and First Results, Ann. Geophys., 19, 18, 59-78, 2001. 1289-1302, 2001. McIntosh, S. and P. Charbonneau, Geometrical Effects in Trotignon, J.G., H.C. Seran, R. Grard, H. Laakso, Avalanche Models of Solar Flares: Implications for N. Meyer-Vernet and R. Manning, In Situ Observa- Coronal Heating, Astrophys. J. Lett., 563, L165-L168, tions of the Ionized Environment of Mars: the AIM 2001. Experiment Proposed as Part of the MARSIS Radar McIntosh, S.W. and P.G. Judge, On the Nature of Onboard Mars Express, Planet. Space Sci., 49, 155- Magnetic Shadows in the Solar Chromosphere, 164, 2001. Astrophys. J., 561, 420-426, 2001. Witasse, O., J.-F. Nouvel, J.-P. Lebreton and W. Kofman, Moullard, O., D. Burgess, C. Salem, A. Mangeney, D.E. HF Radio Wave Attenuation Due to a Meteoric Layer Larson and S.D. Bale, Whistler Waves, Langmuir in the Atmosphere of Mars, Geophys. Res. Lett., Waves and Single Loss Cone Electron Distributions 28(15), 3039-3042, 2001. Inside a Magnetic Cloud: Observations, J. Geophys. Res., 106(A5), 8301-8313, 2001. Moullard, O., R.G. Marsden, T.R. Sanderson et al., Solar & Solar-Terrestrial Missions Division Energetic Ions Observed at Low to High Latitudes in and Planetary Missions Division the Southern Heliosphere during Declining and Rising Proceedings and other Publications, 2001 Solar Activity, Space Sci. Rev., 97(1-4), 289-292, 2001. Appourchaux, T., Results from the Luminosity Norman, J.P., P. Charbonneau, S.W. McIntosh, and Oscillations Imager on board SOHO: Low-Degree H. Liu, Waiting-Time Distributions in Lattice Models p-Mode Parameters for a 4-Year Data Set, ESA SP- of Solar Flares, Astrophys. J., 557, 891-896, 2001. 464, 71-74, 2001. Opgenoorth, H.J., M. Lockwood, D. Alcayde, Appourchaux, T., B. Andersen, G. Berthomieu et al., g- E. Donovan, M. J. Engebretson, A. P. van Eyken, Mode Detection: Where do we Stand? ESA SP-464, K. Kauristie, M. Lester, J. Moen, J. Warterman, 467-471, 2001. H. Alleyne, M. André, M. W. Dunlop, N. Cornilleau- Arends, H., J. Gavira, J. Romstedt, B. Butler, K. Torkar, Werhlin, A. Masson, A. Fazerkerley, H. Reme, et al., G. Coe and M. Yorck, The MIDAS Experiment for the Coordinated Ground-Based, Low Altitude Satellite Rosetta Mission, Proc. of 9th Eur. Space Mech. & and Cluster Observations on Global and Local Scales Tribology Symp. (ESMATS), ESA SP-480, 67-74, During a Transient Postnoon Sector Excursion of the 2001. Magnetospheric Cusp, Ann. Geophys., 19, 1367-1398, Banerjee, D., E. O’Shea, J. G. Doyle, and M. Goossens, 2001. Long Period Ocillations in Polar Plumes as Observed O’Shea, E., D. Banerjee, J.G. Doyle, B. Fleck and by CDS on SOHO In Recent Insights into the Physics F. Murtaugh, Active Region Oscillations, A&A, 368, of the Sun and Heliosphere: Highlights from SOHO 1095-1107, 2001. and Other Space Missions, Proceeding of IAU Palmroth, M., H. Laakso and T. Pulkkinen, Location of Symposium 203, P. Brekke, B. Fleck and J. B. High-Altitude Cusp During Steady Solar Wind Gurman (Eds), 244-246, 2001. Conditions, J. Geophys. Res., 110, 21109-21122, 2001. Banerjee, D., E. O’Shea, J.G. Doyle, M.Goosens and sp1247s4.qxd 3/5/03 3:58 PM Page 124

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B. Fleck, On the Nature of Network Oscillations, ESA Hofer, M.Y., R.G. Marsden, T.R. Sanderson and C. Tran- SP-464, 175-178, 2001. quille, Energetic Particle Composition Measurements Brekke, P., Impact of SOHO, TRACE and Yohkoh on at High Heliographic Latitudes Around the Solar Solar Physics, 11th Cambridge Workshop on Cool Activity Maximum, In Solar and Galactic Stars, Stellar Systems and the Sun, Garcia Lopez, R.J. Composition (ed. R.F. Wimmer-Schweingruber) AIP et al (eds), PASP 223, 311, 2001. Conf. 598, 189-193, 2001. Brekke, P., The Sun’s Role in Climate Changes, Proc. of Huber, M.C.E., Roger Bonnet, The Scientist, ESA the Int. Conf. On Global Warming and the Next Ice Age, SP-493, 81-94, 2001. 19-24 August, Halifax, Nova Scotia, in press, 2001. Kimura, H., I. Mann and E.K. Jessberger, Properties of Brekke, P., Space Weather, Europhys. News 32(6), 232, Local Interstellar Dust derived from Remote 2001. Astronomical Observations, Laboratory Analyses, and Brekke, P., B. Fleck, S.V.H. Haugan, SOHO in its prime in Situ Measurements, Proc. Meteorids 2001 Conf., Years, Nordic Space Activities 9(2), 2001. Kiruna,, ESA SP-495, 633-642, 2001. Chicarro, A.F., The Mars Express Mission and the Search Klecker, B., V. Bothmer, A.C. Cummings, J.S. George, for Life on Mars, Astronomicheski Vestnik 35(6), 1-6, J.W. Keller, E. Salerno, u.J. Sofia, E.C. Stone, F.-K. 2001. Thielemann, M.E. Wiedenbeck, F. Buclin, E.R. Chicarro, A.F., The New Views of the Moon Lunar Christian, E.O. Flückiger, M.Y. Hofer, F.C. Jones, Initiative, Rev. del IAA, 5, 11-12, 2001. D. Kirilova, H. Kunow, M. Laming, C. Tranquille and Donnelly, J., A. Thompson, D. O’Sullivan, A.J. Keane, K.-P. Wenzel, Galactic Abundances: Report of L. O’C. Drury and K.-P. Wenzel, The Abundances of Working Group 3, In Solar and Galactic Composition Actinide Nuclei in the Cosmic Radiation as Clues to R.F. Wimmer-Schweingruber (Ed), AIP Conf. Proc. Cosmic-Ray Origin, Proc. of 27th ICRC (Hamburg), 598, 207-220, 2001. 1715-1716, 2001. Kuitunen, J., G. Drolshagen, J.A.M. McDonnell, Drolshagen, G., H. Svedhem, E. Gruen, Measurements H. Svedhem, M. Leese, H. Mannermaa, M. Kaipi- of Cosmic Dust and Micro-Debris with the GORID ainen and V. Sipinen, Debie – First In Situ Debris Impact Detector, ESA SP-473, 177-184, 2001. Monitoring Instrument, Proc. 3rd European Conf. On Escoubet, C.P., M. Fehringer and P. Bond, Rumba, Salsa, Space Debris, Darmstadt, ESA SP-473, 185-190, Samba and Tango in the Magnetosphere – the Cluster 2001. Quartet’s First Year in Space, ESA Bulletin, 107, 43- Laakso, H. and B.H. Foing, Characteristics of the Plasma 53, 2001. Environment for the SMART-1 Mission, in Proc. of Fleck, B., Highlights from SOHO and Future Space the 7th Spacecraft Charging Technology Conf., Missions in The Dynamic Sun, Proc. 1999 ESTEC, ESA SP-476, 601-608, 2001. Kanzelhoehe Summer School and Workshop (Eds Laakso, H., R. Grard, A. Masson, O. Moullard, S. Bale, A. Hanslmeier et al.) Kluwer Academic Publ., 1-41, F. Mozer, A. Pedersen, M. André, A. Eriksson, 2001. G. Gustaffson and P.-A. Lindqvist, Multi-Point Fleck, B. and the Solar Orbiter Study Team, Solar Orbiter Electric Field Observations in the High-Latitude – A High Resolution Mission to the Sun and Inner Magnetosphere, Proc. Sheffield Space Physics Heliosphere, SPIE Proc. Series, 4498, 1-15, 2001. Conference: Multipoint Measurements Versus Theory, Fleck, B., R.G. Marsden and O. Pace, Solar Orbiter, ESA ESA SP-492, 27-34, 2001. Bulletin, 105, 56-57, 2001. Lanzerotti, L.J. and T.R. Sanderson, Energetic Particles Graps, A.L., E. Gruen, H. Krueger, M. Horanyi and in the Heliosphere. In The Heliosphere Near Solar H. Svedhem, Io Revealed in the Jovian Dust Streams, Minimum, Balogh. A. et al. (Eds), 259-286, 2001. Meteorids 2001, ESA SP-495, 601-608, 2001. Lebreton, J.-P. and D.L. Matson, Cassini/Huygens Grard, R.J.L. and H. Laakso, The Plasma Environment Mission, Encyclopeida of Astronomy and Astro- Around Mercury, in Proc. of the 7th Spacecraft physics, Nature Publishing Group, Basingstoke, UK, Charging Technology Conf. ESA SP-476, 617-622, 37469, 2001. 2001. Mann, I., Charging Effects on Cosmic Dust, ESA SP- Grün, E., M. Baguhl, H. Svedhem and H.A. Zook, In Situ 476, 629-634, 2001. measurements of Cosmic Dust, in Interplanetary Dust Mann, I., H. Kimura, E. Jessberger, M. Fehringer and E. Gruen, Guftafson, Dermott and Fechtig (eds), 295- H. Svedhem, Dust in the Inner Solar System, Proc. First 346, 2001. Solar Orbiter Workshop, ESA SP-493, 445-446, 2001. Haugan, S.V.H., Anomalous Line Shifts on the Marsch, E., R. Harrison, O. Pace, E. Antonucci, SOHO/CDS NIS Detector, In Recent Insights into the P. Bochsler, J.-L. Bougeret, B. Fleck, Y. Langevin, Physics of the Sun and Heliosphere, ASP Conf. Ser. R. Marsden, R. Schwenn and J.-C. Vial, Solar 200, 396-400, 2001. 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Knop, R.A., et al., Panagia, N., et al., ΩM and Ωλ from 11 Nobili, S., et al., Panagia, N., et al., Supernova Type Ia HST-Observed Supernovae at z=0.36-0.86, BAAS, 33, Evolution and Grey Dust Ground and Space Based 1332, 2001. Follow up of a Type Ia Supernova at z=0.54, BAAS, Kuntschner, H., The Stellar Populations of Early-Type 33, 1333, 2001. Galaxies in the Fornax Cluster, Ap&SS, 276, 885, Nugent, P., et al., Panagia, N., et al., Interpretation of 2001. High-z SN Spectra, BAAS, 33, 1370, 2001. Landt, H., P. Padovani, E. Perlman, P. Giommi, The Padovani, P. Deep Blazar Surveys, in Blazar Emission Line Properties of DXRBS Blazars, in Demographics and Physics, P. Padovani, C.M. Urry Blazar Demographics and Physics', P. Padovani, C.M. (eds.), ASP Conf. Ser., 227, 163, 2001. Urry (eds.), ASP Conf. Series, 227, 73, 2001. Padovani, P., C.M. Urry, Issues in Blazar Research, in Maíz-Apellániz, J., Walborn, N.R., Massive young Blazar Demographics and Physics, P. Padovani, C.M. clusters in nearby galaxies, in Galaxies and their Urry (eds.), ASP Conf. Ser., 227, 3, 2001. Constituents at the Highest Angular Resolutions, Padovani, P. Giommi, Mining the Blazar Sky, in Mining Proc. IAU Symposium #205, ed. R.T. Schilizzi, San the Sky, A.J. Banday, S. Zaroubi, M. Bartelmann Francisco, ASP, 222, 2001. (eds.), Springer-Verlag, 494, 2001. Maíz-Apellániz, J., An HST archival study of massive Pain, R., et al., Panagia, N., et al., The Distant Type Ia young clusters, in Highlights of Spanish astrophysics Supernovae Rate, BAAS, 33, 1346, 2001. II, Proc. 4th Scientific Meeting of the Spanish Astron. Panagia, N. & Bono, G., Pre-Supernova Evolution of Soc., ed. J. Zamorano, J. Gorgas, J. Gallego, Massive Stars, invited review at STScI 1999 May Dordrecht, Kluwer Acad. Pubs, p.113, 2001. Symp. The Largest Explosions since the Big Bang Maíz-Apellániz, J., The Scorpius-Centaurus OB associa- Supernovae and Gamma Ray Bursts, eds. M. Livio, N. tion and the origin of the Local Bubble, AAS Meeting Panagia, K. Sahu, Cambridge Univ. Press, p.184-197, 199, #11.03, 2001. 2001. Maíz-Apellániz, J., MacKenty, J.W., Norman, C.A., Panagia, N. The Next Generation Space Telescope, Walborn, N.R. The spectacular warm ISM of NGC invited talk at the 2000 Vulcano Workshop Frontier 4214, in Tetons 4: Galactic Structure, Stars and the Objects in Astrophysics and Particle Physics, eds. F. Interstellar Medium, ASP Conf. Ser., 231, ed. C.E. Giovannelli, G. Mannocchi, Italian Physical Society, Woodward, M.D. Bicay, J.M. Shull, San Francisco, p.587, 2001. ASP, p.362, 2001. Panagia, N., Lamers, H., Bik, A., de Wit, W., Scuderi, S., Mediavilla, E., Arribas, S., Motta, V., Munoz, J., Capetti, A., Romaniello, M., Spaans, M., Kirshner, Kochaneck, C., Falco, E. Extended C[III] & lambda, R.P., Star Formation and Stellar Populations in the 1909 Emission in Q0957+561 Galaxies, the Third Central Regions of M51 in The Central kpc of Dimension, ASP Conf. Ser. (Ed. M. Rosado, L. Starbursts and AGNs, eds. J.H. Knapen, J.E. Binette, L. Arias), 2001. Beckman, I. Shlosman, T.J. Mahoney, ASP Conf. Ser., Meylan G., Internal Dynamics of Globular Clusters, 249, ASP, San Francisco, p.543-549, 2001. Observations, invited review in Stellar Dynamics, Panagia, N., Romaniello, M., Scuderi, S., the SINS from Classic to Modern, Proc. St. Petersburg Collaboration, HST Study of the Stellar Population International Conf., eds. L.P. Ossipkov, I.I. Nikiforov, within 30 pc of SN 1987A, invited review at 1997 St. Petersburg, SPUP, pp.1-10, 2001. ESO/CTIO/LCO Workshop SN 1987A Ten Years After, Meylan, G., Magain P., Deconvolving Spectra, Near-IR eds. M. Phillips, N. Suntzeff, ASP Conf. Ser., in press. Spectroscopy of the Lens and Source in HE 1104- Panagia, N., Stiavelli, M., Ferguson, H.C., Stockman, 1805, in International Astrophysics Conference on H.S., Primordial Stars The Next Generation, BAAS, Gravitational Lensing, Recent Progress and Future 33, 1347. Goals, eds. T.G. Brainerd, C.S. Kochanek, San Panagia, N.,Weiler, K.W., Montes, M.J., Van Dyk, S.D., Francisco, ASP, ASP Conf. Ser., 237, pp.85-96, 2001. Sramek, R.A., Lacey, C.K., Radio Properties of Meylan G., Tidal Tails around Galactic Globular Supernovae and GRB Sources, invited talk, 2000 sp1247s4.qxd 3/5/03 3:59 PM Page 145

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Vulcano Workshop Frontier Objects in Astrophysics Scarlata, C., Stiavelli, M., Panagia, N., Treu, T., Bertin, and Particle Physics, eds. F. Giovannelli, G. G., Bertola, F., Lyman alpha emitters with red colors Mannocchi, Italian Physical Society, p.207, 2001. at z~2.4, BAAS, 33, 1316, 2001. Pasquali, A., Pirzkal, N., Walsh, J.R., Hook, R.N., Schahmaneche, K., et al., Panagia, N., et al., Results Freudling, W., Albrecht, R., Fosbury, R.A.E., The from Recent High-redshift Type Ia Supernovae Effective Spectral Resolution of the WFC and HRC Searches, BAAS, 33, 1333, 2001. Grism, ST-ECF Instrument Science Report 2001-002, Sirianni, M., Nota, A., De Marchi, G., Leitherer, C., 2001. Clampin, M. The low end of the initial mass function Peletier, R.F., Bacon, R., Bureau, M., et al., The in the young LMC cluster NGC 2164, BAAS, 198, SAURON Survey of Early-Type Galaxies in the 42.08, 2001. Nearby Universe, The Newsletter of the Isaac Newton Stiavelli, M., Panagia, N., Scarlata, C., Treu, T., Group of Telescopes (ING Newsl.), issue 5, p.5, 2001. Properties of high-z galaxies with NGST, BAAS, 33, Perlman, E., P. Padovani, H. Landt, J. Stocke, L. 1315, 2001. Costamante, T. Rector, P. Giommi, J.F. Schachter, Stiavelli, M., Scarlata, C., Lilly, S., Panagia, N., Treu, T., Surveys and the Blazar Parameter Space, in Blazar Bertin, G., Bertola, F., Star-formation at z = 2.4 from Demographics and Physics, P. Padovani, C.M. Urry a sample of Lyman-alpha emitters, BAAS, 33, 815, (eds.), ASP Conf. Series, 227, 200, 2001. 2001. Pierfederici, F., Benvenuti, P., Micol, A., Pirenne, B., Tagliaferri, G., Ghisellini, G., Ravasio, M. et al., Two Wicenec, A., ASTROVIRTEL: Accessing Astronom- BeppoSAX observations of BL Lac, Memorie della ical Archives as Virtual Telescopes", ASP Conf. Ser. Societa Astronomica Italiana, 72, 135, 2001. 238, pp.141, 2001. 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Ser., 227, Blazar Pirzkal, N., Hook, R.N., Data fusion and photometric Demographics and Physics, 131, 2001. restoration, in Proc. SPIE, 4477, Astronomical Data Trussoni, E., Feretti, L., Capetti, A., Celotti, A., Analysis, Eds. J.-L. Starck, F.D. Murtagh, 277, 2001. Chiaberge, M., X-ray Properties of FR I Radio Pirzkal, N., Kerber, F., Clayton, G.C., de Marco, O., Galaxies, AIP Conf. Proc. 599, X-ray Astronomy, Rosa, M.R., Estimating the distance to V4334 Sgr Stellar Endpoints, AGN, and the Diffuse X-ray using the extinction method, AAS 199, #136.04, 2001. Background, 987, 2001. Pirzkal, N,. Pasquali, A., Walsh, J.R., Hook, R.N., Weiler, K.W., Panagia, N., Sramek, R.A., Van Dyk, S.D., Freudling, W., Albrecht, R., Fosbury, R.A.E., ACS Montes, M.J., Lacey, C.K., Radio Supernovae and Grism Simulations Using SLIM 1.0, ST-ECF GRB980425, invited review STScI 1999 May Symp. Instrument Science Report 2001-003, 2001. The Largest Explosions since the Big Bang Supernovae Robberto, M., Beckwith, S.V.W., Makidon, R.B., and Gamma Ray Bursts, eds. M. Livio, N. Panagia, K. Panagia, N., HST/WFPC2 image of the Orion Nebula Sahu, Cambridge Univ. Press, p.198-217, 2001. in the U and B bands, BAAS, 33, 852, 2001. Zhang, Y.H., Celotti, A., Treves, A. et al., Energy Romaniello, M., Panagia, N., Scuderi, S., Gilmozzi, R., Dependent X-ray Variability of the TeV Blazars PKS Tolstoy, E., Favata, F., Kirshner, R.P., T Tauri Stars in 2155-304 and MKN 421, AIP Conf. Proc. 599, X-ray the Large Magellanic Cloud, a combined HST and Astronomy, Stellar Endpoints, AGN, and the Diffuse VLT effort, Proc. ESO Workshop The Origin of Stars X-ray Background, 1019, 2001. and Planets The VLT View, eds. J. Alves and M. McCaughrean, ESO, p.275, 2001. Rosa, M.R., Alexov, A., Bristow, P., Kerber, F., FOS Space Telescope Operations Division Blue-side Spectroscopic Data recalibrated by the post Refereed Journals, 2002 operational archive project, ST-ECF Newsletter, 29, 9, 2001. Albrow, M., De Marchi, G., Sahu, K., The spatially Rosa, M.R., Bristow, P.D., Alexov, A., Kerber, F., GIMP resolved mass function of the globular cluster M22, and YBASE Induced Zero-Point Shifts in FOS Data, ApJ, 579, 660, 2002. POA/FOS-2001-01, 2001. Allen, M.G. Sparks, W.B., Koekemoer, A. et al., Rosa, M.R., Bristow, P.D., Alexov, A., Kerber, F., Ultraviolet Hubble Space Telescope Snapshot Survey Physical Model FOS Dispersion Relations, of 3CR Radio Source Counterparts at Low Redshift, POA/FOS-2001-04, 2001. ApJS, 139, 411, 2002. sp1247s4.qxd 3/5/03 3:59 PM Page 146

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Andreani, P., Fosbury, R.A.E., van Bemmel, I., Freud- Linear Reconstruction of Undersampled Images, ling, W., Far-infrared/millimetre emission in 3C PASP, 114, 144, 2002. sources. Dust in radio galaxies and quasars, A&A, Gnedin, O.Y., Zhao, H.S., Pringle, J.E., Fall, S.M., Livio, 381, 389, 2002. M., Meylan, G. The Unique History of the Globular Arribas, S., Colina, L., INTEGRAL Field Spectroscopy Cluster Omega Cent, ApJ, 568, L23-L26, 2002. of IRAS 15206+3342: Gas Inflows and Starbursts in Haemmerle, H., Miralles, J.-M., Schneider, P., Erben, T., an Advanced Merger, ApJ, 573, 576, 2002. Fosbury, R.A.E., Freudling, W., Pirzkal, N., Jain, B., Benítez, N., Maíz-Apellániz, J., Cañelles, M. Evidence White, S.D.M., Cosmic shear from STIS Pure for nearby supernova explosions, PhRvL, 88, 1101, Parallels: II Analysis, A&A, 385, 743, 2002. 2002. 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Pompei, E., Germany, L., Jaunsen, A.O., Letawe, G., Kerber, F., Guglielmetti, F., Mignani, R., Roth, M., Meylan, G., On Optical Time-Delay for the Lensed Proper motion of the central star of the Planetary BAL Quasar HE~2149-2745, A&A, 383, 71-81, Nebula Sh 2-68, A&A, 381, L9, 2002. 2002. Kerber, F., Pirzkal, N., De Marco, O., Asplund, M., Capetti, A., Celotti, A., Chiaberge, M., de Ruiter, H.R., Clayton, G.C., Rosa, M.R., Freshly ionized matter Fanti, R., Morganti, R., Parma, P. The HST survey of around the final Helium shell flash object V4334 Sgr the B2 sample of radio-galaxies: Optical nuclei and (Sakurai’s object), ApJL, 581, L39, 2002. the FR I/BL Lac unified scheme, A&A, 383, 104, King, N.L., Nota, A., Pasquali, A., Nota, A., Panagia, N., 2002. Gull, T.R., Pasquali, A., Clampin, M., Bergeron, L.E., Chiaberge, M., Macchetto, F.D., Sparks, W.B., Capetti, An HST Polarization Study of Dust in the Eta Car A., Allen, M.G., Martel, A.R. The Nuclei of Radio Homunculus, ApJ, 581, 285, 2002. Galaxies in the Ultraviolet: The Signature of Different King, L.J., Clowe, D.I., Lidman, C., Schneider, P., Erben, Emission Processes, ApJ, 571, 247, 2002. T., Kneib, J.-P., Meylan, G., The First Detection of Chiaberge, M., Capetti, A., Celotti, A. Understanding the Weak Gravitational Shear in Infrared Observations: nature of FR II optical nuclei: A new diagnostic plane Abell 1689, A&A, 385, L5-L9, 2002. for radio galaxies, A&A, 394, 791, 2002. Kuntschner, H., Ziegler, B.L., Sharples, R.M., Worthey, Chiaberge, M., Gilli, R., Macchetto, F.D., Sparks, W.B., G., Fricke, K.J., VLT spectroscopy of NGC3115 Capetti, A. 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Supergiants, invited paper at Workshop The Changes Bohlin, R., Cox, C., Krist, J., Sparks, W., De Marchi, in Abundances in Asymptotic Giant Branch Stars, eds. G., Martel, A., McCann, W., Meurer, G., Sirianni, M., V. Caloi, F. D’Antona, Mem. S. A. It., in press, 2002. Tsvetanov, Z., Bartko, F., Lindler, D., An overview of Bristow, P.D., Alexov, A., Kerber, F., Rosa, M.R., Final the HST Advanced Camera for Surveys’ on-orbit Improvement of HST POA FOS/BLUE Archived Data performance, BAAS, 200, 19.01, 2002. and Pipeline Processing, AAS, 200, 5905, 2002. Heydari-Malayeri, M., Charmandaris, V., Deharveng, L., Bristow, P.D., From Theoretical to Observational Via Meynadier, F., Rosa, M.R., Schaerer, D., Zinnecker, Selection Effects, in New Trends in Theoretical and H., HST photometry of stars in N160A, in VizieR On- Observational Cosmology, Eds. K. Sato, T. Shiro- line Data Catalog, J/A+A/381/941, SIMBAD, 2002. mizu, Universal Academy Press, 265, 2002. Heydari-Malayeri, M., Charmandaris, V., Deharveng, L., Bristow, P.D., Alexov, A., Kerber, F., Rosa, M.R., POA Meynadier, F., Rosa, M.R., Schaerer, D., Zinnecker, Investigation of FOS Dark Corrections (12/01), H., Unveiling the properties of low metallicity STECF Technical Report, POA/FOS-2001-07, 2002. massive young star clusters, in Semaine de Capetti, A., Celotti, A., Chiaberge, M., de Ruiter, H.R., l’Astrophysique Francaise, Eds. F. Combes, D. Barret, Fanti, R., Morganti, R., Parma, P., The HST View of Editions de Physique Conf. Ser., 2002. Low Luminosity Radio-Galaxies, ASP Conf. Ser. 258, Hook, R., Optical astronomy goes large, Astronomy Now, Issues in Unification of Active Galactic Nuclei, 159, 16, 29, 2002. 2002. Jakobsen, P., Arribas, S., Burgarella, D., Caraveo, P., Capetti, A., Trussoni, E., Celotti, A., Feretti, L., Cornelisse, J., Davies, R., Ferrara, A., Fosbury, R., Chiaberge, M., Spectral energy distributions of five Hjorth, J., Le Fevre, O., McCaughrean, M., Regan, FR I radio galaxies, New Astronomy Review, 46, M., Schneider, P., Ward, M., Wright, G., van 335, 2002. Dishoeck, E., The NGST Near-Infrared Spectrometer: Charmandaris, V., Heydari-Malayeri, M., Deharveng, L., The Science Case and Main Drivers, AAS 199.0805J, Rosa, M.R., Schaerer, D., Zinnecker, H., HST imaging 2002. and spectroscopy of Compact HII regions in the Käufl, H.U., Locurto, G., Kerber, F., Heijligers, B., V838 Magellanic Clouds: Revealing the youngest massive Mon, IAU Circ. 7831, 2002. star clusters, AAS 199, #124.05, 2002. Kerber, F., Wills, B., Alexov, A., Bristow, P., Seifarth, A., Chiaberge, M., Capetti, A., Celotti, A., Optical synchro- Rosa, M. R., Science from the refurbished FOS/BLUE tron emission from the nuclei of FR I radio galaxies, archive: Interstellar absorption lines in a sample of New Astronomy Review, 46, 339, 2002. low red-shift quasars, AAS, 200, 4018, 2002. Colina, L., Alberdi, A., Torrelles, J.M., Panagia, N., Kerber, F., Pirzkal, N., Rosa, M.R., V4334 Sagittarii, Wilson, A.S., Garrington, S.T., Supernova 2000ft in IAU Circ. 7879, 3, 2002. NGC 7469, IAU Circ. 7838, 2002. Kerber, F., Bristow, P.D., Alexov, A., Luridiana, V., Rosa, Fosbury, R., Albrecht, R., The Space Telescope European M.R., No Internal/External Offsets in the FOS/BLUE Coordinating Facility, STScI Newsletter, 19 (03), 17, Wavelength Calibration Zero Point (12/01), ST-ECF 2002. Technical. Report, POA/FOS-2001-05, 2002. Freudling, W., Arribas, S., Cristiani, S., Fosbury, R., Kerber, F., Bristow, P.D., Alexov, A., Rosa, M.R., Jakobsen, P., Pirzkal, N., Confusion limits on Spectra Science Verification of the POA Corrected FOS taken with the Next Generation Space Telescope Archive (12/01), ST-ECF Technical. Report, Near-Infrared Multi-Object Spectrograph, AAS POA/FOS-2001-06, 2002. 199.0806F, 2002. Lamers, H., Panagia, N., Romaniello, M., Scuderi, S., Giavalisco, M., Riess, A., Casertano, S., Dahlen, T., Spaans, M., Massive Stars in the Bulge of M51 a new Dickinson, M., Ferguson, H., Hook, R., Idzi, R., mode of star formation?, invited paper, Heidelberg Koekemoer, A., Mobasher, B., Moustakas, L.A., Workshop Modes of Star Formation, eds. X.X. Ravindranath, S., Strolger, L., Tonry, J., Challis, P., Brandner, E. Grebel, ASP Conf. Ser., ASP, San Supernovae 2002ez, 2002fv, 2002fw, 2002fx, 2002fy, Francisco, in press, 2002. 2002fz, 2002ga, IAU Circ. 7981, 2002. Maíz-Apellániz, J., Photometry of saturated stars in CCD Grogin, N.A., H.C. Ferguson, M.E. Dickinson, M. images, to appear in 2002 HST Calibration Workshop, Giavalisco, B. Mobasher, P. Padovani, R.E. Williams, STScI, edited by S. Arribas, A. Koekemoer, B. R. Chary, R. Gilli, T.M. Heckman, D. Stern, C. Winge, Whitmore, 2002. The Chandra Deepest Fields in the Infrared: Making Maíz-Apellániz, J., Walborn, N.R., MacKenty, J.W., the Connection between Normal Galaxies and AGN, Norman, C.A., Pérez, E., Mas-Hesse, J.M., Objective- BAAS, 199, #148.02, 2002. prism spectroscopy with STIS-HST, in Galaxies: the Gronwall, C., Pasquali, A., Pirzkal, N., Walsh, J.R., Third Dimension, ed. M. Rosado, L. Binette, L. Arias, Tsvetanov, Z.I., Martel, A.R., Hook, R.N., Freudling, in press, 2002. W., Albrecht, R., Fosbury, R.A.E., Hartig, G., Bohlin, McDowell, J., Clements, D.L., Lamb, S., Borne, K., R.C., Tran, H.D., Benítez, N., Early Observations with Arribas, S., Colina, L., Hearn, N., Mundell, C., Baker, the ACS Grism, AAS 200.6204G, 2002. A., X-Rays From Arp 220 And Its Surroundings, APS Hartig, G., Ford, H., Illingworth, G., Clampin, M., APRJ11003M, 2002. sp1247s4.qxd 3/5/03 3:59 PM Page 149

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Meurer, G., Ford, H., Martel, A., Sirianni, M., Tran, H., Pirzkal, N., Pasquali, A., Daddi, E., Walsh, J.R., Hook, Bohlin, R., Clampin, M., Cox, C., De Marchi, G., R.N., Spectral Extraction from ACS & VLT multi- Hartig, G., Kimble, R., Argabright, V., Performance of object spectroscopic data, AAS, 200, 6208, 2002. the Solar Blind Channel of the HST Advanced Camera Proffitt, C.R. et al., STIS Calibration Status, in 2002 HST for Surveys, BAAS, 200, 62.07, 2002. Calibration Workshop, STScI, eds. S. Arribas, A. Meylan G., Omega Cent: A General Overview, invited Koekemoer, B. Whitmore, in press, 2002. review in Omega Cent, A Unique Window into Quimby, P., et al., Panagia, N., et al. The Supernova Astrophysics, eds. F. van Leeuwen, J. Hughes, G. Cosmology Project Collaboration, The Host Galaxies Piotto, San Francisco, ASP Conf. Ser., 265, pp.3-18. of Type Ia Supernovae at High Redshift, BAAS, 201, Padovani, P., Blazar Surveys, in Blazar Astrophysics with #23.05, 2002. BeppoSAX and other Observatories, P. Giommi, E. Rauch, T., Kerber, F., van Wyk, F., 2p2Team, V838 Mon, Massaro, G. Palumbo eds., ASI, 101. IAU Cir. 7886, 2002. Padovani, P., P. Giommi, H. Landt, E. Perlman, Unifica- Sirianni, M., Clampin, M., Hartig, G., Ford, H., tion of Faint Radio-loud Sources: The DXRBS View, Illingworth, G., Golimowski, D., Martel, A., McCann, in Issues in Unification of AGNs, R. Maiolino, A. W., De Marchi, G., Mutchler, M., Pavlovsky, C., Marconi, N. Nagar (eds.), ASP Conf. Ser., 258, 297, Argabright, V., Burmester, B., Koldewyn, W., Schrein, 2002. R., Sullivan, P. Performance of the ACS WFC and Panagia, N., Primordial Stellar Populations, invited HRC CCDs, BAAS, 200, 62.05, 2002. review in Workshop Origins 2002 The Heavy Element Stockdale, C.J., Perez- Torres, M.A., Marcaide, J.M., Trail from Galaxies to Habitable Worlds, (Jackson Sramek, R.A., Weiler, K.W., Van Dyk, S.D., Panagia, Lake Lodge, Grand Teton National Park, Wyoming, N., Lundqvist, P., Pooley, D., Immler, S., Lewin, W., May 26-29, 2002), eds. C.E. Woodward, E. Smith, Supernova 2001gd IN NGC 5033, IAU Circ. 7830, ASP, San Francisco, in press, 2002. 2002. Panagia, N., Space Telescopes of Today and Tomorrow Stockdale, C.J., Sramek, R.A., Weiler, K.W., Van Dyk, S. HST and NGST, invited talk, 1999 Frascati Workshop D., Perez- Torres, M.A., Marcaide, J.M., Ray, A. Multi-frequency Behaviour of High Energy Cosmic Chandra, P., Panagia, N., Montes, M.J., Radio Sources,, eds. F. Giovannelli, L. Sabau-Graziati, Mem. Observations of SN 2001gd in NGC 5033, BAAS, , S. A. It., 73, 88-98, 2002. 201, #56.02, 2002. Panagia, N., Supernovae at high z clues to the expansion Stockdale, C.J., Sramek, R.A., Rupen, M., Weiler, K.W., of the Universe, in 44th Annual Meeting, Italian Van Dyk, S.D., Panagia, N., Pooley, D., Lewin, W., Astron. Soc., Monte Porzio Catone, 10-15 April 2000, Meyers, S., Taylor, G., Supernova 2002hh IN NGC eds. L.A. Antonelli, G. Bono, G. Giobbi, N. Menci, 6946, IAU Circ. 8018, 2002. Mem. S. A. It., 72, 875-878, 2002. Trussoni, E., Capetti, A., Celotti, A., Chiaberge, M., SED Panagia, N., The Hubble Space Telescope at the of Low Power Radio Galaxies: Test for FR I/BL Lac Beginning of a New Millennium, invited talk, 2001 Unification, in Issues in Unification of Active Galactic Frascati Workshop Multifrequency Behaviour of High Nuclei, ASP Conf. Ser., 258, 177, 2002. Energy Cosmic Sources, eds. F. Giovannelli, L. Weiler, K.W., Panagia, N., Montes, M.J., Radio Sabau-Graziati, Mem. S. A. It., 73, 823, 2002. Observations of GRB Afterglows, invited review, Panagia, N., Ultraviolet Properties of Supernovae, Supernovae and Gamma-Ray Bursts, ed. K.W. Weiler, invited review, Supernovae and Gamma-Ray Bursts, Springer-Verlag, in press. ed. K.W. Weiler, Springer-Verlag, in press, 2002. Weiler, K.W., Panagia, N., Montes, M.J., Sramek, R.A., Panagia, N., Stiavelli, M., Ferguson, H.C., Stockman, Radio Emission from Supernovae and Gamma Ray H.S., Observational Properties of Primordial Stellar Bursters, eds. F. Giovannelli, L. Sabau-Graziati, Mem. Populations, in Galaxy Evolution Theory and S. A. It., in press, 2002. Observations, eds. V. Avila-Reese, C. Firmani, C. Weiler, K.W., Van Dyk, S.D., Panagia, N., Montes, M.J., Frenk, C. Allen, Rev. Mex. A.A. SC, in press, 2002. Sramek, R.A., Lacey, C.K., In the Beginning, Radio Panagia, N., Stiavelli, M., Ferguson, H.C., Stockman, Emission from Supernovae, in Neutron Stars in H.S., Primordial Stellar Populations (abstract), Supernova Remnants, eds. P.O Slane, B.M. Gaensler, Workshop Galaxy Evolution Theory and ASP Conf. Ser., 271, 375-379, 2002. Observations, Cozumel April 8-12, 2002, ADS Zinnecker H., Andersen M., Brandl B., Brandner W., 2002geto.confE..50P, 2002. Hunter D., Larson R., McCaughrean M., Meylan G., Pasquali, A., de Mello, D.F., The Galaxy Population at Moneti A., The Infrared Luminosity Function of the Intermediate Redshifts using STIS Parallel Fields, in 30 Doradus Starburst Cluster: NICMOS/HST H-band The evolution of galaxies. II – Basic Building Blocks, Photometry, in IAU Symposium 207 on Extragalactic eds. M. Sauvage, G. Stasinska, D. Schaerer, Kluwer, Star Clusters, eds. D. Geisler, E. Grebel, D. Minniti, p.541, 2002. San Francisco, ASP, 531-538, 2002. Pavlovsky, C., Clampin, M., De Marchi, G., Gilliland, R., Bohlin, R., Mack, J., Hartig, G., Sirianni, M. ACS sensitivity, BAAS, 200, 62.01, 2002. sp1247s4.qxd 3/5/03 3:59 PM Page 150

150 publications

Chief Scientist (formerly Research Support Division) Foing, B.H., Heather, D., Almeida, M., Racca, G., Refereed Journals, 2001 Marini, A., The SMART-1 Team, ESA’s SMART-1 Mission to the Moon, Lunar & Planetary Science Adelman, S.J., Snow, T.P., Wood, E.L., Ivans, I.I., XXXII, Abstract #1787 (CD-ROM), 2001. Sneden, C., Ehrenfreund, P., Foing, B.H., An ele- Foing, B.H., Heather, D.J., Duke, M., Racca, G., Pieters, mental abundance analysis of the mercury manganese C., Mizutani, H., Galimov, E., Dunkin, S.K., van star HD 29647 2001, MNRAS, 328, 1144, 2001. Susante, P., Frischauf, N., Almeida, M., Results and Foing, B., Van Susante, P., Almeida, M., Heather, D., Recommendations from the International Conference Duke, M., Dunkin, S., Lunar Explorers Society, Lunar on the Exploration and Utilisation of the Moon 4 Explorers Society: Goals And Activities, Earth, Moon (ICEUM4), Lunar & Planetary Science XXXII, and Planets, 85, 533, 2001. Abstract #1712 (CD-ROM), 2001. Foing, B.H., Duke, M., Galimov, E., Mizutani, H., Foing, B.H., Duke, M., Galimov, E., Mizutani, H., Pieters, C., Racca, G., Heather, D.J., Frischauf, N., ILEWG, Next Steps for International Lunar van Susante, P., Almeida, M., Highlights from Exploration, Lunar & Planetary Science XXXII, ICEUM4, the 4th International Conference on the Abstract #1827 (CD-ROM), 2001. Exploration and Utilisation of the Moon, Earth, Moon Foing, B.H., Heather, D.J., Duke, M., Racca, G., Pieters, and Planets, 85, 133, 2001. C.M., Mizutani, H., Galimov, E., Dunkin, S.K., van Foing, B.H., Heather, D.J., Almeida, M., SMART-1 Susante, P., Frischauf, N., Almeida, M., ICEUM4 Science Technology Working Team, The Science participants, Results and Recommendations from the Goals of ESA’s SMART-1 Mission To The Moon, International Conference on the Exploration and Earth, Moon and Planets, 85, 523, 2001. Utilisation of the Moon 4 (ICEUM4), Lunar & Oliveira, J.M., Unruh, Y.C., Foing, B.H., Preliminary Planetary Science XXXII, Abstract #1712 (CD-ROM), MUSICOS 96 results on Balmer line variability on the 2001. TTauri star SU aurigae 2001, Adv. Space Res., 26, Foing, B.H., Heather, D., Almeida, M., Racca, G., Mar- 1747, 2001. ini, A., SMART-1 Team, ESA’s SMART-1 Mission to Oliveira, J.M., Foing, B.H., Preliminary investigation of the Moon, Lunar & Planetary Science XXXII, circumstellar emission and flares in the fast rotating Abstract #1787 (CD-ROM), 2001. giant FK Comae 2001, Adv. Space Res., 26, 1733, Heather, D.J., Dunkin, S.K., Wilson, L., Volcanism on 2001. the Marius Hills Plateau. Lunar & Planetary Science Racca, G.D., Foing, B.H., Coradini, M., SMART-1: The XXXII, Abstract #1542 (CD-ROM), 2001. First Time Of Europe To The Moon; Wandering in the Heather, D.J., Foing, B.H., van Susante, P., Almeida, M., Earth-Moon Space, Earth, Moon and Planets, 85, 379, Outreach and Education from ESA’s SMART-1 2001. Mission to the Moon, Lunar & Planetary Science XXXII, Abstract #1983 (CD-ROM), 2001. Heather, D.J., All Aboard the Mystery Express, Earth Chief Scientist Space Rev., 10 (4), 21-24, 2001. Proceedings and other Publications, 2001 Heather, D.J., The Ultimate Rendezvous, Earth Space Rev., 10 (3), 19-23, 2001. Boudin, N., in Proc. 2nd European Workshop on Exo- Heather, D.J., Last of the big spenders, Earth Space Rev., Astrobiology, ESA SP-518, 37, 2001. 10 (2), 22-25, 2001. Dunkin S.K., Grande M., Browning R., D-CIXS Team, Heather, D.J., Europe goes to the Moon, Astronomy Now, The D-CIXS X-ray spectrometer on ESA’s SMART-1 15 (2), 56-58, 2001. mission to the Moon, Lunar & Planetary Science Heather, D.J., Return to the Forgotten Planet, Earth XXXII, Abstract #1310 (CD-ROM), 2001. Space Rev., 10 (1), 22-24, 2001. Dunkin, S.K., Heather, D.J., Unveiling the face of the Oliveira, J.M., Foing, B.H., Unruh, Y.C., Spectral Line Moon, in Thompson, J.M.T. (ed) Visions of the Variability in the Circumstellar Environment of the Future: Astronomy and Earth Science, Cambridge Classical T Tauri Star SU Aurigae (CD-ROM Univ. Press, 115-130, 2001. Directory: contribs/oliveira), 2001 ASP Conf. Ser. Ehrenfreund, P., O’Tuairisg, S., Foing, B.H., Sonnen- 223: 11th Cambridge Workshop on Cool Stars, Stellar trucker, P., Cami, J., The Diffuse Interstellar Bands Systems and the Sun, 11, p.539, 2001. and Organic Molecules in Space, in The Bridge Petit, P., Donati, J.-F., Wade, G.A., Landstreet, J.D., Between the Big Bang and Biology: Stars, Planetary Oliveira, J.M., Shorlin, S.L.S., Sigut, T.A.A., Systems, Atmospheres, Volcanoes: Their Link to Life, Cameron, A.C., Differential Rotation of Close Binary p.150, 2001. Stars: Application to HR 1099, Astrotomography, Foing, B.H., Exo-astrobiology with ESA space science Indirect Imaging Methods in Observational Astron- missions, in Proc. Exo-astro-biology. Proceedings of omy, p.232, 2001. the First European Workshop, 21-23 May 2001, Ruiterkamp, R., Ehrenfreund, P., Foing, B.H., Salama, F., ESRIN, Frascati, Italy, Eds. P. Ehrenfreund, O. Organics experiment on the International Space Angerer, B. Battrick. ESA SP-496, 121-126, 2001. Station, ESA SP-496, 137, 2001. sp1247s4.qxd 3/5/03 3:59 PM Page 151

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Chief Scientist Berge, S., Bodin, P., Edfors, A., Hussain, A., Kugel- Refereed Journals, 2002 berg, J., Larsson, N., Ljung, B., Meijer, L., Mortsell, A., Nordeback, T., Persson, S., Sjoberg, F., SMART-1 Ehrenfreund, P., Cami, J., Jiménez-Vicente, J., Foing, mission description and development status,Planet. B.H., Kaper, L., van der Meer, A., Cox, N., Space Sci. 50, 1323, 2002. d’Hendecourt, L., Maier, J.P., Salama, F., Sarre, P.J., Ruiterkamp, R., Halasinski, T., Salama, F., Foing, B.H., Snow, T.P., Sonnentrucker, P., Detection of Diffuse Allamandola, L.J., Schmidt, W., Ehrenfreund, P., Interstellar Bands in the Magellanic Clouds, A.J., 576, Spectroscopy of large PAHs. Laboratory studies and L117, 2002. comparison to the Diffuse Interstellar Bands, A&A, Foing, B.H., Heather, D.J., Preface to Lunar Exploration, 390, 1153, 2002. COSPAR B0.2 Symposium, Adv. Space Res., 30 (8), 1867, 2002. Foing, B.H., Lunar Exploration, Planet. Space Sci., 50, Chief Scientist 14-15, v-vi, 2002. Proceedings and other Publications, 2002 Grande, M., Dunkin, S.K., Kellet, B., Perry, C., Browning, R., Waltham, N., Kent, B., Swinyard, B., Almeida, M., Foing, B.H., Vilar, E., Heather, D., Parker, D., Perry, A., Feraday, J., Howe, C., Huovelin, Koschny, D., Marini, A., SMART-1 Science Experi- J., Muhli, P., Hakala, P.J., Vilhu, O., Thomas, N., ments Coordination, ESA SP-514, 55-60, 2002. Hughes, D., Alleyne, H., Grady, M., Russell, S.S., Berghmans, D., Foing, B.H., Fleck, B., Automated detec- Lundin, R., Barabash, S., Baker, D., Clarke, P.E., tion of CMEs in LASCO data in 2002, in Proc. SOHO Murray, C.D., Christou, A., Guest, J., Casanova, I., 11 Symposium on From Solar Min to Max: Half a d’Uston, L.C., Maurice, S., Foing, B.H., Heather, D.J., Solar Cycle with SOHO, 11-15 March 2002, Davos, Kato, M., The D-CIXS X-ray spectrometer, and its Switzerland, A. Wilson (ed), ESA SP-508, 437-440, capabilities for lunar science, Adv. Space Res., 30 (8), 2002. 1901-1908, 2002. Boudin, N., Large Organics in Space: Laboratory Heather, D.J., Dunkin, S.K., Crustal stratigraphy of the Measurements of Gas Phase Spectra and Diffuse Al-Khwarizmi-King/Tsiolkovsky-Stark region of the Interstellar Bands, in Proc. 2nd European Workshop lunar farside as seen by Clementine, Planet. Space on Exo-Astrobiology, ESA SP-518, 37, 2002. Sci., 50, 14-15, 1311-1321. Cox, N. et al. (incl. B.H. Foing), Complex Carbon Heather, D.J., Dunkin, S.K., A Stratigraphic Study Of Chemistry and the Diffuse Interstellar Bands in the Southern Oceanus Procellarum Using Clementine Magellanic Clouds, in Proc. 2nd European Workshop Multispectral Data, Planet. Space Sci., 50, 14-15, on Exo-Astrobiology, ESA SP-518, 447, 2002. 1299-1309. Foing, B. H. Astrobiology with ESA Science Missions, in Huovelin, J., Alha, L., Andersson, H., Andersson, T., ASP Conf. Ser. 269 The Evolving Sun and its Influ- Browning, R., Drummond, D., Foing, B., Grande, M., ence on Planetary Environments, Ed. B. Montesinos, Hamalainen, K., Laukkanen, J., Lamsa, V., Muinonen, A. Gimenez, E.F. Guinan, p.361, 2002. K., Murray, M., Nenonen, S., Salminen, A., Sipila, H., Foing, B.H., Space activities in exo-astrobiology, in Taylor, I., Vilhu, O., Waltham, N., Lopez-Jorkama, M. book: Astrobiology: The quest for the conditions of The SMART-1 X-ray solar monitor (XSM): life, G. Horneck, C. Baumstark-Khan (ed.), Physics calibrations for D-CIXS and independent coronal and astronomy online, Springer, 389-398. science, Planet. Space Sci. 50, 1345, 2002. Foing, B.H., ILEWG, Preface, in Proc. ESLAB36 on Marini, A.E., Racca, G.R., Foing, B.H., SMART-1 Earth-like planets and Moons, ESA SP-514, 3, 2002. Technology Preparation for Future Planetary Foing, B.H. et al., Closing Remarks on ESLAB36, ESA Missions, Adv. Space Res., 30 (8), 1895, 2002. SP-514, 345, 2002. Neiner, C., Hubert, A.-M., Floquet, M., Jankov, S., Ruiterkamp, R., Halasinski, T., Salama, F., Foing, B., Henrichs, H.F., Foing, B., Oliveira, J., Orlando, S., Schmidt, W., Ehrenfreund, P., Laboratory Calibration Abbott, J., Baldry, I.K., Bedding, T.R., Cami, J., Cao, Studies in Support of an ISS Exposure Experiment H., Catala, C., Cheng, K.P., Domiciano de Souza, A., and Comparison to the Diffuse Interstellar Bands, in Janot-Pacheco, E., Hao, J.X., Kaper, L., Kaufer, A., NASA Laboratory Astrophysics Workshop, p.77, 2002. Leister, N.V., Neff, J.E., O’Toole, S.J., Schäfer, D., Ten Kate, I. et al. (incl. B.H. Foing, N. Boudin), Smartt, S.J., Stahl, O., Telting, J., Tubbesing, S., Laboratory Studies on Complex Organic Molecules Zorec, J., Non-radial pulsation, rotation and outburst on Mars: Part 1 – Rationale, ESA SP-514, 293, 2002. in the Be star omega Orionis from the MuSiCoS 1998 Ten Kate, I. et al. (incl. B.H. Foing), Laboratory Studies campaign, A&A, 388, 899, 2002. on Complex Organic Molecules on Mars: Part 2 – Racca, G.D., Marini, A., Stagnaro, L., van Dooren, J., di Experimental Set-Up and Related Work, in Proc. 2nd Napoli, L., Foing, B.H., Lumb, R., Volp, J., Brink- European Workshop on Exo-Astrobiology, ESA SP- mann, J., Grunagel, R., Estublier, D., Tremolizzo, E., 518, 81, 2002. McKay, M., Camino, O., Schoemaekers, J., Hechler, M., Khan, M., Rathsman, P., Andersson, G., Anflo, K., sp1247s4.qxd 3/5/03 3:59 PM Page 152

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Chief Scientist Stagiaire Research Reports and Theses, 2001 Editorials/Books Almeida, M. (U. Lisbon), SMART-1 Science Payload Foing, B.H. & Battrick, B. (eds), Proc. ESLAB36 Earth- Operations. like planets and Moons, ESA SP-514, 356pp, 2002. Dages, O. (DESS Obs. Paris-Meudon), SMART-1 Foing, B.H., Heather, D.J. (eds), Lunar Exploration, Adv. Mission Risk Tree Analysis. Space Res., 30 (8). Lefevre, F. (DESS Obs. Paris-Meudon), Optimisation of Foing, B.H., (Guest Editor), Special Issue on Lunar Payload Operations Timelining. Exploration, Planet. Space Sci., 50. Martinez Sanmartin, S. (U. Vigo), Operational Request Heather, D.J., Foing, B.H. (eds.), First Convention of File Acknowledger Testing Tools. Lunar Explorers Abstract and Program, Paris, March, Oliveira, J. (PhD Thesis, RSSD/U. do Porto), Circum- 58pp, 2001. stellar Environments and Activity in Young and Heather, D.J. (ed), New Views of the Moon, Europe: Evolved Stars, PhD defence at U. do Porto, April Future Lunar Exploration, Science Objectives, and 2001. Integration of Datasets, Abstracts, ESTEC RSSD, Reissaus, P. (TU Munich), Simulation of Meteoroid’s Noordwijk. Re-entry Behaviour in Earth’s Atmosphere.

Stagiaire Research Reports and Theses, 2002

Bonal, L. (U. Orsay), Study of Comet Dust Analogues & Interplanetary Dust Particles with Atomic Force Microscope. Diaz, J. (U. Vigo), Meteor Orbit & Trajectory Determin- ation Software. Hijmering, R. (U. Nijmegen), Astronomical Detectors. Lärfars, K. (U. of Umea/ Kiruna), Test and Character- isation of a Low Noise Multi-channel Customised Application Specific Integrated Circuit. Manaud, N. (DESS Obs. Paris-Meudon), Auxiliary Data in SPICE format: Conversion, Validation, Distribution. O’Sullivan J. (ESTEC YGT report), Optimisation of Dust Impact Time of Flight Mass Spectrometer. Ott, S. (PhD Thesis, RSSD Vilspa/CEA), Observations of the Infrared Sky with the ISOCAM Parallel Mode, PhD defence at IAP Paris, February 2002. Riesen, T.-E. (U. Bern), Planetary Data System Standard Tutorial. Ubeira, M. (U. Vigo), Knowledge Management Video Database Application. Vazquez Garcia, B. (U. Vigo), Study of an Application Programmer Interface for ESA’s Planetary Archives. Vilar, E. (UPC Barcelona), Planning & Optimisation of Science Payload Operations for SMART-1 & Rosetta. Ziljstra, A. (U. Delft), Mission to the Moon: Lunar Scout Lander Design. sp1247s4.qxd 3/5/03 3:59 PM Page 153

ANNEX 3 Seminars and Colloquia sp1247s4.qxd 3/5/03 3:59 PM Page 154

154 seminars and colloquia

Seminars held at ESTEC 30 November The Interior and Evolution of Terrestrial Planets 2001 T. Spohn, University of Munster

12 January 14 December Interstellar Probes Leonid Meteor Observations in Australia – What we I. Mann, Solar System Division Can Learn from their Light Curves D. Koschny, Solar System Division 9 February The Cassini Jupiter Fly-by and the International Jupiter Watch 2002 H.O. Rucker, Austrian Academy of Sciences 25 January 23 February Observations of the Sky with the ISOCAM Parallel 15 years After the Halley Encounter – Are we Entering Mode the Golden Age of Cometary Exploration? S. Ott, ISO, VILSPA G. Schwehm, Solar System Division 7 February 6 April Chemical Composition of Planetary Surfaces from The X-ray/Infrared Connection: New Observations of Remote Sensing Techniques Starburst Galaxies and Active Galactic Nuclei S. Maurice, Observatoire Midi-Pyrenees M. Ward, Leicester University 22 February 27 April Herbig-Haro Objects: A New Class of Astrophysical Spacecraft Mass Modelling in High-Energy Astro- X-ray Sources physics and Some Recent Scientific Results F. Favata, Astrophysics Missions Division A.J. Dean, Southampton University 8 March 1 June The Messenger Mission to Mercury Mars Express: Science, Payload and Mission J. Slavin, NASA Goddard Space Flight Center Overview A. Chicarro, Solar System Division 22 March Re-ionizing the Universe: Why? When? How? 8 June P. Jakobsen, Astrophysics Missions Division Comets and Circumstellar Environments of Young Stars 12 April C. Waelkens, University of Leuven Water in Europa: Evidence from Surface Composition Obtained by Galileo 22 June T. McCord, University of Hawaii The Darwin Mission M. Fridlund, Astrophysics Division 17 May The Astrophysical Virtual Observatory – More Than 10 September Just a Federation of Archives A Novel Method for the Analysis of Planetary Transit P. Benvenuti, ST-ECF, Garching Data: A Bayesian Algorithm for the Analysis of the Eddington Data 31 May S. Aigrain, Astrophysics Division Serendipity in Science: Using Microwave Wind Scatterometers for Non-wind Applications 21 September M. Drinkwater, Earth Sciences Division Optical/Infrared Interferometry with the VLTI W. Jaffe, Leiden University 14 June Search for Extrasolar Planets: Earth Objective 19 October D. Queloz, Observatoire de Geneve Tomography of Stars and Circumstellar Environments A. Collier Cameron, St. Andrews 5 July The Stellar IMF and the Disruption of Globular 17 November Clusters Large Molecules and the Interstellar Medium G. de Marchi, STScI, Baltimore A. Tielens, Kapteyn Astronomical Institute sp1247s4.qxd 3/5/03 3:59 PM Page 155

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6 September Colloquia held at ESTEC Astromineralogy: the Search for the Crystalline Silicates 2001 F. Molster, Research Support Division 8 February 17 September Our Galaxy – In Three Dimensions Discontinuous Cusp: A Spatial or Temporal Feature M. Perryman, Astrophysics Division K.-H. Trattner, Lockheed Martin ATC 21 March 30 September The Taming of Plasmas: Order from Chaos The Public Interest Perspective in Planetary G. Morfill, MPI, Garching Exploration L. Friedman, The Planetary Society 2002 4 October Massive Stars: Observations versus Theoretical 3 June Simulations A Family Portrait of Earth-like Planets and Moons: D. Vanbeveren, Free University of Brussels Similarities and Differences J. Head, Brown University 1 November Search for Aromatic Cations in Interstellar Space 7 June N. Boudin, Research Support Division To the Moon and Beyond H. Schmitt, Annapolis Center 29 November Einstein’s Telescope: Gravitational Lensing as a Cosmological Tool M. Barthelman, Max-Planck-Institute, Garching

13 December Precision Atom Interferometry on Ground and in Space W. Ertmer, University of Hannover sp1247s4.qxd 3/5/03 3:59 PM Page 157

ANNEX 4 Acronyms sp1247s4.qxd 3/5/03 3:59 PM Page 158

158 acronyms

AAS American Astronomical Society CNES Centre National d’Etudes Spatiales AAT Anglo-Australian Telescope CNR Consiglio Nazionale della Ricercha (Italy) ACE Atomic Composition Explorer (NASA) CNRS Centre National de la Recherche Scientifique ACR Anomalous Cosmic Rays (France) ACS Advanced Camera for Surveys (HST) CNSA Chinese National Space Administration ADS Astrophysics Data System (NASA) Co-I Co-Investigator AFM Atomic Force Microscope COMPTEL Compton Telescope (CGRO) AGB Asymptotic Giant Branch CONSERT Comet Nucleus Sounding Experiment by AGN Active Galactic Nuclei Radiowave Transmission (Rosetta) AGU American Geophysical Union COPUOS Committee for the Peaceful Use of Outer AIV Assembly, Integration & Verification Space (United Nations) ALICE Rosetta Orbiter UV imaging spectrometer COROT COnvection, ROtation and planetary Transits ALMA Atacama Large Millimetre Array COS Cosmic Origins Spectrograph (HST) AMIE Asteroid Moon micro-Imager Experiment COSAC Comet Sampling and Composition (SMART-1) Experiment (Rosetta) AO Announcement of Opportunity COSIMA Cometary Secondary Ion Mass Analyser AOT Astronomical Observing Template (Rosetta) COSPAR Committee on Space Research APPLES ACS Pure Parallel Ly-alpha Emission Survey COSPIN Cosmic Ray & Solar Charged Particles APXS Alpha-Proton-X-ray Spectrometer (Rosetta) Investigation (Ulysses) AR Archival Research COSTEP Comprehensive Measurements of the Supra- ASI Italian Space Agency Thermal and Energetic Particles Populations ASIC Application Specific Integrated Circuit (SOHO) ASPOC Active Spacecraft Potential Control (Cluster) CP Charge Parity AU Astronomical Unit CPM Chemical Propulsion Module (BepiColombo) BATSE Burst and Transient Source Experiment CR Carrington Rotation (CGRO) CSA Canadian Space Agency BeppoSAX Satellite per Astronomia in raggi X CSDS Cluster Science Data System (Italy/The Netherlands) CsI caesium iodide CSRC Czech Space Research Centre BHE banded hiss emission CTIO Cerro Tololo Inter-American Observatory BiSON Birmingham Solar Oscillations Network CTTS Classical T-Tauri Star BLR Broad Line Region CXB Cosmic X-ray Background

CBRF Cosmic Background Radiation Field D-CIXS Demonstration of a Compact Imaging X-ray CCD Charge Coupled Device Spectrometer (SMART-1) CDMS Cluster Data Management System D/SCI Directorate of Scientific Programmes (ESA) CDF-S Chandra Deep Field - South DESPA Observatoire de Paris, Département Spatial CDS Coronal Diagnostics Spectrometer (SOHO) DIB Diffuse Interstellar Band CDS Centre de Données astronomiques de DISR Descent Imager/Spectral Radiometer Strasbourg (Huygens) CdTe cadmium telluride DLR Deutsches Zentrum für Luft- und Raumfahrt CELIAS Charge, Element and Isotope Analysis DPC Data Processing Centre System (SOHO) DPU Data Processing Unit CEPHAG Centre d’Etude des Phenomenes Aleatoires DROID distributed readout architecture et Geophysiques (France) DRS disturbance reduction system (SMART-2) CERN Centre Européen de Recherches Nucléaires DSDS Double Star Data System (France) DSN Deep Space Network CESR Centre d'Etude Spatial des Rayonnements DSP Digital Signal Processor; Double Star (France) Programme (China) CETP Centre d’Etudes des Environments Terrestres DSRI Danish Space Research Institute et Planetaires (France) D/TOS Directorate of Technical and Operational CFHT Canadian-French-Hawaiian Telescope Support (ESA) CIR Corotating Interaction Region DTP Darwin Technology Package CIS Cluster Ion Spectrometry DXRBS Deep X-ray Radio Blazar Survey CIVA Comet Infrared and Visible Analyser (Rosetta) EAS European Astronomical Society CMB Cosmic Microwave Background ECF European Coordinating Facility CMD colour magnitude diagram EC European Commission CME Coronal Mass Ejection EDI Electron Drift Instrument (Cluster) CMOS Complementary Metal Oxide Semiconductor ESC Eddington Science Centre sp1247s4.qxd 3/5/03 3:59 PM Page 159

acronyms 159

EFW Electric Field and Wave experiment GMT Greenwich Mean Time (Cluster) GOLF Global Oscillations at Low Frequency EGS European Geophysical Society (SOHO) EIT Extreme UV Imaging Telescope (SOHO) GONG Global Oscillation Network Group EQM Electrical Qualification Model GOODS Great Observatories Origins Deep Survey ELF Extremely Low Frequency GORID Geostationary Orbit Impact Detector EM Electrical Model, Engineering Model GR General Relativity EOF Experiment Operations Facility (SOHO) GRB Gamma Ray Burst EP Equivalence Principle GSE Ground Support Equipment EPAC energetic particle instrument (Ulysses) GSFC Goddard Space Flight Center (NASA) EPDP Electric Propulsion Diagnostic Package GSTP General Support & Technology Programme (SMART-1) (ESA) EPIC European Photon Imaging Camera (XMM- GTO Geostationary Transfer Orbit Newton) EPS European Physical Society HASI Huygens Atmospheric Structure Instrument ERNE Energetic and Relativistic Nuclei and HCS Heliospheric Current Sheet Electron experiment (SOHO) HDF Hubble Deep Field ESA European Space Agency HEASARC High Energy Astrophysics Science Archive ESLAB European Space Laboratory (former name of Center SSD/RSSD) HEB Hot Electron Bolometer ESO European Southern Observatory HEMT High Electron Mobility Transistor ESOC European Space Operations Centre, HEW Half Energy Width Darmstadt (Germany) HFI High Frequency Instrument (Planck) ESPADONS Echelle SpectroPolarimetric Device for the HGA High-Gain Antenna Observation of Stars at CFHT HIFI Heterodyne Instrument for FIRST (Herschel) ESR Emergency Sun Reacquisition (SOHO) HPGSPC High Pressure Gas Scintillation Proportional ESRIN ESA’s Documentation and Information Counter (BeppoSAX) Centre (Italy) HPOC Huygens Probe Operations Centre ESRO European Space Research Organisation HR Hertzsprung-Russell ESTEC European Space Research and Technology HRSC High Resolution Stereo Camera (Mars Centre, Noordwijk Express) (The Netherlands) HSC Herschel Science Centre EUSO Extreme Universe Space Observatory HST Hubble Space Telescope EUV Extreme Ultra-Violet EW equivalent width IAC Instituto de Astrofisica de Canarias IACG Inter-Agency Consultative Group for Space FEEP Field Emission Electric Propulsion Science FES Fine Error Sensor IAEA International Atomic Energy Agency FET field effect transistor IAP Institute of Atmospheric Physics (Czech FGS Fine Guidance Sensor (HST) Republic) FIRST Far Infrared and Submillimetre Space IAS Institut d’Astrophysique Spatiale, Orsay Telescope (now Herschel) (France) FM Flight Model IAS Istituto di Astrofisica Spaziale (Rome) 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) IDC ISO Data Centre FOS Faint Object Spectrograph (HST) IDIS Integrated Data and Information System FOV Field of View (Planck) FP Fabry-Pérot IDP Interplanetary Dust PArticle FSRQ Flat Spectrum Radio Quasar IDT Instrument Dedicated Team FTE Flux Transfer Event IFS Integral Field Spectroscopy FTS Fourier Transform Spectrometer IFSI Istituto Fisica Spazio Interplanetario (Italy) FUV far-ultraviolet IFTS Imaging Fourier Transform Spectrometer FWHM Full Width at Half Maximum IGM intergalactic medium IGPP Institute of Geophysics & Planetary Physics GaAs gallium arsenide ILEWG International Lunar Exploration Working GC Galactic Centre Group GENIE Ground-based European Nulling ILWS International Living With a Star programme Interferometer Experiment IMEWG International Mars Exploration Working GIADA Grain Impact Analyser and Dust Group Accumulator (Rosetta) IMF Initial Mass Function sp1247s4.qxd 3/5/03 3:59 PM Page 160

160 acronyms

IMF Interplanetary Magnetic Field LIC Local Interstellar Cloud IMPACT In-situ Measurements of Particles And CME LISA Laser Interferometer Space Antenna Transients LIST LISA International Science Team INES IUE Newly Extracted Spectra LMC Large Magellanic Cloud INT Isaac Newton Telescope LMXRB Low Mass X-ray Binary INTA Instituto Nacional de Técnica Aerospacial LOI Luminosity Oscillation Imager (SOHO) (Spain) LOWL Ground-based instrument for observing solar IOA Institute of Astronomy (Cambridge, UK) low p-modes, High Altitude Observatory, IPAC Infrared Processing Analysis Center USA IR Infrared LPCE Laboratoire de Physique et Chemie, de IRAS Infrared Astronomy Satellite l’Environnement (France) IRF-U Institute for Space Physics-Uppsala LPSP Laboratoire de Physique Stellaire et (Sweden) Planétaire (France) IRSA Infrared Science Archive LPV Long-Period Variable IRSI InfraRed Space Interferometer LTE Local Thermal Equilibrium ISAAC Infrared Spectrometer and Array Camera LTP LISA Technology Package ISAS Institute of Space and Astronautical Science LWS Long Wavelength Spectrometer (ISO) (Japan) ISDC Integral Science Data Centre MCP Microchannel Plate ISGRI Integral Soft Gamma Ray Imager MDC Mars Dust Counter ISL Instrument Sonde de Langmuir 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 MEDOC Multi-Experiment Data Operations Centre (Switzerland) MHD Magnetohydrodynamics Istituto TeSRE Istituto Technologie e Studio Radiazioni Microscope MICROSatellite à traînée Compensée pour Extraterrestri (Italy) l’Observaton du Principe d’Equivalence ITT Invitation to Tender (CNES) IUE International Ultraviolet Explorer MIDAS Micro-Imaging Dust Analysing System IUEFA IUE Final Archive (Rosetta) IUPAP International Union of Pure and Applied MIP Mutual Impedance Probe (Rosetta) Physics MIRO Microwave Instrument for the Rosetta Orbiter (Rosetta) JCMT James Clark Maxwell Telescope MLT Magnetic Local Time JEM-X Integral X-ray monitor MMO Mercury Magnetospheric Orbiter JPL Jet Propulsion Laboratory (NASA) (BepiColombo) JSOC Joint Science Operation Centre (Cluster) MOC Mission Operations Centre JWST James Webb Space Telescope (formerly MOLA Mars Observer Laser Altimeter NGST) MOS-CCD Metal Oxide Semiconductor Charge Coupled Device KATE X/Ka-band Telemetry & Telecommand MoU Memorandum of Understanding Experiment (SMART-1) MPAE Max-Planck-Institut für Aeronomie MPE Max-Planck-Institut für Extraterrestrische LAEFF Laboratory for Space Astrophysics and Physik Fundamental Physics MPI Max-Planck Institut (Germany) LAP Langmuir Probe (Rosetta) MPIA MPI für Astronomie LAPP Laboratoire d’Annecy-Le-Vieux de Physique MPIK Max-Planck-Institut für Kernphysik des Particules (CNRS, France) MPO Mercury Planetary Orbiter (BepiColombo) LASCO Large Angle Spectroscopic Coronagraph MSE Mercury Surface Element (BepiColombo) (SOHO) MSSL Mullard Space Science Laboratory (UK) LASP Laboratory for Astronomy and Solar Physics MUPUS Multi-Purpose Sensors for Surface and (NASA) Subsurface Science (Rosetta) LBV Luminous Blue Variable MUSICOS Multi-Site Continuous Spectroscopy LECS Low Energy Concentrator Spectrometer MXB Medium X-ray Band (BeppoSAX) LEGSPC Low Energy Gas Scintillation Proportional NAC Narrow Angle Camera (OSIRIS) Counter NARVAL New Echelle Spectropolarimeter at Bernard LET Low Energy Telescope (Ulysses) Lyot Telescope (Pic du Midi, France) LFCTR Laboratorio di Fisica Cosmica e Techologie NASA National Aeronautics & Space Relative del CNR (Italy) Administration (USA) LFI Low Frequency Instrument (Planck) NED NASA Extragalactic Database sp1247s4.qxd 3/5/03 3:59 PM Page 161

acronyms 161

NFI Narrow Field Instrument (BeppoSAX) RHESSI Reuven Ramaty High Energy Solar NGST Next Generation Space Telescope (now Spectroscopic Imager (NASA) James Webb Space Telescope) RMOC Rosetta Mission Operations Centre NHSC NASA Herschel Science Center ROLIS Rosetta Lander Imaging System NICMOS Near-Infrared Camera and Multi-Object ROMAP RoLand Magnetometer & Plasma Monitor Spectrometer (HST) (Rosetta) NIS normal incidence spectrometer ROSINA Rosetta Orbiter Spectrometer for Ion and NLR Narrow Line Region Neutral Analysis (Rosetta) NOT Nordic Optical Telescope ROSITA Roentgen Survey with an Imaging Telescope NRAO National Radio Astronomy Observatory Array (USA) RPC Rosetta Plasma Consortium NRT Near Real Time RSI Radio Science Investigation NSI NASA Science Internet RSOC Rosetta Science Operations Centre NSSDC National Space Science Data Center (at RSSD Research and Scientific Support Department GSFC, USA) (ESA) NSLS National Synchotron Light Source (USA) NTT New Technology Telescope SAO Smithsonian Astrophysical Observatory (US) NVSS NRAO/VLA Sky Survey SAp/Saclay Service d’Astrophysique (Commissariat à l’Energie Atomique; Saclay, France) OAT Osservatorio Astronomico di Trieste SAS Scientific Analysis Software (XMM- OHP Observatoire de Haute-Provence Newton); Science Analysis Subsystem OM Optical Monitor (XMM-Newton) (XMM-Newton) OMC Optical Monitor Camera (Integral) SAX Satellite per Astronomia in raggi X ONC Orion Nebula Cluster (Italy/The Netherlands) OSIRIS Optical and Spectroscopic Remote Imaging SCAM Superconducting Camera System (Rosetta) SciSIM Science Simulator SCUBA Submillimetre Common User Bolometer PACS Photodetector Array Camera and Array Spectrometer (Herschel) SEA Sociedad Española de Astronomia PAH Polycyclic Aromatic Hydrocarbon SED Spectral Energy Distribution pc parsec SEM Scanning Electron Microscope PCD Photon Counting Detector SEP solar energetic particle PDD Payload Definition Document SEPM Solar Electric Propulsion Module PDFE Particle Detector Front End (BepiColombo) PDS Planetary Data System SEPP Solar Electric Primary Propulsion PDS Phoswich Detector System SEPT Solar Energetic Particle Telescope (STEREO PI Principal Investigator mission) PIA (ISO)PHOT Interactive Analysis SESAME Surface Electric, Seismic and PIPS Passivated Implanted Planar Silicon Acoustic Monitoring Experiment (Rosetta) PLM Payload Module SEST ESO sub-mm telescope PMS Pre-Main Sequence SETI Search for Extra-Terrestrial Intelligence PN Planetary Nebula SFH Star Formation History POS Payload Operations Service (Mars Express) SFR Star Formation Rate PP Permittivity Probe (SESAME on Rosetta) SGS Science Ground System (Integral) ppm parts per million SIMBA SEST Imaging Bolometer Array PR Public Relations SIMBAD Set of Identifications, Measurements and PS Project Scientist Bibliography on Astronomical Data PST Project Scientist Team SIR Stream Interacting Region PSF Point Spread Function SIRTF Space Infrared Telescope Facility (NASA) PWA Permitivity, Waves and Altimetry (part of SIS Superconductor-Insulator-Superconductor HASI on Huygens) SLP Segmented Langmuir Probe PWG Payload Working Group SM Servicing Mission (Hubble) SMART Small Mission for Advanced Research in QED Quantum Electrodynamics Technology (ESA) QM Qualification Model SMC Small Magellanic Cloud QPO Quasi Periodic Oscillations SMEX Small Explorer (NASA) QSO Quasi Stellar Object SMOG Survey of Molecular Oxygen in the Galaxy R&D Research and Development (SMART-1) RAL Rutherford Appleton Laboratory (UK) SN Supernova RF Radio Frequency SNR Supernova Remnant RGS Reflection Grating Spectrometer (XMM- SOC Science Operations Centre; self-organising Newton) criticality sp1247s4.qxd 3/5/03 3:59 PM Page 162

162 acronyms

SOHO Solar and Heliospheric Observatory UCB University of California Berkeley SOS Silicon-on-Sapphire UCLA University of California Los Angeles SOT Science Operations Team UH Ultra-heavy (cosmic ray nuclei) SPC Science Programme Committee (ESA) ULIRG ultraluminous infrared galaxy SPEDE Spacecraft Potential, Electron & Dust URSI Union Radio Scientifique Internationale Experiment (SMART-1) USNO US Naval Observatory SPI Integral spectrometer UV Ultra-Violet SPIRE Spectral and Photometric Imaging Receiver UVCS Ultra-Violet Coronal Spectrometer (SOHO) (Herschel) UVES Ultraviolet-Visual Echelle Spectrograph SQUID Superconducting Quantum Interference (ESO VLT) Device (STEP) SRON Space Research Organisation Netherlands VILSPA Villafranca Satellite Tracking Station SRV Semi-Regular Variable VIMOS VLT Visible Multi-Object Spectrograph SSAC Space Science Advisory Committee (ESA) (ESO VLT) SSC Survey Science Consortium VIRGO Variability of Irradiance and Gravity SSD Space Science Department (ESA), now Oscillations (SOHO) RSSD VIRTIS Visible Infra Red Thermal Imaging SSP Surface Science Package (Huygens and Spectrometer (Rosetta) Rosetta) VLA Very Large Array SSWG Solar System Working Group VLBI Very Long Baseline Interferometry ST Science Team; Space Technology (NASA) VLF Very Low Frequency ST-ECF Space Telescope European Coordinating VLT Very Large Telescope Facility VLTI Very Large Telescope Interferometer (ESO STAFF Spatio-Temporal Analyis of Field VLT) Fluctuations (Cluster) VMC Venus Monitoring Camera STEP Satellite Test of the Equivalence Principle VTT Vacuum Tower Telescope STEREO Solar-Terrestrial Relations Observatory (NASA) WACWide Angle Camera (OSIRIS on Rosetta) STIS Space Telescope Imaging Spectrograph WBD Wide Band Data (Cluster) STJ Superconducting Tunnel Junction WEC Wave Experiment Consortium (Cluster) STScI Space Telescope Science Institute WFC Wide-Field Camera (HST) SUMER Solar UV Measurements of Emitted WFPC Wide-Field Planetary Camera (HST) Radiation (SOHO) WHISPER Waves of High Frequency and Sounder for SWAN Solar Wind Anisotropies (SOHO) Probing of Density by Relaxation (Cluster) SWAS Submillimeter Wave Astronomy Satellite WHT William Herschel Telescope (NASA) WTTS Weak-lined T Tauri Star 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

TACTime Allocation Committee YGT Young Graduate Trainee ToOTarget 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 TRM Technology Reference Mission TRP Technology Research Programme (ESA) TSI Total Solar Irradiance