Annual Report 2007 ESO

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ESO

European Organisation for Astronomical Research in the Southern Hemisphere

European Organisation for Astronomical Research in the Southern Hemisphere

Annual Report 2007

presented to the Council by the Director General Prof. Tim de Zeeuw ESO is the pre-eminent intergovernmental science and technology organisation in the field of ground-based astronomy. It is supported by 13 countries: Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. Further countries have expressed interest in membership.

Created in 1962, ESO provides state-of- the-art research facilities to European astronomers. In pursuit of this task, ESO’s activities cover a wide spectrum including the design and construction of world- class ground-based observational facilities for the member-state scientists, large telescope projects, design of innovative scientific instruments, developing new and advanced technologies, further- La Silla. ing European cooperation and carrying out European educational programmes. One of the most exciting features of the In 2007, about 1900 proposals were VLT is the possibility to use it as a giant made for the use of ESO telescopes and ESO operates the La Silla Paranal Ob- optical interferometer (VLT Interferometer more than 700 peer-reviewed papers servatory at several sites in the Atacama or VLTI). This is done by combining the based on data from ESO telescopes were Desert region of Chile. The first site is light from several of the telescopes, al- published. La Silla, a 2 400 m high mountain 600 km lowing astronomers to observe up to north of Santiago de Chile. It is equipped 25 times finer details than can be done ESO is also a major partner in the Ata- with several optical telescopes, with with the individual telescopes. The soon cama Large Millimeter/submillimeter Array mirror diameters of up to 3.6 metres, to come survey telescopes, VST (opti- (ALMA), one of the largest ground-based dedicated to high-profile long-term pro- cal) and VISTA (infrared), will enhance the astronomy projects of the next decade. grammes. The 3.5-m New Technology capabilities of Paranal even further. ALMA will have a main array of fifty 12-m Telescope was the first in the world to have a computer-controlled main mirror.

Whilst La Silla remains one of the scien tifically most productive observing sites in the world, the 2 600 m high Paranal site with the Very Large Telescope array (VLT) is the flagship facility of European astronomy. Paranal is situated about 130 km south of Antofagasta in Chile, 12 km inland from the Pacific Coast in what is probably the driest area in the world.

The VLT’s design, instrument complement and operating principles set the standard for ground-based optical and infrared astronomy. The VLT is composed of four 8.2-m Unit Telescopes and four movable 1.8-m Auxiliary Telescopes. Sci- entific operations began in 1999 and have resulted in a high number of extremely successful research programmes.

The VLT at Paranal.

2 ESO Annual Report 2007 submillimetre quality antennas, with baselines of several kilometres. An additional compact array of four 12-m and twelve 7-m antennas complements the main array. Construction of ALMA started in 2003 and will be completed in 2012; it will become incrementally operational from 2010 on. ALMA is located on the 5 000 m high Llano de Chajnantor, east of the village of San Pedro de Atacama in Chile. The ALMA project is a partnership between Europe, East Asia and North America in cooperation with the Republic of Chile. ALMA is funded in Europe by ESO, in East Asia by the National Insti- tutes of Natural Sciences of Japan in cooperation with the Academia Sinica in Taiwan, and in North America by the US National Science Foundation in cooperation with the National Research Council of Canada. ALMA construction and operations are led on behalf of Europe by The ESO headquarters are located in ALMA at Chajnantor ESO, on behalf of East Asia by the Na- Garching, near Munich, Germany. This is (3D computer render- ing). tional Astronomical Observatory of Japan the scientific, technical and administrative and on behalf of North America by the centre of ESO where technical develop- National Radio Astronomy Observatory, ment programmes are carried out to pro- which is managed by Associated Univer- vide the observatories with the most ad- sities, Inc. vanced instruments. It is also home for the Space Telescope European Coordi- The Chajnantor site is also home of the nating Facility (ST-ECF), operated jointly 12-m APEX submillimetre/millimetre- by ESO and the European Space Agency. wavelength telescope, operated by ESO on behalf of the Onsala Space Observa- tory, the Max-Planck Institute for Radio Astronomy and ESO itself.

ESO has built up considerable expertise in developing, integrating and operating large astronomical telescopes at remote sites. Furthermore, for several years, ESO has been engaged in conceptual studies for an extremely large optical and infra-red adaptive telescope. This expertise forms the backbone of efforts to develop a next-generation extremely large ground-based optical/infrared telescope for Europe’s astronomers. For this project, currently known as the European Extremely Large Telescope (E-ELT), ESO has developed a basic reference design for a 42-m telescope with a novel five- mirror optical concept. The current detailed design phase is scheduled to be completed by the end of 2009.

Artist’s impression of a possible design for the E-ELT.

ESO Annual Report 2007 3

Contents

Foreword 6 Introduction 7 Research Highlights 10 La Silla Paranal Observatory 24 The Observing Programmes Committee 32 Summary of Use of Telescopes by Discipline 33 The Users’ Committee 35 Instrumentation 36 Atacama Large Millimeter/submillimeter Array 44 The European Extremely Large Telescope 53 Software Developments 54 Technical Developments 58 The Science Archive Facility 62 The European Virtual Observatory 65 ST-ECF 67 The Organisation Staff Members 68 Personnel 71 Council 73 Finance Committee 74 Finance 74 The Scientific Technical Committee 76 Public Outreach 80 ESO Press Releases 85 European and International Relations 86 Relations with Chile 90 Four Seasons at a Glance 94 Glossary of Acronyms 98 Publications 101

ESO Annual Report 2007 5 Foreword

From modest beginnings in the 1960’s, ESO has moved inexorably onwards to assume the mantle of a world leader in ground-based optical/NIR astronomy and partner in the global adventure that is ALMA. Its suite of four 8m-class telescopes at Paranal along with their asso- Photo: B. Farncombe, STFC ciated interferometric capabilities, the VLT/I, and the older but powerful facilities on La Silla, are now producing around seven hundred refereed papers per year. With these developments, ESO has em- powered a vibrant and diverse community of astronomers in Europe.

On the ground in Chile, the ALMA project is rapidly becoming a tangible reality with the delivery of the first antennas and the progress towards the completion of the Before assuming the directorship, Tim de support facilities at and near Chajnantor. Zeeuw had been leading the ASTRONET Astronomers in Europe, North America Science Vision exercise that is now be- and East Asia are tooling-up for the ex- ing followed by the construction of the ploitation of these dramatically powerful Facilities Roadmap that will guide the Eu- new capabilities. ropean funding agencies over the next decade or so. He is now in a strong posi- The E-ELT project has moved up a gear tion to influence the process that will and is now engaged in a fully-fledged de- enable the fulfilment of the dreams of the sign study of a 42-m aperture telescope. European astronomers who participated Several substantial industrial contracts so energetically in this exercise. These are now in progress. The various advisory are exciting times for European and World committees have been energetic in moni- astronomy and ESO is well poised to toring and advising ESO on an endeavour continue its leading role. that is moving forward at breathtaking speed.

During 2007, the final formalities were completed to bring Spain and the Czech Republic into ESO as full members. It is highly likely that other new member Prof. Richard Wade states will follow within the next few President of the ESO Council years.

In September, Dr. Catherine Cesarsky handed the Director General’s baton to Prof. Tim de Zeeuw. Catherine steered ESO through a remarkable period of growth and development. We all owe her a great debt of gratitude for her strenu- ous efforts that resulted in an extraordi- narily vibrant organisation. Tim inherits an organisation with a very substantially enlarged membership and a portfolio of projects that was probably unimaginable to ESO’s founders.

6 ESO Annual Report 2007 Introduction

This is the first Annual Report to appear citing results on exoplanet research since I took over from Catherine where HARPS has effectively cornered Cesarsky on 1 September 2007. Most the market. of the activities and developments covered in this report were carried out under The rapid-response mode of the Very her responsibility. It is a pleasure to ac- Large Telescope (VLT) makes it possible knowledge her eight years of leadership to observe gamma-ray bursts within min- which saw many changes at ESO. utes of notification. It has provided some of the earliest spectra of these enigmatic objects. In one case, changes in the fore- New member states ground intergalactic material could be observed. The intense UV radiation from At the beginning of the year, Spain com- the burst ionised the intervening gas in pleted the formal procedure for ratifica- the first hour of the outburst. tion of its accession. The Czech Republic completed its accession soon after- A striking example of joint observations in wards, so that ESO now has thirteen very different wavelength regimes was member states. The June Council Meet- the series of coordinated observations of ing was held in Barcelona in celebration three separate layers in the outer enve- Operations of the Spanish membership. lope of the star S Orionis, carried out with the VLT Interferometer (VLTI) and the Very The start of science operations of the An ESO information day for Czech indus- Long Baseline Array in North America. high-resolution infrared spectrograph try was organised by the Czech Academy CRIRES on Antu (Unit Telescope 1 of the of Sciences in Prague in June. In Octo- The demand on ESO telescopes contin- VLT – UT1) in April marked the comple- ber, the Czech-ESO Committee met to ues to increase, with 943 Period 80 tion of the entire suite of the first-genera- discuss plans for establishing a Technol- and 952 Period 81 proposals submitted, tion VLT instruments, a major milestone. ogy and Training Centre at the Ondrˇejov both record numbers. The number of Astronomical Institute aimed at support- Large Programmes continues to increase The Laser Guide Star Facility (LGSF) ing Czech participation in both ESO and as well. A new category of short propos- achieved its First Light on Yepun (UT4) in ESA. als was introduced to reduce the load on 2006 and had its first year of science the Observing Programmes Committee operations in 2007, demonstrating its Negotiations with Austria progressed with (OPC). New panels were also added to great potential. The reliability of the sys- a meeting for Austrian research insti- cope with the increased number of pro- tem remains, however, a concern. tutes and industry to identify possible in- posals. kind contributions. This was followed by The fourth Auxiliary Telescope (AT) was formal meetings between the Council More than 700 refereed papers were pub- accepted at the beginning of the year, In-kind Negotiating Team and the Aus- lished in 2007 based on data obtained and provides additional flexibility for VLTI trian counterpart, which led to a set of with ESO facilities (including the science operations. AMBER was offered to agreed in-kind contributions. Completion archive). Amongst these was a string the community for the first time with the of the accession agreement could not of impressive first results with AMBER FINITO fringe tracker and the ATs. be achieved before the end of the year, published in a single issue of Astronomy but important progress was made at a & Astrophysics. In November, a major earthquake hit meeting with the Austrian Science Minis- the Tocopilla region of northern Chile. It ter Johannes Hahn in November. The third ESO Fellow Symposium took registered 5.7 on the Richter scale at place in Santiago in November. The re- Paranal, and shook the mountain for search carried out by our Fellows spans nearly two minutes in the early afternoon. Science all of astrophysics and often involves The Observatory survived this without collaboration with astronomers in the a scratch, and regular observations re- A team of Swiss, French and Portuguese community. sumed the same evening! astronomers discovered a five Earth- mass companion to the red dwarf star APEX received its eagerly awaited facility Gliese 581 with the HARPS instrument on bolometer array LABOCA, developed by the 3.6-m telescope on La Silla. This the Max-Planck-Institut für Radioastron- ‘super-Earth’ generated worldwide atten- omie in Bonn. The 11-arcmin field of view tion. Gliese 581 was already known to allowed very sensitive mapping of the be orbited by a Neptune-mass planet, Chandra Deep Field South, surpassing and there is evidence for a third planet of the largest submillimetre surveys previ- about eight Earth masses. This discovery ously achieved. APEX operations have continues the regular flow of new and ex- now reached a mature and stable state.

ESO Annual Report 2007 7 The new ESO User Portal was released In March, the Multi-Conjugate Adaptive The giant infrared camera for the 4.2-m at the end of 2007. The User Portal facil Optics Demonstrator (MAD) saw First Visible Infrared Survey Telescope (VISTA) itates access by astronomers to a broad Light at the Visitor Focus of Melipal (UT3). arrived on Paranal. The telescope en- variety of services provided by ESO MAD demonstrated for the very first time closure made good progress, and polish- (proposal preparation tools, observations that it is possible to perform multi-layer ing of the primary mirror continued at archive, reports on progress of observa- adaptive optics corrections in the K-band LZOS in Moscow. Six exciting Public Sur- tions, etc.) by means of a single user ac- (around 2.2 μm) over a field of view as veys were selected, which together will count. The number of registered users is large as 2 × 2 arcmin using multiple rela- fill most of the first five years of VISTA ob- close to 4000. tively bright natural guide stars. serving time. ESO actively interacted with the respective Principal Investigators The flexible scheduling offered by Service The second-generation VLT instruments to ensure an optimal definition of the Observing continues to be preferred by continue to make good progress. Testing observing strategy and of the derived sci- the users. Approximately 70 % of the ob- of X-Shooter started in Europe and the ence data products. serving time is requested in this mode, designs of KMOS, MUSE and SPHERE all and ESO supports over 1000 such ob- advanced well. Much work has also been serving runs per year. done on technology development for de- ALMA tectors, electronics and lasers. The ESO archive currently contains ESO represents Europe in the construc- 74 terabytes (TB) of data of which 15 TB The ESO workshop on “Science with the tion of the Atacama Large Millimeter/sub- were added during 2007, and its content VLT in the ELT era” – organised as a millimeter Array (ALMA) in Northern Chile, continues to be upgraded. Nearly 60 000 forum to discuss the long-term future of a global astronomy project carried out in pipeline-processed spectra obtained with VLT and VLTI instrumentation – was at- partnership with North America and East UVES since it started operations have tended by astronomers from all over the Asia. ESO is responsible for a number of been released, as well as all the pipeline- world. The Scientific Technical Commit- major deliverables, including front ends, processed spectra obtained with HARPS tee (STC) followed this up with recom- antennas, roads, power supply, and vari- until the end of 2006. The accessibility mendations to take the VLTI instrument ous buildings. of the archive has been improved by new concepts GRAVITY, and MATISSE, and interfaces such as VirGO, an archive vis- later on also VSI, beyond their Phase A Contracts for cryostats, water vapour ra- ual browser allowing data requests and studies. It also recommended launch- diometers, front-end cartridges (Bands 7 interaction with other virtual observatory ing studies of one or more third-genera- and 9) and low noise amplifiers were tools. tion VLT instruments. This includes an signed with institutes in the UK, Sweden, ultra-stable spectrograph at the incoher- France, the Netherlands, and Spain, The ESO Data Centre, a state-of-the-art ent combined focus, which will enable respectively. The first eight cryostats, and computer room designed for extremely the next step in exoplanet research. Band 7 and Band 9 receiver cartridges high safety and reliability, was completed were delivered. The large technical build- in 2007. In addition to most mission-criti- ing at the ALMA Operations Support cal operations computer systems, the Survey Telescopes Facility (OSF), south of San Pedro de Ata- ESO Data Centre hosts the ESO primary cama, progressed substantially, as did archive and a copy of the Hubble Space In mid-2007 the 2.6-m optical VLT Survey work on the road up to the Array Opera- Telescope Archive, and it will also host Telescope (VST) arrived at Paranal and tions Site on the Chajnantor plateau at the European copy of the ALMA archive. its integration was started. The remain- 5 000 m. ing components are now in the hands of industry in Italy, and are expected on The first of two custom-built antenna Visible-infrared projects Paranal in the course of 2008. transporters for ALMA had its ‘roll out’ at the factory in Germany in July and suc- While the complete suite of VLT first gen- cessfully passed a series of demanding eration instruments is now operational, tests. The transporter was presented HAWK-I (High Acuity, Wide field K-band to the press and members of the ESO Imaging) – occasionally described as a Council in October before being readied ‘generation 1.5’ instrument – had its First for shipment to Chile. Light on Yepun on 31 July, followed by commissioning and science verification ALMA operations will be supported by which confirmed the anticipated signifi- the European ALMA Regional Centre, a cant gains in field, depth and image qual- network of nodes coordinated by ESO. ity now achievable at the VLT in the near The main activity in 2007 was to set up infrared. the structure with the ARC nodes, testing software, and participating in the organisation of community events.

8 ESO Annual Report 2007 Other highlights in the ALMA project in- Headquarters building extension Visiting Committee cluded the arrival at the OSF of the first 12-m antennas (from the Japanese and Significant progress was made towards Every three years an external Visiting North American vendors), and obtaining the construction of an extension of the Committee consisting of senior scientists First Fringes with two prototype 12-m ESO Headquarters building. A contract with broad expertise reports to Council antennas at the ALMA Test Facility near was signed in July for the acquisition of about the state of the ESO programme Socorro, New Mexico. additional land to the south of the current and organisation. The 2007 Visiting Com- premises. An international architectural mittee was chaired by Prof. Günther competition took place for the develop- Hasinger. The resulting report has as its Extremely Large Telescope ment of a conceptual design for the ex- main conclusion that: “ESO has be- tension. There were 20 entries from archi- come the premier observatory for optical- The design study for the Extremely Large tectural offices in the member states, infrared astronomy on a world-wide Telescope (E-ELT) is in full swing. The which were ranked by a jury. Council ap- basis”, and contains valuable advice re- baseline design consists of an innovative proved going ahead with a further refine- garding the further evolution of ESO’s five-mirror telescope, with a 42-m segment of the top three prize-winning con- internal structure and expansion of its mented primary mirror. Many industrial cepts. programme into the era of ALMA and the contracts were placed for design of the E-ELT. There is much to look forward to! telescope structure and enclosure, and for prototypes of key optical and mechan ical components. Instrument studies with consortia of research institutes in the member states are also advancing well.

The European Commission awarded an EC FP7 contract to ESO for support of Prof. Tim de Zeeuw the so-called Preparatory Phase of the ESO Director General E-ELT. ESO is the ‘mono-partner’ and represents 25 institutions in the member states. The E-ELT features prominently on the European Strategy Forum on Re- search Infrastructures (ESFRI) list, and also in the ASTRONET Science Vision for European astronomy.

VLT image of supernova SN 2006dr (centre left) in the spiral galaxy NGC 1288.

ESO Annual Report 2007 9 Research Highlights

The ESO facilities are true science ma- lyse the observations, is quite often of the As in previous years, the topics covered chines. The telescopes and the archive order of a year or more. Some survey- range from Solar System objects to were the source of data that resulted in type projects take even longer until com- the edge of the Universe. The ESO tele- 729 refereed publications in 2007, an in- pletion, especially when they span more scopes produce observations for many crease of 10 % over the publication rate than one observing period. Typical exam- different projects and the usage of the in 2006. This increase is due to many fac- ples are surveys or the ESO Large Pro- data is also very varied. In many cases, tors. Several instruments have become grammes, which can be approved for up ESO data are combined with observa- available over the past few years, ex- to two years. The coming years will see tions from other observatories, in particu- panding the capabilities and opening new the start of large public surveys on dedi- lar space telescopes. The combination parameter space. The delay of publica- cated telescopes, but the effect of the of the different strengths of these observ- tions, the time it takes to reduce and ana- Large Programmes can already be seen atories has transformed many fields in as- in the literature. trophysics.

Planetary weather

Saturn’s major moon, Titan, is larger than 120 the planet Mercury. It is the only plane- 2005 Feb VLT 2005 Apr Keck Lower stratospheric haze Xanadu tary satellite in the Solar System with a thick atmosphere, which is comprised 10 0 mostly of nitrogen and resembles Earth’s Nominal haze profile early atmosphere. Because of its ex- (13S, 43W) tremely cold surface temperature – minus 80 Surface 183 degrees Celsius – trace chemicals such as methane and ethane, which are South polar haze (60S, 43W) explosive gases on Earth, exist as liquids 60 or solids on Titan. Some level features on the surface near the poles are thought Altitude (km) to be lakes of liquid hydrocarbon analo- 40 Tropospheric haze gous to Earth’s watery oceans, and pre- Lower troposphere Global solid methane cloud sumably these lakes are filled by methane precipitation. ESA’s Huygens probe 20 observed features that appear to be Liquid methane cloud

controlled by flows down slopes, whether Drizzle caused by precipitation or springs. 0 0.001 0.010 –1 Lower troposphere Actual clouds on Titan were first imaged Aerosol haze extension (km ) with surface removed in 2001 by Imke de Pater’s group and colleagues at Caltech using the Keck II telescope with adaptive optics. The ob- VLT and Keck near-infrared images of Titan’s surface morning drizzle above the huge continent of Xanadu servations confirmed what had been and lower troposphere can be subtracted to reveal (outlined in yellow). At left is a chart of Titan’s aero- widespread cirrus-like clouds of frozen methane sol haze versus altitude, indicating higher density inferred from spectra of Titan’s atmos- (lower images) and a large patch of liquid methane haze over portions of the south pole and the heights phere. These frozen methane clouds hov- (dark area within box) interpreted as clouds and of frozen and liquid methane clouds. ered at an elevation of about 30 kilo metres around Titan’s south pole. Since then, isolated ethane clouds have been methane relative humidity. These data tion like Huygens cannot characterise the observed at the north pole by NASA’s provided evidence for frozen methane meteorology on a planet-wide scale. Cassini spacecraft, while both Cassini clouds between 25 and 30 kilometres in and Keck photographed methane clouds elevation and liquid methane clouds – Spatially resolved spectra from a new scattered at mid-southern latitudes. Also with possible drizzle – between 15 and 25 class of instruments, such as the OH- in 2005, the ESA Huygens probe, re- kilometres high. The extent of the clouds Suppressing InfraRed Imaging Spec- leased by Cassini, plummeted through detected in the descent area was unclear, trograph (OSIRIS) at the W. M. Keck Ob- Titan’s atmosphere, collecting data on however, because a single weather sta- servatory or the Spectrograph for INtegral

10 ESO Annual Report 2007 Field Observations in the Near Infrared ane at a height of 25 to 35 kilometres density in the atmosphere, which makes (SINFONI) at the Very Large Telescope that is consistent with Huygens’ meas- the clouds hard to detect. (VLT) can be used to create a global urements, plus liquid methane clouds picture of Titan’s lower atmosphere and in the tropopause below 20 kilometres The drizzle or mist seems to dissipate surface. Both instruments measure spec- with rain at lower elevations. after local mid-morning, which, because tra at many points in an image rather Titan takes 16 Earth days to rotate once, than averaging over a small aperture or The clouds which are seen are like cirrus is about three Earth days after sunrise slit. By subtracting light reflected from clouds on Earth. One difference is that on Titan. If widespread, such a persistent the surface from the light reflected by the the methane droplets are predicted to be drizzle may be the dominant mechanism clouds, it is possible to obtain images at least millimetre-sized on Titan, that is, for returning methane to the surface from of the clouds covering the entire moon. a thousand times larger than in terrestrial the atmosphere and closing the methane clouds. Since the clouds have about the cycle, analogous to Earth’s water cycle. Observations obtained with these instru- same moisture content as Earth’s clouds, ments at two different epochs reveal this means the droplets on Titan are (Based on M. Ádámkovics et al., 2007, Science, 318, a widespread cloud cover of frozen meth- much more spread out and have a lower 962)

Exoplanets

Finding planets which can harbour life stronger. Thus, Earth-mass planets orbit- Neptune-mass planet is extremely hot. is one of the ‘holy grails’ of modern as- ing low mass M dwarfs are within the By analogy to the Jupiter-mass objects tronomy. While finding planets with reach of HARPS and have been the sub- that are now routinely detected around masses similar to the Earth’s, and orbit- ject of intensive searches by the HARPS solar-type stars – the hot-Jupiters – this ing stars similar to our Sun at a distance consortium (for M dwarfs the habitable- object is called a ‘hot-Neptune’. of a few astronomical units (AU), is be- zone is within 0.1 AU of the star). In the yond the reach of current instruments, course of that search, which included the High Accuracy Radial-velocity Planet about 100 stars, the consortium detected Searcher (HARPS) on the 3.6-m tele- the first Neptune-like planet on a 5.4-day scope at La Silla, with its long-term radial orbit around the star Gliese 581 (the Artist’s impression of the planetary system around velocity precision of better than 1 m/s, 581st entry in the catalogue of nearby the red dwarf Gliese 581, showing the five Earth- mass planet (seen in foreground: Gliese 581c) and its comes as close as we can get today to stars published by W. Gliese in 1969). Be- two sisters, the bluish Neptunian-like planet Gliese that goal. cause of its close distance to the star, this 581b, and the most remote one, Gliese 581d.

The habitable zone of a star is defined as the range of orbital distances for which the surface temperature of a planet would be such that water can exist in a liquid state. If the planet were much closer to the star it would be too hot and water would evaporate, whereas if the planet were too far away, water would be permanently frozen. Implicit in this definition is the assumption that liquid water is essential for the development of life, which is a fair assumption given that we only know life on Earth. The mean distance of the habitable zone from the star depends on the intrinsic brightness of the star, and hence on its mass: for stars with masses lower than the Sun (assuming that they are still on the main sequence), the habitable zone will be closer in, and the radial velocity signal of an orbiting planet will be

ESO Annual Report 2007 11 The hot-Neptune of Gl581 (named The panels display the phase-folded radial-velocity variations for the three planets (Gliese 581b, c, Gl581b) imprints a radial velocity (RV) sig- 10 and d, respectively) discovered around Gliese 581. nature of ± 10m/s on its parent star, Each point represents the observed radial velocities, which is much larger than the accuracy of after removing the effect of the other planets. The HARPS. Thus, further monitoring of the 0 error on one measurement is of the order of 1 m/s. star by the HARPS team led them to detect two additional planets, both induc- ing RV signatures of order ± 3m/s on the –10 parent star. While these values are still well above the accuracy of HARPS, the 5 unique stability of the instrument was required to disentangle the combined sig- 2.5 natures of the three planets. Very careful modelling of the observations allowed 0 lies close to the inner (warm) edge of the the team to fit a three-planet solution to habitable zone of the M3 dwarf, while the observed orbital periods. The first –2.5 Gl581d lies close to the outer (cold) edge. planet corresponds to the already known Radial Velocity (m/s) However, in all other respects these hot-Neptune with a period of P = 5.37 two planets are sufficiently different from –5 days, while the other two have periods the Earth that it is highly unlikely that they of 12.9 days (Gl581c) and 83.4 days 5 may harbour life. (Gl581d), respectively. For the M3V star Gl581 these values correspond to mini- 2.5 A very interesting conclusion of the study mum masses of 5.0 MEarth and 7.7 MEarth, is that small planets (Neptune mass and and orbital distances of 0.07 AU and 0 below) are more frequent than giant plan- 0.25 AU, respectively. With only five times ets (hot-Jupiters) around M dwarfs, and the mass of the Earth, Gl581c is the –2.5 that the Neptune-size planets are much closest ‘Earth-twin’ yet found. If its com- easier to find around M dwarfs than position were similar to the Earth, then –5 around solar-type stars. 0 0.25 0.5 0.75 1 its radius would be only 1.5 times the ra- Orbital Phase dius of our Earth. As it turns out, Gl581c (Based on Udry et al., 2007, A&A, 469, L43)

Low-mass objects

The nature of planets around other stars shown that there might be a circumstellar esses, and as the planets are so cool is of high general interest. The few cases disc around the young planet. that they exhibit real weather patterns, where the planet can be directly inves one can imagine that there is still quite a tigated and not solely inferred from its ef- The observations were obtained in a fol- degree of uncertainty in the models. fect on the parent star (as above) are of low-up programme by an independent Nevertheless, the planet probably has a particular importance. The image of the team to check the masses and the tem- mass eight times that of Jupiter (with an planet around the brown dwarf 2MASS peratures of the objects within the sys- uncertainty of about 25%). This mass J1207334–393254, discovered a few tem. The trick is the separation of the light estimate is about twice as much as ear- years ago with the adaptive optics cam- from the primary and the secondary lier ones. The reason for this lies in the era NAOS-CONICA on the VLT, has objects. From spectroscopy, the authors assumption that the observed brightness started the process of further characteri- infer a low gravity, i.e. small mass, and a is affected by grey dust, i.e. light is ab- sation. Further observations with NAOS- dusty atmosphere for the planet. The sorbed by a disc, which obscures part of CONICA have now shown that the situa- temperature of the planetary surface is the emission from the planet. tion might be complicated by additional about 1600 Kelvin. To derive the mass material in the system. While the colours of the object, its age and a model of the The reason for this new interpretation is a and temperatures derived for the primary evolution of young planets are required. discrepancy of the model luminosities, brown dwarf are consistent with previ- Since there is very little observational colours and ages with the observed lumi- ous measurements, the detailed analysis data, the models have to rely on an accu- nosities. The planet simply appears too of the planetary-mass companion has rate interpretation of the physical proc- faint and too blue to assume that it has

12 ESO Annual Report 2007 the same age as the host star. Since the NAOS-CONICA image in the J-band models work very well in all aspects, of the brown dwarf and its planetary companion 2MASS J1207334- the authors conclude that there must be 393254b. an extra source of extinction, a disc seen edge-on, which obscures part of the light and hence explains the apparent faintness of the planet. This is a rather surprising result.

Observing other planetary systems will have further surprises in store. A fundamental requirement for such observations is the ability to observe objects with a large contrast and with a high angular resolution. Adaptive optics observations with large telescopes are a fundamental requirement for such observations.

(Based on Mohanty et al., 2007, ApJ, 657, 1064)

The case of Eta Carinae

In the course of their rapid evolution, very in the Galaxy. In 1677, Halley observed Spectroscopic monitoring of Eta Carinae massive stars – those with a mass larger Eta Carinae as having magnitude four, showed that some emission lines fade than about 100 solar masses – go through but by 1730 it had brightened considera- every 5.5 years, and that this period has a very short phase (perhaps even as bly and was one of the brightest stars been stable for decades. The radio emis- short as a few tens of thousands of years) towards the Carina constellation. Later it sion and its X-ray brightness also drops where, due to extremely high mass-loss dimmed again, and by 1782 was back to significantly during these ‘events’. These or other mechanisms, they become varia- being about fourth magnitude. It started variations provide strong indications that ble on several different time scales. These brightening again in 1820, so that by 1827 Eta Carinae is indeed a binary star with changes can range from micro-varia- it was more than ten times brighter than a massive hot primary and a lower mass tions of 0.1–0.2 magnitude on scales of before, reaching its highest peak in April secondary on a highly eccentric orbit with days, to variations of 1–2 magnitudes 1843 when it was the second brightest a period of 5.52 years. on time scales of years to decades, or to star in the night sky (after Sirius) with a huge outbursts of 3 magnitudes or more magnitude of −0.8! Eta Carinae is surrounded by an expand- every few centuries. These luminous blue ing bipolar cloud of dust and gas known variables, or LBVs, are a million times After 1843, Eta Carinae faded away, and as the Homunculus (‘little man’ in Latin), more luminous than the Sun, and close to between about 1900 and 1940 it was only believed to have been expelled from the the observed maximum luminosity for of eighth magnitude. A ‘spectroscopic star during the great outburst of 1843 any type of stars. LBVs are extremely rare minimum’ or ‘X-ray eclipse’ occurred in (in fact, since the distance to Eta Carinae (only about a dozen are known in the June 2003, which was intensely observed is about 2 300 parsecs, the eruption must Galaxy and the Magellanic Clouds), and with every available ground-based and have taken place more than 7000 years are thought to be on their way to becom- space observatory, including the VLT, before). Spectroscopic observations of ing Wolf-Rayet stars which will eventually HST, Chandra and Integral. The primary the Homunculus showed that the wind of explode as pair-instability supernovae. goals of these observations were to de- Eta Carinae is aspherical and latitude- The masses of LBVs are close to the the- termine if Eta Carinae is a binary star dependent such that the polar axes of oretical upper mass-limit for stars, which and to identify its companion, as well as the wind and the Homunculus are aligned, is around 120 MA. The most luminous to determine the physical mechanism and the wind speed increases from the LBV known is Eta Carinae, which is also behind the ‘spectroscopic minima’ and to equator (the arms of the little man) to the the closest and the best-studied example understand their relation (if any) to the pole. The central optically thick part of the – in fact, Eta Carinae is currently consid- large-scale eruptions of the 19th century. wind was resolved by VINCI, the precur- ered to be the most luminous star known sor instrument on the VLTI, which meas-

ESO Annual Report 2007 13 ured a size of 0.005 arcseconds (5 mas) P1 P2 IF P3 MR 2004-12-26 Velocity (km/s) and a very large mass-loss rate of over 2.175 µm –100010 000 2 0.001 solar masses per year. 1.5 One of the guaranteed time observing (GTO) programmes with AMBER on the 1 Spectrum VLTI is to obtain the first spectro-inter 0.5 ferometric observations of Eta Carinae. 0 AMBER can combine the light of three 0.9 VLT Unit Telescopes (UTs), thus yielding 0.8 0.7 spectral information with an unprece- 0.6 dented spatial resolution (up to 1 mas), 0.5

Visibility 0.4 and with spectral resolutions of up to 0.3 0.2 R = 12 000. 0.1 0 1.8 On the basis of the wealth of information 1.6 1.4 provided by AMBER at different spectral 1.2 resolutions and different baselines (which 1.0 0.8 give different spatial resolutions), the Diff. Visibility 0.6 0.4 AMBER team was able to construct a de- 0.2 80 tailed model for the wind of Eta Carinae. 2.156 µm The (geometrical) model consists of three 60 HR 2005-02-26 40 components: a dense latitude-depend- 20 ent aspherical stellar wind region of 2.183 µm 0 about 6.5 mas embedded in a spherical –20 –40 Diff. Phase (Degree) wind about 10 mas in size, and a com- –60 pact spherical continuum-emitting region –80 (4 mas), which is indicated by the high- 60 visibilities and low closure phases in the 40 20 continuum region of the spectra. 0 2.135 µm –20 MR 2004-12-26 The AMBER observations provide invalu- –40

Closure Phase (Degree) –60 able information about the stellar wind –80 2.04 2.05 2.06 2.07 of Eta Carinae that can be compared with Wavelength (µm) theoretical models to significantly improve our understanding of the evolution and Raw AMBER interferograms of Eta Carinae with me- The AMBER He i observations of Eta Carinae (top eventual death of massive stars. The ob- dium resolution (MR; R = 1500 – lower panel) and panel) reveal the well-known P-Cygni profile of the high resolution (HR; R = 12 000). The panels show nebular He i lines, but now observed with milliarcsec- servations are also extremely important the spectrally dispersed fringe signals and the pho- ond resolution. The second panel shows the fringe to refine models of supernova explosions tometric calibration signals from the three telescopes contrast or ‘visibility’ as a function of wavelength. because, for these massive stars, the ex- in the near-IR K-band. The wavelength range is in The visibility gives a direct estimate of the size of the plosions take place inside the winds and dicated in the left of the images. The strong feature source – the lower the visibility, the larger the object roughly at the centre of these figures is the Brg line of – so the observations show that the line-emitting the subsequent evolution of the remnants ionised hydrogen. It is broadened to about 50 spec- region is significantly larger than the source of the depends on the properties of these tral channels in the HR spectrum, which allows a continuum, and that the blue (absorption) wing of the wind regions. Whilst the observations are very detailed study of the kinematics of the nebula. line is larger than the emission side. The differential consistent with the presence of a binary, phases and closure phases measure the asymmetry of the source and again, only the absorption compo- as revealed by the asymmetry in the nent shows significant asymmetry. wind-wind collision region, the results are not conclusive. Indeed, if most of the He i emission is generated in the wind-wind collision zone, the asymmetry indicated next spectroscopic eclipse (expected by the closure phases (about –30˚) is too in January 2009) to gain more insight into low compared with what one would pre- this fascinating object, which, however, dict for a binary. Further observations could explode at any time between now with AMBER at different orbital phases and the next hundred thousand years! and better resolution are underway, and astronomers are looking forward to the (Based on Weigelt et al., 2007, A&A, 464, 87)

14 ESO Annual Report 2007 10 10 1.00

Brγ spherical wind 0.804 5 5 Brγ latitude-dependent aspherical stellar wind 0.608 0 0

0.412 Intensity dDEC (mas)

–5 –5 Line-of-sight Continuum 0.216 emitting region

–10 –10 0.020 41˚ 10 50–5 –10 10 50–5 –10 s ma 8 10 10 1.00 s ulu

munc xis N 0.804 Ho r a la 5 5 Po Pole E 0.608 0 0

0.412 Intensity

Illustration of the components of the geometric dDEC (mas) model for an optically thick, latitude-dependent wind –5 –5 0.216 of Eta Carinae (for the weak aspherical wind com ponent, we draw the lines of latitudes to illustrate the 3D-orientation of the ellipsoid). Right panels: for –10 –10 0.020 10 50–5 –10 10 50–5 –10 two representative wavelengths, the total brightness dRA (mas) dRA (mas) distribution of the model including the aspherical wind component (upper rows) and the contributions from the two spherical constituents (lower rows).

Gamma-ray bursts

Observations with ESO telescopes – from bly with the discovery in 2006 of a long the first identification of an optical coun- GRB, with no detected associated super- terpart, to the systematic measurement nova, by Fynbo and his colleagues. of the redshifts of the progenitors – have been instrumental in increasing the ex- Gamma-rays are scattered by particles perimental understanding of the physics in the atmosphere of the Earth, so they of Gamma-Ray Bursts (GRBs). GRBs are must be observed by satellites. The short duration bursts of gamma-ray NASA/STFC/ASI Swift satellite detects photons lasting anything from a few milli- roughly one GRB per day, and X-ray seconds to several minutes. During these and optical instruments on board enables short periods of time, GRBs become the positions to be pinpointed with suffi- the most luminous objects in the Universe cient accuracy to allow the rapid pointing and, despite being at cosmological dis- of giant telescopes on the ground. At the tances, some can even be seen with the VLT, the rapid-response mode (RRM) can unaided eye! GRBs appear to come in slew the UTs to a GRB position within two flavours: the long duration events, minutes of receiving a satellite alert. An lasting between two seconds and several RRM observation is automatically acti- with UVES to study the interstellar mate- minutes, and the short duration bursts vated when an alert is received, thus rial in the parent galaxies of the GRBs are that last less than two seconds. The minimising the time required by observers made possible by the RRM. progenitors of long bursts are widely and operators to make decisions. Be- thought to be very massive stars (such as cause GRB afterglows fade very rapidly, A team led by Paul Vreeswijk (now at the Eta Carinae) exploding as supernovae, the RRM enables astronomers to un Dark Cosmology Centre in Copenhagen, but there is a very rich debate concerning dertake observations which would not be Denmark) triggered RRM observations of the physics of short bursts. The VLT is possible even one hour after the explo- the bright burst GRB060218 with UVES actively contributing to this debate, nota- sion. In particular, high dispersion spectra at the VLT. The first exposure started only

ESO Annual Report 2007 15 10 minutes after Swift detected the burst, –500 50 –500 50 –500 50 ∆T = 11 min 1 10 FeII 6D ∆T = 16 min followed by a sequence of spectra taken 7/2 ∆T = 25 min 5 11, 16, 25, 41, and 71 minutes after the 0.5 ∆T = 41 min CrII λ2056 FeII 6D λ2333 trigger. This made it possible to detect 7/2 0 ∆T = 71 min 0 1 6 and follow for the first time the evolution 6 II Fe D5/2 of metastable interstellar absorption lines 4 0.5 2 II II 6 of Feii and Ni ii in the host galaxy at a red- Zn λ2062 Fe D5/2 λ2607

) 0 shift z = 1.490. 0 –1 1 3 II 6 Fe D3/2

pixel 2 0.5 –2 The UVES observations show how the 1 MgI λ2026 FeII 6D λ2407 cm 3/2 11 0 excitation of the interstellar medium sur- 0 1 6 1.5 FeII D rounding the GRB progenitor responds 1/2 1 0.5 to the intense flash of radiation produced 0.5 MnII λ2576 FeII 6D λ2629 by the explosion. The high quality of the 1/2 0 Normalised Flux 0

1 8 II 4 observations coupled with the unprece- Fe F9/2 6 dented time resolution allowed the team 0.5 4 2 II II 4 to perform detailed modelling with three Si λ1808 Fe F9/2 λ1702

Apparent Column Density10 (× 0 0 different excitation mechanisms: colli- 1 4 FeII D sions, excitation by infrared-photons, and 2 7/2 fluorescence following excitation by ultra- 0.5 1 Al II λ1862 FeII 4D λ2563 7/2 0 violet photons. Indeed, the time resolu- 0 1 2 II 4 Ni F9/2 tion of the observations proved critical in 1.5 distinguishing between the three models 0.5 1 0.5 NiII λ1709 NiII 4F λ2217 9/2 0 and allowed the team to reject the first 0 –500 50 –500 50 –500 50 two mechanisms (collisional and IR exci- Relative Velocity (km/s) Relative Velocity (km/s) tation) with high confidence. On the other hand, UV pumping followed by fluo- of parsecs away. So they could either be Time evolution of the most important lines observed rescence provided a very good fit to the part of a very large star-forming region by UVES in the host galaxy of the gamma-ray burst GRB060218. In order to make the variations more data. The main consequence of the UVES (so-called ‘super-associations’), or fore- apparent, the right-hand side of the figure shows the observations is that they showed that the ground material in the GRB host galaxy. evolution of the column density computed by aver- GRB completely ionised the gas within This means that parameters derived from aging together several lines from the same atomic 1.7 kpc of the progenitor. This implies that absorption line observations on GRB levels. The significant decrease in the (column) density of neutral gas with time can be clearly seen in the very large H i column densities typi- sightlines (such as metallicity for example) the figure. cally observed on GRB sightlines cannot may not be representative of the region be in the immediate vicinity of the GRB where the GRB progenitor was born. itself, but must correspond to neutral gas clouds located up to several thousands (Based on Vreeswijk et al., 2007, A&A, 468, 83)

Massive stars as chemical tracers of gas

Only about one star in a thousand is as to the Milky Way have significantly lower the number of observable objects, pro- massive as 18 times the Sun or more. metallicity, the study of a large sample of vided there are many which can be These stars are extremely luminous and stars provides a way to investigate how observed simultaneously in a given field. can be observed to great distances. stars evolve in different environments. They are also rather young, as massive A FLAMES Large Programme, supple- stars evolve much faster than low-mass Of course, massive stars have been the mented by observations with UVES at the stars such as the Sun. The combination objects of many studies in the past, VLT and FEROS at La Silla, observed of these facts opens the opportunity to but only with large-aperture telescopes over 800 O and B stars in different galax- study massive stars not only nearby, but such as the VLT has it become possible ies to explore the influence of environ- throughout the Milky Way and also in its to observe large numbers of these ob- ment, rotation, and metallicity. The wind companion galaxies, the Magellanic jects fairly quickly. A fibre-optics instru- properties, the surface chemical com Clouds. Since these companion galaxies ment such as FLAMES further increases position and the rotation velocities were

16 ESO Annual Report 2007 measured. For all stars, it was possible nantly observed in low-metallicity galax- and more rapidly rotating stars should to determine the surface abundances of ies. show an enhancement of this element in carbon, nitrogen, oxygen, magnesium their spectra. Although some of this ef- and silicon. The stars studied belong to Slowly rotating stars should maintain the fect has been observed it appears to be a cluster in the Milky Way, one in the chemical composition of their formation not as strong as was expected from the Small Magellanic Cloud and one in the cloud on the surface. This means that models. This is a puzzle, which will need Large Magellanic Cloud. they can be used to measure the abun- to be resolved with the help of future ob- dance of the interstellar gas in the galaxy. servations. Low-metallicity stars are more compact, This allowed the astronomers in the have a lower mass loss and possibly ro- project to determine the abundances of Finally, since the stars had to be ob- tate faster, as less angular momentum various elements in the two Magellanic served several times to cover a large is lost in the wind. Hence, studying mas- Clouds. It emerged that there are differ- spectral range, a velocity offset between sive stars in galaxies with different metal- ences for the individual elements and different epochs was noticed for several licities should reveal significant differ- a simple scaling from the solar composi- of them. The most straightforward ex ences. This is exactly the effect observed tion will not reproduce what has been planation is that these stars are actually in this survey. Stars in the Small Magel- observed in the Magellanic Clouds. This not isolated, but are members of binary lanic Cloud – the galaxy with the low- is an important piece of information, systems. est amount of metals – indeed rotate on as it means that we cannot simply scale average faster than those in the Large what we know from the Sun to the abun- This Large Programme has produced Magellanic Cloud and the Milky Way. This dances of distant galaxies. several publications over the past two means that massive stars in a low metal- years and represents major progress in licity environment will not lose as much Another important measurement is the our understanding of massive stars and matter and possibly explode differently amount of nitrogen at the surface. For how they evolve. than their counterparts in more metal-rich rapidly rotating stars one expects that the environments. This could have important ashes from the nuclear fusion reactor (Based on Mokiem et al., 2006, A&A, 456, 1131; implications for the explosions of gamma- in the centre of the star are mixed to the Mokiem et al., 2007, A&A, 465, 1003, Hunter et al., 2007, A&A, 466, 277; Hunter et al., 2008,A&A, 479, ray bursts, which have been predomi- surface. One ash material is nitrogen, 541; Hunter et al., 2008, ApJ, 676, L29)

Galaxies in the early Universe

It is only a little more than a decade ago the same light with which we observe the ested users, and they have now been that the study of galaxies at large red- nearby objects. used in many publications by independ- shifts started in earnest. And it is even ent teams. The large area (125 square more recently that we have been able All this has led to the creation of deep arcmin) of the survey and its faint limiting to start investigating the objects that surveys of selected fields. Large teams magnitude have been ideal to investigate might have evolved into the Milky Way we have been set up to combine the differ- the Universe from redshifts of about 1 to live in today. A large sample of distant ent ground- and space-based observato- beyond 5. The data were used in different galaxies is required to infer the way gal- ries. The resulting public data sets have ways to explore our distant past. axies evolve from the early Universe to multiple applications and have been used the present. Since these objects are very for several independent studies. A different approach was followed by the faint and distributed fairly sparsely, large VIMOS VLT Deep Survey (VVDS), which area surveys to faint magnitudes are re- One such collaboration is the Great Ob- collected redshifts of a complete sample quired. Spectroscopy for the determina- servatories Optical Deep Survey (GOODS) of galaxies to a limiting magnitude of tion of the redshifts, i.e. look-back time that combines data from several space I < 24 over a large area on the sky. With towards the objects, is essential. In addi- telescopes and many major ground- such a complete sample, slices through tion, the complete accessible wavelength based observatories. ESO contributed the Universe can be assembled which range has to be explored to investigate the deep near-infrared imaging with give snapshots of the galaxies at different the spectral energy distribution as much ISAAC and FORS spectroscopy of the look-back times. as possible. Due to the redshifting faint galaxies in the southern GOODS caused by the expansion of the universe, field through several Large Programmes. To observe the distant galaxies in the the distant galaxies need to be observed The data were processed by an ESO optical rest frame, guaranteed time with at longer wavelengths to sample them in team and provided publicly to all inter- SINFONI was used. The structure and

ESO Annual Report 2007 17 morphology, together with the emission luminous galaxies show excess emis- stellar mass density at these redshifts is line characteristics of the galaxies, tells sion, which most likely comes from addi- considerable. us about their evolutionary state and can tional energy input by an active galactic give indications on how they may trans- nucleus. The star formation rate of these The question of the most massive galax- form into the galaxies we observe today. galaxies at redshift 2 is about 30 times ies at these farthest distances has be- The results very much depend on which higher than in the local Universe. come rather pressing with the putative way the galaxies are selected, i.e. at discovery of a very massive galaxy at a what rest-frame wavelength the selection The deep samples can also be used to redshift of 6.5. A detailed investigation of is done. A sample of about three-dozen explore the very high-redshift Universe. the GOODS-South field checked whether galaxies at a redshift of two shows that Several studies have tried to measure the such massive galaxies are present and galaxies selected in the wavelengths in masses of these most distant observed came to the conclusion that all objects which we observe the local Universe ap- galaxies at redshifts of 5 and higher. Only could be explained with highly obscured pear very much the same as the local the rest-frame UV part of the spectrum galaxies at lower redshifts. This is an ones. However, galaxies selected for their can be observed. Objects are selected in important result as it indicates that the strong submillimetre emission appear to a way that they are unobservable below build-up of mass of the galaxies is more have higher internal velocities and at the the Lyman-a line, as the hydrogen be- gradual. same time seem to be more compact. tween the object and us blocks most of This also means that these latter galaxies the light. This ‘drop-out’ technique (the All these projects are based on massive have a much higher stellar density. While objects are unobservable at certain data sets from many observing nights the UV- and optically-selected galaxies filters, but show up fairly bright at larger (or long integrations with satellites). The probably evolve into the spiral galaxies of wavelengths) has been used very suc- distant Universe is just barely accessible today, the submillimetre galaxies certainly cessfully for the past decade. It is now with the most advanced facilities and have a more complicated history and may applied to collect fairly large samples of instruments. However, it also shows that be the results of recent merging events. these distant galaxies. Using space infra- the same data sets can be applied for red data, astronomers have found that a many different studies and can contribute The GOODS data sets enable the com fairly large fraction of these objects have very significantly to our view of the evo bination of data over a very wide range of indications of an old stellar population, lution of galaxies and the Universe as a wavelengths to very faint flux levels. despite the fact that the age of the Uni- whole. This information was used to test various verse at these redshifts corresponds to models of the star formation rate and in only about 1 billion years. The implica- (Based on Daddi et al., 2007, ApJ, 670, 156; Stark et particular to explore the evolution of mas- tion is that a large fraction of the galaxy al., 2007, ApJ, 659, 84; Verma et al., 2007, MNRAS, 377, 1024; Eyles et al., 2007, MNRAS, 374, 910; sive galaxies at a redshift of 2. As a sur- mass is already in old stars. Also, the Dunlop et al., 2007, 376, 1054; Bouché et al., 2007, prise, it was found that the most infrared ApJ, 671, 303)

Lensed galaxies

The huge mass concentration of clusters servations at the ESO 3.6-m telescope the very same cluster which allowed the of galaxies can act as a magnifying glass by a team led by Geneviève Soucail in 3.6-m telescope to confirm the lensed to aid the detection of faint background 1988, astronomers have dreamed of nature of giant gravitational arcs 20 years sources. Galaxies located behind mas- using large clusters of galaxies as gravi- ago! sive clusters can be amplified and dis- tational telescopes to explore the high- torted by the gravitational lensing effect redshift universe. The advent of powerful The large magnification of lensed galaxies of the cluster, producing luminous giant telescopes on the ground and in space near critical curves makes it possible arcs that are seen in the central regions has finally fulfilled this dream. Systematic not only to find high redshift galaxies and of many clusters. Depending on the lo searches for high-z galaxies along the to study their stellar populations spec cation of the source relative to the cluster critical curves (curves of infinite magnifi- troscopically, but also to perform detailed mass distribution, and its redshift, mag cation) of massive clusters at intermediate studies of their structure and chemical nifications of several magnitudes can be redshifts (z ~ 0.3 to 0.8) have been ex- composition that a few years ago were obtained. tremely successful. In fact, the most dis- only possible for galaxies in the local Uni- tant galaxies known to date have been verse. This breakthrough has been pos Ever since the lensed nature of these found through this technique, including a sible due to the advent of powerful inte giant arcs was demonstrated through ob- galaxy at z = 6.6 magnified by Abell 370, gral-field (3D) spectrometers on 8-m

18 ESO Annual Report 2007 20 class telescopes. A team of astronomers N 20 led by A. Swinbank used VIMOS in the

E A1 optical and SINFONI in the near-infrared 15 15 to perform a detailed study of a galaxy at redshift z = 4.88 lensed by a rich clus- 1 10 R2 10 ter at z = 0.77. 4 2 3 CG6 From the luminosity of the source, the 5 5

observations indicate that this galaxy is Arcseconds CG5 CG3 typical of galaxies at this earlier time. CG1 05 0 0 1. Thus, gravitational lensing makes it pos- A2 R1 CG2 sible to study a typical z ~ 5 galaxy at CG4 1 –5 –5 2. high signal-to-noise ratio and at spatial 89 4. 3.66 scales of 200 pc, which is indeed a re- 4.89 markable achievement. The radial velocity –5 0510 15 20 –10 –5 0510 15 20 gradient across the galaxy implies a to- Arcseconds Arcseconds 10 tal mass of about 10 MA within a radius of 2 kpc. The total [O ii] luminosity in- (Left) HST image of the cluster Abell 370 with the led them to identify at least another 6 high-redshift dicates a fairly hefty star formation rate critical curves indicated, and (right) the integrated candidates (labelled A1–A2 and 1–4 in the figure) VIMOS datacube with the central caustic and the with redshifts between 1.5 and 5.5. The z = 4.88 of more than 10 MA/year, and since the z = 4.89 critical curve superimposed. The left panel galaxy is the large arc inside the white square which [O ii] emission extends over most of the illustrates the power of clusters as gravitational depicts the SINFONI field. Object R1 is the radial observed area, the galaxy is undergoing telescopes and integral field spectroscopy: the com- counter-image of the z = 4.88 arc, which makes it an extended burst of star formation. The bined VIMOS and SINFONI data allowed the team possible to constrain the gravitational lens model to survey all the critical curves from z = 0 to 14. This required to interpret the observations. Lya emission is much more extended than either [O ii] or UV-continuum, and the Lya profiles are asymmetric, indicating the presence of a broad component red- shifted by about +400 km/s. Moreover, the weak Si iv absorption features seen in the VIMOS data are blueshifted from 8 the same systemic velocity by about –400 km/s. The observations therefore 2 suggest that the galaxy is surrounded 6 by a galactic-scale bipolar outflow that 0 has recently burst out of the system. The ejected material appears to be travelling –2 at velocities far exceeding the escape 4 velocity, so it may travel for up to 1 Mpc before losing its momentum and stall- –3 [O II] emission line map ing. At this point, it will have ‘polluted’ a –2–3 –1 0123 2 volume of nearly 3 Mpc3 with metal- enriched material. If this phenomenon is typical of galaxies at that epoch (which remains to be demonstrated on a sample 0

of more than one galaxy), it may help us Arcseconds understand the widespread metal enrichment of the early universe, and may ex- –2 plain why only a small fraction of the baryons in the Universe cool to form stars.

(Based on Swinbank et al., 2007, MNRAS, 376, 479) –4

‘Image plane’ HST observations, that is, the lensed –6 image of the z = 4.88 galaxy discovered, in grey scale, with the VIMOS Lya contours in red and the SINFONI [O ii]3727 contours in white. The inlay shows the continuum-subtracted [OII] VIMOS data, show- –2–3 –1 0 1234ing the structure of the most distorted (central) part Arcseconds of the arc.

ESO Annual Report 2007 19 Fundamental constants

The standard or ‘concordance’ cosmo- possibilities have emerged in the theoret quasars failed to reproduce the variations logical model (referred to as Lambda ical particle physics arena: string theory, of a claimed by the Australian observers. Cold Dark Matter – LCDM) establishes super-gravity, Grand Unified Theories, However, subsequent observations of that our Universe formed 13.7 billion years and others. While none of these theories a large sample of 143 absorption line sys- ago in a dramatic explosion. According to has yet offered concrete testable pre tems by the same team, now using the model, the present energy density of dictions about the nature of dark energy, the Keck telescope, once again claimed a the Universe is dominated by two myste- most require that the fundamental con- positive detection of a variations, Δa/a rious forms of darkness: dark matter and stants of physics (such as the couplings = (–5.7 ± 1.1) × 10 –6. Yet again, new ob- dark energy. Both are dark because they of the fundamental forces for example) servations, using both UVES at the VLT do not emit electromagnetic radiation, should vary with cosmic time. and HARPS on the La Silla 3.6-m tele- but the concordance model is still based scope, failed to confirm this result. The on an impressive body of observations. A particular prediction that could be HARPS observations have higher spec- For example, while dark matter cannot be tested through astronomical observations tral resolution, but lower signal-to-noise seen (that is through our gamma-ray to is the variation of the fine-structure con- ratio, while UVES gives significantly larger radio telescopes), its gravitational effect stant (a), which measures the strength of signal, but at a lower resolution. The ob- on light-emitting matter (baryons and lep- the electromagnetic force. Since elec- servations show that a large number of tons) can be measured. We thus know trons are fundamentally bound to atomic components is required to fit all the that the carriers of dark matter must be nuclei by electrical forces, changes in a bends and wiggles in the spectrum, and cold, that is, must move at relatively have directly observable effects in the that the number of components seems to slow velocities. Otherwise the universe spectra of stars and gas. About 10 years increase with resolution. Since the inter- would have much less structure than ago, a team of astronomers using a tele- stellar medium is known to have a fractal what we observe because it is very diffi- scope in Australia claimed evidence for structure, the number of components cult to cluster particles that are moving changes in a with cosmic time (redshift). used to fit the data will always be a fun- at relativistic speeds. Particle physicists Their method consisted of observing the damental limitation of the method. have coined a name for the cold dark interstellar absorption lines of clouds Clearly, the weaker the line, the smaller matter particles: weakly interacting mas- of neutral gas along sightlines to distant the wavelength shifts they will induce sive particles (WIMPS); these particles quasars, to search for minute shifts in in the neighbouring lines. This fundamen- interact with the rest of the Universe ei- the observed wavelengths of well-charac- tal uncertainty becomes even larger if ther gravitationally or through the weak terised spectral features that could be one averages over many absorption sys- nuclear force (responsible for the beta- ascribed to changes in a. Such observa- tems with different redshifts. Moreover, decay of neutrons). Unfortunately, the tions are extremely challenging because in order to increase the signal-to-noise, standard model of particle physics (which not only does one need to measure the observers not only average over different describes three of the four known funda- positions of the lines with very high accu- redshifts, but also over different ions – mental interactions between elementary racy, but the intervening gas also has typically Mg ii and Fe ii. We know from particles – the fourth being gravity), does multiple components that can mimic ra- GRB observations (see above), however, not predict the existence of any particles dial velocity shifts. These problems push that Mg ii and Fe ii cannot be formed in the that would have the properties of WIMPS. instruments to their limit, so it is not sur- same volume of the intervening absorb- Therefore, even though dark matter is prising that different teams find different ers. So averaging different ions is proba- theoretically better understood than dark results. For example, observations with bly not a good idea. energy, it still poses a big challenge to UVES on the VLT of a sample of bright our understanding of fundamental physics.

Dark energy is much worse: we simply 1 have no idea what this mysterious repul- sive force could be. All we know is that it 0.5 has a negative pressure, and that during Fe II 1608 S/N = 100 the last billion years or so it has caused 0 an acceleration of the expansion of the 1 Universe. Einstein’s ‘greatest blunder’, the cosmological constant, is currently the 0.5 form of dark energy that is most consist- Fe II 2382 S/N = 120 ent with the observations. It poses, how- 0 ever, a formidable challenge to phys- 1 ics because the observed value is several tens of orders of magnitude smaller 0.5 than theory would predict! Dark energy UVES observations of a line of sight to the bright (or equivalently, cosmic acceleration) Fe II 2600 S/N = 120 0 quasar HE 0515-4414 at –100 –90 –80 –70 –60 –50 –40–30 –20 –10 0 10 20 30 40 50 60 70 requires new physics, and a number of Radial Velocity (km/s) z = 1.15.

20 ESO Annual Report 2007 With these considerations in mind, a team of astronomers led by S. Levshakov developed a new method which uses a single ion (Fe ii), and applied the method to a single absorption line system at zabs = 1.15 toward the bright quasar HE 0515-4414. Both the UVES and the HARPS observations failed to detect any variations in a within an accuracy of 0.8 10 –6 for UVES and 2.4 10 –6 for HARPS. When applied to archival UVES observations of another quasar,

Q1101-264 at zabs = 1.839, they also re- jected variability albeit with a lower accuracy of 3.8 10 –6.

Encouraged by their results with the archival data, Levshakov and collaborators reobserved the same quasar with UVES, but now at a higher spectral resolution and higher signal-to-noise to improve their detection limits. The new observation, with a total exposure time of more than 15 hours and a spectral resolution of R = 80 000, allowed them to reach a signal-to-noise per pixel of better than 100 and a wavelength calibration error of only 20 m/s, quite remarkable for a V = 16 quasar.

A careful statistical analysis led them to detect a statistically significant (2s barring unknown systematic errors) variation of Δa/a = (5.4 ± 2.5) × 10 –6. So the game is not over, and more and better observations are required to confirm these results. Among existing instruments, due to its blue sensitivity and excellent resolution and stability, UVES remains the best-suited instrument for this kind of work. Only future instruments such as ESPRESSO at the combined Coudé focus of the VLT or CODEX at the E-ELT will surpass it.

(Based on Levshakov et al., 2007, A&A, 466, 1077)

ESO Annual Report 2007 21 Photo: Y. Beletsky

La Silla Paranal Observatory

In 2007, the La Silla Paranal Observatory 9 % due to bad weather conditions. On New instruments and facilities continued to increase its suite of opera- La Silla bad weather accounted for losses tional telescopes and instruments. With of about 15 %, and technical problems for CRIRES started science operations the start of operation of the fourth 1.8-m 1.5 %. on the Nasmyth A focus of Antu with the Auxiliary Telescope (AT) and of the cry beginning of Period 79 in April 2007. ogenic high-resolution infrared echelle Complementary to regular VLT and CRIRES is an adaptive-optics supported spectrograph CRIRES, the Observatory is La Silla operations, the VLT Interferom- high-resolution infrared (1 to 5 μm) spec- now routinely operating a total of 11 tele- eter (VLTI) was scheduled for an addi- trograph that provides a resolving power scopes with 20 optical, near- and mid- tional 182 nights to execute scientific ob- of up to 100 000 when used with a nar- infrared instruments. On Paranal these servations using baselines with either row slit width of 0.2 arcsec. The astro- are the four 8.2-m Unit Telescopes (UT) the UTs or the ATs. The remaining nights nomical community had responded en- forming the Very Large Telescope (VLT) of the year were used for technical activi- thusiastically to the call for scientific with its ten permanently installed instru- ties and for further development and proposals for this long-awaited new re- ments, and the VLT Interferometer (VLTI), commissioning of the interferometer. Of search tool. The high spectral and spatial which coherently combines the light the scheduled VLTI science time, 3.6 % resolution of CRIRES opens up com- of either the UTs or ATs to feed one of the was lost due to technical problems. pletely new research fields in the detailed two interferometric instruments. On study of spectral lines of chemical ele- La Silla, eight instruments are operated The combination of high operational effi- ments and molecules in the infrared on the New Technology Telescope (NTT), ciency, system reliability and uptime for wavelength regime. The commissioning the 3.6-m, and the 2.2-m telescopes. scientific observations of the La Silla and of this complex instrument continues in Paranal telescopes and instruments has parallel to the science operation, to fur- The Observatory further provides the op- again resulted in high scientific productiv- ther improve its stability and perform- erations support for the Atacama Path- ity. We have counted 493 peer-reviewed ance. finder Experiment (APEX) with its 12-m papers published in different scientific submillimetre radio antenna and its suite journals which are at least partially based The eleventh VLT instrument, HAWK-I of heterodyne and bolometer instruments on data collected with VLT and VLTI in- (High Acuity Wide field K-band Imager) located at the high plateau of Chajnantor struments at Paranal, while telescopes at was installed and commissioned on the at an altitude of 5 000 m. La Silla accounted for 325 refereed pa- last free VLT focus station1, i.e. the Nas- pers. Since the majority of astronomical myth A focus of Yepun (UT4). HAWK-I The high productivity of the Observatory publications are based on contributions is a cryogenic wide-field imager operating relies on the high availability of its tele- from different instruments and observato- in the near-infrared wavelength range scopes and instruments to carry out sci- ries, the individual contributions and from 0.85 to 2.5 μm with an on-sky field entific observations. In 2007, a total of their relative weight are difficult to meas- of view of 7.5 arcmin × 7.5 arcmin. This 2245 nights were scheduled for scientific ure. However, we estimate that in 2007 corresponds to a field of view of about observations with the four UTs at the the La Silla Paranal Observatory has sub- VLT and with the three major telescopes stantially contributed to about two refe- 1 The 12th focus station of the VLT is the Visitor at La Silla. This is equivalent to about reed papers every day of the year. Focus at the Melipal telescope. 89 % of the total number of nights theoretically available over the whole year. The remaining 11% were scheduled for planned engineering and maintenance activities to guarantee the continuous performance of the telescopes and instruments and include time slots for the commissioning of new instruments and facilities. The biggest maintenance operations this year were the recoating with fresh layers of aluminium of the primary and tertiary mirrors of Antu (UT1) and Melipal (UT3), and of the secondary mirrors of Kueyen (UT2) and Melipal. These coating layers measure only a few tens of atomic radii in thickness. For the primary mirrors of the ATs, a regular mirror-washing programme has been established to considerably extend the time between recoating. Out of the available science time for Paranal only 2.6 % was lost due to technical problems and about The CRIRES instrument.

24 ESO Annual Report 2007 nine times that of the very successful VLT The ULTRACAM visitor infrared camera ISAAC, and a field of instrument on the VLT. view comparable to or even larger than that of the optical cameras FORS1 and FORS2. Whenever the atmosphere above Paranal permits, HAWK-I routinely delivers exquisite infrared images with an almost constant full width at half maximum for the stellar point sources of about 0.2 arcsec across the whole field of view. HAWK-I has not only been optimised for best image quality but also for highest sensitivity and allows the deepest views into the infrared sky with the VLT. After its successful commissioning and science verification in 2007, HAWK-I will be offered for the first time to the astronomical community in Period 81 starting in April 2008. To become even more independent from the quality of the atmosphere, and to constantly deliver highest- resolution images, HAWK-I will in the future be supported by the Adaptive Op- tics Facility (AOF). The AOF is intended with the LGS in 2007. In about half of Explorer, is a narrowband imaging instru- to convert Yepun into an adaptive-optics these nights, actual scientific observa- ment developed by the Institute of As- telescope with a large deformable sections with the LGS could be performed. tronomy (Cambridge, UK) and the Anglo- ondary mirror, a four laser guide star fa- We consider this a respectable result Australian Observatory with the single cility (4LGSF) and an adaptive optics for the first year of LGSF operation but aim of detecting the most distant objects module named GRAAL, which is specially with room for further improvement. in the Universe. The Principal Investiga- designed for the needs of HAWK-I and Therefore, the further increase in reliabil- tors of both visitor instruments reported will provide a wide field of view corrected ity and performance of the LGSF and successful observing runs and returned for the effects of the atmosphere. the optimisation of the operational proce- home with large amounts of data from dures remains a continuous effort of the some 20 observing nights at the VLT. The single Laser Guide Star Facility Observatory. (LGSF) achieved its First Light at the The visitor instruments had to compete Yepun telescope in 2006. Since then the In 2007, the VLT Visitor Focus welcomed with MAD, the Multi-conjugate Adaptive LGSF has provided a bright artificial ref again the ULTRACAM and DAZLE visi- optics Demonstrator, a test-bench instru- erence star for the adaptive optics (AO) tor instruments. ULTRACAM is an ultra- ment conceived to demonstrate in the systems of the SINFONI and NACO in- fast camera capable of capturing some of laboratory and on-sky the principles of struments. Such a Laser Guide Star is re- the most rapid astronomical events in the multi-conjugate adaptive optics (MCAO). quired for the AO systems to work in re- cosmos. ULTRACAM is the first UK-built And indeed, MAD succeeded for the very gions of the sky where no bright natural instrument to be mounted on the VLT and first time in demonstrating during several star can be found close enough to the was designed and built by scientists from test runs on the VLT that it is possible to scientific target. After the basic commis- the Universities of Sheffield and Warwick, perform adaptive optics correction in the sioning of the LGSF the AO instruments in collaboration with the UK Astronomy K-band (around 2.2 μm) over a wide field SINFONI and NACO were offered with Technology Centre in Edinburgh. It can of view of 2 × 2 arcmin by using multiple the new LGS mode at the earliest possi- take up to 500 pictures a second in three and relatively bright natural guide stars ble stage to the scientific community, in different colours simultaneously. DAZLE, and multi-layer AO corrections. The spec- order to allow a timely exploitation of this the Dark Age Z (redshift) Lyman-alpha tacular success of this experiment is con- new exciting capability of the VLT. This sidered a major milestone for the devel- early commitment requires a continuous opment of future adaptive telescopes like effort of the maintenance and operations the AOF at the VLT, and also the E-ELT. teams in Paranal, the Garching LGSF In addition, the scientific community has team and the PARSEC laser team from been very excited about the new possibil- MPE in Garching and MPIA in Heidel- ities provided by MAD and several sci- berg. As a result of these efforts, the LGS ence demonstration runs were squeezed was technically available for science into the Paranal schedule to allow the operations with SINFONI and NACO for community to immediately exploit these about half of the 120 nights scheduled new capabilities with the VLT.

ESO Annual Report 2007 25 Upgrades

To maintain the competitiveness of the VLT and VLTI it is not sufficient to continue to deliver new instruments and facilities: a rigorous upgrade programme for the existing instruments must also be followed. In 2007 several such upgrades were carried out by the Instrumentation Division in Garching in collaboration with the instrument builders and the Observa- tory.

FORS1, the optical imager and spectrograph on Kueyen, was equipped with a blue-sensitive CCD detector mosaic complementary to the one in FORS2, which is optimised for the red part of the optical spectrum. The overall sensitivity of FORS1 was further increased by the installation of high-transmission broadband filters.

VISIR, the imager and spectrograph in The multi-fuel the mid-infrared at Melipal, was upgraded power station. with a new filter set for the imager. The new filters permit spectrophotometric observations with a low resolving power of Therefore, a project to purchase a high- The VISA feeds the VLTI infrastructure 10 and quantitative measurements of the reliability, low-maintenance multi-fuel gas and instruments with the light from the most prominent solid-state feature in the turbine generator was initiated. The ability 1.8-m Auxiliary Telescopes (AT) when 10-micron window, the silicate band. of a MFPG to be supplied with different the individual UTs are used for stand- energy sources, from natural gas to ship alone VLT observations. In 2007, the VISA NACO, the adaptive optics infrared cam- diesel, will allow us to react more easily started science operation with four ATs. era on Yepun, received new tools for to the fast-changing market of available The additional fourth AT, which was ac- improved high-contrast imaging. New energy sources. For the time being, the cepted for operation at the beginning four-quadrant phase masks (4QPM) and MFPG will run on liquefied propane gas of the year, provides the VLTI operations an improved Spectral Differential Imager (LPG). The installation and commissioning with additional flexibility in the selection (SDI+) now allow NACO to better identify of the MFPG and the LPG tanks started of different and complementary AT base- close companions such as faint brown in the last quarter of 2007 and its hand lines even in the same observing night dwarfs or even young, giant planets next over to the Observatory is planned for the without having to physically reconfigure to bright stars. first quarter of 2008. the array of telescopes.

An upgrade of a very different nature The AMBER instrument, which allows the but of fundamental importance for The VLT Interferometer interferometric combination of up to three the Paranal site was started in 2007: the beams, was offered to the community installation of a new Multi-Fuel Power In 2007, the VLT Interferometer (VLTI) for the first time with the FINITO fringe Generator (MFPG) to upgrade the Paranal executed about 182 nights of scientific tracker and the ATs. This new mode be- power station from diesel engine genera- observations with MIDI and AMBER using came available in Period 79 in April 2007 tors to a gas turbine generator. Continu- UT and AT baselines – this is 30 % more in visitor mode – only four months after ous and reliable on-site power generation than in the previous year. The remaining it was successfully tested for the first time at a remote and isolated place such as time was intensively used for engineer- on 1 December 2006 on the bright star Paranal, which requires clean and stable ing and commissioning activities to com- b Ceti. Fringe tracking techniques con electrical power and which cannot be plete and improve the interferometer siderably improve the sensitivity of the connected to an electrical grid, is abso- infrastructure and to fully exploit the ca- interferometer because they enable the lutely crucial for the smooth operation pabilities of the VLTI Sub Array (VISA). instruments to integrate longer on the of the Observatory. The experience of the stabilised fringe patterns and therefore past years has shown that a power sta- to observe fainter targets or with higher tion based on diesel engines is a major quality. While AMBER so far has been challenge and costly to run and maintain. limited by the variability of the earth’s at-

26 ESO Annual Report 2007 mosphere to integration times of 25 milli- at sunset. All the systems were operated mirror optics, which had already arrived seconds, with FINITO it is now possible that same night without restrictions, in- in the previous year. Both mirrors are to integrate for up to 10 seconds, equiva- cluding all four UTs (with their instruments ready for their integration into the tele- lent to a gain of a factor of 400. and the LGS) and the ATs with the VLTI. scope. However, the primary mirror cell and the secondary mirror unit remain After this critical milestone was achieved in Italy awaiting their completion before with the ATs, the VLTI team immediately VST and VISTA survey telescopes being delivered to Paranal to complete concentrated its efforts on also providing the VST. FINITO fringe tracking with the UTs. Vi- By mid-2007, the 2.4-m optical VLT Sur- brations of the optical surfaces of the UTs vey Telescope (VST) had been shipped The construction of the 4.2-m infrared transmitted to the VLTI had earlier been to Paranal and its reintegration started in- survey telescope VISTA by the VISTA identified as the primary cause that pre- side the VST enclosure next to the UTs project office continued on its own peak vented fringe tracking with the UTs. In the on the Paranal observing platform. The about 1500 m north-east of the Paranal meantime, active vibration suppression integration of the complete telescope summit. The integration and testing of all systems had been developed in-house structure but with steel dummies for the the major telescope and support sys- and shown to largely overcome this prob- primary mirror cell and the secondary tems has been completed. The manufac- lem. Consequently, the full deployment mirror unit was completed by the end of turing of the secondary mirror optics and commissioning of the vibration sup- the year under the responsibility of Insti- was completed and the mirror has arrived pression system became the primary tuto Nazionale di Astrofisica (INAF) and in at Paranal. The mirror surface was suc- tasks of the VLTI team in 2007. This in- collaboration with La Silla Paranal engi- cessfully coated in the dedicated VISTA cluded the installation of accelerometers neers. The manufacturing of the VST pri- coating plant with a thin layer of silver on all the main vibrating mirrors of the mary mirror optics was completed and to provide highest reflectivity of the opti- UTs and the commissioning of the active the mirror was safely delivered to Paranal. cal surface in the near-infrared wave- Vibration Tracking (VTK) system. By the It is stored together with the secondary lengths where VISTA will survey the sky. end of the year the VLTI team had succeeded in these critical tasks. After an extended characterisation period in early 2008, the team expects to deliver the FINITO fringe tracking with AMBER and the UTs to the science operations team and the community just in time for Peri- od 81 starting in April 2008.

Earthquake

On 14 November at 12:41 LT, an earthquake with Richter magnitude 7.7 and epicentre north of Antofagasta badly affected the north of Chile. The town of Tocopilla was hit hardest, and hundreds of houses were damaged and many people were injured. In Paranal the earthquake was registered with a magnitude of 5.7, a peak ground acceleration of 0.6 m/s2, and for a duration of approximately two minutes. This was the strong- est earthquake since 1997, the first ‘high risk’ earthquake since the start of op erations of the VLT, and the first strong earthquake since the opening of the Paranal hotel, the so-called Residencia. Neither injuries to persons nor damage to the installations were registered. After extended checkout procedures, regular night-time operations could be resumed

The VST telescope structure.

ESO Annual Report 2007 27 Integrating the VISTA camera into the telescope. Also the heart of the VISTA facility, the 64-megapixel infrared camera built from an array of sixteen 2048 × 2048 pixel infrared detectors arrived at Paranal and was successfully integrated in the VISTA telescope. In an extended test phase the camera was successfully operated at its nominal cryogenic temperatures. The instrument mounts to the rotator on the back of the primary mirror cell, and includes a wide-field corrector lens system (three large Infrasil lenses), an autoguider unit and active optics sensors.

The VISTA telescope is now awaiting the arrival of its primary mirror optics. The primary mirror of the VISTA telescope is, with a focal ratio of f/1, the fastest 4.2-m mirror ever manufactured and is still in the phase of final polishing at the manufacturer in Europe. It will be ready to be air-freighted to Paranal in early 2008. für extraterrestrische Physik (Garching, APEX Germany) at the 2.2-m telescope. GROND La Silla is not a facility instrument for general use In 2007, APEX received its eagerly ex- by the ESO community but is operated pected facility bolometer array LABOCA At La Silla the operation of the 3.6-m tele- by the La Silla science operations team developed by the Max-Planck-Institut scope was strongly affected by a severe as part of the 2.2-m telescope. The acti- für Radioastronomie (Bonn, Germany). degradation of the dome rotation mecha- vation to follow up a new, usually satel- LABOCA (the LArge BOlometer CAmera) nism, stalling operations for one full month lite-detected GRB explosion with GROND is a detector array with 295 pixels and and subsequently restricting operations uses the same rapid-response mode operates at a wavelength of 870 microns. for several months in late 2006 and ear- (RRM) mechanism as the VLT. This fully LABOCA was extensively tested during ly 2007. Through a combined effort of the automatic system enables starting the the beginning of the year at Chajnantor engineering and maintenance depart- observation of the GRB or other transient and started regular science operations in ments of the La Silla Paranal Observatory phenomena just few minutes after their mid-2007 after a very successful science the problems identified were corrected. A discovery. verification campaign with strong involve- new system of spring-dampened bogies ment of the astronomical community. The was developed and installed, reenabling Towards the end of the year the Coudé final facility heterodyne receivers from the full-speed rotation of the 300-ton Echelle Spectrograph (CES) was decom- Onsala Space Observatory, which will dome by March 2007. Since then, no missioned after 25 years of operation. cover all atmospheric windows from 200 downtime for the 3.6-m telescope has This is part of the plan for a continued to 1400 GHz, were ready for shipment to been reported as being caused by the streamlining of La Silla operations up to APEX by the end of the year and will be dome. The telescope itself continues the end of 2009. Starting with Period 81 installed during the Bolivian winter break to deliver excellent image quality of better in April 2008 the three large La Silla tele- in January and February 2008. In early than 0.5 arcsec. This achievement is the scopes will all operate with a fixed set 2007, the static sub-reflector of the APEX result of a long series of upgrades to the of instruments. No instrument changes antenna was successfully replaced with telescope, which was concluded this year will be performed anymore except to ac- a chopping sub-reflector, the so-called with the commissioning of the lateral pad commodate visitor instruments. The ‘wobbler’. The wobbler allows the anten- control system for the primary mirror. The 3.6-m telescope will then operate exclu- na to switch quickly between two posi- scientific instruments are taking advan- sively with HARPS, the NTT with EFOSC2 tions on sky. This observing technique in- tage of the improved image quality as de- and SOFI, and the 2.2-m telescope with creases the quality of the observations livered by the telescope: HARPS, the FEROS, WFI and GROND. by eliminating time-dependent instabili- planet search machine at the 3.6-m tele- ties in the receivers and the atmosphere. scope, reports a sensitivity increase of The complete suite of new facility instru- up to 40 %. ments will soon allow APEX to exploit fully the exceptional conditions available The gamma-ray burst (GRB) follow-up at its 5100-m altitude site. instrument GROND was installed and commissioned by the Max-Planck-Institut

28 ESO Annual Report 2007 User Support ported at the VLT, VLTI, and ESO/MPI 2.2-m tion of a variety of calibration and science telescope during 2007 has remained above data products for these instruments. QC The new interface connecting ESO and its the 1000 threshold. APEX Service Mode works closely with the Paranal Science Op- users’ community, the ESO User Portal, was operations (started in April 2006) have ma- erations department to assure that VLT/ successfully launched in mid-November. tured into a stable and organised scheme. VLTI instruments are always performing Within this system, which is the result of a The strong demand for SM observing is within expected and published ranges. Ex- joint effort involving departments of several supported by a constant revision of the cept for a few very specific cases, all the in- ESO divisions, account information (user- preparation and observing tools we offer formation on instrument performance is name, password, contact information) for all to the users and by the implementation of available to the community at large from the science and observations related web- new features and improved operational QC Web pages. Raw calibration data are based applications (e.g. routines for request- workflow. During 2007, the most notable processed into master calibration products ing data from the Archive) and standalone example of these was the implementation that are used not only to monitor instrument software (P2PP, the Phase 2 Proposal Prep- of a new web-based form for Target/Instru- performance but also to process science aration tool) is unified and user-controllable. ment Setup Change Requests that allows data. These master calibration products are It is intended to make the use of ESO web ESO to run a thorough semi-automatic stored in the ESO archive and are available applications and other software simpler, and duplication check when evaluating this type to the community at large. more manageable. of request. Two additional services are provided to A feedback campaign was launched in early The ESO Survey Team (EST) has strength- Service Mode users. First, Service Mode 2007. The questionnaire covered several ened its role by coordinating the preparation science data are processed into science aspects of the ESO Data Flow System, and of the VISTA public survey management products using standard pipelines which, it was especially tailored for Service Mode plans. Six public surveys were selected and by now, cover virtually 100 % of the Paranal (SM) users. All Principal Investigators with the teams worked on a detailed implementa- data stream. Second, data packages are approved SM runs between Periods 69 and tion of their observing strategies with the created that include all raw data, resultant 77 (covering the period from April 2002 to support of the ESO Survey Team. Based on products, and associated information for September 2006) were asked to provide the submitted Survey Management Plans, each and every Service Mode observing feedback on different areas, from the Call final recommendations were prepared. run. These packages are burned onto mass for Proposal and Phase 1, to Phase 2 activi- storage devices such as DVDs or USB disks ties and their follow-up, to the processing and shipped to users. and delivery of the data. The users’ satisfac- Data processing and quality control tion emerged very clearly: most of the serv- During 2007, QC processed more than 7 TB ices we offer and support received a major- Ensuring that data taken on Paranal are of of raw data in 160 000 processing jobs ity of “Very Good” and “Excellent” votes. certified and predictable quality and contin- to create 1100 service mode packages with uously monitoring the health state of the VLT/VLTI data, which were distributed to Service Mode has continued to be the most instruments are cornerstone concepts in the their respective Principal Investigators. The requested observing mode at the VLT: ESO end-to-end data flow model. The Qual- QC group also packages data coming from the demand for SM observing was a factor ity Control and Data Processing (QC) group La Silla, but without performing quality of 2 and 3 higher than the time requested is responsible primarily for the monitoring checks on them. In the year 2007, 122 such for Visitor Mode during Period 79 and 80 and reporting of instrument performance for packages were produced and shipped respectively. The number of SM runs sup- all VLT/VLTI instruments, as well as the crea- to the corresponding Principal Investigators.

La Silla in the morning.

ESO Annual Report 2007 29

The Observing Programmes Committee

on APEX, which is run in collaboration to override both Visitor and Service Mode The Observing Programmes Committee with the Max-Planck Institute for Radio- observations, have positioned the 2007 astronomy and the Onsala Space Ob- VLT and the GRB community of the ESO Danielle Alloin servatory, so that 27% of the total time member states at the forefront of this field Omar Almaini (P80) is available for ESO programmes. The of research. Svetlana Berdyugina (Vice-chair) amount of time requested on the two Hermann Böhnhardt (P80) main La Silla telescopes (3.6-m and NTT) Jan Brand (P81) Jarle Brinchmann (P81) was 10 % higher in 2007 than in 2006. Large Programmes Mike Disney (P80) On the 2.2-m telescope, new contractual Thierry Forveille agreements with the Max-Planck Society Large Programmes (LPs) are projects re- Roland Gredel and the National Observatory of Brazil quiring more than 100 hours of observ- Rodrigo Ibata Leopoldo Infante decreased the amount of time available ing time per year over no more than two Mika Juvela (P81) for execution of ESO programmes. Taking years, and which have the potential to Donald W. Kurtz (P81) into account the time already committed lead to a major advance or breakthrough Claudia Maraston (P81) to Large Programmes started in 2006, in the considered field of study. In P80, Simon Morris (Chair) Antonella Nota (P80) the only new proposals that could be the OPC evaluated 14 LP proposals, and Rafael Rebolo Lopez (P80) accepted for this telescope in 2007 were recommended three of them for imple- Tom Richtler those falling within the framework of mentation. In P81, four of the 24 LP pro- Sabine Schindler (P81) ESO’s agreement with its host state, Chile. posals which were submitted were ap- Stella Seitz (P80) Monica Tosi Among VLT instruments, the demand proved. In total, between the start of VLT Sylvie Vauclair for most instruments is very even, within science operations in 1999 and 2007 10 % of each other. Much less time was (P81), 79 LP proposals which received fa- requested for HAWK-I, offered for the first vourable evaluation from the OPC were In 2007, the Observing Programmes time in P81, and VISIR, which is designed allocated time on the La Silla Paranal Ob- Committee (OPC) held its two regular an- for very specific scientific applications, servatory telescopes. They cover almost nual meetings in May and in November. In while FORS2, in its eighth year of opera- all current astronomical topics, from the addition, a special OPC Panel was con- tion, remains the most popular VLT in- Solar System to cosmological studies. vened in August, for evaluation of propos- strument, with a demand almost twice als submitted in response to a “Delta as high as the average. The visitor instru- Call” for LABOCA, a new instrument that ment DAZLE was also scheduled on OPC procedures had been recently commissioned on the Melipal in P80. APEX telescope. Adding the 51 LABOCA In an attempt to keep the workload of the proposals received in response to this Joint telescope time applications for co- OPC to a manageable level despite the Delta Call to the 892 proposals submitted ordinated observations with the VLT and ever-increasing number of proposals, a by the regular deadline of end March with the XMM-Newton X-ray observa- new proposal type, the Short Programme for the Observing Period 80 (P80 – 1 Oc- tory were invited in P81. These proposals proposals, was introduced in P80. tober 2007 to 31 March 2008), a new all- fall within the framework of an agreement Short Programmes require no more than time record number of 943 proposals between ESO and ESA for a joint tele- 10 hours of observing time. Short Pro- were counted in P80. This total was sur- scope time application scheme, which grammes need a special proposal form, passed again in Period 81 (P81 – 1 April was in its fourth year in 2007. It aims in which the space available for the scien- to 30 September 2008), which saw the at taking full advantage of the comple- tific justification and the accompany- submission of 952 proposals. As already mentarity of ground-based and space- ing figures is half of that in Normal Pro- noticed in previous periods, the increase borne observing facilities. ESO did not re- gramme proposals. About 20 % of the of the demand continues to take place ceive any joint applications in P81, but proposals submitted in P80 and P81 cor- primarily in the ‘Galactic’ scientific areas: two of the eleven joint applications evalu- respond to Short Programmes. interstellar medium, star formation and ated by the XMM Time Allocation Com- planetary systems (OPC category C – mittee were allocated time. On the other hand, as the fraction of pro- see page 33), and stellar evolution (OPC posals in scientific categories C and D category D), while the number of ‘extra- In 2007, the field of gamma-ray bursts continued to grow, one new sub-panel galactic’ proposals of categories A (cos- (GRBs) continued to account for about was added for each of these two catego- mology) and B (galaxies and galactic half of the successful Target of Oppor ries, for the second time in one year. As nuclei) remains approximately constant. tunity (ToO) proposals. A large fraction of a result, the OPC now consists of 12 sub- the GRB proposals make use of the panels (compared to eight until 2005, and The ratio between the requested and Rapid Response Mode (RRM) of the VLT, ten in 2006), i.e. two for each of catego- available time has again reached nearly with which observation of a transient ries A and B, and four for each of catego- six on the most demanded Unit Tele- event can be automatically started within ries C and D. For the longer term, alter scopes (Antu and Yepun). Following the minutes of its triggering. The unique per- native solutions are being investigated to introduction of LABOCA, this ratio formance of the VLT in this mode, com- face the foreseeable continued increase reached an even higher value (6.7 in P80) bined with ESO’s policy of allowing it of the number of proposals.

32 ESO Annual Report 2007 Summary of Use of Telescopes by Discipline

OPC Categories and Sub-Categories B6 Non-thermal processes in galactic C6 Main-sequence stars with circum nuclei (incl. QSRs, QSOs, blazars, stellar matter, early evolution The scientific categories referred to in Seyfert galaxies, BALs, radio galax- C7 Young binaries, brown dwarfs, the following tables correspond to the ies, and LINERS) exosolar planet searches OPC classifications given below: B7 Thermal processes in galactic nuclei C8 Solar system (planets, comets, and starburst galaxies (incl. ultra small bodies) A: Cosmology luminous IR galaxies, outflows, A1 Surveys of AGNs and high-z galax- emission lines, and spectral energy D: Stellar Evolution ies distributions) D1 Main-sequence stars A2 Identification studies of extragalactic B8 Central supermassive objects D2 Post-main-sequence stars, giants, surveys B9 AGN host galaxies supergiants, AGB stars, post-AGB A3 Large scale structure and evolution stars A4 Distance scale C: Interstellar Medium, Star Formation D3 Pulsating stars and stellar activity A5 Groups and clusters of galaxies and Planetary Systems D4 Mass loss and winds A6 Gravitational lensing C1 Gas and dust, giant molecular D5 Supernovae, pulsars A7 Intervening absorption line systems clouds, cool and hot gas, diffuse D6 Planetary nebulae, nova remnants A8 High redshift galaxies (star forma- and translucent clouds and supernova remnants tion and ISM) C2 Chemical processes in the inter D7 Pre-white dwarfs and white dwarfs, stellar medium neutron stars B: Galaxies and Galactic Nuclei C3 Star forming regions, globules, pro- D8 Evolved binaries, black-hole candi- B1 Morphology and galactic structure tostars, H ii regions dates, novae, X-ray binaries, CVs B2 Stellar populations: unresolved and C4 Pre-main-sequence stars (massive D9 Gamma-ray and X-ray bursters resolved PMS stars, Herbig Ae/Be stars and D10 OB associations, open and globular B3 Chemical evolution T Tauri stars) clusters, extragalactic star clusters B4 Galaxy dynamics C5 Outflows, stellar jets, HH objects D11 Individual stars in external galaxies, B5 Peculiar/interacting galaxies resolved stellar populations D12 Distance scale stars

Percentage of scheduled observing time/telescope/instrument/discipline

Scientific Categories Scientific Categories Telescope Instrument A B C D Total Telescope Instrument A B C D Total 2.2-m FEROS 0 1 11 61 73 UT1 CRIRES 0 3 15 14 32 WFI 13 2 4 8 27 FORS2 16 12 4 11 43 Total 13 3 15 69 100 ISAAC 9 3 6 7 25 Total 25 18 25 32 100 3.6-m CES 0 0 0 1 1 EFOSC2 9 6 0 8 23 UT2 FLAMES 1 12 8 12 33 HARPS 0 0 56 12 68 FORS1 7 3 3 17 30 Special 3.6 0 0 1 7 8 UVES 8 3 11 15 37 Total 9 6 57 28 100 Total 16 18 22 44 100

NTT EMMI 19 6 10 17 52 UT3 VIMOS 33 14 2 9 58 SOFI 6 2 16 8 32 VISIR 0 5 22 5 32 SUSI2 0 8 1 5 14 Special UT3 4 0 2 4 10 Special NTT 0 0 2 0 2 Total 37 19 26 18 100 Total 25 16 29 30 100 UT4 NACO 2 8 25 12 47 APEX APEX-2A 4 13 31 4 52 SINFONI 22 17 10 2 51 FLASH 0 5 0 0 5 Special UT4 2 0 0 0 2 LABOCA 40 3 0 0 43 Total 26 25 35 14 100 Total 44 21 31 4 100 VLTI AMBER 11 0 27 25 63 MIDI 0 5 6 26 37 Total 11 5 33 51 100

ESO Annual Report 2007 33

The Users’ Committee

The Users’ Committee (UC) held its an- and with the transparency of the OPC The Users’ Committee nual meeting on 16 and 17 April. The and time allocation processes, has im- 2007 acting chair for the meeting was Walter proved. More generally, significant pro- Belgium Griet Van de Steene Jaffe. gress had been made with respect to the action items and recommendations made Denmark Uffe Gråe Jørgensen Representatives from ESO gave pre by the UC at its 2006 meeting, most of sentations to the Committee about the which could be closed. New action items Finland Merja Tornikoski La Silla Paranal Observatory, ALMA, and recommendations were assigned France Pascale Jablonka the proposal submission and time alloca- to ESO by the UC, reflecting the areas in (Chair) tion processes and the new OPC struc- which the community perceives the need ture, and the publications based on for further improvements. Germany Jochen Heidt observations obtained with the ESO tele- Italy Bianca Maria Poggianti scopes. The UC in turn provided feed- As usual, half a day was devoted to a back from the users on the usage of ESO ‘special topic’, which this time was The Netherlands Walter Jaffe facilities, based in part on the outcome “Current instrument pipelines and future (Vice-chair) of a survey designed and distributed by direction of data processing develop- Portugal Nuno Cardoso Santos the Committee. The level of satisfaction ments”. Two introductory presentations of the users with respect to observations were given by ESO staff, on the current Spain Ignacio Negueruela carried out at the La Silla Paranal Ob- status and the options for future devel Sweden Sofia Feltzing servatory is in general high. The main opments of instrument pipelines and of issue of concern for the users is the avail- associated tools, and on the genera- Switzerland Frédéric Courbin ability of the instrument pipelines, to tion of science-ready data products with which the special topic of the meeting the current instrument pipelines. In the United Kingdom Jacco van Loon was devoted (see below). Users also following general discussion, the UC re- Chile Wolfgang Gieren show great interest in the plans for the ported the deficiencies perceived by the future of the La Silla site and telescopes. users in the data processing tools cur- On the other hand, the degree of user rently made available by ESO and, for the satisfaction with the instrument manuals future, expressed its support for the ESO and online observing documentation, Reflex model developed by Sampo.

In the VLT control room.

ESO Annual Report 2007 35 Instrumentation

The first generation of VLT instruments was completed with the final commissioning, science verification and start of operations of the ESO-built high-res olution infrared spectrograph CRIRES on UT1, Antu, in April. The first refereed scientific papers have already appeared in print and an upgrade to incorporate polarimetry is still planned.

A number of other VLT instruments on Paranal were also upgraded, including the first to be offered in 1999, FORS1, which received a new and larger mosaic of CCDs and filters from Garching. To- gether, these have yielded a sensitivity gain of more than a magnitude in the ultraviolet. Looking to the future, this upgrade also means that the FORS1 detector has the same 4k × 4k format as that in FORS2 and will be interchangeable with it once X-Shooter replaces FORS1. VISIR, the longest wavelength infrared instrument at the VLT was also retrofitted with a new set of filters designed for the optimum study of silicate dust features. Meanwhile, attempts continued to place a development contract for new, larger and better detectors for VISIR.

One of the highlights of 2007 was the successful installation and commissioning of the ESO-built HAWK-I infrared imager on Yepun, the fourth Unit Tele- They fully demonstrate the anticipated Full field 7.5 × 7.5 arcmin HAWK-I com- scope (UT4) of the VLT. In August, the first combination of high resolution and high posite image (J, Brg, K) of the Taran- tula Nebula in the Large Magellanic commissioning run went very smoothly, sensitivity over a field of 7.5 × 7.5 arc- Cloud, whose location in the southern with the instrument meeting most of its min, which is nearly an order of magni- sky was one of the motivations for the scientific specifications from the start. In tude larger than provided so far by the founding of ESO. particular, the image quality proved to be workhorse ISAAC instrument. One re- excellent (seeing-limited down to 0.2 arc- maining problem to be solved is the un- sec) over the entire field of view and the expectedly high vibration produced by total throughput was, as expected, about its closed cycle coolers, which is not a 50–60 % depending on the waveband. problem for HAWK-I but does disturb the One of the few aspects out of specifica- use of the telescope for adaptive optics tion was the flexure, but that was solved and interferometric observations. relatively quickly by adding additional stiffening to the cold structure supports, which has yielded motions of less than two pixels over a full 360-degree rotation. Commissioning and science verification observations were distributed over three runs in 2007 and the start of regular operations is planned for April 2008. Some excellent science verification data on cosmological deep fields, galaxies and Right: The new wide-field infrared imager HAWK-I installed on Yepun, UT4 star-forming regions have already been of the VLT. The image on page 34 was obtained and made publicly available. also obtained with HAWK-I.

36 ESO Annual Report 2007

MAD at the Nasmyth focus of UT3, Melipal. The technique of multi-conjugate adaptive optics (MCAO) has been verified on sky for the first time with MAD, the MCAO Demonstrator. MCAO is used to provide adaptive optics (AO) correction over a much wider field of view than conven- tional adaptive optics. It achieves this by a tomographic reconstruction and correction of the turbulence profile of the atmosphere above the telescope. MAD uses two different methods of wavefront sensing (one using three reference stars, the other using up to eight) to produce spectacular diffraction limited images with homogeneous image quality distribution. MAD also tested the Ground Layer AO technique, a mode to improve the natural seeing which turned out to provide better correction than expected. MAD has demonstrated the potential of these techniques for the VLT and the E-ELT. following commissioning and science (NGC) developed jointly by the Optical Commissioning was successfully com- verification. and Infrared Detector Teams. This system pleted of the Laser Guide Star Facility already outperforms the old IRACE sys- (LGSF), which has started regular opera- KMOS is another ambitious second-gen- tem in the infrared and NGC controllers tions at Paranal. The LGSF is a collabo eration instrument for the VLT, contain- are now under development for MUSE ration between ESO, MPE (Garching) and ing 24 Integral Field Units (IFUs) each in- and SPHERE and new technology (elec- MPIA (Heidelberg). Both SINFONI and dependently deployable over a 7.2 arcmin tron multiplier) CCDs for GALACSI and NACO are now routinely operated in LGS field of view by means of robotic arms GRAAL in the Adaptive Optics facility (see mode and have started producing impor- operating in a cryogenic environment. below). tant astronomical results. The IFUs feed three spectrographs that cover the infrared ZJHK bands with spec- With more than 60 cryogenic stepping X-Shooter, the wide-band UV-IR spectral resolving powers of approximately motors, robotic R-theta arms, and a trograph and first of the second-genera- 3 500. On the ESO side this will be the requirement for precision movements, a tion VLT instruments, made excellent first instrument to be equipped with one critical issue for KMOS is reliability. ESO progress in 2007. ESO delivered the CCD of the New General detector Controllers is therefore interacting more closely than and infrared array detector systems to the consortium partners for integration in the subsystems under their responsibility. After installation and testing in the respective opto-mechanical subsystems, the French, Danish and Italian contributions have been delivered to ESO, where they will undergo further testing. The near-infrared spectrograph has seen first light in the laboratory in the Netherlands. Beta versions of the observing software, exposure time calculator and physical model have been released and are routinely used within the consortium. Data reduction software routines that take account of the specific instrument characteristics and data format have been defined and were partly coded and tested. First light is expected in September 2008, On the left: 20 × 20 arcsec K-band seeing-limited and it is planned to offer the instrument image (0.5 arcsec) of w Centauri obtained with ISAAC. Right: the same field observed with the to the community as soon as possible Multi-Conjugate AO demonstrator (MAD), which achieved a FWHM of 0.090 arcsec.

38 ESO Annual Report 2007 usual with the consortium to achieve this, including the organisation of a particularly demanding series of sub-assembly reviews which culminated in the formal Final Design Review in September. Despite excellent progress and an appar- ently solid design, the formal closure has been postponed to the first half of 2008 to allow time to complete some outstanding prototype testing of the robotic arms and IFUs.

2007 was an important year for MUSE, the second-generation VLT optical integral field spectrograph. This instrument, being developed by a French/German/ Swiss consortium led by the Observatoire de Lyon, will slice a 1 × 1 arcmin field between 24 spectrographs and will be assisted by the GALACSI adaptive optics module (provided mostly by ESO as part of the Adaptive Optics Facility) to achieve the highest possible throughput. MUSE successfully passed its Preliminary and The Adaptive Optics Facility (AOF) is the MUSE prototype image dissector array (IDA; left) and Optical Final Design Reviews (PDR and upgrade of the UT4 telescope of the focusing mirror array (FMA; right). The IDA is made of 24 thin (1-mm width) off-axis spherical mirrors and OFDR) thus paving the way for the early VLT to an adaptive telescope. This implies the FMA of 24 rectangular off-axis spherical mirrors. procurement of a prototype IFU (image replacing the existing secondary mirror Although this is half of one of the 24 MUSE slicers, slicer plus spectrograph optics). Under unit with a new deformable mirror and AO it is already the largest slicer of this type ever manu- direct ESO responsibility, a prototype 4k modules for HAWK-I and MUSE. These factured. × 4k detector has been ordered (the first modules will determine the effect of the of this size at ESO) and an open tender atmospheric turbulence through the anal- for procurement of the remaining ones ysis of the light from four artificial laser was issued. A fundamental milestone for stars, and correct for it by driving the de- the project was the production of a pro formable mirror. The AOF design has pro- Phase A studies which commenced in totype of the image slicer. Composed of gressed in 2007 to the successful Final 2006 for three proposed second-genera- 24 slices and 24 focusing mirrors, it was Designs of the 1.1-m Deformable Second- tion VLTI instruments, namely GRAVITY produced by Winlight and fulfils the tight ary Mirror and of the Ground Layer Adap- (high-precision near-infrared astrometry, MUSE specifications although each final tive Optics system (GRAAL) for HAWK-I. with the Galactic Centre as prime scien- slicer will be twice as large. A parallel tific goal), MATISSE (a mid-infrared imag- study for a metallic slicer is also being Work has continued in 2007 on the devel- ing and spectroscopy successor to the pursued as a back-up. opment of fibre lasers for future LGS sys- MIDI instrument) and VSI (near-infrared tems, in particular towards the 4LGS Fa- imaging and spectroscopy using up to six One of the most interesting astronomical cility of the AOF, and in preparation for telescopes), were completed in 2007. The results of the last few years has been the E-ELT. As part of this work, a method results, including the science cases and a the discovery of hundreds of planets to achieve high-power Raman amplifi summary of the ESO interface and other around other stars (HARPS at the La Silla cation maintaining a narrow line width has considerations were provided and pre- 3.6-m telescope being one of the most been developed and is being patented. It sented to the STC at their October 2007 successful instruments for this). The ex will be transferred to industry to foster meeting. The three instrument consortia istence of these planets is determined in- further research in the area of fibre lasers. also presented their concepts at the “Sci- directly by observing the radial velocity ence with the VLT in the ELT era” work- variations they produce on their parent shop, held just before. The STC recom- star. The VLT Planet Finder, SPHERE, will mendation, based on the above but also use extreme adaptive optics to obtain on the need to phase and coordinate ac- images, polarimetry and spectra of plan- tivities with the PRIMA deployment in ets, allowing direct observations. In 2007, Paranal, is to proceed immediately with SPHERE passed its preliminary design GRAVITY and MATISSE and more slowly review. The deformable mirror with the with VSI. This also implies some exten- world largest number of actuators (1377) sion of PRIMA to all telescopes, as well has been delivered by industry. as the study and realisation of a 4–6-way

ESO Annual Report 2007 39 Fringe Tracker. These recommendations European Extremely Large Telescope concept, and on a first assessment of the were positively endorsed by the ESO resources which might be available for Council at its December 2007 meeting The European Extremely Large Telescope the instrument development within the and are currently being implemented. (E-ELT) project is very much based on the E-ELT Programme. Following approval by heritage of the ESO Very Large Tele- Council of the Phase B study, a detailed The workshop on “Science with the VLT scope. The VLT started operation in 1999 plan of E-ELT instrument studies was fi- in the ELT era” held in Garching in Oc and, with its arsenal of 11 instruments per- nalised in April 2007 in discussion with tober was organised to provide another manently online at the Unit Telescopes, the STC. As foreseen in this plan, ESO opportunity for the ESO community to two at the VLTI combined focus, and a launched in 2007 six Phase A studies on debate the future use of the VLT/I and its Visitor focus, has proved to be the most instruments and one on a complementary instrumentation needs approximately a powerful facility for ground-based astron- post-focal Adaptive Optics system. Exter- decade hence when ALMA, JWST and, omy at optical and infrared wavelengths. nal consortia are studying a Wide Field, hopefully, a European Extremely Large In the case of the VLT, an Instrumenta- High Angular Resolution Camera; a Sin- Telescope will also be operational. A very tion Plan Proposal was distributed to the gle Field, Wide Band Spectrograph; and large attendance, oversubscription of community as early as 1989 and this ap- a Wide Field, Multi IFU, NIR Spectrograph presentations and several extremely lively proach, with corrections and upgrades with a distributed AO system (MOAO) and discussion sessions testified to the inter- introduced on the way, has been very ef- a Multi-Conjugate Adaptive Optics modest in future second-generation VLT/I in- fective in developing a coherent set of ule. Furthermore, ESO is leading institutes strumentation and to the scientific syner- very successful instruments in collabora- in different member states in the studies gies and complementarities anticipated tion between ESO, universities and insti- of a High Resolution, High Stability Visual between these major facilities with Euro- tutes in the ESO member states. Spectrograph and of a Planetary Imag- pean participation. ing Camera with an associated, very high The proposal for the E-ELT Phase B Strehl, AO module. A call for proposals At its meeting shortly afterwards the study presented to Council in December for a study of a mid-infrared instrument STC not only recommended proceeding 2006 contained an overview of the instru- has been also distributed with the goal of with the VLTI instruments mentioned ments of highest scientific priority based selecting a consortium in 2008. above (which originated from an earlier on the work of the ELT Science and ELT workshop in 2005) but also with a high- Instrumentation Working Groups, on the The reports of these studies, due in win- resolution spectrograph at the incoherent parallel Instrument Small Studies carried ter 2009, will include the simulated sci focus of the VLT plus a variety of possible out under the FP6 ELT Study, on the de- entific capabilities, a discussion of the other instruments including (a) new multi- sign work at ESO for the 42-m telescope unique advantages with respect to instru- object spectrograph(s). mentation at 8-m telescopes and of the synergies with ALMA and the JWST, At ESO, various background technical the cost and the required FTE effort to developments essential for future projects build the instrument, and a construction also progressed. In the area of detectors, schedule. These data will eventually be apart from the systems delivered to spe- the basis for the choice of the first-gener- cific instruments mentioned above, work ation instruments and will be used to continued to test an ASIC (acquisition prepare the technical specifications and system on a single chip), prototype AO the Statement of Work of the construc- sensors, such as CALICO and near-infra- tion agreements. red HgCdTe electron photo avalanche a r r a y s .

Workers are busy at the ALMA OSF, where several antennas already arrived.

40 ESO Annual Report 2007

Atacama Large Millimeter/submillimeter Array

The intersection of the Chilean highway 23 and the ALMA road, with the completed gatehouse. The Atacama Large Millimeter/submillimeter Array (ALMA) is a highly sensitive, high-resolution array of telescopes. Once completed, the ALMA observatory will operate 54 antennas of 12-metre diam eter and 12 antennas of 7-metre diameter in an interferometric mode. All antennas will be equipped with seven receiver bands, with the possibility to install three more receiver bands, thus covering the frequency range from 30 GHz to 950 GHz (or, roughly, 0.3 to 10 mm).

Site construction work

The ALMA Observatory will be operated at two sites. There will be the base camp – the ALMA Operations Support Facilities (OSF) – for the everyday, routine operations of the observatory. Built at an altitude of 2 900 metres, it will not only serve tance of 15 kilometres to the OSF. The any given time. Most of these workers as the location for operating the Joint road then continues another 28 kilome- were involved in the construction of the ALMA Observatory (JAO) but also as As- tres to the AOS. This access road is OSF Technical Facilities. sembly, Integration, Verification and Com- up to 14 metres wide since it will be used missioning (AIVC) station for all the high to move the completely operational In August 2006 ESO signed the contract technology equipment before moving it to antennas from the OSF to the AOS. The for the construction of the OSF Techni- the Array Operations Site (AOS), located gatehouse, at the intersection of the cal Facilities with a projected completion at 5 000 metres altitude. Because of the ALMA road with the highway, was com- date of the end of January 2008. During harsh environment, operations at the AOS pleted in 2007. 2006 and 2007 the OSF technical build- will be limited to an absolute minimum. ings were constructed. No major prob- The AOS Technical Building will house The OSF is a facility which serves differ- lems or delays occurred during the con- the antenna data outputs and the Corre- ent purposes and which will host a vari- struction period and some buildings of lator. Digitised signals received from the ety of activities over the duration of the the entire OSF complex were already pro- radio antennas will be processed there project. During 2007 the camp accom- visionally accepted by ESO before the and further transmitted to data storage modated all ALMA Site contractors and end of 2007. facilities located at the OSF. their staff. Personnel lived in the tempo- rary camps and worked either at the During the next years the OSF will be- The OSF and the AOS are at a remote lo- OSF or at the AOS. Work was organised come the central point of all antenna cation and cannot be accessed by public in periods of 19 working days, followed assembly and AIVC activities. Antennas roads. Therefore the ALMA project had by 11 days rest. The camps were laid out, will be assembled at the OSF area in to construct an access road. It leads first including the necessary infrastructure, three separate zones, one each for the from the Chilean highway 23 over a dis- to accommodate up to 500 workers at antennas provided by North America (Vertex), Japan (Melco) and Europe (AEM The OSF facilities. Consortium). AIVC activities will be carried out at the OSF after preliminary acceptance of the antennas, and prior to moving them to the AOS. The corresponding zones for Vertex and Melco have been completed. The AEM zone is, as scheduled, in preparation and will be completed in the first quarter of 2008.

44 ESO Annual Report 2007 Supplying energy for an isolated observa- Inside the AOS Techni- tory at altitudes of 2 900 and 5 000 me- cal Building. tres in the Chilean desert of Atacama is not at all trivial. Initially, it was planned to generate power for the OSF and AOS using dual-fuel (natural gas and diesel) generators, installed at the OSF premises. This scheme was expected to be the most cost efficient and reliable for the required power demand of about 8 MW. However, during the last years energy supply and prices have rapidly and dras- tically changed. Chile proved to be short of natural gas availability. Power generation based on diesel supply only is very costly and, in consideration of an expected operation time of 30 years, not af- fordable. In view of these developments The antennas review scrutinised the complete design on the energy market, ALMA decided with particular emphasis on the design to change the baseline configuration for Activities of this ALMA sub-project fo- changes with respect to the prototype, the power supply of the observatory and cused on the design, manufacture and on which the AEM serial antenna design move forward using electricity provided assembly of antennas and two antenna is based, which was extensively tested by Northern Chilean electricity suppliers. transporters. at the ALMA Test Facility in Socorro (USA) This scheme requires the erection and during the first phase of the project. operation of an overhead power line from At the end of the year 2005 ESO had Consequently, any relevant technological the best-suited electricity generator to signed a contract for the design, manu- choice deviating from the antenna pro the OSF and further on to the AOS. In facture and transport of 25 antennas of totype had to be validated by appropriate 2007 ALMA released a call for tender for 12-metre diameter with the Alcatel Alenia qualification tests, which were also re- the construction of an overhead line to Space, European Industrial Engineering, viewed at the PPDR. Numerous ALMA provide electrical power to the OSF site. and MT Aerospace (AEM) Consortium. experts, either responsible for the an- Technical documentation for the power In the course of 2007 the corporate name tenna manufacture or involved in interfac- supply within the ALMA premises from of Alcatel Alenia Space was changed to ing with the antennas, participated in the OSF to the AOS is under preparation. Thales Alenia Space without any contrac- the PPDR. The review conclusions on the tual consequences regarding technical design were positive and no issue was The construction of the AOS Technical specifications, schedule, price, contrac- found preventing the AEM Consortium Building, a project to be delivered by the tual terms, etc. During the year 2006 from proceeding to manufacturing. North American partner in ALMA, was work carried out under this contract was completed at the end of 2007. centred on conceptual studies, simula- In the months following the PPDR, the tions and detailed designs. This work was AEM Consortium finalised the manufac- carefully and extensively reviewed at the turing drawings and optimised the man Pre-Production Design Review (PPDR) ufacturing process in view of the serial held in February 2007 in Venice. This manufacturing. AEM selected key suppli-

Key suppliers for the major subassemblies of the AEM antennas

Component Supplier Steel Structure Asturfeito (Spain) Carbon Fibre Receiver Cabin Multiplast (France) and Jallais (France) Backup Structure Duqueine (France) Reflector Panels Media Lario Technologies (Italy) Adjuster Heads RUAG (Switzerland) Subreflector Mechanism Physik Instrumente (Germany) Quadropod Legs Xperion (Germany) Linear Motors Phase Motion Control (Italy) Control System Microgate (Italy) Pre-Assembly of First Antenna Asturfeito (Spain) On-Site Antenna Assembly DSD (Chile)

ESO Annual Report 2007 45 ers for the major subassemblies (see box Assembly of the first on previous page), and manufacturing ac- Backup Structure. tivities started in late spring.

In the second half of the year, the ESO antenna group concentrated efforts in following the production closely, monitoring progress and ensuring that the experience gathered with the prototype was fully used. The schedule of the serial production foresees the delivery of three antennas every four months from 2009 onwards. To achieve this production rate various Carbon Fibre Reinforced Plastic moulds and jigs were designed, fabri- cated and qualified, in particular for the fabrication of the Receiver Cabin and the Backup Structure. By the end of 2007, be used for transporting antennas at the time of the special, large size tires, which the construction of the first cabin was two ALMA sites, the OSF and AOS. were foreseen in the original design. The approaching completion and the next use of smaller and more easily available two cabins were in different stages of In January the Final Design Review of the tires demanded a complete rework of the production. Assembly of the first Backup antenna transporters was held at the site vehicle architecture. Structure has started and a few of the of the manufacturer, Scheuerle Fahrzeug- 16 individual slices have been assembled fabrik GmbH (Germany). This review con- Further design challenges were imposed together. The main parts of the steel cluded the design phase during which by the requirements related to preci- structure for the first antenna have been the concept of the transporters had to be sion driving when approaching the anten- manufactured and assembly and inte substantially changed. This was neces- nas, as well as to the lifting and position- gration has started. In spring 2008 the sary in response to the too long delivery ing processes of the antennas on the first structure and the first receiver cabin will be assembled at Asturfeito and af terwards shipped to the OSF. The first Backup Structure will be test-assembled elsewhere and shipped separately to the site. Production of the subsequent units is proceeding well. Steel for the first batch of antennas has been cut. Panels and adjusters for three units have already been produced and other parts (quadropod legs, subreflector, motors, etc.) are in serial production.

Preparation at the OSF to support the integration of the antennas is well advanced. The site has been graded flat and five antenna foundations have been prepared. The AEM consortium will start work at the site in the beginning of 2008, starting with the assembling of tempo- rary facilities, in particular the hangar foreseen for mounting the Backup Struc- ture, the panels and the apex structure. Delivery of the first antenna is planned for the end of 2008. Loading the ALMA antenna transporters on a barge for further trans- The other major construction activity fol- port to Chile. lowed up by the ESO antenna group concerns the design, manufacture, assembly and transport of two special vehicles to

46 ESO Annual Report 2007 stations. Precision driving is achieved by Design activities of major sub-assem- the implementation of various steering Most important Front End contracts blies, e.g. the Band 7 (270–373 GHz) and modes, including sideways steering that signed in 2007 Band 9 (620–702 GHz) receivers, were allows these vehicles of 20 metres length finalised by passing the major ‘Critical and 10 metres width to move in an ex- – Supply of 45 Cryostats by the Sci- Design Reviews’ (CDRs). During these tremely compact space. The addition of ence and Technology Facilities Coun- CDRs a thorough and formal assessment positioning lasers, an anti-collision sys- cil/Rutherford Appleton Laboratory was made of the design of a sub-assem- (RAL), near Didcot, UK; tem and numerous cameras guarantees bly by a review panel composed of inter- – Supply of 48 Band 7 cartridges by a safe approach to the antennas even nal and external experts. After successful the Institut de Radio Astronomie when they are positioned in the compact Millimétrique in Grenoble, France; completion of the CDR the design was array. The lifting and positioning system – Supply of 48 Band 9 cartridges by frozen for series production. The Band 9 of the antenna is based on a fail-safe, re- the Nederlandse Onderzoekschool cartridge CDR was held on 6 and 7 Feb- dundant system where a large X-Y table Voor Astronomie in Groningen, the ruary and the Band 7 cartridge CDR was is fastened to the antenna, then lifts the Netherlands; held on 8 and 9 August. antenna using the hydraulics suspension – Detailed design and delivery of of the vehicles, and brings it to the final 53 Water Vapour Radiometers oper- During the year, ESO signed several pro- position using hydraulic-driven lifting ating at 183 GHz to be supplied by duction and integration contracts for ramps. Omnisys Instruments AB in Gothen- the manufacturing and delivery of Front burg, Sweden; End sub-assemblies, for a total value Manufacturing of the first vehicle was fin- – Supply of 198 cryogenic amplifiers of approximately 40 M€. All of these con- ished in September, while the second unit operating between 4 and 8 GHz to be tracts were signed after the successful supplied by Tecnologías de Tele- followed closely thereafter. In October conclusion of the pre-production. At the comunicaciones y de la Informacíon and November a complete programme of end of 2007, ESO has accepted eight in Santander (Cantabria), Spain; testing was performed at the factory. – Supply of 198 cryogenic amplifiers cryostats, eight Band 7 cartridges, eight These tests included moving a concrete operating between 4 and 12 GHz to Band 9 cartridges, 42 cryogenic ampli structure of the same weight and size be supplied by the Fundación General fiers for Band 7 and 18 cryogenic amplifi- as an antenna from a foundation specially de la Universidad de Alcalá/Observa- ers for Band 9. constructed for these tests at the manu- torio Astronómico Nacional in Alcalá facturer’s premises. Tests were also car- de Henares (Madrid), Spain. Substantial progress was made on es- ried out proving the braking power of the tablishing the European Front End Inte- transporters, simulating high altitude and gration Centre (EU FEIC). Several options, slope conditions. The test programme and bandwidth, could be achieved. In including having an EU FEIC in Garching, was formally concluded by the ‘Factory 2007 further evidence was provided that were investigated. After a careful assess- Acceptance Review’, held successfully on this exceptional performance could also ment and consultation with the ESO 29 November. Afterwards, the transport- be achieved in a repeatable and control- and ALMA management, it was decided ers were dismantled and transported by led way for the larger quantities — more to set up the EU FEIC at the Rutherford trucks to the Heilbronn harbour. There than 70 units — which must be con- Appleton Laboratory (RAL), near Didcot they were loaded on a barge for further structed for ALMA. in the UK. The FEIC activities require a transport to Antwerp (Belgium), and load- very close involvement of ESO in the EU ing onto the ship to Chile. The ship left for Chile at Christmas and arrival at the OSF site is foreseen for mid-February 2008.

The Front End

The year 2007 was a landmark for the European Front End tasks under the responsibility of ESO, showing significant progress in the transition from the design phase, including pre-production, to the full series production phase.

ALMA receivers have a major influence on the performance and quality of the ALMA system. In previous years it had already been proven that the demanding performance, especially the sensitivity Band 9 pre-production cartridges.

ESO Annual Report 2007 47 FEIC for technical and programmatic NAOJ, by 2011 at the latest. The under In order to support the activities related matters. Therefore it has been agreed to lying reason for this acceleration of pro- to the optical components’ manufactur- appoint a dedicated EU FEIC work pack- duction is to keep up with the project an- ing, assembling and testing, a facility was age manager within the ESO ALMA Divi- tenna delivery schedule. set-up in the ALMA building at ESO. It sion, who will be located permanently is a fully equipped electro-optical labora- at RAL to direct, in close collaboration tory that will enable the thorough testing with the local RAL manager, and oversee The Back End and quality evaluation of the various op- the activities at this integration centre. toelectronic components, and in the long After approval by the ESO Finance Com- The ALMA Back End (BE) system en term, support the remote maintenance of mittee, the contract for the set up and compasses a wide variety of different the ALMA observatory equipment. integration of 26 Front End assemblies electronic modules to be produced in rel- was signed in October. The kick-off meet- atively large amounts. Each antenna is ing for this activity was held on 22 and equipped with two electronics racks, im- The correlator 23 November at RAL. plementing the ‘Antenna Back End’, while several racks are installed in the AOS After extensive tests in the laboratory the In the framework of an EC FP6 project Technical Building to implement the ‘Cen- first parts of the ALMA correlator are led by ESO, “Enhancement of ALMA tral Back End’. now ready to be shipped and installed on Early Science” (E-ALMA), further progress the site. The delivery of the first of four was made in the Band 5 (163–211 GHz) The Antenna Back End performs the quadrants is planned for the beginning of receiver project. Chalmers University’s frequency down-conversion of the sig- 2008. The assembly of the second quad- Onsala Space Observatory in Sweden nals transmitted by the Front End receiv- rant is almost complete. continued with the detailed design of this ers as well as their digitisation and trans- receiver. Following the earlier discussion mission to the AOS Technical Building Each quadrant includes 128 Tunable Filter with RAL about the Band 5 local oscilla- through fibre optics. The Central Back Bank (TFB) electronic modules, devel- tor, RAL submitted a formal proposal to End provides the timing signals to the oped and manufactured by the Observa- ESO. This proposal described the design whole array, the fibre management and tory of Bordeaux (France), under an ESO of a suitable oscillator circuit, compatible the reception of the signals coming from contract. with the ALMA Front End concept, and the antennas. In total there will be 112 An- the delivery of six units. Based on this tenna Back End Racks and 20 Central After an initial period necessary to under- proposal it was decided to include RAL Back End Racks. stand the high complexity of the TFBs as a participant in the E-ALMA pro- and to implement the European Commu- ject. A kick-off meeting, with participation During 2007, all the components of the nity’s directive on the “Restriction Of of ESO, Chalmers and RAL delegates, ALMA Back End underwent final de- Hazardous Substances” (ROHS), the pro- for this essential component was held on sign, pre-production and validation tests duction has reached a steady state 18 December at Chalmers University in both in the laboratory and at the Antenna with yields in excess of 95 %, an ex- Gothenburg, Sweden. Test Facility (ATF) in New Mexico. Most tremely high yield taking into account the of the Back End equipment has been complexity of the devices. In June, ESO and the National Observa- successfully prototyped and by the end tory of Japan (NAOJ) signed a Collabo of 2007 was moving towards the produc- rative Agreement in which ESO will ex- tion phase. The status was reviewed at tend the quantity of units which ESO is the Back End production workshop held The Tunable Filter Bank already procuring for its own needs, in in November. Consequently, all Euro- order to also cover the needs of NAOJ to pean production contracts, except one, The Tunable Filter Bank (TFB) is an ex- outfit their antennas with identical equip- were approved and are progressing as tremely complex piece of electronics ment. Subsequently, there has been a planned. The only outstanding Back End using the latest generation of Field Pro- close interaction between ESO and NAOJ series production contract concerns the grammable Gate Array chips to implement thirty-two 125 MHz digital filters. defining all Front End products, includ- procurement of the photomixers, and is, Each chip contains the equivalent of ing schedule. By the end of the year, ESO as scheduled, expected to be placed in several million logic gates and has more had already ordered the first Front End 2008. than 700 Ball Grid Array connections; products for NAOJ. sixteen of such chips are mounted on The delivery of Back End components to one 12-layer TFB printed circuit board. In November, in close collaboration with the ALMA site began in December with the JAO management and institutes in- the shipment of the ‘Test Racks’ that will volved, ESO started to investigate options allow testing of incoming components. to accelerate the series production of The shipment of the first pair of ‘Antenna Front End components. The aim was to Racks’ is scheduled for the early months complete all European Front End produc- of 2008. Subsequent antenna racks tion tasks, including those additional are planned to arrive on a timetable which deliveries for the ALMA Compact Array to tracks the delivery of the antennas.

48 ESO Annual Report 2007 Screenshot of the ALMA operator’s console, as used at the ATF with the two prototype antennas and also at the Operations Support Facility for the antenna tests in Chile. The panel shows one of the many that are nor- mally displayed on three operator con- soles. In parallel with the manufacturing of the TFB modules, the optimisation of the firmware continued to identify algorithms and implementations that reduce power dissipation. In fact, due to the low air density at the AOS, the power dissipation is a major concern since the temperature of the devices is directly related to their lifetime. Simulations, analysis and oper ational testing in the correlator station racks show that, with the latest digital filter implementation, thermal stresses are well within boundaries and guarantee a suitable lifetime of the components at the AOS.

In addition to the main correlator, a down- scaled version (referred also as the ‘two- antenna correlator’, since it can correlate only the signals coming from two antennas) has been developed and two units have been manufactured to support the The main achievements made by the End was finalised and the report issued. test activity at the ATF and at the OSF Software Development team during 2007 The analysis confirmed the design and sites, respectively. Due to the modular ar- are: will be used to predict the science per- chitecture of the correlator and to the fact – First delivery of the end-to-end soft- formance and help define the calibration that the same boards are used, the two- ware capable of performing Optical procedures. The ALMA Product Assur- antenna correlator did not require a sig- Pointing and Holography, as validated ance (PA) was specifically analysed at the nificant design effort. The first unit was in- at the ATF and required for the com- review meeting and during the different stalled at the ATF in the course of 2007 missioning of antennas at the OSF; equipment acceptances. Specific PA au- and is currently in use, while the second – Support of the achievement of the so- dits were also done. one is being shipped to the OSF where it called ‘First Fringes’ (basic interfer- will be installed at the beginning of 2008. ometry mode) at the ATF in the spring The management of the ALMA Test Fa There it will be used to test antennas and and achievement of stable dynamic cility (ATF) was handed over to the com their equipment on the sky before reloca- fringes (including automatic delay puting Integrated Project Team (IPT) in tion to the AOS. tracking) in autumn; September and it was decided to leave – Intensive use of the ATF as a platform the ATF operational until June 2008 to to test the software; continue software development, commis- Software Development – Support of the acceptance tests per- sioning and system testing. formed by the Japanese ALMA team The ALMA Software has been planned for their first antennas at the OSF. Activities in AIVC in Chile increased sub- and developed from the beginning as an stantially in 2007. More than 20 addition- end-to-end system including proposal al people were hired, including the head preparation, dynamic scheduling, instru- System Engineering of the group, and more than 30 people ment control, data handling and format- are now working for AIVC. Training for the ting, data archiving and retrieval, auto- The project-wide requirements and Inter- newly hired staff is ongoing. Work fo- matic and manual data processing, and face Control Documents are now 95 % cused on the AIVC infrastructure needed support for observatory operations. and 89 % completed, respectively. Front for equipment acceptance and the inte- End and Back End requirements were gration work. The holography system and Work in Europe is organised through formally released in line with system and the optical pointing telescope were ac- ESO, with many software packages being science requirements. The requirements cepted. They are essential tools for an- developed by ESO in collaboration with database DOORS is kept up to date and tenna acceptance. First holography maps European institutes which have experi- used for verification and acceptance. for the antenna procured by NAOJ show ence and qualified staff to develop and Support was given to all Integrated Pro- promising results. test the required software. ject Teams (IPTs) for their technical activities. ALMA system block diagrams and the sensitivity budget were further refined and used for system design trade-offs and analysis tasks. The ALMA optical detailed analysis for antennas and Front

ESO Annual Report 2007 49 Science Activities The European ALMA Regional Centre essential in order to make the software One of the major highlights in 2007 as available for regular scientific use, at a suffi- far as science activities are concerned The mission of the European ALMA Re- ciently early stage that the pipeline system has been the support of the software and gional Centre (ARC), set up in mid-2006, is can be developed. Furthermore, getting hardware tests at the ATF in Socorro, to provide the science and technical sup- acquainted with the software at an early which culminated with the achievement of port services necessary for the European stage will help train the ARC staff who will user community to exploit ALMA to its full take part in the commissioning and first as- first fringes on planets in spring and dy- scientific potential. The ARC will form the tronomer-on-duty shifts in Chile. namical interferometry on quasars in the interface between the ALMA Observatory second half of the year. in Chile and the European user communi- During 2007, the ARC staff actively partici- ty. Similar ARCs are currently being es pated in user tests organised by the de The staff of the science IPT is currently tablished in North America and East Asia, velopers of the offline data reduction sys- ramping up to ensure that a fully func- ESO’s partners in the trilateral ALMA pro- tem (CASA). The various ARCs form the tional commissioning team will be availa- ject. For European users, the ARC is be- primary point of contact for the users and ble in Chile for the start of the commis- ing set up as a cluster of nodes located testers of the offline software. A main con- sioning activities in 2008. throughout Europe, with the main coordi- tact astronomer at ESO, together with nating centre at the ESO headquarters three additional astronomers consisting of In September two major events were in Garching. In this distributed network, ARC node staff and ESO Fellows, operate organised at ESO in Garching: the “ALMA user support and operations experience at as ‘user support specialists’. They are the Community Days” and the “Surveys for ESO can be mixed with millimetre-wave interface between the users and the de ALMA” workshop. At the ALMA Commu- astronomy experience that exists in the velopers, collecting feedback from the community, to create optimal science sup- users and organising it in a useful way for nity Days the European astronomers port services. the developers. The ARC staff also partic were informed about the progress of the ipated in user tests of the ALMA Observing ALMA construction and the current plans At present, one of the main activities of Tool and the archive interface, and per- for the organisation of the European the ESO ARC is to test the main user-soft- formed in-house testing of the offline sys- ALMA Regional Centre. During the “Sur- ware system. This early involvement is tem. veys for ALMA” workshop the status of plans for large preparatory surveys for ALMA, and in particular the role of Her- schel and APEX, were discussed. The community showed a strong interest and is engaged in a vigorous preparatory plan to maximise the scientific potential of An example of the viewer, part of the the ALMA observatory when it becomes offline data reduction software CASA currently being developed for the available. analysis of ALMA data. The viewer is very flexible in showing images and data cubes, as well as raw visibilities, and allows interactive flagging.

Right: View from above the OSF.

50 ESO Annual Report 2007

The European Extremely Large Telescope

Following the December 2006 Council The project Mid Term Review (a contrac- tailed design phase, and the results were resolution on the European Extremely tual milestone) was held on 13–14 June consistent with similar studies under- Large Telescope (E-ELT) Phase B design, 2007. Over 40 participants took part; ex- taken by ESO outside the framework of the project was formally launched. A ternal attendees included a representa- the ELT Design Study. Enclosure models number of major contracts were immedi- tive of the European Commission (EC). were tested in wind tunnels, and CFD ately launched through the tendering The EC formally accepted the results of modeling produced useful results, which phase, and preliminary designs have now the Mid Term Review on 22 October may be factored into the eventual design. been developed for the telescope mount, 2007. In parallel with the Mid Term Re- Adaptive optics work proceeded well, the dome and the primary mirror cell. In view, the progress of the project was sub- with detailed designs of hardware com- parallel, longer-term contracts have been ject to a critical review by a panel of ex- ponents (detectors, actuators, mirror tech- placed for the preliminary design and ternal, world-leading experts (Technical nologies), and a potential breakthrough prototyping of the adaptive quaternary Advisory Committee – TAC) in the relevant on the issue of wavefront sensing with mirror and the field stabilisation electro- fields. The TAC Report was received in Laser Guide Stars. Three detailed studies mechanical unit. Towards the end of the July 2007 and was fully supportive of the for instruments were in progress. Site year the tendering and contract award managerial and technical progress that characterisation suffered from accumu- process was concluded for the procure- had been achieved. lated delays but the failing software ment of prototype primary mirror seg- was being fixed, with a view to start syn- ments from two potential polishing sup- Work continued on the APE (Active Phas- chronised and standardised measure- pliers. ing Experiment), which should achieve ments early in 2008. ‘laboratory first light’ early in 2008, with In parallel, a substantial effort has been direct measurements of the 61-segment The E-ELT is part of the ESFRI roadmap undertaken to analyse the performance mirror with the internal metrology sys- of future facilities. As such it is eligible for of the telescope designs, and a con- tem, down to nanometre accuracy. Posi- FP7 support (Preparatory Phase for Con- tract has been placed with Lund Observ- tion (edge) sensors, with nanometre- struction). We submitted such a proposal atory to further develop their integrated accuracy, were delivered. Civil work for in mid 2007. It was accepted and will modeling effort. A number of smaller con- the Wind Evaluation Breadboard also start in January 2008. Unlike the FP6 ini- tracts have been placed to evaluate vari- progressed and the Friction Drive Bread- tiative, ESO is a ‘mono’ partner for this ous technological solutions in the board was being tested. Optical fabrica- initiative, with 25 third-party institutions in area of control and software. Conceptual tion progressed more slowly than de- the member countries as collaborators. studies into novel detectors for the Laser sired, but so far no show-stoppers have The aim of this activity is to complement Guide Stars have also been undertaken. emerged. The enclosure concepts se- the E-ELT Phase B and help to ESO to lected in 2006 went through a more de- be fully prepared for an early 2010 deci- The EC-supported FP6 ELT Design Study sion on whether to start construction. initiative is a partnership between 28 institutes, led by ESO. It started as a design-independent R&D activity to foster industrial preparedness for the construction of an ELT, but was aligned to the E-ELT specifications once the community converged on a common European ELT concept in 2006.

During the first half of 2007, management activities continued to concentrate on improving overall project performance by focusing participant organisations’ efforts on meeting-agreed technical milestones. Steady progress was made across all work packages. As of the end of 2007, over 75 % of the EC grant intended for participant organisations had been distributed to them.

Left: Artist’s impression of a possible E-ELT The Active Phasing design. Experiment.

ESO Annual Report 2007 53 Software Developments

The Software Development Division was System Engineering jects have similar needs for their software created in December 2006 as a merger process, several SED internal tasks of three different software departments, The System Engineering Department started in the course of 2007 to compare with the aim of preparing for the chal- (SED) provides the development teams the current practices and identify the lenges arising from the fact that ESO has with software engineering services, such best one in areas such as version control, become a multi-project organisation. The as the environment and tools to support building, integration, test, metrics, Prob- mission of the new division is to serve the software life cycle, software quality lem Reporting System, and software life the VLT, ALMA and ELT projects and to assurance and control. The department is cycle. A Software Engineering Working maintain a high level of quality while en- also in charge of integrating software Group (SEWG), with representatives from suring cost-effectiveness. Therefore it modules and preparing and validating re- all divisions dealing with software de is clear that the division has to be more leases before they are delivered to the velopment, has been set up and meets than a simple ‘labour shop’ and that it customer. All planned releases of the VLT once a month to provide recommen must create an environment in which re- (VLTSW FEB2007, DFS FEB2007 and dations on the software standards to be sources are optimised and synergies User Portal) and ALMA Software (4.1 and used by ESO projects. It has, amongst promoted and encouraged wherever 5.0) have been successfully validated and other results, produced a document possible. The division is organised around deployed. defining the basic requirements of the three major development departments Software Engineering process at ESO. and a systems engineering department, The department is the result of the merg- which provides services to all developing of three groups of software engineers In order to reduce the impact of new ment departments. involved in different projects (VLT Con- VLTSW releases on Paranal opera- trol, VLT DFS and ALMA). Because pro- tions and in agreement with the Paranal The challenge for 2007 was to build the division while making sure none of our commitments were compromised. A main division objective was to define and op timise the interface to our stakeholders and in particular to the Observatory. With the view of continuing the development and maintenance of the software for VLT/ VLTI, ALMA and E-ELT, and with the three projects in very different stages of their life cycle, we have started to work on a roadmap linking the evolution of the projects’ software. We want to identify common development paths so that the evolution of the more advanced projects can proceed smoothly alongside the choices made in the newer ones. This is made possible by the matrix structure as it allows the involvement, to a limited extent, of team members from all projects in common activities and job rotation and by a comprehensive personnel training and development plan.

SysML is used to model the E-ELT Technology Demonstrator. This picture shows an outline of the model required and of the physical deployment of the system.

54 ESO Annual Report 2007 Software Group, the plan and contents of VLTSW annual releases have been changed. Each release containing new functionalities (e.g. 2007) is followed by one containing bug fixes only (e.g. 2008). Only the latter is deployed at Paranal. In this scheme new features are used inter- nally and debugged for at least one year before they actually enter operations.

Control and Instrument Software

The Control and Instrument Software (CIS) Department is responsible for the design, implementation and maintenance of control and common software for the VLT, VLTI and their instruments, as well as for ALMA and E-ELT. Following a matrix organisational model, the members of the team are assigned to the different projects while they also work together to build a common vision and profit from the synergies that emerge from the different activities. The main control panel of the SHAPS sensor for the active phasing The development of control software for experiment. Superim- the VLT and VLTI is far from being composed are two panels pleted, with many new-generation instru- showing the image anal- ments being constructed or designed ysis of the PYPS sensor and the position of and with major upgrades in core facilities the elements of the ac- such as the multiple laser guide star or tive segmented mirror. the adaptive optics facility being undertaken. For this reason, more than half of the team worked during 2007 on the development of control software for the VLT, work done in the VLT area can thus be lar, the ALMA Common Software (ACS), VLTI and their instruments. Following an considered pure maintenance, while the whose overall coordination is under the annual release cycle to follow up with the rest constitutes new developments. responsibility of ESO and CIS team mem- evolution of control hardware used in bers, is made available outside ALMA as Paranal and by second-generation instru- The ALMA project relies on a consistent a public domain middleware framework. ments, the VLTSW FEB2007 version group of software engineers from the Several astronomical projects, including of the VLT common infrastructure and in- CIS Department. They are involved in the APEX, have adopted ACS as the base for strumentation software was released at Common Software, Control, Executive their Control Systems. A community of the beginning of the year, followed by the and Observation Preparation subsystems users has developed, and a fruitful collab- development of the 2008 release now in with coordination, design and develop- oration with Universidad Técnica Federico its final testing phase in Paranal. Stand- ment roles in collaboration with software Santa Maria in Valparaíso (Chile) is push- ard support for new hardware has been engineers from the partner organisations. ing the diffusion of ACS in Chilean univer- provided, while at the same time new re- More details are provided in the ALMA sities with the effect of training young quirements imposed by the increasing section of this annual report, where the software engineers who can be (and have complexity of the new facilities have been major milestones achieved this year are been) hired by ALMA and other ESO pro- satisfied. The team has played a ma- described. The team members have been jects. jor role in the development of the active heavily involved in missions at the An- phasing experiment (APE), PRIMA, tenna Test Facility in Socorro. In particu- A limited amount of resources has been HAWK-I and other instruments. Also, fol- allocated in 2007 to begin the work on lowing up and consulting external con- the E-ELT software architecture and infra- sortia has been extremely valuable in en- structure, in collaboration with the E-ELT suring uniformity between the different office. Software will play a very impor- developments and in identifying new re- tant role in this project as an integrated quirements. Only a small portion of the part of the system together with mechan-

ESO Annual Report 2007 55 posal Submission System, WebLetters and P2PP through a common login. Most existing applications had to be modified to integrate with the new environment and the actual introduction of the system required a switch-over of the complete support infrastructure at the same time. The ‘big-bang’ happened in November and was very successful as it did not generate any disruption in operations. The project was also an excellent team-building opportunity as it involved not only software engineers developing front-end and back-end software but also scientists and engineers belonging to operation groups and departments. A major challenge for the department was to develop those new applications (including support for survey facilities) while providing support, including implementation of new requirements, to Phase I tools and infrastructure for the two observing periods which started in April and in October. The back-end team continued to con centrate on the development of applications that are critical to the execution of data reduction pipelines and quality control procedures. This includes automatic Elements of the models used in the functional tools for organising, classifying and as specifications for GALACSI, the Adaptive Optics sys- sociating data and executing reduction tem for the MUSE second-generation instrument. Together with the high-level architecture, a use-case pipelines on multi-core computers. diagram and a sequence diagram are shown. Sequence diagrams are extremely valuable in the The involvement of the department in the analysis of the flow of actions in a process. development of ALMA data-flow applications is slowly increasing. In 2007, it was limited to the participation in the develop- ics, optics and electronics. Therefore ACS has been evaluated and considered ment of the ALMA archive. The develop- we are making a contribution to the over- suitable for use in the VLT, although a ment of ALMA Observatory Operations all system engineering and requirement decision on the middleware to be used Support tools will start in 2008 and we capture activities. At the same time, we for the E-ELT is still premature. An E-ELT hope that ideas and concepts from the are collaborating on the definition of the technology demonstrator is now being VLT can be shared with these new tools. Telescope Control System architecture developed to examine promising hard- and on the selection of the technologies ware and software technologies, includ- to be used for the overall software infra- ing ACS, and the ease of integrating them structure. The matrix structure of the seamlessly. department enables it to profit from the experience accumulated in the software development for VLT/VLTI and ALMA. Data Flow Infrastructure

In 2007 the Data Flow Infrastructure (DFI) Department put a lot of effort into the development and deployment of the VLT/ VLTI User Portal (see page 29). The project was challenging both in terms of its technical and organisational impact. In- ternal and external stakeholders can now use single sign-on to access all their web and desktop applications. For instance, a principal investigator can access the Pro-

56 ESO Annual Report 2007 Pipeline systems Elements of the HAWK-I user interfaces. The main panel is the Instrument Control Software Engineer- ing GUI and is shown together with the OS control All ESO pipelines are now based on the panel, a real-time display showing the handling of ESO Common Pipeline Library in order the gaps between the detectors, and the Telescope to facilitate maintenance and sharing Offset Display GUI, used to provide a graphical rep- of functionalities, and have been released resentation of offset sequences. for public use. Many new algorithm and pipeline developments were presented at the ESO Calibration Workshop. Among the new developments, the CRIRES pipeline was finalised and released for oper ations for the P79 observing period. The CRIRES pipeline provides recipes for wavelength calibration and sensitivity of the instrument, as well as for the science reduction procedures.

The HAWK-I pipeline was evaluated during the first commissioning run in Au- gust 2007. This pipeline was developed in-house and closely follows the data processing scheme of ISAAC software imaging. Development has been acceler- ated by reusing CPL recipes from the ISAAC pipeline for single-quadrant tasks. Only a few recipes had to be developed explicitly for HAWK-I to support astrometry/distortion correction and to merge the four individual quadrants into one image. The HAWK-I pipeline is foreseen to be released for operations in April 2008.

A new library, CLIP (Common Library for Image Processing), has been developed as a flexible and scaleable framework to provide an interface between CPL-based data processing capabilities and the instrument acquisition process. CLIP is binding software which includes high-level interface libraries with the control software system, support for the VLT Real-Time Display tool, an image- processing library extending the CPL by common instrument-related functions (e.g. for instrument adjustment such as the X-Shooter hardware flexure measurement), and a standard architecture for instrument-specific plug-ins (e.g. CPL- based recipes for KMOS image reconstruction). The CLIP library has been tested by the X-Shooter and KMOS consortia.

ESO Annual Report 2007 57 Technology Developments

The Technology Division provided engi- Here, we highlight a few examples where They should not only meet the foreseen neering support to over 150 different ESO inter-disciplinary teams from the Technol- performance and environmental require- projects and work packages in 2007, ogy Division have been active in the serv- ments, but they should also have devel- maintaining the record levels of 2006. ice of ESO’s current and future projects. opment potential, and be based on rising While support for VLT operations and up- rather than falling technologies as the grades remains an important background project will only be completed in the next activity, ALMA and second-generation Electronic standards decade and must be maintained through- VLT instruments were the main priorities out its whole operational life. Standards of the division. Electronic standards were an important should also have a broad industrial ac- issue during the construction of the VLT ceptance to allow multi-vendor procure- As well as contributing to these key pro- and were a major contribution to its ment. Even if all these factors are posi- jects, the division has also worked on a widely recognised reliability. With equip- tive, extensive testing and evaluation of large number of preparatory studies and ment provided by dozens of firms and components under the expected environ- developments which have specific rele- institutions, maintenance would have mental and operational conditions at a vance for the technological challenges of been extremely troublesome if each sup- high-altitude observatory are necessary building and operating an extremely large plier selected their own components and to provide assurance of long-term serv- optical telescope. These E-ELT-related standards. Not only would the number iceability. activities have increased rapidly in 2007 of spare parts have had to be greatly in- and will continue to do so. creased, but maintenance and upgrades would have been made more difficult E-ELT Technology Demonstrator Although some of these activities were and the software would also be much funded by the ESO E-ELT Phase-B pro- larger and more error-prone. Now that we The E-ELT Technology Demonstrator programme, a considerable number of other are starting the E-ELT design, it is equally ject, which was started in 2007, is in- studies and developments have been important to establish the minimum level tended to test and benchmark key tech- partly funded through contributions from of technical standards necessary for each nologies available on the market today, the EC Sixth Framework Programme phase of the project. and provide an indication as to their suit- (FP6). The E-ELT Phase-B and FP6 pro- ability for an extremely large optical tele- grammes have involved many European It is obviously still too early to specify all scope and assess the development po- institutions and industries, and the divi- the E-ELT standards; and these will in any tential. sion’s staff have played an important role case evolve as the project develops. Man- in their planning and management, as ufacturers receiving major contracts may The E-ELT, being an adaptive telescope, well as in their execution in some cases. also select standards that will thereafter requires a control system that is far more There has deliberately been a clear syn- become de facto E-ELT standards. But complex than those of previous genera- ergy developed between these activities the process of selecting standards is not tions of telescopes. The initial analyses to allow maximum overall benefit. easy and requires many considerations. of the control system requirements indicate the need for a substantial increase in the number of I/O channels, much faster computers and higher communication bandwidths. In addition, there will be a stronger coupling between subsystems than with previous projects. The advances in technologies that have occurred during the last decade make it reasonable to expect that these goals can be achieved in a cost effective way, with much reduced cost per I/O channel.

Tests will not only be carried out under laboratory conditions, but also under the conditions expected at the future E-ELT observatory. For this, the recently acquired climatic chamber will allow equipment to be tested over the full range of temperatures and humidities that it will eventually be exposed to in operation.

Gas treatment with UV light to improve the quantum efficiency of the FORS1 CCD.

58 ESO Annual Report 2007 Cryo-testing 2 Antenna accelerations without (blue) and with (red) additional damping Electro-mechanical functions that oper- 1.5 system. ate reliably under vacuum and at cryogenic temperatures are another field where development and testing has been 1 carried out by the Mechanical Systems and Electronics departments. The reliabil- 0.5 ity of vacuum-cryogenic functions is extremely critical, as any failure in an op- Acceleration 0 erational cryogenic instrument typically means a week of lost observation time due to the need to warm up the instru- –0.5 ment, repair the function, pump down the vacuum and re-cool. Not only must cryo- –1 genic functions work reliably, they should 0 123456789 also produce very little heat. Some of Time the proposed E-ELT instruments will require very complex cryogenic functions. ALMA transporter damping system out delaying the critical delivery schedule As most commercial components are for these vehicles. not designed to operate at cryogenic During the development of the ALMA temperatures, a test programme was Transporters, it became apparent that Taking the vehicle characteristics calcu- started to evaluate a number of compo- there was a potential danger to the ALMA lated by the manufacturer, dynamic simu- nents such as motors and encoders telescopes if they were transported lations were carried out and analysed to validate them under these conditions. at critical speeds over ‘washboard’ road by ESO experts and a solution was found Even if a product works mechanically surfaces. These surfaces can develop to limit the accelerations to acceptable when cold, the associated drive or inter- rather rapidly on non-metalled roads values. The hydraulic support systems of face electronics may not. These problems such as that connecting the ALMA OSF each of the 14 transporter wheels were and limitations need to be well under- to the high site. Analysis showed that, in fitted with a nitrogen-charged accumula- stood before the components can be ac- the worst case, the accelerations felt by tor and a throttle/check valve. Both these cepted for use in cryogenic instruments. the telescope could considerably exceed components were carefully selected A vacuum cryogenic test facility has been the seismic accelerations for which the and adjusted so that they change the res- developed to facilitate the evaluation of vehicles were designed. Engineers from onance frequency in case of an over- new devices. One particularly interesting the division created a task force to find a load situation and detune the system in product currently being tested is the method of damping such vibrations that order to avoid critical resonance ampli Squiggle motor. These can provide linear could be easily retrofitted to the transport- fications. Additionally, electronic sensors movements of up to 50 mm with a resolu- ers, which were almost complete, with- have been installed to bring the vehicle tion as small as 20 nm. They are not only automatically to a safe stop in such a sit- vacuum compatible and require no hold- uation. ing power, but are very compact – down to 6 mm in length – and could be of potential interest for moving slitlet jaws, for example. Looking at the transporter damping system.

ESO Annual Report 2007 59 Wind characterisation Another wind study, carried out in July Right: The summit of 2007 under the division’s leadership, has Cerro Paranal with VISTA in the foreground. Wind disturbance is a major concern for been to investigate the turbulent flow the performance of any telescope, but characteristics inside a real telescope en- particularly so for the E-ELT because of closure. Due to the large scale factors the enormous optical surfaces. In open in the wind tunnel and CFD models, it is space, the wind forces can be very high, difficult to characterise the flow charac- although with a relatively small turbulent teristics behind special structures like component. Protecting the telescope by the wind screen. For this campaign, four placing it inside an enclosure can reduce high frequency (32 Hz) ultrasonic ane- the absolute wind forces, but create tur- mometers were installed in the vacant bulence that can give problems for con- VST enclosure on Paranal. A row of four trolling the mirror surface. Although wind anemometers were placed at different tunnel testing and computational fluid locations within the enclosure volume. In dynamics (CFD) modelling are both valua- each configuration, the wind speed ver- ble techniques, there always remains a sus time histories were recorded, from problem of validating these models, both which the PSD of wind speed turbulence in terms of scaling and understanding and all the parameters which characterise the correct disturbance spectra to apply. the turbulent flow, like the mean speed The Jodrell-Bank wind experiment that turbulence intensity and integral length, was initiated in 2006 and is now in opera- were calculated. This was carried out for tion is intended to obtain direct measure- various windscreen positions and enclo- ments on a large telescope structure sure orientations. standing in a relatively unhindered airflow. Of interest are not only the absolute pressure variations but also the pressure correlations across the reflector surface. Another related experiment is the FP6 Wind Evaluation Breadboard project that is now being installed on Tenerife. It consists of a representative subset of a segmented aperture mirror with seven E-ELT- sized mirror segments equipped with active mirror supports and edge sensors. It will investigate optimum Servo Control Architectures for mirror control under varying wind exposures and orientations.

Anemometers arranged in a vertical line behind the windscreen of the VST enclosure. In the configuration shown, one anemometer is located in front of the enclosure to have a reference of the outside flow velocity.

60 ESO Annual Report 2007

The Science Archive Facility

The ESO Science Archive Facility (SAF) New archive web pages were deployed. As of 2006, the APEX submillimetre stores all raw data taken at the ESO sites They are now served through a con- antenna on the Llano de Chajnantor has in Chile, as well as processed products tent management system with ESO’s new been routinely producing science data. for selected datasets. The facility also corporate design. In the process, their The data belonging to two of the three contains a copy of the HST archive, man- content was updated and their structure APEX partners1, ESO itself and the On- aged in cooperation with the Space streamlined. A significant fraction of the sala Space Observatory in Sweden, are Telescope European Coordinating Facility new web pages was implemented as part stored in the ESO archive. As with any (ST-ECF) and the raw data from the UKIRT of the in-kind contribution provided by other ESO data, APEX files are also avail- Infrared Deep Sky Survey (UKIDSS) Spain. able to the community at large, once taken with the Wide Field Infrared Cam- the usual proprietary period has expired. era (WFCAM). The ESO archive currently holds 376 GB Archive holdings and data handling from just over 62 000 files of APEX data, Users around the world can access the 253 GB of which were produced and ESO archive via a Web-based data re- The ESO archive currently contains 74 TB processed in 2007. quest submission system. In addition to of data in 14 million files. Except for a few the general archive Web interface, all special cases, all science observations In the course of 2007 a dedicated key- current VLT instruments, the VLTI MIDI in- have a proprietary period of one year. word repository based on Sybase IQ strument, the HARPS instrument on After this period the archival datasets are database technology was deployed to La Silla, and APEX on Chajnantor have available worldwide to the general astro- store the complete and updated descrip- dedicated instrument-specific forms nomical community for further scientific tion of the science data contained in to query the data. Dedicated query forms exploitation. More than 15 TB of new data the archive, e.g. what objects were ob- are also available to browse and retrieve were archived during 2007, a 15 % in- served, when they were observed, and reduced data products. In 2007, work crease over the previous year. While the how they were observed. The database on the ESO Science Archive Facility pro- volume of HST data is smaller than that currently stores information on 7.9 mil- gressed towards setting up the infra- of ESO data by a factor of 37 to 1, the lion files and is being backfilled to include structure necessary to build a Virtual Ob- difference in the number of files archived all science files in the archive. servatory-compliant archive. for the two observatories is much less pronounced: 10 million ESO files and Also, the ESO archive stores all kinds of A visual browser to the SAF was released 4 million files from HST. data to monitor the status of virtually in 2007. VirGO, a plug-in to the open every single function of the VLT/VLTI ma- source tool Stellarium, provides a new way More than 11000 unique archive requests chinery. This database currently holds to access ESO data by displaying on the were served in 2007, totalling 16.1 TB 2.3 billion entries and grew in the past sky the field of view of imaging detectors of data. Of those requests, 8 800 were for year by a quarter of a billion entries. and slits of spectrographs, with the actual ESO data (12.3 TB in nearly three quar- orientation. As such, it allows a global ters of a million files), while the remain- VISTA/VIRCAM is the new wide-field in- and intuitive view of the areas of the sky ing 2 500 were for HST data (3.8 TB in frared imager on Cerro Paranal, sched- observed by ESO telescopes, which nearly a quarter of a million files). We pre- uled to start operations soon. With an ex- is fundamental especially in the case of pared and delivered to Principal Investi- pected data rate of 150 TB a year, this highly studied regions. The visual pres gators data packages containing proprie- instrument alone will produce a ten-fold entation is unprecedented in the field tary data for more than 1100 VLT/VLTI increase of data volume compared to of archive browsers. The real strength of and 120 La Silla observing programmes. all other instruments combined! Handling VirGO, however, is that it can filter out In addition, 170 calibrated pre-imaging this massive amount of data will pose and select relevant observations in a sim- datasets were delivered automatically to new challenges for archive operations ple way, and its Virtual Observatory com- Principal Investigators within 48 hours and will also serve to pave the way for fu- pliancy allows it to interact with other Vir- of acquisition at the telescope to allow ture high throughput instruments like tual Observatory (VO) tools. Among many them to prepare follow-up spectroscopic MUSE, a second-generation VLT instru- other features, VirGO includes a ‘shop- observations with the following instrument which is foreseen to be composed ping basket’, as used by many commer- ments: FORS1, FORS2, VIMOS, VISIR, of 24 integral field units. cial Web sites, which can be used to ISAAC, NACO and SINFONI. store a group of observations for further 1 The third partner being the Max Planck Institute for retrieval from the ESO archive. Raw data from the UKIRT Infrared Deep Radio Astronomy in Bonn, Germany. Sky Survey (UKIDSS) executed with the WFCAM instrument at the UK Infrared Telescope (UKIRT) have kept flowing into the ESO archive. During 2007 the ESO archive received 4.6 TB worth of UKIDSS data (260 000 files), which brought the total holdings to 13.1 TB (737000 files).

62 ESO Annual Report 2007 Processed data products – The final (v2.0) release of the Great – Advanced data products for the Large Observatories Origins Deep Survey Programme zCosmos (The evolution- A number of processed data products, (GOODS)/ISAAC data went online on ary links between galaxies, their nuclei, which astronomers can directly use 10 September. GOODS unites ex- their morphologies and their environ- for most scientific purposes, were made tremely deep observations from many ments) were released on 30 October. available during 2007: space observatories and from the They include 1264 one- and two-di- most powerful ground-based facilities, mensional VIMOS spectra. This is the – All non-Guaranteed Time Observation to survey the distant Universe to the first release of reduced data from an High Accuracy Radial velocity Planet faintest flux limits across the broadest external ESO Large Programme. Pro- Searcher (HARPS) spectra taken be- range of wavelengths. This release posers of Large Programmes are in tween the start of science operations includes fully calibrated mosaics (26 fact requested to deliver to ESO final and the end of 2006 were reprocessed fields in the infrared J- and Ks-bands, data products at the time of publica- with the latest HARPS consortium 24 in the infrared H-band) and ac tion of their results. This enhances the pipeline and made accessible. HARPS cumulates data acquired in 12 814 sci- legacy value of ESO data, facilitating is mainly dedicated to the detection ence exposures between October further scientific exploitation, assures of extra-solar planets and has discov- 1999 and January 2007 totalling uniform distribution of data products ered many such objects; 1.3 Msec of integration time. The fully through the Science Archive Facility, – All the spectra obtained with the UV- automated processing of the entire and gives them higher visibility. Visual Echelle Spectrograph (UVES) data set consists of 13964 raw science since the beginning of its operations in images, 20 699 calibration frames, and Finally, preview images (re-binned JPG February 2000 – nearly 60 000 raw 6 290 photometric standard stars; and FITS) with accurate astrometry from frames of point-like observations – – The final (v3.0) release of the GOODS/ Wide Field Imager (WFI) archival data were processed at ESO with the latest FORS2 spectra went online on 31 Oc- have been produced. These allow a version of the instrument pipeline tober. This includes 1715 spectra of ‘quick look’ at the data before submitting (v3.2). This new pipeline implements 1225 unique targets, providing in total a request. an adaptive scheme to consistently 1165 redshift measurements; and efficiently perform optimal spectral extraction over a wide range of signal- to-noise ratios, up to the maximum Poisson limit of several hundred dic- tated by pixel saturation. Only quality- controlled master calibration frames ESO VLT/FORS2 spec- were used for the processing and all tra slits overlaid with VirGO on a VLT/ISAAC science products have undergone a preview image in the certification procedure. This approach GOODS south area. results in a large data set processed in a homogeneous, controlled and well understood way. This massive data processing was made possible by applying to the UVES catalogue the new tools and concepts developed to cope with the large amount of data that is expected to be produced by the up- coming survey instruments. UVES data were processed in a VO-compliant manner and are accessible through an interface which includes target information obtained via cross-identification with astronomical objects in the SIMBAD and NED databases. Archive users can search by target name, object class, redshift or radial velocity and look, for example, for all quasars at redshift larger than 3 observed by UVES;

ESO Annual Report 2007 63 The ESO Data Centre The construction of the ESO Data Centre mission-critical database servers were has enabled the consolidation of the moved on short notice. The ESO Data Centre was completed in majority of the mission-critical operations June 2007. It is a state-of-the-art com computer systems into one location. During a power outage from 1 to 2 De- puter room, currently equipped with eight The relocation of the operational compu- cember 2007, the Uninterruptible Power actively cooled racks, seven standard ter systems took meticulous planning Supply proved its worth, which enabled racks, three network racks and one Blade and was executed within three weeks. all mission-critical computer systems and Centre. The technical equipment in this A downtime for the entire Archive was not services to continue without interruption. Data Centre comprises redundant Liquid required, because the Primary Archive Cooling Packages (LCPs), a leakage de- consists of twenty-four individual sys- Database replacement servers for the tection system, and smoke and particle tems, which could be relocated individu- remote observatory sites have also been detectors in a controlled and air-condi- ally one at a time. In addition, most procured. These servers are situated tioned environment. The entire ESO Data in the ESO Data Centre and are being in- Centre is powered through a centralised stalled, configured and tested prior to Uninterruptible Power Supply (UPS), handover to the La Silla Paranal Observa- which is located directly underneath the tory. Data Centre.

The ESO Data Centre in Garching.

64 ESO Annual Report 2007 The European Virtual Observatory

The EURO-VO project aims at deploying A EURO-VO workshop on how to publish The fourth cycle of the VOTech project, an operational Virtual Observatory (VO) data to the Virtual Observatory, organised which works by six months cycles, was in Europe, allowing users easy and seam- by ESO and ESA in collaboration with the completed in March 2007. Project mem- less access to the huge amount of astro- other EURO-VO partners, took place at bers met at ESO, on 12–15 March, to nomical data currently available, to facili- ESAC, Madrid, in June. It attracted about assess the work done and present plans tate their exploitation and foster new 60 participants (many astronomers) and for the next cycle. The project mid-term science. ESO is a founding member of 20 advisers/organisers. It was geared review and Cycle 6 planning was held on EURO-VO, which is partly funded by the towards data centres and large projects 8–11 October in Edinburgh, UK. European Community. in order for them to acquire the knowledge and experience necessary to allow The ESO-led design study group on new The EURO-VO project, through its Sci- them to become ‘publishers’ in the VO. user tools released its report. Many of the ence Advisory Committee (SAC) and the In hands-on sessions, participants were new prototype components made it into ESO/ESA managed Facility Centre, introduced to VO protocols in the view production software such as archival ac- selected three projects (two of which are of publishing their data holdings through cess to spectra or display of instrumental being supported by ESO staff) making the VO. Implementation feedback was footprints and filter transmission curves. use of VO tools and applications to carry collected on the VO protocols and tools. out astronomical research. The projects ESO was instrumental in developing a have received scientific support and The second meeting of the EURO-VO query protocol for standardised access technical contact points and should soon Data Centre Alliance board took place on to spectroscopic data. The technical complete their work. 1–2 February at ESO. The main topic of specifications of the Simple Spectral Ac- discussion was the EURO-VO proposal in cess (SSA) Protocol were approved and The ESO/EURO-VO project was present response to the first Framework Pro- adopted by all 16 IVOA members. SSA at the European Astronomical Society gramme 7 (FP7) Infrastructure call, pub- constitutes the most significant technical Symposium on “Science with Virtual Ob- lished on 22 December 2006. The third contribution of ESO in the VO era. servatories” (JENAM, Yerevan, Armenia, meeting of the EURO-VO Data Centre 20–25 August), at the workshop “Astron- was held in Trieste, Italy, on 4–5 October. The EURO-VO proposal “Astronomical omy with Virtual Observatories” held in Topics of discussion included the assess- Infrastructure for Data Access (AIDA)” Pune, India, on 15–19 October, and at the ment of Cycle 1 activity, preparation of submitted to the first FP7 Infrastructure Lithuanian Summer School “Virtual Ob- the revised Project Plan for Cycle 2, prep- call INFRA-2007-1.2.1 “Scientific Digital servatories”, held in the Moletai Observa- aration of the first periodic report to Repositories” was selected for funding at tory, Lithuania, on 23–26 October. the EC, and discussion of the Data Cen- the 2.7 M€ level. The project starting tre census information collection and col- date is 1 February 2008. This ensures the The EURO-VO SAC met for the third time lation. continuation of European-wide VO activi- on 18 June at ESTEC, Noordwijk, the ties at least until 2010. Netherlands. SAC members were updated on the latest EURO-VO develop- ESO maintains the EURO-VO project web ments. site, which in 2007 served 112 GB of content resulting from 230 000 user sessions. ESO is also in charge of the IVOA project web site, which served 116 GB of web content resulting from 500 000 user sessions.

ESO Annual Report 2007 65

ST-ECF

ESO and the European Space Agency ACS back to full functionality. ST-ECF of the highlights of the year was the start continued their successful collabora- staff are supporting these activities by of the production of the Hubblecasts in tion through the Space Telescope Euro- generating technical documentation and Full HD, which prompted an enormous in- pean Coordinating Facility (ST-ECF). The by participating in the reviewing process. crease in the number of web downloads. Hubble Space Telescope (HST) is cur- In total, 1.8 million Hubblecasts (12 epi- rently in observing cycle 16, routinely The European HST Archive is now oper- sodes) were distributed during the last achieving observing efficiencies between ating within the new ESO Archive infra- nine months of 2007. These Hubblecasts 45 and 50 per cent. It is performing nom- structure. The total Hubble data hold- continue to rank among the most suc- inally in two-gyro mode, with the possi ings are now about 2 Terabytes in un- cessful science-related materials in, for bility to operate in one-gyro mode, should processed and compressed form. During instance, iTunes. It was voted among the this be required. Science highlights in- 2007, 2512 requests for data (3.1 TB) Top-25 video podcasts of 2007 (one of clude the observation of ‘Lego-block’ gal- were served and distributed to 405 users. two science vodcasts in Top-25), and axies, from which today’s galaxies are In collaboration with the STScI and the even used in a demo by Apple CEO Steve assumed to have evolved. The dark mat- CADC, work on the Hubble Legacy Ar- Jobs at the keynote address at MacWorld ter scaffolding of the universe was chive continued. The goal is to collect 2007. mapped. 2007 also marked the 20th an- and generate selected High Level Sci- niversary of Supernova 1987a; it has now ence Data Products and make them avail- In collaboration with IAU Commission 55, been monitored by the HST for 17 years, able to the community through a science- the journal “Communicating Astronomy completely revolutionising our knowledge oriented user interface. User support with the Public” (CAP) was created. It is of supernovae.European observing time continued through the Newsletter, the to appear on a quarterly basis and is de- allocation continued to be well above the HST email hotline, and the production of signed to meet the clear need for a pub nominal 15 %. technical documents. ST-ECF staff also lication addressing the specific needs of monitored the TAC process and contin- the public astronomy communication Currently the ST-ECF is operating under ued to support the ESO SAMPO Project. community. This is particularly important the terms of the original MoU between Moreover, ST-ECF staff takes care of the as 2009 has been declared the Interna- NASA and ESA, which foresees a staffing editorship of the ESO Messenger. tional Year of Astronomy (IYA2009) by the level of seven ESA and ESO funded po United Nations. In collaboration with the sitions. The MoU will expire at the end of The ST-ECF has been active in the dis- IAU the IYA2009 Secretariat was set up 2010. The focus of the ST-ECF efforts semination of the discoveries from at ST-ECF’s outreach group in August was on the generation of Advanced Sci- Hubble to the public during 2007. Twenty 2007. Two conferences were organised: ence Data Products: both the ACS and news and photo releases and sixteen The International Year of Astronomy 2009 the NICMOS instruments on HST have smaller ‘Hubble Updates’ were produced. Meeting at ESO and Communicating As- integral-field spectroscopic capabilities. The European Hubble website had tronomy with the Public 2007 in Athens. The data produced in these modes 7.5 million visits (up 160 %) and distributed Five new websites were created – the are complex to analyse and require tech- 110 TB of multimedia materials (up one for the International Year of Astron- niques unfamiliar to most astronomers. 200 %). 150 new Full High Definition omy 2009 was the most popular of these. ST-ECF has therefore developed software (1080 p) video clips were produced. One that is able to extract spectra from the As part of the continuing ESA-ESO sci- data frames and to calibrate them, with ence strategy coordination, a fourth topi- the aim of making them directly avail- cal working group, chaired by Catherine able to the community. This capability is Turon, is preparing a report on Galactic also applicable to Wide Field Camera 3 Structure with particular reference to the (WFC3), one of the two new scientific forthcoming GAIA mission. This will be instruments that will be installed on the the latest addition to the existing set of HST during Servicing Mission 4 (SM4). reports: Extrasolar Planets (M. Perryman, chair); The Herschel-ALMA Synergies Intense preparations for SM4 continued (T. Wilson) and Fundamental Cosmology throughout the reporting period. The mis- (J. Peacock); and will be published in sion is currently scheduled to launch in mid-2008. August or September 2008. It will restore the HST to 3-gyro configuration. In addition to the installation of the Cosmic Ori- gins Spectrograph (COS) and the WFC3, the mission will attempt to bring STIS and

ESO Annual Report 2007 67 The Organisation

Office of the Director Administration Division La Silla Paranal General1 Observatory

Tim de Zeeuw Hans Jahreiss Andreas Kaufer

Fatme Allouche Claus Madsen Patricia Adriazola Nancy Ageorges Victor González Ernesto Orrego Catarina Alves de Vincenzo Mainieri Eduardo Arenas Luis Aguila Charlotte Groothuis Oscar Orrego Oliveira Gautier Mathys Andres Arias Claudio Agurto Patricia Guajardo Juan Osorio Gonzalo Argandoña Jorge Melnick Angela Arndt Bernardo Ahumada Carlos Guerra Juan Carlos Palacio Mustafa Basbilir Steffen Mieske Samantha Austin-May Mario Alfaro Stéphane Guisard Ricardo Parra Giuseppina Battaglia Igor-Félix Mirabel Juan Carlo Avanti Jaime Alonso Serge Guniat Jose Parra Mary Bauerle Ingo Misgeld Roland Block Nilso Alquinta Flavio Gutiérrez Andres Parraguez Yuri Beletsky Lorenzo Monaco Jean-Michel Bonneau Jose Luis Alvarez Fernando Gutiérrez Marcus Pavez Angelika Beller Dominique Naef Renate Brunner Paola Amico Nicolas Haddad Eduardo Peña Thomas Lennart Bensby Thomas Naets Cecilia Carrasco Andreas Andersson Juan Pablo Haddad Jorge Pilquinao Michael Böcker Nadine Neumayer Karina Celedon Lundgren Pierre Haguenauer Juan Pineda Henri Boffin Pasquier Noterdaeme Claudia Silvina Cerda Gaetano Andreoni Olivier Hainaut Andres Pino Konstantina Boutsia Eniko˝ Patkós Laura Comendador Ernesto Araya George Harding Manuel Pizarro Jutta Boxheimer Silvia Pedicelli Frutos Juan Carlos Arcos Volker Heinz Aldo Pizarro Pamela Bristow Douglas Pierce-Price Tommaso Di Dio Javier Argomedo Juan Pablo Henriquez Andres Pizarro Karsten Brogaard Olga Pinto Moreira Andrea Dinkel Karla Aubel Cristian Herrera Emanuela Pompei Benoît Carry Farid Rahoui Günther Dremel Francisco Azagra Leonardo Herrera Hugo Quijón Catherine Cesarsky Anna Raiter Willem Arie Dirk Eng Jose Baez Swetlana Hubrig David Rabanus Mary Cesetti Suzanna Randall Sonia Garnica Pedro Baksai Gerhard Hüdepohl Andrés Ramírez Lise Bech Christensen Paula Valentina Rebonto Guha Emilio Barrios Rodrigo Huerta Fredrik Rantakyrö Blair Campbell Conn Rodriguez Adriana Gutierrez Rogelio Bascunan Ramon Huidobro Johnny Reveco Silvia Cristiani Francesco Saitta Priya Nirmala Hein Juan Beltran Gerardo Ihle Vincent Reveret Itziar De Gregorio Hugues Sana Charlotte Hermant Eduardo Bendek Valentin Ivanov Miguel Riquelme Monsalvo Julia Scharwächter Nathalie Kastelyn Per Mikael Bergman Jorge Jimenez Christophe Risacher Gayandhi Manomala Zhixia Shen Elizabeth Kerk Guillaume Blanchard Nestor Jimenez Thomas Rivinius De Silva Colin Snodgrass Hans-Jürgen Kraus Carlos Bolados Ismo Kastinen Pascal Robert Antonio De Ugarte Veronica Sommariva Katjuscha Lockhart Stéphane Brillant Nicholas Charles William Robinson Postigo Thomas Stanke Ignacio Lopez Gil Armando Bruna Kornweibel Chester Rojas Jörg Dietrich Christina Stoffer Maria Madrazo Erich Bugueno Carlos La Fuente Gorky Roman Michelle Doherty Masayuki Tanaka Silvia Madrid Pariente Blanca Camucet Francisco Labraña Jose Rosas Michaela Döllinger Leonardo Testi Jorge Moreno Massimiliano Camuri Octavio Lavin Felix Alberto Rozas Brigitta Eder Svea Teupke Maria Angelica Moya Luis Alejandro Paul Le Saux Francisco G. Ruseler Christopher Erdmann Sune Toft Hélène Neuville Caniguante Cedric Ledoux Claudio Saguez Robert Fischer Ezequiel Treister Christine Nieuwenkamp Michael Cantzler Alfredo Leiva Daniel Salazar Andrew Fox Elena Valenti Thomas Penker Ruben Carcamo Ramon Leyton Antonio Saldias Diego Alex Gerrit van der Plas Rolando Quintana Cesar Cardenas Christopher Lidman Fernando Salgado Garcia-Appadoo Stefan Vehoff Mauricio Quintana Giovanni Carraro Gaspare Lo Curto Alejandro Salinas Mark Gieles Giulia Ventimiglia Andre Ritz Duncan Castex Gianluca Lombardi Ariel Sanchez Carla Gil Elisabeth Völk Rosa Ivonne Riveros Roberto Castillo Ignacio Lopez Stefan Sandrock Rachel Emily Gilmour Rein Warmels Francky Rombout Monica Castillo Ariel Lopez Roberto Sanhueza Raphael Gobat Michael Weigand Marcia Saavedra Jorge Castizaga Fernando Luco Pierre Sansgasset María Eugenia Gómez Michael West Nadja Sababa Susana Cerda Felipe Mac-Auliffe Jorge Santana Luis Calçada Thomas Wilson Maria Soledad Silva Cecilia Ceron Agustin Macchino Lilian Sanzana Claudio Grillo Gabriele Zech Erich Siml Claudia Cid Gianni Marconi Ivo Saviane Uta Grothkopf Herbert Zodet Beatrice Sivertsen Alex Correa Pedro Mardones Linda Schmidtobreick Karin Hansen Roswitha Slater Jose Ignacio Cortes Pedro Marin Ricardo Schmutzer Camilla Juul Hansen Albert Triat Angela Cortes Kiriako Markar Markus Schöller Hans Hermann Heyer Lone Vedsø Jaime Costa Mauricio Martinez Oliver Schuetz Renate Hoppe-Lentner Marschollek Claudio De Figueiredo Elena Mason Alex Segovia Gaitee Hussain Sabine Weiser Melo Eduardo Matamoros Fernando Selman Gaël James Yves Wesse Reinaldo Donoso Rolando Medina Waldo Siclari Edmund Janssen Gerd Wieland Javier Duk Angel Mellado Peter Sinclaire Paulina Jiron Christophe Dumas Alejandra Mena Alain Smette Eric Jullo Michael Dumke Jorge Miranda Fabio Somboli Georg Junker Domingo Duran Juan Molina Stanislav Stefl Katarina Kiupel Carlos Durán Nelson Montano Michael Fritz Sterzik Heidi Helena Korhonen Yves Durand Alex Morales Sandra Strunk Isolde Kreutle Carlos Ebensperger Sebastien Morel Thomas Szeifert Daniel Kubas Alessandro Ederoclite Merilio Morell Roberto Tamai Milla Laaksonen Cristian Esparza Ivan Muñoz Mario Tapia Jean Baptiste Lorena Faundez Julio Navarrete Manuel Torres Le Bouquin José Figueroa Hernan Nievas Soraya Torres Bruno Leibundgut Erito Flores Dieter Nürnberger Josefina Urrutia Silvia Leurini Juan Carlos Fluxa Herman Nuñez Guillermo Valdes Karin Lind Sergio Gaete Kieran O’Brien Jose Javier Valenzuela Luis Felipe Lira Jose Gardiazabal Rodrigo Olivares Karen Vallejo Cristian Lopez Gordon Gillet Francisco Olivares Leonardo Vanzi Paul Lynam Alain Gilliotte Oscar Varas Mariya Lyubenova Philippe Gitton Enrique Vera Percy Glaves Jorge Vilaza 1 Including all the Leonardo González Stefan Wehner Fellows and Students Domingo González Ueli Weilenmann under the Studentship Andrés González Luis Wendegass Programme. Sergio González Andrew Wright

68 ESO Annual Report 2007 Telescope System Data Management and Software Development Instrumentation Technology Division ALMA Division Division Operations Division Division Division

Roberto Gilmozzi Fernando Comerón Michèle Péron Alan Moorwood Martin Cullum Hans Rykaczewski

Constanza Araujo Paola Andreani Roberto Abuter Matteo Accardo Bertrand Bauvir Gareth Aspinall Hauck Andrew Burrows Eric Allaert Gerardo Avila Henri Bonnet Fabio Biancat Marchet Dina Arbogast Fabien Chereau Luigi Andolfato Dietrich Baade Roland Brast Claus Dierksmeier Robin Arsenault Carlos De Breuck Pascal Ballester Andrea Balestra Enzo Brunetto Preben Grosbøl Domenico Bonaccini Nausicaa Delmotte Klaus Banse Paul Bristow Bernard Buzzoni Christoph Haupt Calia Danuta Dobrzycka Peter Biereichel Iris Bronnert Ralf Dieter Conzelmann Jennifer Hewitson Marc Cayrel Adam Dobrzycki Thomas Bierwirth Mark Casali Bernard-Alexis Delabre Andreas Kempf Richard Clare Markus Dolensky Reynald Bourtembourg Claudio Cumani Nicola Di Lieto Hervé Kurlandczyk Jeroen de Jong Nina Felber Alessandro Caproni Sebastian Deiries Canio Dichirico Robert Alexander Laing Françoise Delplancke Nathalie Fourniol Sandra Maria Castro Klaas Johannes Dekker Martin Dimmler Massimiliano Marchesi Frédéric Derie Monika Gotzens Maurizio Chavan Sandro D’Odorico Michel Duchateau Pascal Martinez Philippe Dierickx Reinhard Hanuschik Gianluca Chiozzi Reinhold Dorn Toomas Erm Beate Marx Robert Donaldson Evanthia Hatziminaoglou Mauro Comin Mark Desmond Raul Esteves Eric Pangole Enrico Fedrigo Michael Hilker Livio Condorelli Downing Giorgio Filippi Ferdinand Patt Yan Feng Wolfgang Hummel Paulo Correia Nunes Christophe Dupuy Gerhard Fischer Gianni Raffi Wolfgang Hackenberg Christian Hummel Stéphane Di Cesare Siegfried Eschbaumer Christoph Frank Silvio Rossi Ronald Holzlöhner John Lockhart Dario Dorigo Gert Finger Domingo Gojak Hans Rudolf Norbert Hubin Jean-Christophe Philippe Duhoux Christoph Geimer Frederic Yves Joseph Joseph Schwarz Lieselotte Jochum Malapert Sylvie Feyrin Andreas Glindemann Gonté Stefano Stanghellini Markus Kasper Stephane Marteau Robert Frahm Juan Carlos Gonzalez Ivan Maria Guidolin Donald Tait Bertrand Koehler Sabine Mengel Bruno Gilli Stefan Hötzl Andreas Haimerl Gie Han Tan Johann Kolb Sabine Moehler Carlos Guirao Sanchez Olaf Iwert Florian Heissenhuber Eugenio Ureta Visa Korkiakoski Palle Møller Birger Gustafsson Gerd Jakob Guy Hess Elena Zuffanelli Paolo La Penna Petra Nass Karim Haggouchi Hans-Ulrich Käufl Renate Hinterschuster Miska Kristian Le Louarn Mark Neeser Carlo Izzo Florian Kerber Georgette Hubert Samuel Lévêque Paolo Padovani Bogdan Jeram Jean Paul Kirchbauer Georg Igl Jochen Liske Ferdinando Patat Yves Jung Jean-Louis Lizon à Paul Jolley Pierre-Yves Madec Isabelle Percheron Robert Karban L’A l l e m a n d Andreas Jost Space Telescope – Enrico Marchetti Francesca Primas Maurice klein Gebbinck Antonio Ramon Barbara Klein European Coordination Patrice Martinez John Pritchard Jens Knudstrup Manescau Hernandez Franz Koch Facility Serge Menardi Marina Rejkuba Antonio Longinotti Leander H. Mehrgan Heinz E. Kotzlowski Samantha Milligan Jörg Retzlaff Henning Lorch Manfred Meyer Maximilian Kraus Lars Lindberg Guy Monnet Bruno Rino Lars Kristian Lundin Luca Pasquini Simon Lowery Christensen Riccardo Muradore Charles Rite Holger Meuss Markus Patig Christian Lucuix Wolfram Freudling Sylvain Oberti Jesus Rodriguez Ulloa Andrea Modigliani Jean-François Pirard Ruben Mazzoleni Jonas Haase Jérôme Paufique Martino Romaniello Christophe Moins Suzanne Ramsay Jean-Michel Moresmau Richard Hook Duc Thanh Phan Piero Rosati Ralf Palsa Roland Reiss Michael Müller Martin Kornmesser Florence Puech María del Mar Sierra Moreno Pasquato Javier Reyes Michael Naumann Martin Kümmel Mark Robinson González Martine Peltzer Andrea Richichi Frank Nittel Harald Kuntschner Johannes Sahlmann Remco Slijkhuis Werther Pirani Gero Rupprecht Lothar Noethe Marco Lombardi Marc Sarazin Dieter Suchar Dan Popovic Ralf Siebenmorgen Edouard Pomaroli Pedro Miguel Russo Nicolas Schuhler Lowell Tacconi-Garman Eszter Pozna Jörg Stegmeier Marco Quattri Britt Sjöberg Christian Soenke Mario Van Den Ancker Marcus Schilling Sebastien Tordo Jutta Quentin Felix Stoehr Jason Spyromilio Ignacio Vera Sequeiros Diego Sforna Joël Daniel Roger Vernet Michael Schneermann Jeremy Walsh Josef Strasser Andreas Wicenec Paola Sivera Babak Sedghi Stefan Ströbele Markus Wittkowski Fabio Sogni Armin Silber Isabelle Surdej Burkhard Wolff Heiko Andreas Sommer Jesper Thillerup Arkadiusz Swat Bodo Ziegler Stefano Turolla Arno Van Kesteren Luke Taylor Martin A. Zwaan Jakob Vinther Véronique Ziegler Seconded Staff Gerard van Belle Michele Zamparelli M e m b e r s Elise Vernet Stefano Zampieri Anders Wallander ALMA Joint Office Nataliya Yaitskova Massimo Tarenghi

Paulina Bocaz Richard Hills Jacques Lassalle Lars Å. Nyman Russell Smeback

ESO Annual Report 2007 69

Personnel

As defined in its Rules and Regulations, ESO has five categories of staff mem- Administrative Engineers bers, whose distribution at the end of 16.7 % 44.4 % 2007 was the following: – International Staff Members (371 staff; 56.1%) – Local Staff (176; 26.6 %) Technical – Fellows (36; 5.4 %) 11.3 % – Paid Associates (46; 7%) – Students (32; 4.8 %). Their purpose is to reflect the variety of circumstances and diverse work at ESO, and to provide flexibility. ESO has seen Astronomer/ a steady increase in staff numbers over Scientists 27.6 % the last 3 years, and it is positive to note that the number of female staff has increased by a higher percentage than male staff (17% and 4 %, respectively). ESO staff are distributed across four main job cate- tific nature of the work, engineers and astronomers During 2007 we introduced e-Recruit- gories: administrative and technical staff, astrono- make up 44 % and 28 %, respectively, of the organi- mers, and engineers. Given the technical and scien- sation. ment to facilitate the recruitment process for applicants and the management of human resources (HR) activities, enabling internal and external applicants to apply for vacancies online. Applicants get automatic confirmation that their application has been received, and HR can request Others Belgium additional information electronically, thus 7.9 % 4.1 % reducing the administration activities, and Sweden Switzerland 1.6 % 1.1 % speeding up the recruitment process. Portugal Czech Republic 0.3 % 0.3 % Throughout 2007, ESO advertised 88 va- The Netherlands cancy notices and 1744 applications 4.1 % Germany were received. In 2007, 54 International 33.0 % Staff Members and 23 Local Staff Mem- Italy 18.0 % Denmark bers were recruited. In addition, 11 Stu- 3.0 % dents, Fellows, Paid and Unpaid Associ- Spain ates joined ESO. United Kingdom 2.7 % 6.8 % France Finland 17.7 % 0.3 % HR development

Throughout 2007 we have been working to further develop the terms and con- This was an active working group, which Distribution of International Staff Members by ditions of employment at ESO. Working compared ESO to other scientific organi- Nationality as of 31 December 2007. with the International Staff Committee in sations. The group produced a number of Chile, a revision of the terms of employ- recommendations that do not only focus ment for astronomers working in Chile on women-related matters but also affect was agreed, with particular note taken of organisation-wide issues. Some of the the annual review of scientific activity, the key areas for development have included: assignment and career development, and a review of maternity and adoption leave; the working schedules for astronomers. the participation in a common ‘Kinder- krippe’ and ‘Kindergarten’ with neigh- Another important activity concerns bouring institutions; management and equal opportunity issues. This work com- leadership training; a proposal to intro- menced in 2006 with the purpose of as- duce a ‘Harassment and Bullying’ policy; certaining if we are providing an environ- and a review of the approach to flexible ment conducive to attracting women to, working at ESO. This work will continue in and allowing them to develop in, science. 2008 with the working group.

ESO Annual Report 2007 71 During 2007, Human Resources made Age and implemented the following improve- 70 ments/changes as far as Rules and Regulation developments are concerned: – Recognition of same sex marriages; 65 – Recognition of same sex and opposite sex partnerships; 60 – Paid paternity leave increased; – Paid maternity leave increased for the second and the following children; 55 – Special leave in the event of illness of a close relative was introduced; – Unpaid special leave to care for mem- 50 bers of the family or close relatives; – Amendment in the application of offi- 45 cial holidays in Chile and Garching; – Amendment in the application of the Cost of Living differential to the Expa- 40 triation Allowance; – Amendment of the Education Grant and its related Circular; 35 – Contract Policy for International Staff Members; 30 – Guidelines for commuting of Staff Members in Chile; – Recruitment and Selection Proce- 25 dures.

Moreover, the Human Resources depart- 20 ment has led a working group to look at 15 10 5 0 5 10 15 20 25 30 Headcount the impact of the recommendations from the ‘Future of La Silla’ working group. Age distribution of ESO staff on 31 December 2007. This has focused on matters relating to The average age is 42 years, and within the age range of 35 to 45 years, the spread is fairly homoge- resources including; internal reassign- nous, for both male (dark blue) and female (light blue). ments; future early retirement schemes, and the selection of skilled staff for the core positions for the future operation of La Silla.

Throughout the year, considerable advice and guidance has been provided to the ALMA Human Resources Advisory Group, specifically in the areas of internal regulations; compensation and benefit programmes; review and definition of the recruitment processes for Local Staff and International Staff; clarification on process of performance and advancement reviews; and resource requirements for the JAO HR Department.

Further activities included the organisation of two meetings of the ESO Tripartite Group; the participation in the HR working group of EIROforum; the implementation of two new Collective Contracts for Santiago and the sites; the implementation of the Leave Module of the Navision system in Garching and Vitacura.

72 ESO Annual Report 2007 Council

The Council is ESO’s ruling body, which In March, an In-Kind Negotiation Team for delegates the day-to-day responsibility the accession of Austria was appointed, Council and Committee of Council to the Executive under ESO’s Director chaired by Prof. Jens Viggo Clausen. The 2007 General. In 2007, Council held two ordi- Team reported to Council in June and President Richard Wade nary meetings, in Barcelona in June Council agreed by consensus that the and in Garching in December. The Com- negotiations should continue along the Belgium Monnik Desmeth mittee of Council met twice, in Potsdam lines drawn up by the team with the ob- Christoffel Waelkens in March, and in Oxfordshire in October. jective of presenting a draft agreement Czech Republic Jan Marek The President of Council, Prof. Richard to Council for approval at a later stage. Jan Palousˇ Wade, chaired all the meetings. ESO is still in dire need of an extension Denmark Jens Viggo Clausen Henrik Grage In June, Council approved a Collaborative to the Headquarters’ Building in Garching Agreement concerning the construction and an agreement about lease and Finland Kalevi Mattila of the Atacama Large Millimeter/submil- subsequent purchase of the necessary Pentti Pulkkinen limeter Array with the National Astronomi- land was signed by the landowners and France Julien Galabru cal Observatory of Japan (NAOJ). This ESO. An architects’ competition was Laurent Vigroux Agreement governs the financial and pro- initiated and an international jury met in cedural aspects related to goods pur- October and awarded two first prizes, Germany Andreas Drechsler chased and services performed by ESO a third and a fourth prize, and recognised Thomas Henning in the interests of NAOJ. (with a ‘purchase prize’) one additional Italy Vicenzo Dovì design which, although innovative, did Bruno Marano Having spent time at the sites in Chile in not meet local building regulations. Coun- January and in Garching in February, cil approved that a revised call for The Netherlands Jan A. C. van de Donk Piet C. van der Kruit the Visiting Committee delivered its re- tenders would be issued to the top three (until 30 June 2007) port to Council in June. The then Director prize winners in the course of spring 2008. Konrad H. Kuijken General, Catherine Cesarsky, presented (as of 1 July 2007) an initial response to the report but it was At the meeting in December, Prof. Portugal Fernando Bello left to the new Director General, Tim Richard Wade was re-elected President Teresa Lago de Zeeuw, to provide an action plan to of Council for 2008 and Prof. Thomas Council on how to respond to the individ- Henning was elected Vice-President. Spain Xavier Barcons ual points. This was done later in 2007. Mr Alain Heynen was appointed Chair Jordi Torra of the Finance Committee for 2008. Sweden Claes Fransson In June, Council also approved a resolu- Dr Monica Tosi was appointed Chair of Finn Karlsson tion stating that the La Silla 2010+ sce- the Observing Programmes Committee nario would allow ESO to maintain the for 2008 and Dr Svetlana Berdyugina Switzerland Michel Mayor Martin Steinacher availability of the La Silla site for the ESO was re-appointed Vice-Chair. community at a reduced level. United Kingdom Gerry Gilmore Membership of the ALMA Board was (until 30 June 2007) Council received the usual VLT/VLTI, In- confirmed for a year or until the possible Patrick Roche (as of 1 July 2007) strumentation and ALMA biannual re- restructuring of the Board had taken Rowena Sirey ports, and the reports from the Chairs of place. the Finance Committee, the Scientific Technical Committee and the Observing The ELT Standing Review Committee The ESO Tripartite Group met twice in Programmes Committee. In addition a chaired by Prof. Roger Davies met twice 2007. The meeting in March was chaired biannual E-ELT Design Phase Status Re- in 2007 and subsequently reported to by Dr Ugo Sessi and the meeting in Sep- port was introduced. Council approved Council. tember by the new Chair, Dr Patricia an agreement with NOVA regarding Laplaud. The Group received updates re- ASSIST – a test bench used to test the The Scientific Strategy Working Group, garding the CERN Pension Fund and was Adaptive Optics Facility. chaired by Prof. Bruno Marano, met three kept informed about the measures taken times in 2007. In February and in May it for personnel regarding the reduction In June, Council reaffirmed its approval elaborated on scenarios for ESO’s future of operations at La Silla. Changes to the of the Phase B Work Plan for the E-ELT. direction within astronomy in Europe. Staff Rules and Regulations concerning In December, Council approved the In September, it convened, together with the education grant were discussed as Terms of Reference and the membership a number of renowned experts, to dis- well as changes to the calculation of the of an FP7 E-ELT Preparation Steering cuss surveys. Reports on the outcome cost-of-living adjustment. The Tripartite Committee. This oversight committee were presented to Council. Group received information regarding the would take up work on 25 January 2008. collective bargaining for local staff in Chile and the advancement review and salary adjustments for international staff.

ESO Annual Report 2007 73 Finance Committee Finance

In 2007 the Finance Committee held two As in the last four years, the ESO finan- ordinary meetings and two extraordi- Finance Committee cial statements showed a positive annual nary sessions, which were all chaired by 2007 cash flow in 2007. The 2007 figure of Ms. Rowena Sirey. They all took place Chair Rowena Sirey +55.3 M€ included the one-time receipt at ESO Garching, except for the regular of Spain’s entrance fee, following the meeting in November 2007 which was Belgium Alain Heynen country’s accession in 2006. During held in Paranal. On this occasion, mem- 2007, ESO also received the first regular Czech Republic Jaroslava Jeslínková bers of the committee had the chance contribution from the Czech Republic, to see the offices in Santiago, the observ- Denmark Cecilie Tornøe the ESO thirteenth member state. The atories in Paranal and La Silla, and dis- cash and short term deposits as of 31 De- cover the latest developments at the Finland Jaana Aalto cember 2007 amounted to 144.5 M€. ALMA site. France Patricia Laplaud The statement of income and expendi- The committee dealt with various finan- Germany Marlene Lohkamp- ture for 2007 showed a slight excess cial issues (annual accounts, budget, Himmighofen of expenditure over income of 0.17 M€. cash-flow situation, financial projections, Italy Ugo Sessi member state contributions) and with Emanuela De Lauretis The budget for 2008 was approved by personnel issues concerning International the ESO Council in December 2007. The as well as Local Staff. These subjects The Netherlands Coen J. van Riel budget comprises three sections: the were discussed in detail and recommen- Portugal Fernando Bello income budget, the payment budget and dations were made to Council. the commitment budget. Spain Luis E. Ruiz López de la The Finance Committee approved the Torre Ayllón With 189.7 M€, the payment budget awarding of 16 contracts exceeding Sweden Sofie Björling covers in particular the 2008 require- 300 000 € and 24 single-source procure- Johan Holmberg ments for the ALMA construction and for ments exceeding 150 000 €. The Colla the European ELT detail design phase. borative Agreement between the National Switzerland Jean-Pierre Ruder In total, it is expected to be significantly Astronomical Observatory of Japan and United Kingdom Colin Vincent higher than the 2008 income budget, ESO was approved, and information was which amounts to 164.0 M€. The commit- received concerning procurement statis- ment budget for 2008 is 232.7 M€. tics, forthcoming calls for tenders and price enquiries. The New Headquarters’ Agreement on the lease and subsequent purchase of the land has also been approved, thereby enabling ESO to advance the planning for the extension of the headquarters building in Garching.

Some contracts for the design phase of the E-ELT could also be presented and approved by the Committee.

A meeting of the Finance Department.

74 ESO Annual Report 2007 Financial Statements 2007 Budget for 2008 (in € 1000) (in € 1000)

Balance Sheet 31.12.2007 31.12.2006 Income budget 2008 Contributions from member states 123 364 Assets Other income from member states 7736 Cash and short-term deposits 144544 89 222 Income from third parties 27628 Claims, advances, refundable taxes and other assets 4488 60 402 Various income 5 300 Total assets 149 032 149 624 Total income budget 164 028

Liabilities and equity Dues 12 371 6 803 Payment budget 2008 Advance payments received and other liabilities 14 627 20 616 Personnel cost 57423 Total liabilities 26 998 27 419 Other cost 132 316 Cumulated result previous years 122 205 46 675 Total payment budget 189 739 Annual result – 171 75 530 Total equity 122 034 122 205 Total liabilities and equity 149 032 149 624 Commitment budget 2008 Personnel cost 57423 Projects commitments w/o personnel 123 099 Statement of Income and Expenditure 01.01.2007–31.12.2007 Operations commitments w/o personnel 52 220 Total commitment budget 232 742 Income Contributions from member states 134 649 Contributions from third parties and partners 5 227 Income from sales and other income 7643 Total income 147 519

Expenditure Expenditure for staff 51 893 Operating and other expenditure 95797 Total expenditure 147 69 0

Annual Result – 171

Statement of Cash flow 01.01.2007–31.12.2007

Cash flow from operating activities Receipts Income 147 519 Net movements on accounts receivable 55 913 Total 203 432 Payments Expenditure –147 690 Net movements on accounts payable 7449 Total – 140 241 Net cash flow from operating activities 63 191

Net cash flow from financing activities –7870

Net cash flow = Net increase/decrease in cash and short-term deposits 55 321

ESO Annual Report 2007 75 The Scientific Technical Committee

STC expressed their concern about the In discussing the 2010+ outlook for The Scientific Technical Committee tight schedule for the E-ELT site selection La Silla, STC encouraged ESO to con- 2007 and encouraged ESO to study aggres- tinue monitoring the scientific produc- José Afonso (P) (Chair ALMA/APEX sively and thoroughly more sites. In addi- tivity as the operations model and instru- sub-panel) tion, STC proposed that the ELT project ment plan for La Silla 2010+ converge. Rafael Bachiller (E) office assesses the validity of the current Since the plan foresees no travel and sci- Willy Benz (CH) models used in testing the proposed entific support beyond 2009, STC rec- Joris Blommaert (B) Jean-Gabriel Cuby (F) ELT sites by applying these models to the ommended to leave open the possibility Raffaele Gratton (I) La Silla and Paranal sites and compare of limited financial support for some Lauri Haikala (FIN) the results with the real data. programmes from the ESO community Thomas Michael Herbst (D) (Co-chair E-ELT requesting the La Silla facilities beyond sub-panel) Richard Hills (UK) (until first meeting in 2007) STC recognised the continuing vitality of 2010. This would enable groups from Hans Kjeldsen (DK) La Silla and the excellence of the science smaller institutions to continue to exploit Yannick Mellier (F) it delivers. The STC was convinced that the scientific potential of La Silla. Dante Minniti (RCH) the La Silla facilities remain unique for a Goran Olofsson (SE) Michael Prouza (CZ) large community of European astrono- STC was concerned that the continuing Patrick Roche (UK) (Vice-chair, chair VLTI mers, and that they will continue to de- delay of the VLT Survey Telescope (VST) sub-panel) liver excellent science for many years is impacting key components of ESO’s Linda Tacconi (D) (Chair) to come. Thus, STC recommended that scientific programme and indicated that Leonardo Testi (I) (until first meeting in 2007) Huib Jan van Langevelde (NL) every effort be made to ensure that the completion of the project is very ur- La Silla is preserved beyond 2010. ESO gent. Moreover, STC was seriously con- presented a plan to refocus and stream- cerned about the potential absence of line operations on La Silla, which includes competitive optical wide field facilities at STC 66th Meeting dedicating the 3.6-m to HARPS, restrict- ESO on the short time scale, and urged ing the NTT to EFOSC2 and a visitor ESO to start immediately a study of al At its 66th meeting, held on 18–19 April, focus, and not offering the 2.2-m on ESO ternative plans or possible backup solu- the Scientific Technical Committee (STC) time beyond 2009. The plan, that fore- endorsed the recommendation of the sees starting preparations in Period 81 by Science Working Group (SWG) that the moving EFOSC2 to the NTT and stopping Scientific productivity of La Silla compared to the major ground-based optical observatories in the ELT project office continues to study service mode observations, was en- world. Since the h-index increases with time and the design of a 42-m telescope because dorsed by STC that also anticipated that La Silla is significantly older than the other observa- the superior spatial resolution and speed the La Silla facility will evolve towards tories included, only the rate of change of h with are required by two of the three primary observing runs of one week or longer in time is relevant in this comparison. The slopes are seen to be comparable for La Silla, Keck, Gemini, science cases. The choice of a 42-m order to gain additional savings in opera- and Subaru, but the growth rate is clearly steeper for diameter will give ESO the best telescope tions costs. the VLT. in the world. h-index STC endorsed the plan presented by the 120 ELT Project Office for launching the instrument and adaptive optics studies during Phase B. The plan foresees that the 10 0 selection of instrument studies should be based on a mixture of single source 80 procurements (SSP) and open calls. STC recommended not to initiate any further SSP for the new instrument concepts, 60 but rather to issue well advertised open calls for instrument concept studies. Depending on the outcome of these open 40 calls, STC considered that it could be necessary to support more than the two 20 new instrument concept slots currently envisaged by the plan. STC also urged ESO to request proposals from the SSP 0 teams, since all concepts will ultimately 0 1 2 3 4 5 6 7 8 9 10 need evaluation. Years after publication

Keck VLT Gemini La Silla Subaru

76 ESO Annual Report 2007 Planet Jupiter is seen between the 3.6-m and the CAT at La Silla, while the Milky Way is seen in its full splendour. Photo: S. Brunier

tions, such as technical studies to enable STC 67th meeting committees. This would be crucial to op- optical wide-field capability at the NTT timise the effectiveness of the commu or at the VLT. On the longer term, STC The 67th meeting of the STC took place nication between the sub-committees asked ESO to look for cost effective ways on 23 and 24 October. The main items and the STC, to provide redundancy of to enable and maintain wide-field imag- considered were the sub-committees, STC presence at the sub-committee ing and spectroscopic facilities for the the next generation instruments for the meetings, and to expedite the discussion ESO community without jeopardising the VLT and VLTI, ESO’s short term wide- of the varied individual topics at the STC other major approved ESO projects. In field survey capabilities, and multi-conju- meetings. particular, and although full participation gated adaptive optics. in the Large Synoptic Survey Telescope STC noted that with the imminent PRIMA (LSST) may require an unrealistically large Because of the increasing diversity and commissioning, the VLTI is about to gain financial commitment from ESO, STC rec- complexity of the ESO programmes, new capabilities in high precision astrom- ommended that ESO continues the dia- three expert committees on, respectively, etry, while enhanced capabilities from logue with the LSST consortium. Along ALMA, the E-ELT, and the VLTI, now second generation instruments will con- the same lines, STC recommended to in- advise STC. For historical reasons, these solidate its position as the world-leading vestigate optimum ways to realise leader- committees, which evolved from the infrared interferometer over the next ship and/or major participation in com- ESAC in the case of ALMA, and the ESE decade. Therefore, STC recommended petitive wide-field facilities in the ELT era. in the case of the E-ELT, have different that ESO follows a phased development terms of reference. STC recommended aimed at bringing these instruments to that the terms of reference for the three sub-panels be reassessed and updated to reflect the evolving situations of the projects, and that more than one STC member be present on each of these

ESO Annual Report 2007 77 the VLTI in the period 2012 to 2015. Since VLT into the ELT era. The initial set of VLT The STC strongly advocated that any new the ultimate performance of the instru- instruments will be old at that time and instrument concepts should not include ments is tied to the performance of the would have accomplished most of its changing the fundamental design of any VLTI infrastructure, which will need to goals. Noting that adequate funding has of the VLT’s Unit Telescopes, nor com- be improved to allow them to realise their been reserved for new instrumentation promise the VLTI capabilities or put se- full scientific potential, STC recommend in the mid- and long-terms plans, STC vere stress on ESO’s resources. STC rec- that continuing improvements in the infra- warmly thanked ESO for the efforts in ommended that an open plan including structure should be pursued vigorously, collecting new ideas for future plans from these instruments, as well as at least one integrated with the PRIMA commissioning the community by means of the “VLT in open slot for new concepts, be estab- programme so that PRIMA reaches its the ELT era” workshop, held in Garching lished following procedures similar to design goals at the end of the commis- the week prior to the STC meeting. those followed for second-generation VLT sioning period. The commissioning of instruments. PRIMA should be the highest priority for Following this workshop and their own the VLTI, in addition, of course, to contin- ensuing discussions, STC recommended STC welcomed the positive news, pre- uing to obtain high profile science results that a new long-term instrumentation plan sented at the meeting, about the pro- with the current VLTI system. be devised, commencing nearer to com- gress and recovery plans for the VST and pletion of the current second-generation the foreseen start of operations in 2009. STC recognised that all three second- VLT instrument suite. This plan should in- Stressing that the successful operations generation VLTI instruments presented at clude at least the following instrument of both VISTA and VST are of very high the meeting have high scientific poten- concepts: priority for the study of dark energy, STC tial, but considered that GRAVITY and – A very stable, high resolution spec- stressed that it continues to be important MATISSE should be given the highest pri- trograph, able to measure radial veloci- for ESO to look for cost effective ways orities and should now proceed to the ties with very high precision in order to enable and maintain wide-field imaging next design phase. The third, VSI, which to search for rocky planets, measure and spectroscopic facilities for the ESO will make it possible to combine up to possible variations of physical con- community without jeopardising the other six telescopes simultaneously and will be stants, and make detailed analysis of major approved ESO projects. As an ex- a unique capability in the southern hemi- the chemical composition of stars in ample, STC recommended that, together sphere, could proceed more slowly than nearby galaxies; with the OPC, ESO investigates ways to the other two. However, STC stressed – A wide field, very high multiplex spec- begin soon spectroscopic public sur- their wish to see a global and phased troscopic facility to exploit the wide veys with VIMOS, urging ESO to upgrade VLTI development plan considering the field imaging capabilities that will be VIMOS with CCDs with higher quantum three instruments and optimising the com- available in the near future; efficiency in the red for this purpose. mon requirements on infrastructure, such – Upgrades and/or replacements of the In the vision of STC, such surveys would as the physical space in the VLTI labora- VLT ‘work-horse’ instrument capabili- provide an essential complement to tory, adaptive optics, and fringe tracking. ties. In particular, these would include the VISTA and VST imaging surveys in the a multiplex near-infrared (NIR) spectro- short term, while new next generation STC stressed the importance of develop- scopic capability, intermediate to high instrumentation for the VLT would ensure ing and maintaining a broad and inno spectral resolution optical and NIR ESO competitiveness in this field in the vative instrumentation suite for preserving spectroscopy, and NIR diffraction lim- longer term. the long-term competitiveness of the ited imaging. The STC continued to be impressed with the performance of the Multi-Conjugate Sunset over Paranal Adaptive Optics Demonstrator (MAD), and the VLT. and applauded ESO and the MAD team for this remarkable demonstrator. Noting

Photo: S. Guisard that an instrument able to further exploit multi-conjugate adaptive optics on a short timescale would be highly welcome, STC encouraged ESO to investigate ways to continue to make MAD available to the community for additional observing runs to exhaust the potential observing opportunities available with this system.

78 ESO Annual Report 2007

Public Outreach

Cover of the 48-page ESO brochure. ESO’s outreach and education pro- guages will be ready for distribution in gramme includes a wide range of activi- early 2008, while the remaining three will ties, encompassing, for example, press be completed by mid-2008. releases, videos, printed matter, exhibitions, open houses, high-level events, contests, education material and summer Videos schools. As already alluded to above, a special ef- In 2007, ESO issued a record 55 press fort is made as regards to providing video releases: 23 presented outstanding sci- material (footage, interviews, animations) ence results made possible with ESO to broadcasters. This is distributed via telescopes, 10 were press photos, 7 con- video newsreel on the occasion of impor- cerned new instruments, 9 dealt with ESO tant press releases, or as regular updates as an organisation, and 6 were ALMA re- to the ‘collection tapes’ on La Silla, leases. Among the very successful press Paranal, and ALMA. A list of broadcasters releases was the discovery of Gliese 581c is maintained for this purpose. This effort with the HARPS instrument in La Silla. led to many broadcasts, reaching a very This is the most Earth-like planet ever wide audience that is otherwise very dif found around another star, where water ficult to address. In addition, we provide possibly flows on the surface, although support to journalists, including TV crews, this has recently become subject to fur- coming to the various ESO sites. The ther debate. Thanks to its intrinsic news video material is also distributed through value, but also to dedicated effort involv- the ESO website, as well as on sites such ing the distribution of custom broadcast- as YouTube. On these sites, users also quality video and background material, contribute new material based on ESO- Because the importance of television as a the news received worldwide coverage. made videos. This shows how well ESO distribution channel for science cannot The story reached several hundred million is entering into the public sphere and be overstated, the ESO Public Affairs viewers on TV, including during prime adding hundreds of thousands of young Department also participated in the World time, and millions of readers through the viewers to the ESO audience. Congress of Science and Factual pro- written press. It goes without saying that ducers that took place in New York in the equivalent advertisement value is In September 2007, on the occasion of November. This annual event brought to- tremendous. The interest in this story did the first visit of Tim de Zeeuw as ESO Di- gether more than 550 international not fade throughout the year, with many rector General to the Chilean sites, a broadcasters, producers and distributors requests coming from producers, mag group of Dutch journalists paid a visit to from more than 20 countries, providing azines and authors of books. Other high- ESO’s Vitacura Centre, and the Paranal a unique chance to meet the key actors lights were the images of the Great and Chajnantor sites. This resulted in very in this field and promote ESO. Comet McNaught, the anniversary of su- wide coverage of ESO in Dutch media, pernova SN 1987A, the ALMA transport- including on TV. In November a group of As far as video is concerned, it is worth ers, the superb image of the galaxy taken ten journalists – including two TV crews – noting that a new movie was made, pre- in the presence of European Commis- from French-speaking Belgium visited senting ESO and its various activities and sioner Potocˇnik, and the UN Resolution Paranal, together with the Walloon Minis- sites. The movie was made available on on the International Year of Astronomy, in ter for Research, Marie-Dominique DVD, as well as on the ESO website, and which ESO played an important role. Simonet. This also resulted in very exten- in five languages. sive media coverage. These are but two For the ALMA transporters, a dedicated examples of activities were ESO colla press and industry event was arranged in borate actively with institutes or funding The ESO Web collaboration with the company that built agencies in member states. Other exam- them, Scheuerle GmbH. This also en- ples include the participation of ESO to Another major milestone in 2007 was the sured that ESO was visible in a very dif- the STFC Town Hall meeting on outreach complete overhaul of the ESO website, ferent section of the press than usual, and education and to the ISSI Forum on which received 2.5 million visits over the i.e. the truck and special vehicle press. Space Science and Education. year. This revamping was clearly needed to reflect the changes in its usage since In the area of printed matter, a completely its conception in 1994. Since then the new 48-page ESO brochure was pub- ESO Web has expanded rapidly, both in lished in English and German. This bro- the amount of information and services chure will also be made available in most that are provided as well as in terms of of the other languages spoken in ESO access rates. In spite of the information member states, and translation work was and services that have been continu- in progress in 2007. A total of eight lan- ously added to the ESO Web over the

80 ESO Annual Report 2007 past years, its structure had not been meeting, which was held jointly with the ers, as well as an opportunity to get adapted; the ‘Look and Feel’ still reflected Annual Meeting of the American Associa- in touch with a large number of science the predominantly science-oriented ap- tion of Physics Teachers, gathered over journalists in a very short time-span. proach and usage of the ESO Web in the five days about 3 000 astronomers and With its 30 m2 information stand at these mid-nineties. New information and serv- hundreds of teachers, and also attracted two major events, ESO and its ambi- ices were added arbitrarily to the old many journalists. On account of its shear tious projects have been well represented structure and could not easily be inte- size, the AAS Winter Meeting is one of across the Atlantic. grated into the existing navigation. Con- the astronomical events of the year, es- sequently, the ESO Web became increas- pecially for years in which there is no IAU In Europe, an important event was ingly complex, barely maintainable and General Assembly, and it is thus no sur- JENAM, the Joint European and National it became increasingly difficult to store prise that ESO decided to be present Astronomy Meeting, organised annually new information and services that would with an exhibition stand, featuring a VLT in one of the European countries jointly be easy to find and use. model. ESO’s presence was very much by the European Astronomical Society appreciated and many astronomers and and one of the national astronomical so- The new ESO Web addresses these is- teachers came by to get the latest infor- cieties. In 2007, JENAM took place in sues. It is now divided in three major user mation on the most recent developments. Yerevan, Armenia, allowing many visitors, areas: In particular interest was high in the Laser especially from the West, to discover a 1. Public. This area is intended for the Guide Star project, ALMA and, of course, unique culture and country. ESO was of general public, press and media, the E-ELT. ALMA was also represented at course present at this European astro- (potential) industrial partners and peo- the AAS meeting on the NRAO stand, our nomical event with, among others, an ex- ple interested in working at ESO. colleagues in this global project. In addi- hibition, providing thereby an occasion The area is partially based on existing tion to the exhibition, ESO was present at for the young astronomers from Eastern information, but also with new content. some of the press briefings, including the Europe to become acquainted with ESO. 2. Science Users. The area is intended one on the discovery of the first triple for professional astronomers who quasar and on results from the COSMOS A French version of the ESO exhibition are doing, or are planning to do, re- survey. This, in turn, resulted in an went on a real tour de France, travelling search using ESO facilities. enhanced presence of ESO in the media, from Meursault to Paris, and then to 3. Intranet. This area is for ESO Staff only. ironically also on the European scene. Meudon. At the end of May, the city of ESO’s first participation in the Winter Meursault in Burgundy was renamed In its current implementation the ESO Meeting of the AAS appeared therefore ‘Meursault les Etoiles’ for five days, as it Web still consists of many single web well justified and we look forward to at- featured many astronomical activities for pages that use a common style and navi- tending next year’s event in Austin, Texas. schools and the general public. In June, gation. In the near future it is planned From Seattle, the exhibition stand of ESO participated for the third time in the to move to a database-backed Content ESO was then transferred a little bit fur- European Research and Innovation Ex Management System. This will substan- ther south, to San Francisco, where hibition in Paris, an event that attracted tially improve maintainability of the site from 15 to 19 February, the Annual Meet- about 25 000 visitors. In 2007, ESO and will serve all web users with the most ing of the American Association for formed a partnership for this exhibition current information and a common Look the Advancement of Science took place. with three astronomical institutes from and Feel. With an estimated 10 000 participants Paris that develop instruments together and visitors, it is a privileged place for ex- with ESO, or make use of ESO tele- changes between American and Euro- scopes: the Paris Observatory, the Insti- A string of exhibitions pean scientists and science policy mak- tut d’Astrophysique and the CEA/Saclay

As part of our aim to be known to as Senior high school stu- many people as possible and to share dents, crowding the ESO stand at the Inter- our passion and efforts to understand national Festival for the Universe, we try to engage with Astronomy, were partic- the public as often as possible. For many ularly interested in the years now, ESO has therefore partici- ALMA project. pated in exhibitions aimed either at the general public or specific groups. The year 2007 was no exception and ESO participated in a string of exhibitions in many countries.

For the first time, ESO was present at the Winter Meeting of the American Astro- nomical Society (AAS) which took place in early January in Seattle, USA. The

ESO Annual Report 2007 81 Service d’Astrophysique. Staff from these institutes manned the ESO stand and interacted with the public. Most were former ESO staff and they greatly enjoyed sharing their knowledge of the organisation. They also helped present the video- conferences that took place daily from Paranal, with Olivier Hainaut at the other end of the line. Later, in October, the ESO exhibition was featured at the Meudon site of the Paris Observatory during the Science Week. About 1000 kids came along to see it with their schools, while on the Sunday, 1600 people visited.

France was not the only country visited of course, and ESO was also present in Switzerland, Germany and the Nether- lands. In Switzerland, ESO participated in the first Swiss Astronomy day, which took place on 20 September on the Üetli Long Night of Science, berg near Zurich. One of the organisers, October 2007. Ms Barbara Burtscher, had won ESO’s special donated prize of a trip to Paranal, In October, ESO also participated to the to Ernst-Peter Fischer, Dieter Ronte, and at the 16th European Union Contest golden anniversary of the Garching Cam- Elmar Zorn, on the interplay between the for Young Scientists in 2004. The Sep- pus, home to the ESO headquarters two very different sensitivities and how tember event in Zurich featured Bruno in Germany. The campus has indeed ex- they can apprehend the world. The event, Leibundgut as one of the speakers. isted since 1957, when the ‘Garching which was broadcast on Bavarian TV, Bruno also moderated several videocon- Atom-egg’ was inaugurated. Since then, was very successful, drawing participants ferences from Paranal, this time with the Garching Campus has developed ex- from all over Germany and abroad, and Thomas Szeifert on the other side. The tensively. There are now about 4 000 allowed people to see the ESO Head- event attracted some 1500 visitors. people who work on the campus, in addi- quarters building in a new and unique tion to the 8 500 students, making the setting: on this occasion, paintings by In Germany, ESO had a stand during the campus almost as populous as the town Rita Adolff-Wollfarth, a German painter 80th Annual Scientific Meeting of the of Garching itself. Albeit ESO only joined who also participated in the discussion, Astronomische Gesellschaft, which also the Campus in 1980, it participated fully were on display in the building. hosted the 5th biennial Workshop on in the activities for the 50th Anniversary, Astroparticle Physics. The event, where organising or taking part in several public On 13 October, the campus organised a ESO’s Director General presented the events. The set of activities started on ‘Long Night of Science’, running from ASTRONET Science Vision book, took 26 September, with a gala evening, fea- 18:00 till midnight. As usual, ESO, with place on 24–28 September and was at- turing high-level politicians, including the participation of staff from all the di tended by some 300 participants. the then Prime Minister of Bavaria, Dr Ed- visions, set up a wide range of activities. mund Stoiber, and the German Fed- The visitors could watch the latest ESO Finally, in the Netherlands, ESO was eral Secretary of State for Research, movie or attend short scientific talks on present with an information stand at the Dr Thomas Rachel. On 2 October, ESO many subjects – from the history of the International Festival for Astronomy (IFA) organised a round-table discussion on telescope to the principles of interferom- that took place near Utrecht. This three- the topic of “Arts and Science”. The dis- etry, from the study of exoplanets to the day event, which focuses on senior high cussion was moderated by a well-known interaction of galaxies. They could also school students and beyond, was organ- space-science journalist, Dirk Lorenzen. glance at the exhibition, featuring panels ised by the Dutch Youth Working Group Hans-Ulrich Käufl from ESO responded and models, or talk with the many staff for Astronomy and The Royal Netherlands present. They could address their ques- Society for Meteorology and Astronomy. tions to Nancy Ageorges in Paranal over Amongst many other interesting sessions, the video link, with Christian Hummel the winners of the Catch a Star 2007 in Garching taking the role of moderator. competition (see below), Jan Meˇsˇt’an and Activities were also organised for the Jan Kotek from the Czech Republic, young, such as puzzles, a stamp quest, a showed a presentation of their trip to the quiz and a planetarium show. As the Paranal Observatory. weather was fine and the skies clear, the members of the AGAPE hobby astron-

82 ESO Annual Report 2007 omy group were able to share their en- tity and develop a completely new, cen- Republic. Their project on “Research and thusiasm with visitors. The Charity group tralised ALMA web site. Observation of the Solar Eclipse” told also set up a very successful stand, sell- how they had studied solar eclipses, and ing a variety of food from different Euro- involved their fellow students in observa- pean countries that had been generously Education activities tions of an eclipse from their school in prepared by many ESO staff and their 2006. The winners were announced at families. Particularly popular were the “Catch a Star” is ESO’s flagship educa- the EIROforum “Science on Stage 2” fes- Belgian waffles, whose mouth-watering tion activity for school students, and tival in Grenoble. smell attracted many people. By the in 2007 this international competition took end of the night, about 1800 people had place for the fifth time. It was named The Artists competition also proved to be visited ESO’s headquarters during the “Catch a Star 2007” as the deadline oc- extremely popular, with 395 artworks six-hour period. A remarkable achieve- curred in this year, although the competi- submitted – a large increase over the pre- ment, since at the same time, the national tion opened in late 2006. The competi- vious year’s figure of 60. Efficient hand soccer team was playing a qualifying tion is organised in collaboration with the ling of the larger number of registrations, match for the European Championship! European Association for Astronomy as well as the public Artists gallery, was Education (EAAE), and is open to school made possible by a complete overhaul of students worldwide (although certain the competition’s web-based infrastruc- ALMA EPO prizes are restricted to entrants from Eu- ture, with the implementation of dynami- rope and Chile). cally-generated pages, a database back- ALMA is a project involving several part- end, and an interface for students to ners split over different continents, who “Catch a Star” has now evolved to in- submit their work and edit their registra- are working together to build the largest clude three different categories, to ensure tion details themselves. This technical and highest astronomical observatory that all students are able to take part, development put the competition on a in the world. It is important that these no matter what their level. In the Re- robust footing for the launch of “Catch a partners also work together on outreach searchers category, written projects with Star 2008”, which opened in late 2007. activities, avoiding duplicate work and an astronomical theme are judged by an instead enhancing and coordinating their international jury, with the top prize being In April 2007, the second EIROforum work. At the General Assembly of the a trip to visit the VLT on Paranal. In the “Science on Stage” European science International Astronomical Union in the Adventurers category, prizes are awarded teaching festival took place in Grenoble, summer of 2006 an Education and Public by lottery, to avoid a sense of elitism. In France. This international festival was Outreach Working Group (EPO WG) the Artists category, students enter astro- attended by about 500 educators, who was formally set up, composed of mem- nomically-themed artwork which is dis- had been selected from national events bers from the outreach groups of the played in a public gallery, and prizes are in 28 countries. As with the first “Science three partners (ESO, NRAO and NAOJ), awarded with the help of a web-based on Stage” festival, the aim was to stimu- as well as the respective ALMA scientists vote. late original and high-quality science in the Executives and at the Joint ALMA Observatory (JAO). In 2007, the JAO also Over 100 written projects were submitted recruited a Press Officer, who now chairs from 22 countries, and the top prize this working group and coordinates activ- was won by Jan Meˇsˇt’an, Jan Kotek and ities in Chile where all three partners are their teacher Marek Tyle, from the Czech present. One or two face-to-face meetings will take place annually, and the one in 2007 took place at the JAO headquarters in Santiago, Chile. Regular phone conferences, as well as a dedicated mail- ing list, allow the members of the working groups to share information.

Apart from promoting ALMA in several events or with dedicated news releases, press conferences, and production of material, the EPO WG also started the complete process of defining a strategic, short-, and long-range plan, a budget, and guidelines and procedures for working together. These were submitted for approval to the ALMA board. The next Report from Catch a steps to be taken in the first part of 2008 Star winners in the are to define the ALMA Corporate Iden- Winter 2007 issue of Science in School.

ESO Annual Report 2007 83 teaching in Europe, and to expose teachers to cutting-edge scientific research, as part of the EIROforum “European Sci- ence Teaching Initiative” (ESTI). Over the course of “Science on Stage” 1 and 2, and the earlier three “Physics on Stage” events, it is estimated that approximately 2 000 teachers participated in the international festivals and 30 000 in the national events.

The other pillar of the ESTI project is the European science education journal, “Science in School”. This journal was launched in March 2006, and offers a mix of teaching materials, articles on cutting- edge science, interviews with scientists, and more. It is published quarterly by the EIROforum, with a print run of 30 000 copies, and is also freely available on the web, where translated articles are also The fair at the Science present. ESO has participated in the jour- on Stage 2 festival. nal’s editorial board, and has also used it as a powerful way to communicate about our activities to teachers and other edu- The first joint ESO-EAAE Summer astronomers on the latest work of the cators. During 2007, the journal regularly School, for teachers with an interest in organisation. These comprised talks by featured ESO- and astronomy-related astronomy, took place in July 2007 at Roberto Gilmozzi (on the E-ELT), Paola stories, and these have been among the the ESO headquarters in Garching. ESO Andreani (on ALMA), and Ferdinando most popular according to reader feed- had supported the previous EAAE sum- Patat (on supernovae), which were all back. Science in School as a whole is mer schools, by providing speakers and very well received by the teachers. In ad- very popular among readers; in evalua- taking care of the printing of proceedings. dition, there were amateur observing tion activities, readers reported that it Building on a decade of success with sessions kindly arranged by AGAPE, the was “a useful teaching tool which effec- these EAAE schools, the idea behind a group of hobby astronomers at ESO, and tively inspires teachers and provides cre- joint ESO-EAAE summer school was a live video link to the VLT on Paranal. ative ideas for teaching science”. to encourage a stronger interaction be- This school was part of the EC Comenius tween teachers and active scientists, Programme, meaning that participants and to introduce the teachers to the latest could apply for funding from the EC to at- news and results from ESO. tend. At the end of 2007, the second joint ESO-EAAE summer school was being The first joint school had the topic “Strat- organised, and it is planned to take place egies for Effective Teaching of Astron- in Granada, Spain, in July 2008. omy”, and brought together 50 educators from 16 European countries plus Chile, who took part in astronomy-teaching workshops, sharing ideas and best prac- tice. Claus Madsen gave a presentation on science education in a European context, and Douglas Pierce-Price spoke about ESO’s educational programmes. There was also a series of talks by ESO

84 ESO Annual Report 2007 ESO Press Releases

ESO Press Photo 01/07 (3 January): ESO PR High- ESO Science Release 18/07 (29 March): The Impos- lights in 2006 sible Siblings ESO Science Release 02/07 (8 January): It Is No ESO Instrument Release 19/07 (30 March): New Mirage! Adaptive Optics Technique Demonstrated ESO Organisation Release 03/07 (11 January): ESO ALMA Release 20/07 (3 April): ALMA to Help Tim de Zeeuw to Become the Next Director Solving Acute Mountain Sickness Mystery General of ESO ESO Organisation News 21/07 (13 April): School ESO Instrument Release 04/07 (17 January): Big Red students “Catch a Star”! Eye is Ready ESO Science Release 22/07 (25 April): Astronomers ESO Press Photo 05/07 (19 January): The Great Find First Earth-like Planet in Habitable Zone Cometary Show ESO Science Release 23/07 (10 May): A Galactic ESO Instrument Release 06/07 (21 February): Fossil The Sky Through Three Giant Eyes ESO Science Release 24/07 (23 May): A Brown ESO Press Photo 07/07 (23 February): The Celestial Dwarf Joins the Jet-Set Whirligig ESO Science Release 25/07 (31 May): Chronicle of a ESO Science Release 08/07 (24 February): Death Foretold SN 1987A’s Twentieth Anniversary ESO Science Release 26/07 (12 June): Matter ESO Press Photo 09/07 (7 March): The Giant that Flashed at Ultra Speed Turned Out to be a Dwarf ESO Instrument Release 27/07 (13 June): Free from ESO ALMA Release 10/07 (7 March): The Antenna the Atmosphere Bride and Bridegroom ESO Science Release 28/07 (19 June): Back on Track ESO Science Release 11/07 (7 March): Solar Power ESO Science Release 29/07 (6 July): Star Surface at Play Polluted by Planetary Debris ESO Science Release 12/07 (13 March): Star Family ESO Instrument Release 30/07 (6 July): GROND Seen Through Dusty Fog Takes Off ESO ALMA Release 13/07 (14 March): A Roof for ESO Science Release 31/07 (12 July): The Gobbling ALMA Dwarf that Exploded ESO EIROforum Release 14/07 (15 March): Waking- ESO ALMA Release 32/07 (30 July): Birth of a Colos- up to Science! sus on Wheels ESO Science Release 15/07 (22 March): Fingerprint- ESO Press Photo 33/07 (2 August): The Planet, the ing the Milky Way Galaxy and the Laser ESO Instrument Release 36/07 (22 August): HAWK-I ESO Press Photo 16/07 (27 March): The Purple Rose ESO Science Release 34/07 (3 August): Star Caught Takes Off of Virgo Smoking ESO Press Photo 37/07 (23 August): Edge-on! ESO Science Release 17/07 (28 March): Controlled ESO Instrument Release 35/07 (4 August): First Light ESO Web Release 38/07 (3 September): Professor by Distant Explosions for World’s Largest ‘Thermometer Camera’ Tim de Zeeuw Takes Up Duty as New ESO Direc- tor General ESO Press Photo 39/07 (3 September): Stellar Fire- work in a Whirlwind ESO Science Release 40/07 (14 September): Galaxy ‘Hunting’ Made Easy ESO Science Release 41/07 (18 September): A Warm South Pole? Yes, on Neptune! ESO Science Release 42/07 (27 September): The Frugal Cosmic Ant ESO Science Release 43/07 (27 September): Into the Chrysalis ESO ASTRONET Release 44/07 (28 September): A Grand Vision for European Astronomy ESO ALMA Release 45/07 (5 October): A Colossus Gets its Name ESO Organisation Release 46/07 (5 October): Catch a Star 2008! ESO Science Release 47/07 (11 October): Drizzly Mornings on Xanadu ESO Organisation Release 48/07 (29 October): Commissioner Potocˇnik at Paranal Observatory ESO Press Photo 49/07 (9 November): A Galaxy for Science and Research ESO ALMA Release 50/07 (22 November): Close to the Sky ESO Organisation Release 51/07 (23 November): ESO Helps Antofagasta Region after the Earth- quake ESO Science Release 52/07 (28 November): Discov- ering Teenage Galaxies ESO Science Release 53/07 (19 December): Speedy Mic’s Photograph ESO Organisation Release 54/07 (20 December): 2009 to be the International Year of Astronomy The discovery of ESO Press Photo 55/07 (21 December): Anatomy of Gliese 581c got world- a Bird wide attention.

ESO Annual Report 2007 85 European and International Relations

Even to the casual observer of how in EU-matters for enhanced cooperation between ternational science is conducted and them, e.g. as expressed in the EIRO managed, it is clear that complexity has In the frame of the EIROforum partner- forum partnership, as well as with the Eu- increased during the recent years. This ship, in February we participated in the ropean Commission. development is at least technology-ena- MIT European Career Fair and Science bled, as is manifest in the emergence of Policy Meeting in Boston, which was The FP6 funded ASTRONET programme e-science (including AVO and grid tech- organised jointly by the European Com- is pursued by 18 funding agencies across nologies), but probably at a deeper lev- mission and the MIT European Club, Europe, in addition to ESA and ESO. One el even technology-driven. This happens, with support from several ESO member fundamental goal is to set up an overall so to speak, as collateral of the wider state embassies and the MIT Interna- European astrophysical strategic plan, issue of globalisation. This is also the tional Science and Technology Initiatives covering all branches of astronomy and case for the European Research Area (MISTI). The purpose of this recurrent all nations of the enlarged European Re- (ERA), which has been conceived in the event is to raise awareness among young search Area, for the next 20 years, using light of Europe’s so-called Lisbon Strat- researchers of the European Research a two-step procedure. The first step was egy. With the ERA, new networks and Area as an attractive place to work and to produce an integrated Science Vision modes of collaboration in science have live in. from thematic panels and a Science Vi- surfaced, impacting the way that ESO sion Working Group, both drawn from the interacts with the scientific community as In April 2007 the European Commission scientific community. Detailed mid-term well as with funding agencies and sci- published for public consultation its feedback from the community was se- ence policy-making bodies. Simply put, Green Paper entitled “The European Re- cured through a web forum and an open in the past our relations with the outside search Area: New Perspectives” symposium that took place in January world were predominantly bilateral, (COM(2007) 161 final). The paper basically in Poitiers, France, with participation from whereas today we see a multilayered web constituted a catalogue of 35 concrete 31 countries. The Science Vision effort, of relations both within Europe and be- questions covering a wide spectrum of led by Prof. Tim de Zeeuw (then at Leiden yond our shores. possible actions to support the further University) and managed by ESO, was development of the ERA. Among these completed this year, with the Science Aside from ALMA, where ESO represents questions was also the possibility of EC Vision document aired and widely distrib- its member states in a quasi-global pro- membership of the intergovernmental or- uted by the end of September. The subject, other examples include ASTRONET, ganisations “to increase the coherence, sequent task of drawing up by the au- a so-called ERA-net under the Europe- quality and delivery of European efforts in tumn of 2008 a prioritised infrastructure an Community Framework Programme, a number of research fields.” In its joint roadmap to implement the Vision began whose aim is to establish a comprehen- response published in September, EIRO- in May under STFC leadership and with sive long-term plan for the development forum acknowledged the suggestion of significant ESO staff involvement. of European astronomy. ESO is a full par- closer cooperation between the EC and ticipant in ASTRONET. the intergovernmental organisations, based on the principle of reciprocity and Participation in the 7th Framework At the same time, the EIROforum partner- underpinned by targeted practical agree- Programme ship, of which ESO is an active member, ments, subject to negotiations between is now widely recognised as a key ac- the individual organisations and the EC. In 2007 ESO submitted three proposals tor in the European Research Area. Since to the 7th Research and Development July 2007, CERN has held the rotating The Green Paper and the many reactions Framework Programme (FP7): EVALSO, Chairmanship. In July 2008, ESO will fol- were discussed at a high-level Con EuroVO-AIDA, and E-ELT Prep. All three low. ference on “The Future of Science and were accepted by the European Commis- Technology in Europe” in Lisbon, be- sion for funding. Even what appears to be straightforward tween 8 and 10 October 2007 under the bilateral cooperation projects may oc auspices of the Portuguese EU Presi- The EVALSO project (Enabling Virtual Ac- casionally involve European Union fund- dency. Among the conclusions were a cess to Latin-American Southern Observ- ing with related policy aspects. confirmation of the important role that the atories) aims to connect ESO’s La Silla intergovernmental organisations play in Paranal Observatory to the Chilean data At the other end of the ‘geographical the context of the ERA, but also the need network and to develop new ways of scale’, ESO was granted observer status doing astronomy using ICT and large ca- at the United Nations Committee for pacity networks. It complements the in- Peaceful Uses of Outer Space (UNCOP- ternational infrastructures created in the UOS), both to raise support for the Inter- last years with the EC support (GÉANT, national Year of Astronomy and also ALICE/RedCLARA) and will be another with a view to wider issues such as the step in the creation of an advanced in- protection of the skies. strumentation data Grid in Latin America. In the context of European and international relations, it is yet another example

86 ESO Annual Report 2007 of how R&D projects, international co Visit of European operation, EU funded actions and ESO’s Research Commissioner Janez Potocˇnik. own activities are intertwined. EVALSO has an overall budget of 3.6 M€, of which 1.6 M€ will be covered by European Commission (EC) funding. ESO’s share of the cost is 0.5 M€, with the rest covered by eight partners, including Coope ración Latino Americana de Redes Avan- zadas (CLARA) and Red Universitaria Nacional (REUNA). The project is led by INAF.

The EuroVO-AIDA project will lead the transition of Euro-VO into an operational phase. The aim is to integrate the technology, networking and service activities of Euro-VO into a fully functioning e-infrastructure. This project brings together Visit of Marie-Dominique eight partners, with CRNS/INSU as coor- Simonet, Minister of Research in the Walloon dinator. The overall budget is 3.4 M€ in- Regional Government. cluding a 2.9 M€ EC contribution.

The E-ELT Prep project complements the 2007–2009 Phase B (final design) of the European Extremely Large Telescope (E-ELT), presently conducted by ESO. E-ELT Prep has a total budget of 6.1 M€, including a 5.0 M€ contribution from the European Commission and will run for two years, in 2008–2009. ESO acts as a mono-partner in this project on behalf of all its member states, coordinating contributions from 25 institutes in eight member states. The EC involvement became possible as the E-ELT is included in the Roadmap established in 2006 by the Eu- ropean Strategy Forum for Research In- High-level visits frastructures (ESFRI). During the year, several science policy Besides the new contracts, ESO par makers took the opportunity to visit ticipates in 11 FP6 contracts running for ESO’s facilities in Chile. The visits in- some more years. cluded ESFRI Chairman John Wood (in March), European Research Commis- sioner Janez Potocˇnik with key Commis- sion officials (in October), Minister of Research in the Walloon Regional Gov- ernment Marie-Dominique Simonet (in November) as well as a high-level delegation from France, led by CNRS President Catherine Bréchignac (in December). Furthermore, members of the Budget Committee of the German Federal Parlia- ment visited Paranal in August.

ESO Annual Report 2007 87 Bilateral relations The Czech Industry Day.

In the course of the year, informal ex- changes took place with several countries potentially interested in joining ESO. The formal negotiations with Austria that had been initiated in 2006 at the request of the Austrian government continued.

With respect to current member states, ESO organised an Information Day for Czech Industry on 8 June in Prague, with same-day participation in a side-event for Czech students taking part in an ‘As- tronomy Olympiad’ at the Czech Acad- emy of Sciences. Earlier in the year, we had organised an event for Finnish Indus- try in collaboration with Finpro, an asso ciation to support Finnish industry in the international marketplace. This event took fort to win adoption by the United Na- nates the United Nations Educational, place at the ESO Headquarters, as did tions’ General Assembly of the necessary Scientific and Cultural Organization a similar meeting with potential Austrian resolution for the formal declaration of (UNESCO) as the lead agency and focal companies and institutes as part of the the Year. The support has been war- point for the Year, to organise activities process to identify possible in-kind con- ranted as ESO and its member state as- to be realised during the Year, in collabo- tributions from Austria in case of Austria tronomers have a strong interest in rais- ration with other relevant entities of the joining ESO. ing public awareness of our science and United Nations system, the International the IYA 2009 promises to become an Astronomical Union, the European South- Furthermore, a joint ESO-Czech working excellent and unique vehicle for this. It is ern Observatory and Astronomical so group was convened in the autumn to therefore with satisfaction that we note cieties and groups throughout the world.” consider the creation of a “Centre for Co- the approval of the IYA 2009 Resolution It is the first time in ESO’s history that operation with ESO and ESA”, or – for through the UN General Assembly on our organisation has been named in a short – the “E2S Centre”, to be placed on 19 December. The resolution “[…] desig- formal UN Resolution. the site of the Ondrˇejov Observatory. The planned centre, which would be largely funded by means from the European The United Nations Union Structural Funds might serve as a delegation. – Regional Training Centre (RTC), – ALMA Regional Centre (ARClet), – VLT/VLTI and E-ELT involvements co- ordinator, – Technology Information Centre (TIC), and – Public Outreach Centre (POC) for the Czech Republic and possibly for neighbouring Eastern European countries.

The International Year of Astronomy

With IAU as its main partner, but also in cooperation with UNESCO, INAF and others, ESO has provided significant support for the International Year of Astron- Right: Twisted Spiral omy (IYA 2009). The support includes Galaxy NGC 134 ob- hosting of the IAU IYA Secretariat at the served during the visit of European Commissioner ESO Headquarters but also help and for Science and Re- assistance in the year-long diplomatic ef- search, Janez Potocˇnik.

88 ESO Annual Report 2007

Relations with Chile

For the very first time, the Chilean Minis- ESO’s collaboration with the town of observations of the flora and fauna of the try of Foreign Affairs hosted an interna- Taltal, the nearest town to Paranal, con- ALMA region. Copies of the book were tional workshop on Astronomy. The event, tinued. ESO provides a scholarship distributed to all schools in the area, as a held on 4 and 5 December 2007 and programme for schoolchildren and uni- contribution to the education of students called “Chile: A Window into the Uni- versity students. This year, an educa- and young people in northern Chile. verse”, was jointly organised by the Minis- tional astronomy exhibit was inaugurated try and all international observatories at the city’s museum, presenting the In March, an official ‘topping out’ cere- currently operating in Chile, including VLT in a visual way, and highlighting the mony took place on the 2 900 m site of ESO, as well as the Chilean Astronomical importance for astronomical observa- the ALMA Operations Support Facility. Society and the National Commission for tions of protecting the night sky against The ceremony marked the completion of Science and Technology. light pollution. the structural works and was attended by Region II Senator C. Cantero and rep- The workshop provided the opportunity resentatives of the local community, of bringing together a wide range of ALMA-related activities including the Mayor of San Pedro, who institutions, including local universities, joined more than 40 representatives of representatives of local governments, In November, a new ALMA outreach and ESO, NRAO and NAOJ. members of industry, officers dealing with educational book was publicly presented legal affairs, and Chilean national agen- to officials of San Pedro de Atacama, in The programme to prevent environmental cies in charge of key issues, such as the the context of the celebrations of the an- damage to the ALMA site continued in environment, light pollution control, min- niversary of the Andean village. Entitled 2007. One highlight was the introduction ing and the administration of the electro- “Close to the sky: Biological heritage in of film cameras to monitor vizcachas magnetic spectrum. This event produced the ALMA area”, and published in English and abrocoma species. This is the first a rich, lively discussion on future chal- and Spanish by ESO in Chile, the book is time that this kind of surveillance has lenges for astronomical activities in the a collection by experts of unique on-site been done in Chile, representing a tech- country, including the protection of the sky and the possible installation of new international facilities in the next decades.

The year 2007 also marked the continuation and systematisation of a wide range of educational and public outreach activities in the country, as part of ESO’s programme of engagement with Chilean society.

In collaboration with the Education De- partment of San Pedro de Atacama and the EXPLORA Programme, an interactive exhibition on Physics was offered to the local community in October. More than 90 % of the primary schools in the area participated, enjoying the lively displays and demonstrations. Also with EXPLORA, ESO contributed to the Chil- ean National Science Week, with the organisation of an exhibition in Santiago on the VLT, ALMA and the ELT, attended by more than 30 000 people. In addition, secondary students from Antofa- gasta, La Serena and San Pedro de Ata- cama had the opportunity of visiting Paranal, La Silla and APEX during their regular classes, as ESO participated for the first time to the “Open Labs and Observatories” programme. Students from a school in San Pedro de Ata- cama, Chile, read the new ALMA book on the fauna and flora in the region.

90 ESO Annual Report 2007 ALMA has started a programme to help solving acute mountain sickness mystery.

nological milestone in the country. The and highways during the long journey The ESO/Government of Chile Joint films spotted the presence of Chinchilla from the port of Mejillones to San Pedro Committee for the Development of As- Andina, a highly endangered species, not de Atacama and the ALMA site. tronomy in Chile received 24 proposals found in the area before. for funding from Chilean institutions this year. This Committee was estab- During a ceremony held in April in Anto Public Affairs lished according to the Supplementary fagasta, representatives from ESO and Agreement with the Government a dec- the University of Antofagasta officially Due to the increase in the price of cop- ade ago, and has played a crucial role launched a collaborative agreement that per, ESO has had to face efforts from in the establishment and strengthening also involves the University of Chile and mining companies trying to establish min- of Astronomy Departments in Chilean the University of Copenhagen. The newly ing rights within the zones declared as Universities. This year, funds were allo- established cooperation will promote “area of scientific interest”, mostly in cated to several post-doctoral pro- teaching and research on work at high al- La Silla. For the first time, we had to op- grammes, support to research groups, titudes. The valuable data collected will pose requests submitted by mining com- and outreach, in a selection process that enhance our knowledge of human phys panies to the President of the Republic, involved representatives from the Chilean iology in extreme environments, generat- seeking permission to carry out mining Government and ESO. ing recommendations that will improve works within protected areas. well-being and health not only in high-alti- Vitacura was the focus of several talks tude observatories, but also for personnel A possible site in Region II for the future on astronomy for the general public, in the mining industry and in the Antarc- E-ELT project has been found and vari- drawing large enthusiastic audiences. tic. ous negotiations and administrative pro- Lectures and courses on subjects at the cedures have taken place, to obtain frontiers of astronomy were delivered Moreover, the Representative’s Office leasing and to proceed with the protec- by outstanding astronomers who visited has been involved in negotiations to pro- tion of the site. Vitacura for periods of one or two months. vide permanent power supply for the ALMA site. This was done together with Finally, an official farewell from Chile was the local communities who would great- organised for former ESO Director ly benefit by a connection to the Chilean General, Catherine Cesarsky, at the ESO electricity grid. The arrival of the first Guesthouse. It was attended by repre- antennas at the site also called for nego sentatives of the Ministry of Foreign Af- tiations with local authorities, Police fairs, regional authorities and the Ambas- Corps, and others, in order to obtain per- sadors from member states in Chile, as mits and collaboration to clear the roads well as the Chilean astronomical community.

ESO Annual Report 2007 91

Four Seasons at a Glance

January

The fourth Auxiliary Telescope (AT) is commissioned and accepted for operations.

The first commissioning of NACO with the Laser Guide System is completed.

The VISTA Infrared Camera arrives at Paranal.

Comet McNaught, the Great Comet of 2007, puts on an amazing show at Paranal.

The ESO Council appoints Tim de Zeeuw as the next Director General of ESO.

Final Design Review of the ALMA antenna transporters.

The ESO co-sponsored Third Chilean During the Finnish Advanced School of Astrophysics, Industry Day. “Insights into the Galaxy Evolution from Resolved Stellar Populations”, takes ESO is present at the annual AAAS meet- A Roof-Topping ceremony is held for the place at the Universidad de Concepción, ing in San Francisco, USA. ALMA Operations Support Facility. Chile. EIROforum participates in the MIT An ESO workshop, “Observing Planetary The 2007 ESO Instrument Calibration European Career Fair and Science Policy Systems”, takes place at ESO Santiago. Workshop takes place at ESO Garching. Meeting in Boston, USA. A Finnish Industry Day takes place at The Astronet Symposium, “A Science ESO Garching. Vision for European Astronomy in the March Next 20 Years”, brings together the Euro- The ESFRI Chairman John Wood visits pean astronomical community in Poitiers, The VLT automatically takes detailed ESO’s facilities in Chile. France. spectra of gamma-ray burst afterglows only minutes after the burst’s discovery. The Committee of Council meets in ESO is present at the winter AAS meeting Potsdam, Germany. in Seattle, USA. ‘First Fringes’ at the ALMA Test Facility with two prototype antennas. The ALMA Board meets in Tokyo, Japan.

February The Multi-Conjugate Adaptive Optics Demonstrator (MAD) achieves First Light April A special section on AMBER scientific re- on the VLT. sults appears in Astronomy & Astrophys- Astronomers discover with HARPS the ics. The first commissioning of SINFONI with most Earth-like planet outside our Solar the Laser Guide System is completed. System to date, Gliese 581c. The astronomical community celebrates the twentieth anniversary of Supernova The recoating of the secondary mirror of CRIRES, the ESO-built high-resolution 1987A. UT2 is successfully completed. infrared spectrograph on UT1, starts operations. Pre-Production Design Review of the The dome of the 3.6-m telescope at European ALMA antennas, built by the La Silla is fully restored, and moves with Science Operation of AMBER with three AEM consortium. nominal speed. ATs starts. Fringe tracking with FINITO is available in visitor mode. Critical Design Review of ALMA Band 9 cartrige. The FORS1 CCD upgrade is completed.

94 ESO Annual Report 2007 A detailed plan of E-ELT instrument stud- Claudie Haigneré, ies is finalised. former French Minister for European Affairs and former astronaut, Representatives from ALMA, ESO and visits the ESO stand in the University of Antofagasta officially Meursault. launch a collaborative agreement to help improve the understanding of acute mountain sickness.

The EIROforum Science on Stage 2 festival, held in Grenoble, France, brings together some 500 science educators from 27 European countries. The winners of ESO’s flagship educational competition ‘Catch a Star’ are announced.

The Scientific Technical Committee meets. June The ESO Council meets in Barcelona, The 31st Meeting of the ESO Users’ Spain. Committee takes place. The ESO Data Centre is completed. It is a state-of-the-art computer room, cur- The ALMA Board meets in Santiago, rently equipped with eight actively cooled Chile. May racks, seven standard racks, three network racks and one Blade Centre. ESO participates for the third time in the Using the VLT, astronomers measure the European Research and Innovation Ex age of a star located in our Galaxy as The UVES and spectroscopic FORS hibition in Paris, France. 13.2 billion years. It was formed just 500 pipelines are publicly released. million years after the Big Bang. ESO participates in the ISSI Forum on An Information Day for Czech Industry is Space Science and Education. The VISTA secondary mirror arrives at held in Prague. Paranal. The ESO workshop “Obscured AGN July A VLTI Summer School, “Circumstellar Across Cosmic Time” is held in Seeon, discs and planets at very high angular Bavaria, Germany. The first of two ALMA antenna transport- resolution”, takes place in Ofir, Portugal. ers rolls out of its hangar and successfully passes a series of tests. The newly revamped ESO web site goes live.

ESO is present with an exhibition stand at “Meursault les Etoiles”, France.

Finance Committee meets.

The Observing Programmes Committee meets for P80.

The ALMA Science Advisory Committee meets face-to-face in Tokyo, Japan.

An ALMA Front End optics Concept De- sign Review is held at IRAM, France.

The ESO Data Centre.

ESO Annual Report 2007 95 First Light for GROND, the gamma-ray The EAAE burst chaser, on the 2.2-m telescope at summer school. La Silla.

The recoating of the primary mirror of UT1 is successfully completed.

MUSE successfully passes its Preliminary Design Review.

The ESO workshop “12 Questions on Star and Massive Star Cluster Formation” is held.

The first ESO-EAAE Astronomy Summer School for Teachers is held at ESO Garching.

August

First Light for HAWK-I on the VLT. Work- ing in the near-infrared, HAWK-I covers about one tenth of the area of the Full Moon in a single exposure.

The world’s largest bolometer camera for submillimetre astronomy, LABOCA, en- ters service at the 12-m APEX telescope on Chajnantor.

Critical Design Review of the ALMA Band 7 cartrige.

The Joint European and National Astron- omy Meeting is organised in Yerevan, September The 6th NEON Observing School is or- Armenia, with ESO presence. ganised at the Asiago Observatory, Italy. Using the VLT, astronomers discover that A VLTI Summer School, “Active Galactic the south pole of Neptune is much hotter ESO is present at the 80th Annual Scien- Nuclei at the highest angular resolution: than the rest of the planet. tific Meeting of the Astronomische Ge theory and observations”, takes place in sellschaft. Torun, Poland. Professor Tim de Zeeuw takes up duty as the new ESO Director General. ESO participates in the first Swiss Astron- The LABOCA Panel of the Observing omy day. Programmes Committee meets. KMOS passes its Final Design Review and SPHERE its Preliminary Design Re- The ASTRONET Science Vision for Euro- view. pean Astronomy is published.

The “ALMA Community Days” and the Finance Committee meets. “Surveys for ALMA” workshop take place at ESO.

The MPA/ESO/MPE/USM 2007 Joint Astronomy Conference on Gas Accretion and Star Formation in Galaxies takes place in Garching.

96 ESO Annual Report 2007 October The “Arts and Science” event at ESO Garching. New near-infrared images from the VLT and Keck show for the first time a nearly global cloud cover at high elevations in the atmosphere of Saturn’s largest moon, Titan.

The European Science and Research Commissioner, Janez Potocˇnik, visits Paranal, together with key European Commission officials.

ESO organises a round-table discussion on the topic of “Arts and Science”, broadcast on Bavarian TV. Long Night of Science, The ‘Long Night of Science’ Open House ESO Open House. event at ESO Garching draws 1800 visitors.

At a ceremony at their manufacturer, the ALMA antenna transporters get their names: Otto and Lore.

The Catch a Star 2008 international astronomy education competition is launched.

The “Science with the VLT in the ELT era” workshop takes place at ESO, Garching.

The Committee of Council meeting is A new ALMA outreach and educational The 81st Meeting of the Scientific Tech held in the UK. book, ‘Close to the Sky: Biological he nical Committee takes place at ESO, ritage in the ALMA area’, is publicly pre- Garching. The ALMA Board meets in Santiago, sented to city officials of San Pedro de Chile. Atacama in Chile. Finance Committee meets.

The Scientific Technical Committee The ESO User Portal is launched. meets. December The CRIRES pipeline 1.5.0 is publicly ESO participates in the EC high-level released. The 62nd General Assembly of the United Conference on “The Future of Science Nations proclaims 2009 the International and Technology in Europe”, in Lisbon, The Minister of Research in the Walloon Year of Astronomy. Portugal. Regional Government, Marie-Dominique Simonet, visits Paranal. The Workshop “Science from UKIDSS” takes place at ESO Garching. November The ESO Fellowship Symposium is held at ESO Santiago. MUSE successfully passes its Optical A major earthquake with magnitude 7.7 Final Design Review. on the Richter scale affects the north of ESO is present with an information Chile. stand at the ‘International Festival for As- ESO Council meets at ESO, Garching. tronomy’, in Utrecht, the Netherlands. The two ALMA antenna transporters pass A high-level delegation from France, their ‘Factory Acceptance Review’. The ESO exhibition is featured at the led by CNRS President Catherine Paris Observatory Meudon site of Bréchignac, visits ESO in Chile. the Paris Observatory during the French Science Week, drawing 1600 pupils and more than 1000 other people.

ESO Annual Report 2007 97 Glossary of Acronyms

4LGSF Four-Laser Guide Star Facility EAAE European Association for Astronomy FWHM Full width half maximum 4QPM Four-quadrant phase masks Education GALACSI Ground Atmospheric Layer Adaptive AAAS American Association for the E-ALMA Enhancement of ALMA Early Science Optics for Spectroscopic Imaging Advancement of Science EC European Commission GB GigaBytes A&A Journal Astronomy & Astrophysics EFOSC ESO Faint Object Spectrograph and GÉANT Multi-gigabit Pan-European Data AAS American Astronomical Society Camera (3.6-m) Communications Network ACS ALMA Common Software EIS ESO Imaging Survey GENIE Ground based European Nulling AEM Alcatel Alenia Space France, Alcatel ELT Extremely Large Telescope Interferometer Experiment (VLTI) Alenia Space Italy, European Indus- E-ELT European Extremely Large Tele- GHz Gigahertz trial Engineering s.r.L., MT Aero- scope GOODS Great Observatories Optical Deep space Consortium (ALMA) EMMI ESO Multi-Mode Instrument (NTT) Survey AIDA Astronomical Infrastructure for Data EPO Education and Public Outreach GRAAL GRound-layer Adaptive optics Access ERA European Research Area Assisted by Lasers AIVC Assembly, Integration, Verification ERA-net European Research Area Network GRAVITY AO assisted, two-object, multiple- and Commissioning ESA European Space Agency beam-combiner (VLTI) AGAPE Amateur Group for Astronomy ESAC European Science Advisory Com- GRB Gamma-Ray Burst Projects at ESO mittee (for ALMA) GROND Gamma-Ray burst Optical/Near- ALMA Atacama Large Millimeter/submilli- EST ESO Survey Team infrared Detector meter Array ESE ELT Science and Engineering GUI Graphical User Interface ARClet ALMA Regional Centre node ESFRI European Strategy Forum on HARPS High Accuracy Radial Velocity Plane- ALICE America Latina Interconectada Con Research Infrastructures tary Searcher (3.6-m) Europa ESPRESSO Super stable high resolution optical HAWK-I High Acuity Wide field K-band AMBER Astronomical Multi-BEam combineR spectrograph for the VLT Imager (VLT) (VLTI Instrument) ESTEC European Space Research and HD High Definition AO Adaptive Optics Technology Centre (ESA) HR High Resolution AOF Adaptive Optics Facility ESTI EIROforum European Science HST Hubble Space Telescope AOS Array Operations Site (ALMA) Teaching Initiative IAU International Astronomical Union APE Active Phasing Experiment (E-ELT) EU FEIC European Front End Integration ICD Interface Control Document APEX Atacama Pathfinder Experiment C e n t r e ICT Information and Communication ASAC ALMA Science Advisory Committee EURO-VO European Virtual Observatory Technology ASI Italian Space Agency (Agenzia EVALSO Enabling Virtual Access to Latin- IDA Image Dissector Array Spaziale Italiana) American Southern Observatories IQ Image Quality ASIC Acquisition System on a single chip EXPLORA Chilean Programme for non formal IFA International Festival for Astronomy ASSIST Adaptive Secondary Setup and education in Science and Technol- IFU Integral Field Units Instrument Simulator ogy INAF Istituto Nazionale di Astrofisica (Italy) ASTRONET Astronomy ERA-net FDR Final Design Review INSU Institut National des Sciences de AT Auxiliary Telescope for the VLTI FE Front End l’Univers (France) ATF Antenna Test Facility (ALMA) FEIC Front End Integration Centres INTA Instituto Nacional de Técnica Aero- AU Astronomical Unit FEROS Fibre-fed, Extended Range, Échelle espacial (Spain) AVO Astrophysical Virtual Observatory Spectrograph (2.2-m) I/O Input/Output BE Back End FINITO Fringe Tracking Instrument Nice IPP Max-Planck-Institut für Plasmaphysik CADC Canadian Astronomy Data Centre Torino (VLTI) IPT Integrated Project Team (ALMA) CAP Journal “Communicating Astronomy FITS Flexible Image Transport System IR InfraRed with the Public” FLAMES Fibre Large Array Multi Element IRACE InfraRed detector high speed Array CASA Offline data reduction software for Spectrograph (VLT) Control and processing Electronics ALMA data FMA Focusing Mirror Array IRAM Institut de Radioastronomie Milli- CAT Coudé Auxiliary Telescope FORS FOcal Reducer/low dispersion Spec- métrique (France) CCD Charge-Coupled Device trograph (VLT) ISAAC Infrared Spectrometer And Array CEA Commissariat à l’énergie atomique FP6 Sixth EC Framework Programme Camera (VLT) CES Coudé Echelle Spectrograph (3.6-m) FP7 Seventh EC Framework Programme ISSI International Space Science Institute CERN European Organisation for Nuclear FTE Full-time equivalent IT Information Technology Research (Conseil Européen pour la ITF Interferometry Task Force Recherche Nucléaire, Switzerland) IVOA International Virtual Observatory CDR Critical Design Review A l l i a n c e CFD Computational Fluid Dynamics IYA International Year of Astronomy CIS Control and Instrument Software JAO Joint ALMA Observatory CLARA Cooperación Latino Americana de JENAM Joint European and National Astron- Redes Avanzadas omy Meeting CLIP Common Library for Image Process- JPG Joint Photographic Experts Group ing (standard for images) CNRS Centre National de la Recherche Sci- JWST James Webb Space Telescope entifique (France) KMOS K -band multi-object spectrograph CODEX Cosmic Dynamics Experiment (VLT) (E-ELT) LABOCA Large APEX Bolometer CAmera CONICA COudé Near-Infrared CAmera (VLT) LBV Luminous Blue Variables COS Cosmic Origins Spectrograph (HST) LCP Liquid Cooling Packages COSMOS Cosmological Evolution Survey LGS Laser Guide Star CPL Common Pipeline Library LGSF Laser Guide Star Facility CRIRES Cryogenic InfraRed Echelle Spectro- LP Large Programme meter (VLT) LPG Liquefied Propane Gas DAZLE Dark Age ‘Z’ Lyman-alpha Explorer LSST Large Synoptic Survey Telescope DFI Data Flow Infrastructure LZOS Lytkarino Optical Glass Factory, DFS Data Flow System Moscow DOORS Requirement management software

98 ESO Annual Report 2007 MACAO Multi-Application Curvature Adaptive OPTICON Optical Infrared Coordination Net- TMT Thirty Meter Telescope Optics (VLT/VLTI) work for Astronomy ToO Target of Opportunity MAD Multi-Conjugate Adaptive Optics OSF ALMA Operations Support Facilities UC Users’ Committee Demonstrator OSIRIS OH-Suppressing InfraRed Imaging UK United Kingdom MATISSE Multi AperTure mid-Infrared Spectro- Spectrograph UKIDSS UKIRT Infrared Deep Sky Survey Scopic Experiment (VLTI) OSO Onsala Space Observatory UKIRT UK Infrared Telescope MCAO Multi-Conjugate Adaptive Optics P2PP Phase 2 Preparation Tool ULTRACAM ULTRA-fast, triple-beam CCD MFPG Multi-Fuel Power Generator P79 Observing Period 79 CAMera (visitors, VLT) MIDI Mid-Infrared Interferometric P80 Observing Period 80 UN United Nations Instrument (VLTI) P81 Observing Period 81 UNCOPUOS United Nations Committee for MISTI MIT International Science and Tech- PA Product Assurance Peaceful Uses of Outer Space nology Initiatives PAD Public Affairs Department UNESCO United Nations Educational, Scien- MIT Massachusetts Institute of Technol- PAE Preliminary Acceptance Europe tific and Cultural Organization ogy PARSEC Sodium line laser for VLT AO UPS Uninterruptible Power Supply MOAO Multi-Objects Adaptive Optics PDR Preliminary Design Review US United States MoU Memorandum of Understanding PI Principal Investigator USB Universal Serial Bus MPE Max Planck Institute for Extraterres- PPDR Pre-Production Design Review UT Unit Telescope of the VLT trial Physics (Germany) PRIMA Phase-Referenced Imaging and UT1–4 VLT Unit Telescope 1–4: Antu, MPI Max Planck Institute Micro-arcsecond Astrometry facility Kueyen, Melipal and Yepun MPIA Max Planck Institute for Astronomy (VLTI) UV UltraViolet (Germany) POC Public Outreach Centre UVES UV-Visual Echelle Spectrograph MPIfR Max Planck Institute for Radioastron- PSD Power Spectral Density (VLT) omy (Germany) PYPS PYramid Phasing Sensor VIMOS VIsible MultiObject Spectrograph MR Medium Resolution QC Quality Control and Data Processing (VLT) MRIP Medium Range Implementation Plan RAL Rutherford Appleton Laboratory VINCI VLT INterferometer Commissionning MUSE Multi Unit Spectroscopic Explorer R&D Research and Development Instrument (VLT) RADIONET Radio Astronomy Network in Europe VIRCAM VISTA IR Camera MW Milky Way REUNA Red Universitaria Nacional VirGO Visual Archive Browser NACO NAOS-CONICA (VLT) ROHS Restriction Of Hazardous Sub- VISA VLTI Sub-Array NAOJ National Astronomical Observatory stances VISIR VLT Mid-Infrared Imager Spectrom of Japan RRM Rapid-Response Mode eter NAOS Nasmyth Adaptive Optics System RTC Regional Training Centre VISTA Visible and Infrared Survey Tele- (VLT) RV Radial Velocity scope for Astronomy NASA National Air and Space Administra- SAC EURO-VO Science Advisory Com- VITRUV Near-IR spectro-imager using fibre tion (US) mittee (VLTI) NED NASA/IPAC Extragalactic Database SAF Science Archive Facility VLT Very Large Telescope NGAS Next Generation Archiving System SDI+ Spectral Differential Imager VLTI Very Large Telescope Interferometer NGC New General detector Controller SED System Engineering Department VLTSW VLT Software NIR Near-InfraRed SEI System Engineering and Integration VO Virtual Observatory NOVA Dutch Research School for Astron- SEWG Software Engineering Working Group VSI VLTI Spectro Imager omy (Nederlandse Onderzoekschool SHAPS Shack-Hartmann sensor VST VLT Survey Telescope voor Astronomie) SINFONI Spectrograph for INtegral Field Ob- VTK Vibration Tracking NRAO National Radio Astronomy Observa- servations in the Near Infrared (VLT) VVDS VIMOS VLT Deep Survey tory SIMBAD Astronomical database WFCAM Wide-Field Infrared Camera NSF National Science Foundation SM Service Mode (UKIDSS) NTT New Technology Telescope SM4 Servicing Mission 4 (HST) WFI Wide Field Imager (2.2-m) OFDR Optical Final Design Review SOCHIAS Chilean Astronomical Society WG Working Group OmegaCAM Optical Camera for the VST SOFI SOn oF Isaac (NTT) WIMPS Weakly Interacting Massive Particles OPC Observing Programmes Committee SPHERE Spectro-Polarimetric High-contrast X-Shooter Wideband UV-IR single target spec- OPD Optical Path Differences Exoplanet Research instrument trograph (VLT) SPIE International Society for Optical XMM-Newton X-ray Multi-Mirror satellite (ESA) Engineering SSA Simple Spectral Access SSP Single Source Procurement SSWG Scientific Strategy Planning Working Group STC Scientific Technical Committee ST-ECF Space Telescope European Coordi- nation Facility STFC Science and Technology Facilities Council (UK) STIS Slit spectrograph (HST) STScI Space Telescope Science Institute (USA) SUSI SUperb Seeing Imager (NTT) SWG Science Working Group SysML System Modeling Language TAC Time Allocation Committee TAC Technical Advisory Committee TB TeraBytes TFB Tunable Filter Bank TIC Technology Information Centre TIMMI Thermal Infrared MultiMode Instru- ment (3.6-m)

ESO Annual Report 2007 99

Publications

Publications in refereed journals based on ESO data

Adami, C.; Ulmer, M. P.; Durret, F.; Covone, G.; Arnouts, S.; Walcher, C. J.; Le Fèvre, O.; Zamorani, Barr, J. M.; Bedregal, A. G.; Aragón-Salamanca, A.; Cypriano, E.; Holden, B. P.; Kron, R.; Lima Neto, G.; Ilbert, O.; Le Brun, V.; Pozzetti, L.; Bardelli, S.; Merrifield, M. R.; Bamford, S. P.; The formation of G. B.; Romer, A. K.; Russeil, D.; Wilhite, B.; An ex- Tresse, L.; Zucca, E.; Charlot, S.; Lamareille, F.; S0 galaxies: evidence from globular clusters; A&A tension of the SHARC survey; A&A 472, 373–381 McCracken, H. J.; Bolzonella, M.; Iovino, A.; 470, 173–178 Ádámkovics, M.; Wong, M. H.; Laver, C.; de Pater, I.; Lonsdale, C.; Polletta, M.; Surace, J.; Bottini, D.; Bazot, M.; Bouchy, F.; Kjeldsen, H.; Charpinet, S.; Widespread Morning Drizzle on Titan; Sci 318, 962 Garilli, B.; Maccagni, D.; Picat, J. P.; Scaramella, Laymand, M.; Vauclair, S.; Asteroseismology of α Agafonova, I. I.; Levshakov, S. A.; Reimers, D.; R.; Scodeggio, M.; Vettolani, G.; Zanichelli, A.; Centauri A. Evidence of rotational splitting; A&A Fechner, C.; Tytler, D.; Simcoe, R. A.; Songaila, A.; Adami, C.; Cappi, A.; Ciliegi, P.; Contini, T.; de La 470, 295–302 Spectral shape of the UV ionizing background and Torre, S.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Bedding, T. R.; Kjeldsen, H.; Arentoft, T.; Bouchy, F.; Heii absorption at redshifts 1.8 < z < 2.9; A&A 461, Guzzo, L.; Marano, B.; Marinoni, C.; Mazure, A.; Brandbyge, J.; Brewer, B. J.; Butler, R. P.; 893–909 Meneux, B.; Merighi, R.; Paltani, S.; Pellò, R.; Christensen-Dalsgaard, J.; Dall, T.; Frandsen, S.; Ahmic, M.; Jayawardhana, R.; Brandeker, A.; Scholz, Pollo, A.; Radovich, M.; Temporin, S.; Vergani, D.; Karoff, C.; Kiss, L. L.; Monteiro, M. J. P. F. G.; Pi- A.; van Kerkwijk, M. H.; Delgado-Donate, E.; The SWIRE-VVDS-CFHTLS surveys: stellar mass jpers, F. P.; Teixeira, T. C.; Tinney, C. G.; Baldry, I. Froebrich, D.; Multiplicity among Young Brown assembly over the last 10 Gyr. Evidence for a K.; Carrier, F.; O’Toole, S. J.; Solar-like Oscillations Dwarfs and Very Low Mass Stars; ApJ 671, major build up of the red sequence between z = 2 in the G2 Subgiant ß Hydri from Dual-Site Obser- 2074–2081 and z = 1; A&A 476, 137–150 vations; ApJ 663, 1315–1324 Aigrain, S.; Hodgkin, S.; Irwin, J.; Hebb, L.; Irwin, M.; Ascenso, J.; Alves, J.; Beletsky, Y.; Lago, M. T. V. T.; Beers, T. C.; Flynn, C.; Rossi, S.; Sommer-Larsen, J.; Favata, F.; Moraux, E.; Pont, F.; The Monitor Near-IR imaging of Galactic massive clusters: Wilhelm, R.; Marsteller, B.; Lee, Y. S.; De Lee, N.; project: searching for occultations in young open Westerlund 2; A&A 466, 137–149 Krugler, J.; Deliyannis, C. P.; Simmons, A. T.; Mills, clusters; MNRAS 375, 29–52 Ascenso, J.; Alves, J.; Vicente, S.; Lago, M. T. V. T.; E.; Zickgraf, F.-J.; Holmberg, J.; Önehag, A.; Albrecht, M.; Krügel, E.; Chini, R.; Dust and CO NTT and VLT diffraction limited imaging of Eriksson, A.; Terndrup, D. M.; Salim, S.; Andersen, emission towards the centers of normal galaxies, Trumpler 14: revealing a massive core-halo cluster; J.; Nordström, B.; Christlieb, N.; Frebel, A.; Rhee,

starburst galaxies and active galactic nuclei. A&A 476, 199–215 J.; Broadband UBVRCIC Photometry of Horizontal- – I. New data and updated catalogue; A&A 462, Azevedo, R.; Folha, D. F. M.; Gameiro, J. F.; Calvet, Branch and Metal-poor Candidates from the HK 575–579 N.; Extended Wind in Jetless Classical T Tauri and Hamburg/ESO Surveys. I.; ApJS 168, Allard, F.; Allard, N. F.; Homeier, D.; Kielkopf, J.; Star TW Hya; ApJ 670, 1234–1239 128–139

McCaughrean, M. J.; Spiegelman, F.; K-H2 quasi- Ballero, S. K.; Matteucci, F.; Origlia, L.; Rich, R. M.; Benaglia, P.; Vink, J. S.; Martí, J.; Maíz Apellániz, J.; molecular absorption detected in the T-dwarf e Formation and evolution of the Galactic bulge: Koribalski, B.; Crowther, P. A.; Testing the pre- Indi Ba; A&A 474, L21–L24 constraints from stellar abundances; A&A 467, dicted mass-loss bi-stability jump at radio wave- Allen, D. M.; Porto de Mello, G. F.; Ruthenium and 123–136 lengths; A&A 467, 1265–1274 hafnium abundances in giant and dwarf barium Ballo, L.; Cristiani, S.; Fasano, G.; Fontanot, F.; Benjamin, J.; Heymans, C.; Semboloni, E.; van stars; A&A 474, 221–228 Monaco, P.; Nonino, M.; Pignatelli, E.; Tozzi, P.; Waerbeke, L.; Hoekstra, H.; Erben, T.; Gladders, Altavilla, G.; Stehle, M.; Ruiz-Lapuente, P.; Mazzali, Vanzella, E.; Fontana, A.; Giallongo, E.; Grazian, M. D.; Hetterscheidt, M.; Mellier, Y.; Yee, H. K. C.; P.; Pignata, G.; Balastegui, A.; Benetti, S.; A.; Danese, L.; Black Hole Masses and Eddington Cosmological constraints from the 100-deg2 Blanc, G.; Canal, R.; Elias-Rosa, N.; Goobar, A.; Ratios of AGNs at z < 1: Evidence of Retriggering weak-lensing survey; MNRAS 381, 702–712 Harutyunyan, A.; Pastorello, A.; Patat, F.; Rich, for a Representative Sample of X-Ray-selected Bensby, T.; Zenn, A. R.; Oey, M. S.; Feltzing, S.; J.; Salvo, M.; Schmidt, B. P.; Stanishev, V.; AGNs; ApJ 667, 97–116 Tracing the Galactic Thick Disk to Solar Metallici- Taubenberger, S.; Turatto, M.; Hillebrandt, W.; Bamford, S. P.; Milvang-Jensen, B.; Aragón- ties; ApJ 663, L13–L16 The early spectral evolution of SN 2004dt; A&A Salamanca, A.; The sizes of disc galaxies in inter- Bergond, G.; Athanassoula, E.; Leon, S.; Balkowski, 475, 585–595 mediate-redshift clusters; MNRAS 378, L6–L10 C.; Cayatte, V.; Chemin, L.; Guzmán, R.; Meylan, Alvarez-Candal, A.; Barucci, M. A.; Merlin, F.; Barbá, R. H.; Arias, J. I.; Geysers in the Lagoon: new G.; Prugniel, P.; Globular clusters and dwarf Guilbert, A.; de Bergh, C.; A search for rotational Herbig-Haro objects in M8; A&A 471, 841–847 galaxies in Fornax. – I. Kinematics in the cluster variations on trans-Neptunian objects; A&A 475, Barbuy, B.; Zoccali, M.; Ortolani, S.; Minniti, D.; Hill, core from multi-object spectroscopy; A&A 464, 369 – 374 V.; Renzini, A.; Bica, E.; Gómez, A.; NGC 6558: A L21–L24 Amram, P.; Mendes de Oliveira, C.; Plana, H.; Blue Horizontal Branch Moderately Metal-Poor Berger, E.; Fox, D. B.; Price, P. A.; Nakar, E.; Balkowski, C.; Hernandez, O.; HCG 31: a multiple Globular Cluster in the Bulge; AJ 134, 1613–1625 Gal-Yam, A.; Holz, D. E.; Schmidt, B. P.; merger in progress; A&A 471, 753–764 Barcons, X.; Carrera, F. J.; Ceballos, M. T.; Page, M. Cucchiara, A.; Cenko, S. B.; Kulkarni, S. R.; Andrievsky, S. M.; Spite, M.; Korotin, S. A.; Spite, F.; J.; Bussons-Gordo, J.; Corral, A.; Ebrero, J.; Soderberg, A. M.; Frail, D. A.; Penprase, B. E.; Bonifacio, P.; Cayrel, R.; Hill, V.; François, P.; Mateos, S.; Tedds, J. A.; Watson, M. G.; Baskill, Rau, A.; Ofek, E.; Burnell, S. J. Bell; Cameron, P. NLTE determination of the sodium abundance in D.; Birkinshaw, M.; Boller, T.; Borisov, N.; Bremer, B.; Cowie, L. L.; Dopita, M. A.; Hook, I.; Peterson, a homogeneous sample of extremely metal-poor M.; Bromage, G. E.; Brunner, H.; Caccianiga, A.; B. A.; Podsiadlowski, P.; Roth, K. C.; Rutledge, stars; A&A 464, 1081–1087 Crawford, C. S.; Cropper, M. S.; Della Ceca, R.; R. E.; Sheppard, S. S.; Songaila, A.; A New Popu- Apai, D.; Bik, A.; Kaper, L.; Henning, T.; Zinnecker, Derry, P.; Fabian, A. C.; Guillout, P.; Hashimoto, Y.; lation of High-Redshift Short-Duration Gamma- H.; Massive Binaries in High-Mass Star-forming Hasinger, G.; Hassall, B. J. M.; Lamer, G.; Loaring, Ray Bursts; ApJ 664, 1000–1010 Regions: A Multiepoch Radial Velocity Survey of N. S.; Maccacaro, T.; Mason, K. O.; McMahon, Bertram, T.; Eckart, A.; Fischer, S.; Zuther, J.; Embedded O Stars; ApJ 655, 484–491 R. G.; Mirioni, L.; Mittaz, J. P. D.; Motch, C.; Straubmeier, C.; Wisotzki, L.; Krips, M.; Molecular Arentoft, T.; de Ridder, J.; Grundahl, F.; Glowienka, Negueruela, I.; Osborne, J. P.; Panessa, F.; Pérez- gas in nearby low-luminosity QSO host galaxies; L.; Waelkens, C.; Dupret, M.-A.; Grigahcène, A.; Fournon, I.; Pye, J. P.; Roberts, T. P.; Rosen, S.; A&A 470, 571–583 Lefever, K.; Jensen, H. R.; Reyniers, M.; Frandsen, Schartel, N.; Schurch, N.; Schwope, A.; Severgnini, Bertoldi, F.; Carilli, C.; Aravena, M.; Schinnerer, E.; S.; Kjeldsen, H.; Oscillating blue stragglers, γ Do- P.; Sharp, R.; Stewart, G. C.; Szokoly, G.; Ullán, Voss, H.; Smolcic, V.; Jahnke, K.; Scoville, N.; radus stars and eclipsing binaries in the open A.; Ward, M. J.; Warwick, R. S.; Wheatley, P. J.; Blain, A.; Menten, K. M.; Lutz, D.; Brusa, M.; cluster NGC 2506; A&A 465, 965–979 Webb, N. A.; Worrall, D.; Yuan, W.; Ziaeepour, H.; Taniguchi, Y.; Capak, P.; Mobasher, B.; Lilly, S.; Arias, J. I.; Barbá, R. H.; Morrell, N. I.; Pre-main- The XMM-Newton serendipitous survey. – IV. Op- Thompson, D.; Aussel, H.; Kreysa, E.; Hasinger, sequence stars in the Lagoon Nebula (M8); tical identification of the XMM-Newton medium G.; Aguirre, J.; Schlaerth, J.; Koekemoer, A.; MNRAS 374, 1253–1263 sensitivity survey (XMS); A&A 476, 1191–1203 COSBO: The MAMBO 1.2 Millimeter Imaging Barnes, A. D.; Casares, J.; Cornelisse, R.; Charles, P. Survey of the COSMOS Field; ApJS 172, 132–149 A.; Steeghs, D.; Hynes, R. I.; O’Brien, K.; Kine- matical studies of the low-mass X-ray binary GRMus (XB 1254–690); MNRAS 380, 1182–1190 Barros, S. C. C.; Marsh, T. R.; Dhillon, V. S.; Groot, P. J.; Littlefair, S.; Nelemans, G.; Roelofs, G.; Steeghs, D.; Wheatley, P. J.; ULTRACAM photometry of the ultracompact binaries V407 Vul and HM Cnc; MNRAS 374, 1334–1346

ESO Annual Report 2007 101 Berta, S.; Lonsdale, C. J.; Polletta, M.; Savage, R. S.; Bonifacio, P.; Pasquini, L.; Molaro, P.; Carretta, E.; Bruntt, H.; Stello, D.; Suárez, J. C.; Arentoft, T.; Franceschini, A.; Buttery, H.; Cimatti, A.; Dias, J.; François, P.; Gratton, R. G.; James, G.; Sbordone, Bedding, T. R.; Bouzid, M. Y.; Csubry, Z.; Dall, T. Feruglio, C.; Fiore, F.; Held, E. V.; La Franca, F.; L.; Spite, F.; Zoccali, M.; Variations in the H.; Dind, Z. E.; Frandsen, S.; Gilliland, R. L.; Maiolino, R.; Marconi, A.; Matute, I.; Oliver, S. J.; lithium abundances of turn off stars in the globular Jacob, A. P.; Jensen, H. R.; Kang, Y. B.; Kim, Ricciardelli, E.; Rubele, S.; Sacchi, N.; Shupe, D.; cluster 47 Tucanae; A&A 470, 153–159 S.-L.; Kiss, L. L.; Kjeldsen, H.; Koo, J.-R.; Lee, Surace, J.; The contribution of very massive high- Borges Fernandes, M.; Kraus, M.; Lorenz Martins, S.; J.-A.; Lee, C.-U.; Nuspl, J.; Sterken, C.; Szabó, R.; redshift SWIRE galaxies to the stellar mass func- de Araújo, F. X.; On the evolutionary stage of the Multisite campaign on the open cluster M67 – III. δ tion; A&A 476, 151–175 unclassified B[e] star CD-42°11721; MNRAS 377, Scuti pulsations in the blue stragglers; MNRAS Beuermann, K.; Euchner, F.; Reinsch, K.; Jordan, S.; 1343–1362 378, 1371–1384 Gänsicke, B. T.; Zeeman tomography of magnetic Borissova, J.; Ivanov, V. D.; Stephens, A. W.; Brusa, M.; Zamorani, G.; Comastri, A.; Hasinger, G.; white dwarfs. – IV. The complex field structure of Catelan, M.; Minniti, D.; Prieto, G.; A deep near-in- Cappelluti, N.; Civano, F.; Finoguenov, A.; Mainieri, the polars EF Eridani, BL Hydri and CP Tucanae; frared view of the Galactic globular cluster 2 V.; Salvato, M.; Vignali, C.; Elvis, M.; Fiore, F.; Gilli, A&A 463, 647–655 MASS GC 02; A&A 474, 121–127 R.; Impey, C. D.; Lilly, S. J.; Mignoli, M.; Silverman, Biazzo, K.; Pasquini, L.; Girardi, L.; Frasca, A.; da Bornancini, C. G.; De Breuck, C.; de Vries, W.; Croft, J.; Trump, J.; Urry, C. M.; Bender, R.; Capak, P.; Silva, L.; Setiawan, J.; Marilli, E.; Hatzes, A. P.; S.; van Breugel, W.; Röttgering, H.; Minniti, D.; Im- Huchra, J. P.; Kneib, J. P.; Koekemoer, A.; Catalano, S.; Deriving temperature, mass, and aging and spectroscopy of ultrasteep spectrum Leauthaud, A.; Lehmann, I.; Massey, R.; Matute, age of evolved stars from high-resolution spectra. radio sources; MNRAS 378, 551–562 I.; McCarthy, P. J.; McCracken, H. J.; Rhodes, J.; Application to field stars and the open cluster Bosch-Ramon, V.; Motch, C.; Ribó, M.; Lopes de Scoville, N. Z.; Taniguchi, Y.; Thompson, D.; The IC 4651; A&A 475, 981–989 Oliveira, R.; Janot-Pacheco, E.; Negueruela, I.; XMM-Newton Wide-Field Survey in the COSMOS Biller, B. A.; Close, L. M.; Masciadri, E.; Nielsen, E.; Paredes, J. M.; Martocchia, A.; Exploring the con- Field. – III. Optical Identification and Multiwave- Lenzen, R.; Brandner, W.; McCarthy, D.; Hartung, nection between the stellar wind and the non- length Properties of a Large Sample of X-Ray-Se- M.; Kellner, S.; Mamajek, E.; Henning, T.; Miller, thermal emission in LS 5039; A&A 473, 545–550 lected Sources; ApJS 172, 353–367 D.; Kenworthy, M.; Kulesa, C.; An Imaging Survey Bot, C.; Boulanger, F.; Rubio, M.; Rantakyro, F.; Bujarrabal, V.; van Winckel, H.; Neri, R.; Alcolea, J.; for Extrasolar Planets around 45 Close, Young Millimeter dust continuum emission revealing the Castro-Carrizo, A.; Deroo, P.; The nebula around Stars with the Simultaneous Differential Imager at true mass of giant molecular clouds in the Small the post-AGB star 89 Herculis; A&A 468, L45–L48 the Very Large Telescope and MMT; ApJS 173, Magellanic Cloud; A&A 471, 103–112 Burenin, R. A.; Vikhlinin, A.; Hornstrup, A.; Ebeling, 143–165 Bouché, N.; Murphy, M. T.; Péroux, C.; Davies, R.; H.; Quintana, H.; Mescheryakov, A.; The 400 Blundell, K. M.; Bowler, M. G.; Schmidtobreick, L.; Eisenhauer, F.; Förster Schreiber, N. M.; Tacconi, Square Degree ROSAT PSPC Galaxy Cluster Sur- Fluctuations and symmetry in the speed and di- L.; The SINFONI Mg ii Program for Line Emitters vey: Catalog and Statistical Calibration; ApJS 172, rection of the jets of SS 433 on different time (SIMPLE): Discovering Starbursts near QSO Sight 561–582 scales; A&A 474, 903–910 Lines; ApJ 669, L5–L8 Butler, D. J.; Martínez-Delgado, D.; Rix, H.-W.; Boehnhardt, H.; Pompei, E.; Tozzi, G. P.; Hainaut, O.; Bouché, N.; Cresci, G.; Davies, R.; Eisenhauer, F.; Peñarrubia, J.; de Jong, J. T. A.; A Canis Major Ageorges, N.; Bagnulo, S.; Barrera, L.; Bonev, T.; Förster Schreiber, N. M.; Genzel, R.; Gillessen, S.; Overdensity Imaging Survey. – I. Stellar Content Käufl, H. U.; Kerber, F.; Locurto, G.; Marco, O.; Lehnert, M.; Lutz, D.; Nesvadba, N.; Shapiro, K. and Star-Count Maps: A Distinctly Elongated Pantin, E.; Rauer, H.; Saviane, I.; Selman, F.; L.; Sternberg, A.; Tacconi, L. J.; Verma, A.; Body of Main-Sequence Stars; AJ 133, Sterken, C.; Weiler, M.; Broad- and narrowband Cimatti, A.; Daddi, E.; Renzini, A.; Erb, D. K.; 2274–2290 visible imaging of comet 9P/Tempel 1 at ESO Shapley, A.; Steidel, C. C.; Dynamical Properties Caballero, J. A.; Béjar, V. J. S.; Rebolo, R.; Eislöffel, around the time of the Deep Impact event; A&A of z ~ 2 Star-forming Galaxies and a Universal J.; Zapatero Osorio, M. R.; Mundt, R.; Barrado Y 470, 1175–1183 Star Formation Relation; ApJ 671, 303–309 Navascués, D.; Bihain, G.; Bailer-Jones, C. A. L.; Böhm, A.; Ziegler, B. L.; Evolution of Field Spiral Bouvier, J.; Alencar, S. H. P.; Boutelier, T.; Dougados, Forveille, T.; Martín, E. L.; The substellar mass Galaxies up to Redshifts z = 1; ApJ 668, 846–852 C.; Balog, Z.; Grankin, K.; Hodgkin, S. T.; function in σ Orionis. – II. Optical, near-infrared Bondar, A.; Kozak, M.; Gnacin´ski, P.; Galazutdinov, Ibrahimov, M. A.; Kun, M.; Magakian, T. Y.; Pinte, and IRAC/Spitzer photometry of young cluster G. A.; Beletsky, Y.; Krełowski, J.; CaFe interstellar C.; Magnetospheric accretion-ejection processes brown dwarfs and planetary-mass objects; A&A clouds; MNRAS 378, 893–900 in the classical T Tauri star AA Tauri; A&A 463, 470, 903–918 Bonfils, X.; Mayor, M.; Delfosse, X.; Forveille, T.; 1017–1028 Caccianiga, A.; Severgnini, P.; Della Ceca, R.; Gillon, M.; Perrier, C.; Udry, S.; Bouchy, F.; Lovis, Bouy, H.; Huélamo, N.; Martín, E. L.; Barrado Y Maccacaro, T.; Carrera, F. J.; Page, M. J.; Elusive C.; Pepe, F.; Queloz, D.; Santos, N. C.; Bertaux, Navascués, D.; Sterzik, M.; Pantin, E.; A mid- AGN in the XMM-Newton bright serendipitous J.-L.; The HARPS search for southern extra-solar infrared study of very low mass stars and brown survey; A&A 470, 557–570

planets. – X. A m sin i = 11 M⊕ planet around the dwarfs in Upper Scorpius; A&A 463, 641–646 Cadolle Bel, M.; Ribó, M.; Rodriguez, J.; Chaty, S.; nearby spotted M dwarf GJ 674; A&A 474, Braglia, F.; Pierini, D.; Böhringer, H.; Flaming, bright Corbel, S.; Goldwurm, A.; Frontera, F.; Farinelli, R.; 293–299 galaxies along the filaments of A 2744; A&A 470, D’Avanzo, P.; Tarana, A.; Ubertini, P.; Laurent, P.; Bongiorno, A.; Zamorani, G.; Gavignaud, I.; Marano, 425–429 Goldoni, P.; Mirabel, I. F.; Simultaneous B.; Paltani, S.; Mathez, G.; Møller, P.; Picat, Brand, J.; Wouterloot, J. G. A.; A star cluster at the Multiwavelength Observations of the Low/Hard J. P.; Cirasuolo, M.; Lamareille, F.; Bottini, D.; edge of the Galaxy; A&A 464, 909–920 State of the X-Ray Transient Source SWIFT Garilli, B.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Bresolin, F.; Urbaneja, M. A.; Gieren, W.; Pietrzyn´ski, J1753.5–0127; ApJ 659, 549–560 Scaramella, R.; Scodeggio, M.; Tresse, L.; G.; Kudritzki, R.-P.; VLT Spectroscopy of Blue Su- Caffau, E.; Faraggiana, R.; Bonifacio, P.; Ludwig, Vettolani, G.; Zanichelli, A.; Adami, C.; Arnouts, S.; pergiants in IC 1613; ApJ 671, 2028–2039 H.-G.; Steffen, M.; Sulphur abundances from the Bardelli, S.; Bolzonella, M.; Cappi, A.; Charlot, S.; Briquet, M.; Hubrig, S.; Schöller, M.; De Cat, P.; S i near-infrared triplet at 1045 nm; A&A 470, Ciliegi, P.; Contini, T.; Foucaud, S.; Franzetti, P.; Discovery of magnetic fields in three He variable 699–708 Guzzo, L.; Ilbert, O.; Iovino, A.; McCracken, H. J.; Bp stars with He and Si spots; AN 328, 41–45 Calamida, A.; Bono, G.; Stetson, P. B.; Freyhammer, Marinoni, C.; Mazure, A.; Meneux, B.; Merighi, R.; Broderick, J. W.; De Breuck, C.; Hunstead, R. W.; L. M.; Cassisi, S.; Grundahl, F.; Pietrinferni, A.; Pellò, R.; Pollo, A.; Pozzetti, L.; Radovich, M.; Seymour, N.; An extreme rotation measure in Hilker, M.; Primas, F.; Richtler, T.; Romaniello, M.; Zucca, E.; Hatziminaoglou, E.; Polletta, M.; Bondi, the high-redshift radio galaxy PKS B0529–549; Buonanno, R.; Caputo, F.; Castellani, M.; Corsi, C. M.; Brinchmann, J.; Cucciati, O.; de La Torre, S.; MNRAS 375, 1059–1069 E.; Ferraro, I.; Iannicola, G.; Pulone, L.; Strömgren Gregorini, L.; Mellier, Y.; Merluzzi, P.; Temporin, S.; Broeg, C.; Schmidt, T. O. B.; Guenther, E.; Gaedke, Photometry of Galactic Globular Clusters. – I. New Vergani, D.; Walcher, C. J.; The VVDS type-1 AGN A.; Bedalov, A.; Neuhäuser, R.; Walter, F. M.; Rota- Calibrations of the Metallicity Index; ApJ 670, sample: the faint end of the luminosity function; tional period of GQ Lupi; A&A 468, 1039–1044 400–422 A&A 472, 443–454 Cameron, E.; Driver, S. P.; The galaxy luminosity-size Bonifacio, P.; Molaro, P.; Sivarani, T.; Cayrel, R.; relation and selection biases in the Hubble Ultra Spite, M.; Spite, F.; Plez, B.; Andersen, J.; Barbuy, Deep Field; MNRAS 377, 523–534 B.; Beers, T. C.; Depagne, E.; Hill, V.; François, P.; Nordström, B.; Primas, F.; First stars VII – Lithium in extremely metal poor dwarfs; A&A 462, 851–864

102 ESO Annual Report 2007 Camilo, F.; Ransom, S. M.; Peñalver, J.; Karastergiou, Carrera, R.; Gallart, C.; Pancino, E.; Zinn, R.; The Chesneau, O.; Lykou, F.; Balick, B.; Lagadec, E.; A.; van Kerkwijk, M. H.; Durant, M.; Halpern, J. P.; Infrared Ca ii Triplet as Metallicity Indicator; AJ Matsuura, M.; Smith, N.; Spang, A.; Wolf, S.; Reynolds, J.; Thum, C.; Helfand, D. J.; Zimmerman, 134, 1298–1314 Zijlstra, A. A.; A silicate disk in the heart of the Ant; N.; Cognard, I.; The Variable Radio-to-X-Ray Carretta, E.; Bragaglia, A.; Gratton, R. G.; The A&A 473, L29–L32 Spectrum of the Magnetar XTE J1810–197; ApJ chemical abundance of the very metal-rich old Chieregato, M.; Miranda, M.; Jetzer, P.; Q0045-3337: 669, 561–569 open clusters NGC 6253 and NGC 6791; A&A 473, models including strong lensing by a spiral galaxy; Campeggio, L.; Strafella, F.; Maiolo, B.; Elia, D.; 129–141 A&A 474, 777–782 Aiello, S.; Total to Selective Extinction in the Dark Carraro, G.; Geisler, D.; Villanova, S.; Frinchaboy, P. Chilingarian, I.; Cayatte, V.; Chemin, L.; Durret, F.; Globule CB 107; ApJ 668, 316–330 M.; Majewski, S. R.; Old open clusters in the outer Laganá, T. F.; Adami, C.; Slezak, E.; Discovery of Cantalupo, S.; Lilly, S. J.; Porciani, C.; Plausible Galactic disk; A&A 476, 217–227 a new M32-like “Compact Elliptical” galaxy in the Fluorescent Lyα Emitters around the z = 3.1 QSO Carretta, E.; Recio-Blanco, A.; Gratton, R. G.; Piotto, halo of the Abell 496 cD galaxy; A&A 466, 0420–388; ApJ 657, 135–144 G.; Bragaglia, A.; The Link between Chemical L21–L24 Caputi, K. I.; Lagache, G.; Yan, L.; Dole, H.; Anomalies along the Red Giant Branch and the Civano, F.; Mignoli, M.; Comastri, A.; Vignali, C.; Bavouzet, N.; Le Floc’h, E.; Choi, P. I.; Helou, G.; Horizontal Branch Extension in Globular Clusters; Fiore, F.; Pozzetti, L.; Brusa, M.; La Franca, F.; Matt, Reddy, N.; The Infrared Luminosity Function of ApJ 671, L125–L128 G.; Puccetti, S.; Cocchia, F.; The HELLAS2XMM Galaxies at Redshifts z = 1 and z ~ 2 in the Casares, J.; Bonifacio, P.; González Hernández, J. I.; survey. – XI. Unveiling the nature of X-ray bright GOODS Fields; ApJ 660, 97–116 Molaro, P.; Zoccali, M.; The isotopic 6Li/7Li ratio in optically normal galaxies; A&A 476, 1223–1233 Carmona, A.; van den Ancker, M. E.; Henning, T.; Centaurus X-4 and the origin of Li in X-ray bina- Clausen, J. V.; Helt, B. E.; Giménez, A.; Vaz, L. P. R.; Optical spectroscopy of close companions to ries; A&A 470, 1033–1041 García, J. M.; Olsen, E. H.; Southworth, J.; Four- nearby Herbig Ae/Be and T Tauri stars; A&A 464, Casassus, S.; Nyman, L.-Å.; Dickinson, C.; Pearson, colour photometry of eclipsing binaries. 687–695 T. J.; A centimetre-wave excess over free-free – XL. uvby light curves for the B-type systems DW Carmona, A.; van den Ancker, M. E.; Henning, T.; emission in planetary nebulae; MNRAS 382, Carinae, BF Centauri, AC Velorum, and NSV 5783; Goto, M.; Fedele, D.; Stecklum, B.; A search for 1607–1622 A&A 461, 1065–1075 near-infrared molecular hydrogen emission in the Cassata, P.; Guzzo, L.; Franceschini, A.; Scoville, N.; Close, L. M.; Thatte, N.; Nielsen, E. L.; Abuter, R.; CTTS LkHα 264 and the debris disk 49 Ceti; A&A Capak, P.; Ellis, R. S.; Koekemoer, A.; McCracken, Clarke, F.; Tecza, M.; New Photometry and Spec- 476, 853–862 H. J.; Mobasher, B.; Renzini, A.; Ricciardelli, E.; tra of AB Doradus C: An Accurate Mass Determi- Carpano, S.; Pollock, A. M. T.; Wilms, J.; Ehle, M.; Scodeggio, M.; Taniguchi, Y.; Thompson, D.; nation of a Young Low-Mass Object with Theoreti- Schirmer, M.; A Wolf-Rayet/black-hole X-ray bi- The Cosmic Evolution Survey (COSMOS): The cal Evolutionary Tracks; ApJ 665, 736–743 nary candidate in NGC 300; A&A 461, L9–L12 Morphological Content and Environmental De- Cocchia, F.; Fiore, F.; Vignali, C.; Mignoli, M.; Brusa, Carquillat, J.-M.; Prieur, J.-L.; Contribution to the pendence of the Galaxy Color-Magnitude Relation M.; Comastri, A.; Feruglio, C.; Baldi, A.; Carangelo, study of composite spectra: XI. Orbital elements at z ~ 0.7; ApJS 172, 270–283 N.; Ciliegi, P.; D’Elia, V.; La Franca, F.; Maiolino, R.; of some faint systems; AN 328, 46–54 Castellani, V.; Calamida, A.; Bono, G.; Stetson, P. B.; Matt, G.; Molendi, S.; Perola, G. C.; Puccetti, S.; Carretta, E.; Bragaglia, A.; Gratton, R. G.; Momany, Freyhammer, L. M.; Degl’Innocenti, S.; Moroni, P. The HELLAS2XMM survey. – VIII. Optical identifi- Y.; Recio-Blanco, A.; Cassisi, S.; François, P.; Prada; Monelli, M.; Corsi, C. E.; Nonino, M.; cations of the extended sample; A&A 466, 31–40 James, G.; Lucatello, S.; Moehler, S.; Na-O Buonanno, R.; Caputo, F.; Castellani, M.; Dall’Ora, Coccato, L.; Corsini, E. M.; Pizzella, A.; Bertola, F.; anticorrelation and horizontal branches. – VI. M.; Del Principe, M.; Ferraro, I.; Iannicola, G.; The search for inner polar disks with integral The chemical composition of the peculiar bulge Piersimoni, A. M.; Pulone, L.; Vuerli, C.; Star field spectroscopy: the case of NGC 2855 and globular cluster NGC 6388; A&A 464, 967–981 Counts in the Globular Cluster ω Centauri. – I. NGC 7049; A&A 465, 777–786 Carretta, E.; Bragaglia, A.; Gratton, R. G.; Catanzaro, Bright Stellar Components; ApJ 663, 1021–1039 Codella, C.; Cabrit, S.; Gueth, F.; Cesaroni, R.; G.; Leone, F.; Sabbi, E.; Cassisi, S.; Claudi, R.; Castelli, F.; Hubrig, S.; A refined analysis of the Bacciotti, F.; Lefloch, B.; McCaughrean, M. J.; A D’Antona, F.; François, P.; James, G.; Piotto, G.; remarkable Bp star HR 6000; A&A 475, 1041–1052 highly-collimated SiO jet in the HH212 protostellar Na-O anticorrelation and horizontal branches. Castellano, M.; Salimbeni, S.; Trevese, D.; Grazian, outflow; A&A 462, L53–L56 – IV. Detection of He-rich and He-poor stellar A.; Pentericci, L.; Fiore, F.; Fontana, A.; Giallongo, Comerón, F.; Schneider, N.; A close look at the heart populations in the globular cluster NGC 6218; E.; Santini, P.; Cristiani, S.; Nonino, M.; Vanzella, of RCW 108; A&A 473, 149–162 A&A 464, 939–951 E.; A Photometrically Detected Forming Cluster of Cooke, R.; Kuncic, Z.; Sharp, R.; Bland-Hawthorn, Carretta, E.; Bragaglia, A.; Gratton, R. G.; Lucatello, Galaxies at Redshift 1.6 in the GOODS Field; ApJ J.; Spectacular Trailing Streamers near LMC X-1: S.; Momany, Y.; Na-O anticorrelation and horizon- 671, 1497–1502 The First Evidence of a Jet?; ApJ 667, L163–L166 tal branches. – II. The Na-O anticorrelation in the Cayrel, R.; Steffen, M.; Chand, H.; Bonifacio, P.; Copetti, M. V. F.; Oliveira, V. A.; Riffel, R.; Castañeda, globular cluster NGC 6752; A&A 464, 927–937 Spite, M.; Spite, F.; Petitjean, P.; Ludwig, H.-G.; H. O.; Sanmartim, D.; A study of the neglected Carraro, G.; Zinn, R.; Moni Bidin, C.; Whiting 1: the Caffau, E.; Line shift, line asymmetry, and the Galactic H ii region NGC 2579 and its companion youngest globular cluster associated with the 6Li/7Li isotopic ratio determination; A&A 473, ESO 370–9; A&A 472, 847–854 Sagittarius dwarf spheroidal galaxy; A&A 466, L37–L40 Cornelisse, R.; Casares, J.; Steeghs, D.; Barnes, A. 181–189 Chauvin, G.; Lagrange, A.-M.; Udry, S.; Mayor, M.; D.; Charles, P. A.; Hynes, R. I.; O’Brien, K.; A de- Carraro, G.; de La Fuente Marcos, R.; Villanova, S.; Characterization of the long-period companions tection of the donor star of Aquila X-1 during its Moni Bidin, C.; de La Fuente Marcos, C.; of the exoplanet host stars: HD 196885, HD 1237 2004 outburst?; MNRAS 375, 1463–1470 Baumgardt, H.; Solivella, G.; Observational tem- and HD 27442. VLT/NACO and SINFONI near-in- Cornelisse, R.; Steeghs, D.; Casares, J.; Charles, P. plates of star cluster disruption. The stellar group frared, follow-up imaging and spectroscopy; A&A A.; Barnes, A. D.; Hynes, R. I.; O’Brien, K.; Optical NGC 1901 in front of the Large Magellanic Cloud; 475, 723–727 spectroscopy of the low-mass X-ray binary A&A 466, 931–941 Chen, H.-W.; Prochaska, J. X.; Ramirez-Ruiz, E.; GX9+9; MNRAS 380, 1219–1229 Carrier, F.; Kjeldsen, H.; Bedding, T. R.; Brewer, B. J.; Bloom, J. S.; Dessauges-Zavadsky, M.; Foley, R. Cornelisse, R.; Steeghs, D.; Casares, J.; Charles, P. Butler, R. P.; Eggenberger, P.; Grundahl, F.; J.; On the Absence of Wind Signatures in GRB Af- A.; Shih, I. C.; Hynes, R. I.; O’Brien, K.; A signa- McCarthy, C.; Retter, A.; Tinney, C. G.; Solar-like terglow Spectra: Constraints on the Wolf-Rayet ture of the donor star in the extra-galactic X-ray oscillations in the metal-poor subgiant ν Indi. Winds of GRB Progenitors; ApJ 663, 420–436 binary LMCX-2; MNRAS 381, 194–200 – II. Acoustic spectrum and mode lifetime; A&A Chen, X. P.; Launhardt, R.; Henning, T.; VLT/NACO Corradi, R. L. M.; Steffen, M.; Schönberner, D.; 470, 1059–1063 adaptive optics imaging of GSS 30 IRS1: a proto- Jacob, R.; A hydrodynamical study of multiple- Carrier, F.; Eggenberger, P.; Leyder, J.-C.; Debernardi, stellar binary system?; A&A 475, 277–280 shell planetary nebulae. – II. Measuring the post- Y.; Royer, F.; A search for solar-like oscillations in Chesneau, O.; Nardetto, N.; Millour, F.; Hummel, C.; shock velocities in the shells; A&A 474, 529–539 the Am star HD 209625; A&A 470, 1009–1012 Domiciano de Souza, A.; Bonneau, D.; Vannier, Corsini, E. M.; Aguerri, J. A. L.; Debattista, Victor P.; M.; Rantakyrö, F.; Spang, A.; Malbet, F.; Mourard, Pizzella, A.; Barazza, F. D.; Jerjen, H.; The Bar D.; Bode, M. F.; O’Brien, T. J.; Skinner, G.; Petrov, Pattern Speed of Dwarf Galaxy NGC 4431; ApJ R. G.; Stee, P.; Tatulli, E.; Vakili, F.; AMBER/VLTI 659, L121–L124 interferometric observations of the recurrent Nova RS Ophiuchii 5.5 days after outburst; A&A 464, 119–126

ESO Annual Report 2007 103 Cortese, L.; Marcillac, D.; Richard, J.; Bravo-Alfaro, Dasyra, K. M.; Tacconi, L. J.; Davies, R. I.; Genzel, de Ugarte Postigo, A.; Fatkhullin, T. A.; Jóhannesson, H.; Kneib, J.-P.; Rieke, G.; Covone, G.; Egami, E.; R.; Lutz, D.; Peterson, B. M.; Veilleux, S.; Baker, A. G.; Gorosabel, J.; Sokolov, V. V.; Castro-Tirado, A. Rigby, J.; Czoske, O.; Davies, J.; The strong trans- J.; Schweitzer, M.; Sturm, E.; Host Dynamics and J.; Balega, Y. Y.; Spiridonova, O. I.; Jelínek, M.; formation of spiral galaxies infalling into massive Origin of Palomar-Green QSOs; ApJ 657, 102–115 Guziy, S.; Pérez-Ramírez, D.; Hjorth, J.; Laursen, clusters at z ~ 0.2; MNRAS 376, 157–172 Davies, R. I.; Mueller Sánchez, F.; Genzel, R.; P.; Bersier, D.; Pandey, S. B.; Bremer, M.; Cowley, C. R.; Hubrig, S.; Castelli, F.; González, J. F.; Tacconi, L. J.; Hicks, E. K. S.; Friedrich, S.; Monfardini, A.; Huang, K. Y.; Urata, Y.; Ip, W. H.; Wolff, B.; Heavy calcium in CP stars; MNRAS 377, Sternberg, A.; A Close Look at Star Formation Tamagawa, T.; Kinoshita, D.; Mizuno, T.; Arai, Y.; 1579–1587 around Active Galactic Nuclei; ApJ 671, 1388–1412 Yamagishi, H.; Soyano, T.; Usui, F.; Tashiro, M.; Cox, N. L. J.; Cordiner, M. A.; Ehrenfreund, P.; Kaper, de Jong, J. T. A.; Butler, D. J.; Rix, H. W.; Dolphin, A. Abe, K.; Onda, K.; Aslan, Z.; Khamitov, I.; Ozisik, L.; Sarre, P. J.; Foing, B. H.; Spaans, M.; Cami, J.; E.; Martínez-Delgado, D.; Modeling the Stellar T.; Kiziloglu, U.; Bikmaev, I.; Sakhibullin, N.; Bu- Sofia, U. J.; Clayton, G. C.; Gordon, K. D.; Salama, Populations in the Canis Major Overdensity: The renin, R.; Pavlinsky, M.; Sunyaev, R.; F.; Interstellar gas, dust and diffuse bands in the Relation between the Old and Young Populations; Bhattacharya, D.; Kamble, A. P.; Ishwara Chandra, SMC; A&A 470, 941–955 ApJ 662, 259–271 C. H.; Trushkin, S. A.; Extensive multiband study Cresci, G.; Mannucci, F.; Della Valle, M.; Maiolino, R.; De Lucia, G.; Poggianti, B. M.; Aragón-Salamanca, of the X-ray rich GRB 050408. A likely off-axis A NICMOS search for obscured supernovae in A.; White, S.D. M.; Zaritsky, D.; Clowe, D.; event with an intense energy injection; A&A 462, starburst galaxies; A&A 462, 927–931 Halliday, C.; Jablonka, P.; von der Linden, A.; L57–L60 Crowther, P. A.; Carpano, S.; Hadfield, L. J.; Pollock, Milvang-Jensen, B.; Pelló, R.; Rudnick, G.; Saglia, de Vries, N.; Snellen, I. A. G.; Schilizzi, R. T.; Lehnert, A. M. T.; On the optical counterpart of NGC 300 R. P.; Simard, L.; The build-up of the colour-mag- M. D.; Bremer, M. N.; Complete identification of X-1 and the global Wolf-Rayet content of NGC 300; nitude relation in galaxy clusters since z ~ 0.8; the Parkes half-Jansky sample of GHz peaked A&A 469, L31–L34 MNRAS 374, 809–822 spectrum radio galaxies; A&A 464, 879–883 Cuby, J.-G.; Hibon, P.; Lidman, C.; Le Fèvre, O.; de Lapparent, V.; Slezak, E.; Spatial clustering in the de Wit, W. J.; Hoare, M. G.; Oudmaijer, R. D.; Gilmozzi, R.; Moorwood, A.; van der Werf, P.; A ESO-Sculptor survey: two-point correlation func- Mottram, J. C.; VLTI/MIDI 10 μm Interferometry narrow-band search for Lyα emitting galaxies at tions by galaxy type at redshifts 0.1–0.5; A&A 472, of the Forming Massive Star W33A; ApJ 671, L1 z = 8.8; A&A 461, 911–916 29–49 69–L172 Curran, S. J.; Tzanavaris, P.; Murphy, M. T.; Webb, J. de Luca, M.; Giannini, T.; Lorenzetti, D.; Massi, F.; Dehaes, S.; Groenewegen, M. A. T.; Decin, L.; Hony, K.; Pihlström, Y. M.; Detection of broad 21-cm ab- Elia, D.; Nisini, B.; Near- and far-infrared counter- S.; Raskin, G.; Blommaert, J. A. D. L.; Continuum sorption at zabs = 0.656 in the complex sight-line parts of millimeter dust cores in the Vela molecu- emission around AGB stars at 1.2 mm; MNRAS towards 3C336; MNRAS 381, L6–L10 lar ridge cloud D; A&A 474, 863–872 377, 931–944 D’Elia, V.; Fiore, F.; Meurs, E. J. A.; Chincarini, G.; de La Torre, S.; Le Fèvre, O.; Arnouts, S.; Guzzo, L.; Delbò, M.; Cellino, A.; Tedesco, E. F.; Albedo and Melandri, A.; Norci, L.; Pellizza, L.; Perna, R.; Pi- Farrah, D.; Iovino, A.; Lonsdale, C. J.; Meneux, B.; size determination of potentially hazardous aster- ranomonte, S.; Sbordone, L.; Stella, L.; Oliver, S. J.; Pollo, A.; Waddington, I.; Bottini, D.; oids: (99942) Apophis; Icar 188, 266–269 Tagliaferri, G.; Vergani, S. D.; Ward, P.; Angelini, Fang, F.; Garilli, B.; Le Brun, V.; Maccagni, D.; Demarco, R.; Rosati, P.; Lidman, C.; Girardi, M.; L.; Antonelli, L. A.; Burrows, D. N.; Campana, S.; Picat, J. P.; Scaramella, R.; Scodeggio, M.; Nonino, M.; Rettura, A.; Strazzullo, V.; van der Capalbi, M.; Cimatti, A.; Costa, E.; Cusumano, G.; Shupe, D.; Surace, J.; Tresse, L.; Vettolani, G.; Wel, A.; Ford, H. C.; Mainieri, V.; Holden, B. P.; Della Valle, M.; Filliatre, P.; Fontana, A.; Frontera, Zanichelli, A.; Adami, C.; Bardelli, S.; Bolzonella, Stanford, S. A.; Blakeslee, J. P.; Gobat, R.; F.; Fugazza, D.; Gehrels, N.; Giannini, T.; Giommi, M.; Cappi, A.; Charlot, S.; Ciliegi, P.; Contini, T.; Postman, M.; Tozzi, P.; Overzier, R. A.; Zirm, A. P.; Goldoni, P.; Guetta, D.; Israel, G.; Lazzati, D.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Ilbert, O.; W.; Benítez, N.; Homeier, N. L.; Illingworth, G. D.; Malesani, D.; Marconi, G.; Mason, K.; Mereghetti, Lamareille, F.; McCracken, H. J.; Marano, B.; Ma- Infante, L.; Jee, M. J.; Mei, S.; Menanteau, F.; S.; Mirabel, F.; Molinari, E.; Moretti, A.; Nousek, J.; rinoni, C.; Mazure, A.; Merighi, R.; Paltani, S.; Motta, V.; Zheng, W.; Clampin, M.; Hartig, G.; VLT Perri, M.; Piro, L.; Stratta, G.; Testa, V.; Vietri, M.; Pellò, R.; Pozzetti, L.; Radovich, M.; Zamorani, G.; and ACS Observations of RDCS J1252.9–2927: UVES/VLT high resolution spectroscopy of Zucca, E.; Bondi, M.; Bongiorno, A.; Brinchmann, Dynamical Structure and Galaxy Populations in a GRB 050730 afterglow: probing the features of J.; Cucciati, O.; Mellier, Y.; Merluzzi, P.; Temporin, Massive Cluster at z = 1.237; ApJ 663, 164–182 the GRB environment; A&A 467, 629–639 S.; Vergani, D.; Walcher, C. J.; VVDS-SWIRE. Demory, B.-O.; Gillon, M.; Barman, T.; Bonfils, X.; D’Odorico, V.; A cold metal-poor cloud traced by a Clustering evolution from a spectroscopic sample Mayor, M.; Mazeh, T.; Queloz, D.; Udry, S.; weak Mg ii absorption at z Q 0.45. First detection of galaxies with redshift 0.2 < z < 2.1 selected Bouchy, F.; Delfosse, X.; Forveille, T.; Mallmann, F.; of Si i, Ca i, and Fe i in a QSO absorber; A&A 470, from Spitzer IRAC 3.6 μm and 4.5 μm photometry; Pepe, F.; Perrier, C.; Characterization of the hot 523–529 A&A 475, 443–451 Neptune GJ 436 b with Spitzer and ground-based Daddi, E.; Dickinson, M.; Morrison, G.; Chary, R.; de Luise, F.; Perna, D.; Dotto, E.; Fornasier, S.; observations; A&A 475, 1125–1129 Cimatti, A.; Elbaz, D.; Frayer, D.; Renzini, A.; Pope, Belskaya, I. N.; Boattini, A.; Valsecchi, G. B.; Mi- Deroo, P.; van Winckel, H.; Verhoelst, T.; Min, M.; A.; Alexander, D. M.; Bauer, F. E.; Giavalisco, M.; lani, A.; Rossi, A.; Lazzarin, M.; Paolicchi, P.; Reyniers, M.; Waters, L. B. F. M.; The circumbinary Huynh, M.; Kurk, J.; Mignoli, M.; Multiwavelength Fulchignoni, M.; Physical investigation of the po- disc around the J-type C-star IRAS 18006-3213; Study of Massive Galaxies at z ~ 2. – I. Star For- tentially hazardous Asteroid (144898) 2004 VD17; A&A 467, 1093–1101 mation and Galaxy Growth; ApJ 670, 156–172 Icar 191, 628–635 Deroo, P.; Acke, B.; Verhoelst, T.; Dominik, C.; Tatulli, Daflon, S.; Cunha, K.; de Araújo, F. X.; Wolff, S.; De Rijcke, S.; Zeilinger, W. W.; Hau, G. K. T.; Prugniel, E.; van Winckel, H.; AMBER and MIDI interfer Przybilla, N.; The Projected Rotational Velocity P.; Dejonghe, H.; Generalizations of the Tully- ometric observations of the post-AGB binary Distribution of a Sample of OB stars from a Fisher Relation for Early- and Late-Type Galaxies; IRAS 08544-4431: the circumbinary disc resolved; Calibration Based on Synthetic He i Lines; AJ 134, ApJ 659, 1172–1175 A&A 474, L45–L48 1570–1578 De Silva, G. M.; Freeman, K. C.; Asplund, M.; Bland- Desai, V.; Dalcanton, J. J.; Aragón-Salamanca, A.; Dahlen, T.; Mobasher, B.; Dickinson, M.; Ferguson, Hawthorn, J.; Bessell, M. S.; Collet, R.; Chemical Jablonka, P.; Poggianti, B.; Gogarten, S. M.; Si- H. C.; Giavalisco, M.; Kretchmer, C.; Ravindranath, Homogeneity in Collinder 261 and Implications for mard, L.; Milvang-Jensen, B.; Rudnick, G.; S.; Evolution of the Luminosity Function, Star Chemical Tagging; AJ 133, 1161–1175 Zaritsky, D.; Clowe, D.; Halliday, C.; Pelló, R.; Formation Rate, Morphology, and Size of Star- Saglia, R.; White, S.; The Morphological Content forming Galaxies Selected at Rest-Frame 1500 of 10 EDisCS Clusters at 0.5 < z < 0.8; ApJ 660, and 2 800 Å; ApJ 654, 172–185 1151–1164 Dall, T. H.; Foellmi, C.; Pritchard, J.; Lo Curto, G.; Descamps, P.; Marchis, F.; Michalowski, T.; Vachier, Allende Prieto, C.; Bruntt, H.; Amado, P. J.; F.; Colas, F.; Berthier, J.; Assafin, M.; Dunckel, P. Arentoft, T.; Baes, M.; Depagne, E.; Fernandez, B.; Polinska, M.; Pych, W.; Hestroffer, D.; Miller, K. M.; Ivanov, V.; Koesterke, L.; Monaco, L.; O’Brien, P. M.; Vieira-Martins, R.; Birlan, M.; Teng-Chuen- K.; Sarro, L. M.; Saviane, I.; Scharwächter, J.; Yu, J.-P.; Peyrot, A.; Payet, B.; Dorseuil, J.; Léonie, Schmidtobreick, L.; Schütz, O.; Seifahrt, A.; Y.; Dijoux, T.; Figure of the double Asteroid 90 An- Selman, F.; Stefanon, M.; Sterzik, M.; VSOP: the tiope from adaptive optics and lightcurve observa- variable star one-shot project. – I. Project presen- tions; Icar 187, 482–499 tation and first data release; A&A 470, 1201–1214

104 ESO Annual Report 2007 Desidera, S.; Gratton, R. G.; Lucatello, S.; Endl, M.; Duchêne, G.; Bontemps, S.; Bouvier, J.; André, P.; Fedele, D.; van den Ancker, M. E.; Petr-Gotzens, M. Udry, S.; Accretion of chemically fractionated ma- Djupvik, A. A.; Ghez, A. M.; Multiple protostellar G.; Rafanelli, P.; Optical and infrared properties of terial on a wide binary with a blue straggler; A&A systems. – II. A high resolution near-infrared V1647 Orionis during the 2003–2006 outburst. 462, 1039–1049 imaging survey in nearby star-forming regions; – II. Temporal evolution of the eruptive source; Desort, M.; Lagrange, A.-M.; Galland, F.; Udry, S.; A&A 476, 229–242 A&A 472, 207–217 Mayor, M.; Search for exoplanets with the radial- Ducourant, C.; Teixeira, R.; Hambly, N. C.; Fedele, D.; van den Ancker, M. E.; Petr-Gotzens, M. velocity technique: quantitative diagnostics of Oppenheimer, B. R.; Hawkins, M. R. S.; Rapaport, G.; Ageorges, N.; Rafanelli, P.; Optical and infrared stellar activity; A&A 473, 983–993 M.; Modolo, J.; Lecampion, J. F.; Trigonometric properties of V1647 Orionis during the 2003–2006 Dessauges-Zavadsky, M.; Calura, F.; Prochaska, J. parallaxes of high velocity halo white dwarf candi- outburst. – I. The reflection nebula; A&A 472, X.; D’Odorico, S.; Matteucci, F.; A new compre- dates; A&A 470, 387–394 199–205 hensive set of elemental abundances in DLAs. Duerbeck, H. W.; Rucinski, S. M.; Radial Velocity Feltzing, S.; Fohlman, M.; Bensby, T.; Manganese – III. Star formation histories; A&A 470, 431–448 Studies of Southern Close Binary Stars. trends in a sample of thin and thick disk stars. Díaz-Sánchez, A.; Villo-Pérez, I.; Pérez-Garrido, A.; – II. Spring/Summer Systems; AJ 133, 169–176 The origin of Mn; A&A 467, 665–677 Rebolo, R.; A low mass cluster of extremely red Dumas, C.; Merlin, F.; Barucci, M. A.; de Bergh, C.; Ferrero, P.; Sanchez, S. F.; Kann, D. A.; Klose, S.; galaxies at z = 1.10 in the GOODS Southern Field; Hainault, O.; Guilbert, A.; Vernazza, P.; Greiner, J.; Gorosabel, J.; Hartmann, D. H.; MNRAS 377, 516–522 Doressoundiram, A.; Surface composition of the Henden, A. A.; Møller, P.; Palazzi, E.; Rau, A.;

Díaz, R. F.; Ramírez, S.; Fernández, J. M.; Gallardo, largest dwarf planet 136199 Eris (2003 UB313); Stecklum, B.; Castro-Tirado, A. J.; Fynbo, J. P. U.; J.; Gieren, W.; Ivanov, V. D.; Mauas, P.; Minniti, D.; A&A 471, 331–334 Hjorth, J.; Jakobsson, P.; Kouveliotou, C.; Masetti, Pietrzynski, G.; Pérez, F.; Ruíz, M. T.; Udalski, A.; Dunlop, J. S.; Cirasuolo, M.; McLure, R. J.; A N.; Pian, E.; Tanvir, N. R.; Wijers, R. A. M. J.; Zoccali, M.; Millimagnitude Photometry for Transit- systematic search for very massive galaxies at Constraints on an Optical Afterglow and ing Extrasolar Planetary Candidates. – II. Transits z > 4; MNRAS 376, 1054–1064 on Supernova Light Following the Short Burst of OGLE-TR-113-b in the Optical and Near-IR; ApJ Eggenberger, A.; Udry, S.; Chauvin, G.; Beuzit, J.-L.; GRB 050813; AJ 134, 2118–2123 660, 850–857 Lagrange, A.-M.; Ségransan, D.; Mayor, M.; The Feulner, G.; Goranova, Y.; Hopp, U.; Gabasch, A.; Dietrich, J. P.; Erben, T.; Lamer, G.; Schneider, P.; impact of stellar duplicity on planet occurrence Bender, R.; Botzler, C. S.; Drory, N.; The Munich Schwope, A.; Hartlap, J.; Maturi, M.; BLOX: the and properties. – I. Observational results of a Near-Infrared Cluster Survey – IX. Galaxy evolu- Bonn lensing, optical, and X-ray selected galaxy VLT/NACO search for stellar companions to 130 tion to z ~ 2 from optically selected catalogues; clusters. – I. Cluster catalog construction; A&A nearby stars with and without planets; A&A 474, MNRAS 378, 429–448 470, 821–834 273–291 Firth, P.; Drinkwater, M. J.; Evstigneeva, E. A.; Dimitrijevic´, M. S.; Ryabchikova, T.; Simic´, Z.; Eigenbrod, A.; Courbin, F.; Meylan, G.; Gregg, M. D.; Karick, A. M.; Jones, J. B.; Phillipps, Popovic´, L. Cˇ .; Dacˇic´, M.; The influence of Stark COSMOGRAIL: the COSmological MOnitoring of S.; Compact stellar systems around NGC 1399; broadening on Cr ii spectral line shapes in stellar GRAvItational Lenses. VI. Redshift of the lensing MNRAS 382, 1342–1352 atmospheres; A&A 469, 681–686 galaxy in seven gravitationally lensed quasars; Fivet, V.; Quinet, P.; Biémont, É.; Jorissen, A.; Djorgovski, S. G.; Courbin, F.; Meylan, G.; Sluse, D.; A&A 465, 51–56 Yushchenko, A. V.; van Eck, S.; Transition proba- Thompson, D.; Mahabal, A.; Glikman, E.; Discov- Eisenbeiss, T.; Seifahrt, A.; Mugrauer, M.; Schmidt, bilities in singly ionized promethium and the iden- ery of a Probable Physical Triple Quasar; ApJ 662, T. O. B.; Neuhäuser, R.; Roell, T.; Low-mass visual tification of Pm ii lines in Przybylski’s star and HR L1–L5 binaries in the solar neighbourhood: The case of 465; MNRAS 380, 771–780 Domiciano de Souza, A.; Driebe, T.; Chesneau, O.; HD 141272; AN 328, 521 Foellmi, C.; Dall, T. H.; Depagne, E.; On the abun- Hofmann, K.-H.; Kraus, S.; Miroshnichenko, A. S.; Elia, D.; Massi, F.; Strafella, F.; De Luca, M.; Giannini, dances of GRO J1655-40; A&A 464, L61–L64 Ohnaka, K.; Petrov, R. G.; Preisbisch, T.; Stee, P.; T.; Lorenzetti, D.; Nisini, B.; Campeggio, L.; Folkes, S. L.; Pinfield, D. J.; Kendall, T. R.; Jones, H. Weigelt, G.; Lisi, F.; Malbet, F.; Richichi, A.; Maiolo, B. M. T.; Mapping Molecular Emission in R. A.; Discovery of a nearby L-T transition object AMBER/VLTI and MIDI/VLTI spectro-interferom Vela Molecular Ridge Cloud D; ApJ 655, 316–331 in the Southern Galactic plane; MNRAS 378, etric observations of the B[e] supergiant Ellison, S. L.; Prochaska, J. X.; Lopez, S.; The 901–909 CPD-57°2874. Size and geometry of the circum- Galactic deuterium abundance and dust deple- Folsom, C. P.; Wade, G. A.; Bagnulo, S.; Landstreet, stellar envelope in the near- and mid-IR; A&A 464, tion: insights from an expanded Ti/H sample; J. D.; Rotation and chemical abundances of 81–86 MNRAS 380, 1245–1254 Ap/Bp stars in the open cluster NGC 6475; Doucet, C.; Habart, E.; Pantin, E.; Dullemond, C.; Esposito, M.; Covino, E.; Alcalá, J. M.; Guenther, E. MNRAS 376, 361–370 Lagage, P. O.; Pinte, C.; Duchêne, G.; Ménard, F.; W.; Schisano, E.; MO Lup: a hierarchical triple T Forbrich, J.; Preibisch, T.; Menten, K. M.; Neuhäuser, HD 97048: a closer look at the disk; A&A 470, Tauri system; MNRAS 376, 1805–1813 R.; Walter, F. M.; Tamura, M.; Matsunaga, N.; Ku- 625–631 Evans, C. J.; Bresolin, F.; Urbaneja, M. A.; sakabe, N.; Nakajima, Y.; Brandeker, A.; Douglas, L. S.; Bremer, M. N.; Stanway, E. R.; Pietrzyn´ski, G.; Gieren, W.; Kudritzki, R.-P.; The Fornasier, S.; Posselt, B.; Tachihara, K.; Broeg, C.; Lehnert, M. D.; Discovery of a single faint AGN in ARAUCARIA Project: VLT-FORS Spectroscopy Simultaneous X-ray, radio, near-infrared, and a large sample of z > 5 Lyman break galaxies; of Blue Supergiants in NGC 3109-Classifications, optical monitoring of young stellar objects in the MNRAS 376, 1393–1398 First Abundances, and Kinematics; ApJ 659, Coronet cluster; A&A 464, 1003–1013 Dow-Hygelund, C. C.; Holden, B. P.; Bouwens, R. J.; 1198–1211 Forbrich, J.; Massi, M.; Ros, E.; Brunthaler, A.; Illingworth, G. D.; van der Wel, A.; Franx, M.; van Eyles, L. P.; Bunker, A. J.; Ellis, R. S.; Lacy, M.; Menten, K. M.; Searching for coronal radio emis- Dokkum, P. G.; Ford, H.; Rosati, P.; Magee, D.; Stanway, E. R.; Stark, D. P.; Chiu, K.; The stellar sion from protostars using very-long-baseline Zirm, A.; Spectroscopy of z ~ 6 i-Dropout Galax- mass density at z ~ 6 from Spitzer imaging of interferometry; A&A 469, 985–992 ies: Frequency of Lyα Emission and the Sizes of i’-drop galaxies; MNRAS 374, 910–930 Fornasier, S.; Dotto, E.; Hainaut, O.; Marzari, F.; Lyα-emitting Galaxies; ApJ 660, 47–61 Fangano, A. P. M.; Ferrara, A.; Richter, P.; Absorption Boehnhardt, H.; de Luise, F.; Barucci, M. A.; Driver, S. P.; Popescu, C. C.; Tuffs, R. J.; Liske, J.; features of high-redshift galactic winds; MNRAS Visible spectroscopic and photometric survey of Graham, A. W.; Allen, P. D.; de Propris, R.; The 381, 469–488 Jupiter Trojans: Final results on dynamical fami- Millennium Galaxy Catalogue: the B-band attenu- Faure, C.; Giraud, E.; Melnick, J.; Quintana, H.; lies; Icar 190, 622–642 ation of bulge and disc light and the implied cos- Selman, F.; Wambsganss, J.; An S-shaped arc in Fornasier, S.; Marzari, F.; Dotto, E.; Barucci, M. A.; mic dust and stellar mass densities; MNRAS 379, the galaxy cluster RX J0054.0-2823; A&A 463, Migliorini, A.; Are the E-type asteroids (2867) 1022–1036 833–837 Steins, a target of the Rosetta mission, and NEA Duc, P.-A.; Braine, J.; Lisenfeld, U.; Brinks, E.; Feain, I. J.; Papadopoulos, P. P.; Ekers, R. D.; (3103) Eger remnants of an old asteroid family?; Boquien, M.; VCC 2062: an old tidal dwarf Middelberg, E.; Dressing a Naked Quasar: Star A&A 474, L29–L32 galaxy in the Virgo cluster?; A&A 475, 187–197 Formation and Active Galactic Nucleus Feedback in HE 0450–2958; ApJ 662, 872–877 Fechner, C.; Reimers, D.; Fluctuations of the intergalactic UV background towards two lines of sight; A&A 461, 847–859

ESO Annual Report 2007 105 Fox, A. J.; Petitjean, P.; Ledoux, C.; Srianand, R.; Garavini, G.; Folatelli, G.; Nobili, S.; Aldering, G.; Gilbert, A. M.; Graham, J. R.; Feedback in the Hot halos around high redshift protogalaxies. Ob- Amanullah, R.; Antilogus, P.; Astier, P.; Blanc, G.; Antennae Galaxies (NGC 4038/9). – I. High-Reso- servations of O v i and N v absorption in damped Bronder, T.; Burns, M. S.; Conley, A.; Deustua, S. lution Infrared Spectroscopy of Winds from Super Lyman-α systems; A&A 465, 171–184 E.; Doi, M.; Fabbro, S.; Fadeyev, V.; Gibbons, R.; Star Clusters; ApJ 668, 168–181 Fox, A. J.; Ledoux, C.; Petitjean, P.; Srianand, R.; Goldhaber, G.; Goobar, A.; Groom, D. E.; Hook, I.; Gillon, M.; Pont, F.; Moutou, C.; Santos, N. C.; C iv absorption in damped and sub-damped Howell, D. A.; Kashikawa, N.; Kim, A. G.; Bouchy, F.; Hartman, J. D.; Mayor, M.; Melo, C.; Lyman-α systems. Correlations with metallicity Kowalski, M.; Kuznetsova, N.; Lee, B. C.; Lidman, Queloz, D.; Udry, S.; Magain, P.; The transiting and implications for galactic winds at z ≈ 2–3; C.; Mendez, J.; Morokuma, T.; Motohara, K.; Nu- planet OGLE-TR-132b revisited with new spec- A&A 473, 791–803 gent, P. E.; Pain, R.; Perlmutter, S.; Quimby, R.; troscopy and deconvolution photometry,; A&A Fox, A. J.; Petitjean, P.; Ledoux, C.; Srianand, R.; Raux, J.; Regnault, N.; Ruiz-Lapuente, P.; Sainton, 466, 743–748 Multiphase Plasma in Sub-Damped Lyα Systems: G.; Schahmaneche, K.; Smith, E.; Spadafora, A. Gillon, M.; Pont, F.; Demory, B.-O.; Mallmann, F.; A Hidden Metal Reservoir; ApJ 668, L15–L18 L.; Stanishev, V.; Thomas, R. C.; Walton, N. A.; Mayor, M.; Mazeh, T.; Queloz, D.; Shporer, A.; Franzetti, P.; Scodeggio, M.; Garilli, B.; Vergani, D.; Wang, L.; Wood-Vasey, W. M.; Yasuda, N.; Quan- Udry, S.; Vuissoz, C.; Detection of transits of the Maccagni, D.; Guzzo, L.; Tresse, L.; Ilbert, O.; titative comparison between type Ia supernova nearby hot Neptune GJ 436 b; A&A 472, L13–L16 Lamareille, F.; Contini, T.; Le Fèvre, O.; Zamorani, spectra at low and high redshifts: a case study; Girard, P.; Köppen, J.; Acker, A.; Chemical composi- G.; Brinchmann, J.; Charlot, S.; Bottini, D.; Le A&A 470, 411–424 tions and plasma parameters of planetary nebulae Brun, V.; Picat, J. P.; Scaramella, R.; Vettolani, G.; Garavini, G.; Nobili, S.; Taubenberger, S.; Pastorello, with Wolf-Rayet and wels type central stars; A&A Zanichelli, A.; Adami, C.; Arnouts, S.; Bardelli, S.; A.; Elias-Rosa, N.; Stanishev, V.; Blanc, G.; 463, 265–274 Bolzonella, M.; Cappi, A.; Ciliegi, P.; Foucaud, S.; Benetti, S.; Goobar, A.; Mazzali, P. A.; Sanchez, S. Girart, J. M.; Viti, S.; The origin of the molecular Gavignaud, I.; Iovino, A.; McCracken, H. J.; F.; Salvo, M.; Schmidt, B. P.; Hillebrandt, W.; ESC emission around the southern hemisphere Re 4 Marano, B.; Marinoni, C.; Mazure, A.; Meneux, B.; observations of SN 2005cf. – II. Optical spectros- IRS – HH 188 region; A&A 470, 633–638 Merighi, R.; Paltani, S.; Pellò, R.; Pollo, A.; copy and the high-velocity features; A&A 471, Gorgas, J.; Jablonka, P.; Goudfrooij, P.; Stellar popu- Pozzetti, L.; Radovich, M.; Zucca, E.; Cucciati, O.; 527–535 lation gradients in bulges along the Hubble se- Walcher, C. J.; The VIMOS-VLT deep survey. Garay, G.; Mardones, D.; Brooks, K. J.; Videla, L.; quence. – I. The data; A&A 474, 1081–1092 Color bimodality and the mix of galaxy popula- Contreras, Y.; A Multiwavelength Study of Young Gorlova, N.; Balog, Z.; Rieke, G. H.; Muzerolle, J.; tions up to z ~ 2; A&A 465, 711–723 Massive Star Forming Regions. – II. The Dust En- Su, K. Y. L.; Ivanov, V. D.; Young, E. T.; Debris Frandsen, S.; Bruntt, H.; Grundahl, F.; Kopacki, G.; vironment; ApJ 666, 309–320 Disks in NGC 2547; ApJ 670, 516–535 Kjeldsen, H.; Arentoft, T.; Stello, D.; Bedding, T. García-Hernández, D. A.; García-Lario, P.; Plez, B.; Gosling, A. J.; Bandyopadhyay, R. M.; Miller-Jones, R.; Jacob, A. P.; Gilliland, R. L.; Edmonds, P. D.; Manchado, A.; D’Antona, F.; Lub, J.; Habing, H.; J. C. A.; Farrell, S. A.; GRO J1744–28, search for Michel, E.; Matthiesen, J.; A search for solar-like Lithium and zirconium abundances in massive the counterpart: infrared photometry and spec- oscillations in K giants in the globular cluster M4; Galactic O-rich AGB stars; A&A 462, 711–730 troscopy; MNRAS 380, 1511–1520 A&A 475, 991–1002 Garcet, O.; Gandhi, P.; Gosset, E.; Sprimont, P. G.; Graham, A. W.; Driver, S. P.; Allen, P. D.; Liske, J.; François, P.; Depagne, E.; Hill, V.; Spite, M.; Spite, F.; Surdej, J.; Borkowski, V.; Tajer, M.; Pacaud, F.; The Millennium Galaxy Catalogue: the local su- Plez, B.; Beers, T. C.; Andersen, J.; James, G.; Pierre, M.; Chiappetti, L.; Maccagni, D.; Page, M. permassive black hole mass function in early- and Barbuy, B.; Cayrel, R.; Bonifacio, P.; Molaro, P.; J.; Carrera, F. J.; Tedds, J. A.; Mateos, S.; late-type galaxies; MNRAS 378, 198–210 Nordström, B.; Primas, F.; First stars. – VIII. Enrich- Krumpe, M.; Contini, T.; Corral, A.; Ebrero, J.; Granvik, M.; Muinonen, K.; Jones, L.; Bhattacharya, ment of the neutron-capture elements in the early Gavignaud, I.; Schwope, A.; Le Fèvre, O.; Polletta, B.; Delbo, M.; Saba, L.; Cellino, A.; Tedesco, E.; Galaxy; A&A 476, 935–950 M.; Rosen, S.; Lonsdale, C.; Watson, M.; Borczyk, Davis, D.; Meadows, V.; Linking large-parallax Frebel, A.; Christlieb, N.; Norris, J. E.; Thom, C.; W.; Vaisanen, P.; The XMM large scale structure Spitzer–CFHT–VLT astrometry of asteroids; Icar Beers, T. C.; Rhee, J.; Discovery of HE 1523–0901, survey: optical vs. X-ray classifications of active 192, 475–490 a Strongly r-Process-enhanced Metal-poor Star galactic nuclei and the unified scheme; A&A 474, Gratton, R. G.; Lucatello, S.; Bragaglia, A.; Carretta, with Detected Uranium; ApJ 660, L117–L120 473–489 E.; Cassisi, S.; Momany, Y.; Pancino, E.; Valenti, Froebrich, D.; Meusinger, H.; Scholz, A.; FSR1735 García-Rojas, J.; Esteban, C.; On the Abundance E.; Caloi, V.; Claudi, R.; D’Antona, F.; Desidera, S.; – a new globular cluster candidate in the inner Discrepancy Problem in H ii Regions; ApJ 670, François, P.; James, G.; Moehler, S.; Ortolani, S.; Galaxy; MNRAS 377, L54–L58 457–470 Pasquini, L.; Piotto, G.; Recio-Blanco, A.; Na-O Frye, B. L.; Coe, D.; Bowen, D. V.; Benítez, N.; Geers, V. C.; Pontoppidan, K. M.; van Dishoeck, E. anticorrelation and horizontal branches. – V. The Broadhurst, T.; Guhathakurta, P.; Illingworth, G.; F.; Dullemond, C. P.; Augereau, J.-C.; Merín, B.; Na-O anticorrelation in NGC 6441 from Giraffe Menanteau, F.; Sharon, K.; Lupton, R.; Meylan, G.; Oliveira, I.; Pel, J. W.; Spatial separation of small spectra; A&A 464, 953–965 Zekser, K.; Meurer, G.; Hurley, M.; The Sextet and large grains in the transitional disk around the Grave, J. M. C.; Kumar, M. S. N.; Probing the close Arcs: A Strongly Lensed Lyman Break Galaxy in young star IRS 48; A&A 469, L35–L38 environment of massive young stars with spectro- the ACS Spectroscopic Galaxy Survey toward Geers, V. C.; van Dishoeck, E. F.; Visser, R.; astrometry; A&A 462, L37–L40 Abell 1689; ApJ 665, 921–935 Pontoppidan, K. M.; Augereau, J.-C.; Habart, E.; Grazian, A.; Salimbeni, S.; Pentericci, L.; Fontana, Fuhrmeister, B.; Liefke, C.; Schmitt, J. H. M. M.; Lagrange, A. M.; Spatially extended polycyclic ar- A.; Nonino, M.; Vanzella, E.; Cristiani, S.; de Simultaneous XMM-Newton and VLT/UVES ob- omatic hydrocarbons in circumstellar disks Santis, C.; Gallozzi, S.; Giallongo, E.; Santini, P.; A servations of the flare star CN Leonis; A&A 468, around T Tauri and Herbig Ae stars; A&A 476, comparison of LBGs, DRGs, and BzK galaxies: 221–231 279–289 their contribution to the stellar mass density in the Gâlfalk, M.; Olofsson, G.; Herbig-Haro flows in B335; Geißler, K.; Kellner, S.; Brandner, W.; Masciadri, E.; GOODS-MUSIC sample; A&A 465, 393–404 A&A 475, 281–300 Hartung, M.; Henning, T.; Lenzen, R.; Close, L.; Gredel, R.; Quantitative optical and near-infrared

Garay, G.; Mardones, D.; Bronfman, L.; Brooks, K. Endl, M.; Kürster, M.; A direct and differential im- spectroscopy of H2 towards HH91A; A&A 474, J.; Rodríguez, L. F.; Güsten, R.; Nyman, L.-Å.; aging search for sub-stellar companions to e Indi 941–950 Franco-Hernández, R.; Moran, J. M.; Discovery of A; A&A 461, 665–668 Grin, D.; Covone, G.; Kneib, J.-P.; Kamionkowski, M.; an energetic bipolar molecular outflow towards Geier, S.; Nesslinger, S.; Heber, U.; Przybilla, N.; Blain, A.; Jullo, E.; Telescope search for decaying IRAS 16547–4247; A&A 463, 217–224 Napiwotzki, R.; Kudritzki, R.-P.; The hot subdwarf relic axions; PhRvD 75, 105018– B + white dwarf binary KPD 1930+2752. A super- Grocholski, A. J.; Sarajedini, A.; Olsen, K. A. G.; nova type Ia progenitor candidate; A&A 464, Tiede, G. P.; Mancone, C. L.; Distances to Popu- 299–307 lous Clusters in the Large Magellanic Cloud via Georgantopoulos, I.; Georgakakis, A.; Akylas, A.; the K-band Luminosity of the Red Clump; AJ 134, Chandra and Spitzer observations of CDFS X-ray 680–693 obscured QSOs; A&A 466, 823–830 Groenewegen, M. A. T.; Decin, L.; Salaris, M.; De Gielen, C.; van Winckel, H.; Waters, L. B. F. M.; Min, Cat, P.; The Pleiades eclipsing binary HD 23642 M.; Dominik, C.; Dust-grain processing in circum- revisited; A&A 463, 579–587 binary discs around evolved binaries. The RV Tauri spectral twins RU Centauri and AC Herculis; A&A 475, 629–637

106 ESO Annual Report 2007 Grundstrom, E. D.; Gies, D. R.; Hillwig, T. C.; Harris, A. W.; Mueller, M.; Delbó, M.; Bus, S. J.; Hintz, E. G.; Brown, P. J.; Revised Periods for QS McSwain, M. V.; Smith, N.; Gehrz, R. D.; Stahl, O.; Physical characterization of the potentially hazard- Geminorum and V367 Geminorum; PASP 119, Kaufer, A.; A Spectroscopic Study of Mass Out- ous high-albedo Asteroid (33342) 1998 WT24 274–283 flows in the Interacting Binary RY Scuti; ApJ 667, from thermal-infrared observations; Icar 188, Hirtzig, M.; Coustenis, A.; Gendron, E.; Drossart, P.; 505–519 414–424 Hartung, M.; Negrão, A.; Rannou, P.; Combes, M.; Grützbauch, R.; Trinchieri, G.; Rampazzo, R.; Held, Hayashi, M.; Shimasaku, K.; Motohara, K.; Yoshida, Titan: Atmospheric and surface features as ob- E. V.; Rizzi, L.; Sulentic, J. W.; Zeilinger, W. W.; M.; Okamura, S.; Kashikawa, N.; Luminosity-De- served with Nasmyth Adaptive Optics System Small-Scale Systems of Galaxies. – III. X-Ray-dependent Clustering of Star-forming BzK Galaxies Near-Infrared Imager and Spectrograph at the tected Elliptical + Spiral Galaxy Pairs in Low-Den- at Redshift 2; ApJ 660, 72–80 time of the Huygens mission; JGRE 112 sity Environments; AJ 133, 220–254 Hayes, M.; Östlin, G.; Atek, H.; Kunth, D.; Mas-Hesse, Holden, B. P.; Illingworth, G. D.; Franx, M.; Blakeslee, Guarcello, M. G.; Prisinzano, L.; Micela, G.; Damiani, J. M.; Leitherer, C.; Jiménez-Bailón, E.; Adamo, J. P.; Postman, M.; Kelson, D. D.; van der Wel, A.; F.; Peres, G.; Sciortino, S.; Correlation between A.; The escape of Lyman photons from a young Demarco, R.; Magee, D. K.; Tran, K.-V.; Zirm, A.; the spatial distribution of circumstellar disks and starburst: the case of Haro11; MNRAS 382, Ford, H.; Rosati, P.; Homeier, N.; Mass Selection massive stars in the open cluster NGC 6611. Com- 1465–1480 and the Evolution of the Morphology-Density Re- piled catalog and cluster parameters; A&A 462, Helfand, D. J.; Chatterjee, S.; Brisken, W. F.; Camilo, lation from z = 0.8 to 0; ApJ 670, 190–205 245–255 F.; Reynolds, J.; van Kerkwijk, M. H.; Halpern, J. Holland, S. T.; Boyd, P. T.; Gorosabel, J.; Hjorth, J.; Guenther, E. W.; Esposito, M.; Mundt, R.; Covino, E.; P.; Ransom, S. M.; VLBA Measurement of Schady, P.; Thomsen, B.; Augusteijn, T.; Blustin, Alcalá, J. M.; Cusano, F.; Stecklum, B.; Pre-main the Transverse Velocity of the Magnetar XTE A. J.; Breeveld, A.; De Pasquale, M.; Fynbo, J. P. sequence spectroscopic binaries suitable for VLTI J1810–197; ApJ 662, 1198–1203 U.; Gehrels, N.; Gronwall, C.; Hunsberger, S.; observations; A&A 467, 1147–1155 Hempel, M.; Kissler-Patig, M.; Puzia, T. H.; Hilker, M.; Ivanushkina, M.; Landsman, W.; Laursen, P.; Gullieuszik, M.; Held, E. V.; Rizzi, L.; Saviane, I.; The age structure of globular cluster systems in McGowan, K.; Mangano, V.; Markwardt, C. B.; Momany, Y.; Ortolani, S.; Near-infrared observa- early-type galaxies and its dependence on host Marshall, F.; Mason, K. O.; Moretti, A.; Page, M. tions of the Fornax dwarf galaxy. – I. The red giant galaxy properties; A&A 463, 493–502 J.; Poole, T.; Roming, P.; Rosen, S.; Still, M.; Opti- branch; A&A 467, 1025–1036 Hempel, M.; Zepf, S.; Kundu, A.; Geisler, D.; cal, Infrared, and Ultraviolet Observations of the Gullieuszik, M.; Rejkuba, M.; Cioni, M. R.; Habing, H. Maccarone, T. J.; Near-Infrared Observations of X-Ray Flash XRF 050416A; AJ 133, 122–129 J.; Held, E. V.; Near-infrared photometry of carbon Globular Clusters in NGC 4472, NGC 4594, Holmberg, J.; Nordström, B.; Andersen, J.; The stars in the Sagittarius dwarf irregular galaxy and NGC 3585, and NGC 5813 and Implications for Geneva-Copenhagen survey of the Solar neigh- DDO 210; A&A 475, 467–477 Their Ages and Metallicities; ApJ 661, 768–778 bourhood II. New uvby calibrations and rediscus- Guseva, N. G.; Izotov, Y. I.; Papaderos, P.; Fricke, K. Hensberge, H.; Nitschelm, C.; Olsen, E. H.; Sterken, sion of stellar ages, the G dwarf problem, age- J.; Balmer jump temperature determination in a C.; David, M.; Freyhammer, L. M.; Landin, N. R.; metallicity diagram, and heating mechanisms of large sample of low-metallicity H ii regions; A&A Bouzid, M. Y.; Papadaki, C.; Pritchard, J. D.; the disk; A&A 475, 519–537 464, 885–893 Clausen, J. V.; Vaz, L. P. R.; The eclipsing double- Holt, J.; Tadhunter, C. N.; González Delgado, R. M.; Guy, J.; Astier, P.; Baumont, S.; Hardin, D.; Pain, R.; lined binaries V883Cen and η Mus; MNRAS 379, Inskip, K. J.; Rodriguez, J.; Emonts, B. H. C.; Regnault, N.; Basa, S.; Carlberg, R. G.; Conley, A.; 349–356 Morganti, R.; Wills, K. A.; The properties of the Fabbro, S.; Fouchez, D.; Hook, I. M.; Howell, D. Herbst, T. M.; Hartung, M.; Kasper, M. E.; Leinert, C.; young stellar populations in powerful radio galax- A.; Perrett, K.; Pritchet, C. J.; Rich, J.; Sullivan, M.; Ratzka, T.; Molecular Hydrogen Outflows in the ies at low and intermediate redshifts; MNRAS 381, Antilogus, P.; Aubourg, E.; Bazin, G.; Bronder, J.; Central Arcseconds of the T Tauri System; AJ 134, 611–639 Filiol, M.; Palanque-Delabrouille, N.; Ripoche, P.; 359–366 Hopp, U.; Schulte-Ladbeck, R. E.; Kerp, J.; Ruhlmann-Kleider, V.; SALT2: using distant super- Hetterscheidt, M.; Simon, P.; Schirmer, M.; Searching for stars in compact high-velocity novae to improve the use of type Ia supernovae as Hildebrandt, H.; Schrabback, T.; Erben, T.; clouds – II; MNRAS 374, 1164–1168 distance indicators; A&A 466, 11–21 Schneider, P.; GaBoDS: The Garching-Bonn deep Hovatta, T.; Tornikoski, M.; Lainela, M.; Lehto, H. J.; Guzzo, L.; Cassata, P.; Finoguenov, A.; Massey, R.; survey. – VII. Cosmic shear analysis; A&A 468, Valtaoja, E.; Torniainen, I.; Aller, M. F.; Aller, H. D.; Scoville, N. Z.; Capak, P.; Ellis, R. S.; Mobasher, 859–876 Statistical analyses of long-term variability of AGN B.; Taniguchi, Y.; Thompson, D.; Ajiki, M.; Aussel, Hicks, A. K.; Ellingson, E.; Hoekstra, H.; Gladders, at high radio frequencies; A&A 469, 899–912 H.; Böhringer, H.; Brusa, M.; Calzetti, D.; M.; Yee, H. K. C.; Bautz, M.; Gilbank, D.; Webb, T.; Hoyer, S.; Ramírez Alegría, S.; Ivanov, V. D.; Minniti, Comastri, A.; Franceschini, A.; Hasinger, G.; Ivison, R.; A Multiwavelength Analysis of the D.; Pietrzyn´ski, G.; Ruíz, M. T.; Gieren, W.; Udalski, Kasliwal, M. M.; Kitzbichler, M. G.; Kneib, J.-P.; Strong Lensing Cluster RCS 022434-0002.5 at A.; Zoccali, M.; Carrasco, E. R.; Díaz, R. F.; Koekemoer, A.; Leauthaud, A.; McCracken, H. J.; z = 0.778; ApJ 671, 1446–1455 Fernández, J. M.; Gallardo, J.; Rejkuba, M.; Pérez, Murayama, T.; Nagao, T.; Rhodes, J.; Sanders, D. Hidalgo-Gámez, A. M.; Peimbert, A.; Diffuse Ionized F.; Millimagnitude Photometry for Transiting Extra- B.; Sasaki, S.; Shioya, Y.; Tasca, L.; Taylor, J. E.; Gas inside the Dwarf Irregular Galaxy NGC 6822; solar Planetary Candidates. – IV. Solution to The Cosmic Evolution Survey (COSMOS): A AJ 133, 1874–1882 the Puzzle of the Extremely Red OGLE-TR-82 Pri- Large-Scale Structure at z = 0.73 and the Relation Hildebrandt, H.; Pielorz, J.; Erben, T.; Schneider, P.; mary; ApJ 669, 1345–1353 of Galaxy Morphologies to Local Environment; Eifler, T.; Simon, P.; Dietrich, J. P.; GaBoDS: the Hubrig, S.; Pogodin, M. A.; Yudin, R. V.; Schöller, M.; ApJS 172, 254–269 Garching-Bonn deep survey. – VIII. Lyman-break Schnerr, R. S.; The magnetic field in the phot- Haas, M.; Siebenmorgen, R.; Pantin, E.; Horst, H.; galaxies in the ESO deep public survey; A&A 462, ospheric and circumstellar components of Herbig Smette, A.; Käufl, H.-U.; Lagage, P.-O.; Chini, R.; 865–873 Ae stars; A&A 463, 1039–1046 VISIR / VLT mid-infrared imaging of Seyfert nuclei: Hilker, M.; Baumgardt, H.; Infante, L.; Drinkwater, M.; Hubrig, S.; González, J. F.; Detection of variable Si ii, nuclear dust emission and the Seyfert-2 dichot- Evstigneeva, E.; Gregg, M.; Dynamical masses of M n ii, and Fe ii emission lines in the magnetic Bp omy; A&A 473, 369–376 ultra-compact dwarf galaxies in Fornax; A&A 463, star a Centauri; A&A 466, 1083–1087 Haberzettl, L.; Bomans, D. J.; Dettmar, R.-J.; Low 119–130 Hubrig, S.; Nesvacil, N.; Two new chemically peculiar surface brightness galaxies around the HDF-S. Hilton, M.; Collins, C. A.; Stanford, S. A.; Lidman, C.; stars with resolved, magnetically split lines; – II. Distances and volume densities; A&A 471, Dawson, K. S.; Davidson, M.; Kay, S. T.; Liddle, A. MNRAS 378, L16–L19 787–794 R.; Mann, R. G.; Miller, C. J.; Nichol, R. C.; Romer, Hubrig, S.; Marco, O.; Stelzer, B.; Schöller, M.; Hadfield, L. J.; Crowther, P. A.; A survey of the A. K.; Sabirli, K.; Viana, P. T. P.; West, M. J.; The Huélamo, N.; Establishing the nature of compan- Wolf-Rayet population of the barred, spiral galaxy XMM Cluster Survey: The Dynamical State of XM- ion candidates to X-ray-emitting late B-type stars; NGC 1313; MNRAS 381, 418–432 MXCS J2215.9–1738 at z = 1.457; ApJ 670, MNRAS 381, 1569–1574 Haikala, L. K.; Olberg, M.; The structure of the 1000–1009 Hubrig, S.; Yudin, R. V.; Pogodin, M.; Schöller, M.; cometary globule CG 12: a high-latitude star- Peters, G. J.; Evidence for weak magnetic fields in forming region; A&A 466, 191–200 early-type emission stars; AN 328, 1133 Hall, P. B.; Sadavoy, S. I.; Hutsemekers, D.; Everett, Huélamo, N.; Melo, C.; Sterzik, M. F.; Santos, N. C.; J. E.; Rafiee, A.; Acceleration and Substructure Mardones, D.; Looking into the cradle: new mid-IR Constraints in a Quasar Outflow; ApJ 665, observations of multiple proto-stars; A&A 464, 174–186 625–629

ESO Annual Report 2007 107 Huertas-Company, M.; Rouan, D.; Soucail, G.; Le Johnas, C. M. S.; Guenther, E. W.; Joergens, V.; Kim, T.-S.; Bolton, J. S.; Viel, M.; Haehnelt, M. G.; Fèvre, O.; Tasca, L.; Contini, T.; Morphological ev- Schweitzer, A.; Hauschildt, P. H.; Lithium Carswell, R. F.; An improved measurement of the olution of z ~ 1 galaxies from deep K-band AO im- abundances of very low mass members of flux distribution of the Lyα forest in QSO absorp- aging in the COSMOS deep field; A&A 468, Chamaeleon I; A&A 475, 667–675 tion spectra: the effect of continuum fitting, metal 937–950 Jonker, P. G.; Nelemans, G.; Bassa, C. G.; Detection contamination and noise properties; MNRAS 382, Hügelmeyer, S. D.; Dreizler, S.; Homeier, D.; Reiners, of the radial velocity curve of the B5–A0 super- 1657–1674 A.; Investigation of transit-selected exoplanet can- giant companion star of Cir X-1?; MNRAS 374, Kjær, K.; Leibundgut, B.; Fransson, C.; Gröningsson, didates from the MACHO survey; A&A 469, 999–1005 P.; Spyromilio, J.; Kissler-Patig, M.; Infrared inte- 1163 –1168 Joos, F.; Schmid, H. M.; Limb polarization of Uranus gral field spectroscopy of SN 1987A; A&A 471, Hultzsch, P. J. N.; Puls, J.; Méndez, R. H.; Pauldrach, and Neptune. – II. Spectropolarimetric observa- 617–624 A. W. A.; Kudritzki, R.-P.; Hoffmann, T. L.; tions; A&A 463, 1201–1210 Kniazev, A. Y.; Grebel, E. K.; Pustilnik, S. A.; Pramskij, McCarthy, J. K.; Central stars of planetary nebu- Jordan, S.; Aznar Cuadrado, R.; Napiwotzki, R.; A. G.; High-quality spectrophotometry of the lae in the Galactic bulge; A&A 467, 1253–1264 Schmid, H. M.; Solanki, S. K.; The fraction of DA planetary nebula in the Fornax dSph; A&A 468, Humphrey, A.; Villar-Martín, M.; Fosbury, R.; Binette, white dwarfs with kilo-Gauss magnetic fields; A&A 121–128 L.; Vernet, J.; De Breuck, C.; di Serego Alighieri, 462, 1097–1101 Knudsen, K. K.; Walter, F.; Weiss, A.; Bolatto, A.; S.; Giant Lyα nebulae around z > 2 radio galaxies: Kacprzak, G. G.; Churchill, C. W.; Steidel, C. C.; Riechers, D. A.; Menten, K.; New Insights on the evidence for infall; MNRAS 375, 705–714 Murphy, M. T.; Evans, J. L.; A Correlation between Dense Molecular Gas in NGC 253 as Traced by Hunter, I.; Dufton, P. L.; Smartt, S. J.; Ryans, R. S. I.; Galaxy Morphology and Mg ii Halo Absorption HCN and HCO+; ApJ 666, 156–164 Evans, C. J.; Lennon, D. J.; Trundle, C.; Hubeny, I.; Strength; ApJ 662, 909–922 Kocevski, D. D.; Ebeling, H.; Mullis, C. R.; Tully, R. B.; Lanz, T.; The VLT-FLAMES survey of massive Kainulainen, J.; Lehtinen, K.; Väisänen, P.; Bronfman, A Systematic X-Ray Search for Clusters of Galax- stars: surface chemical compositions of B-type L.; Knude, J.; A comparison of density structures ies behind the Milky Way. – II. The Second CIZA stars in the Magellanic Clouds; A&A 466, 277–300 of a star forming and a non-star-forming globule. Subsample; ApJ 662, 224–235 Hyvönen, T.; Kotilainen, J. K.; Falomo, R.; Örndahl, DCld303.8-14.2 and Thumbprint nebula; A&A Koch, A.; Grebel, E. K.; Kleyna, J. T.; Wilkinson, M. I.; E.; Pursimo, T.; The stellar content of low redshift 463, 1029–1037 Harbeck, D. R.; Gilmore, G. F.; Wyse, R. F. G.; BL Lacertae host galaxies from multicolour imag- Kampczyk, P.; Lilly, S. J.; Carollo, C. M.; Scarlata, C.; Evans, N. W.; Complexity on Small Scales. – II. ing; A&A 476, 723–734 Feldmann, R.; Koekemoer, A.; Leauthaud, A.; Metallicities and Ages in the Leo II Dwarf Spheroi- Idiart, T. P.; Maciel, W. J.; Costa, R. D. D.; Chemical Sargent, M. T.; Taniguchi, Y.; Capak, P.; Simulating dal Galaxy; AJ 133, 270–283 evolution of the Small Magellanic Cloud based on the Cosmos: The Fraction of Merging Galaxies at Kochukhov, O.; Ryabchikova, T.; Weiss, W. W.; planetary nebulae; A&A 472, 101–110 High Redshift; ApJS 172, 329–340 Landstreet, J. D.; Lyashko, D.; Line profile varia- Inskip, K. J.; Tadhunter, C. N.; Dicken, D.; Holt, J.; Kaplan, D. L.; van Kerkwijk, M. H.; Anderson, J.; The tions in rapidly oscillating Ap stars: resolution of Villar-Martín, M.; Morganti, R.; PKS1932–46: a Distance to the Isolated Neutron Star RX the enigma; MNRAS 376, 651–672 radio source in an interacting group?; MNRAS J0720.4–3125; ApJ 660, 1428–1443 Koch, A.; Kleyna, J. T.; Wilkinson, M. I.; Grebel, E. K.; 382, 95–108 Karoff, C.; High-frequency modes in solar-like stars; Gilmore, G. F.; Evans, N. W.; Wyse, R. F. G.; Irwin, J.; Aigrain, S.; Hodgkin, S.; Stassun, K. G.; MNRAS 381, 1001–1008 Harbeck, Daniel R.; Stellar Kinematics in the Re- Hebb, L.; Irwin, M.; Moraux, E.; Bouvier, J.; Kasper, M.; Biller, B. A.; Burrows, A.; Brandner, W.; mote Leo II Dwarf Spheroidal Galaxy-Another Alapini, A.; Alexander, R.; Bramich, D. M.; Budaj, J.; Close, L. M.; The very nearby M/T dwarf Brick in the Wall; AJ 134, 566–578 Holtzman, J.; Martín, E. L.; McCaughrean, M. J.; binary SCR 1845-6357; A&A 471, 655–659 Kodama, T.; Tanaka, I.; Kajisawa, M.; Kurk, J.; Pont, F.; Verrier, P. E.; Zapatero Osorio, M. R.; The Kasper, M.; Apai, D.; Janson, M.; Brandner, W.; A Venemans, B.; De Breuck, C.; Vernet, J.; Lidman, Monitor project: JW 380 – a 0.26-, 0.15-Msolar, n o v e l L-band imaging search for giant planets in C.; The first appearance of the red sequence of pre-main-sequence eclipsing binary in the Orion the Tucana and ß Pictoris moving groups; A&A galaxies in proto-clusters at 2 <~ z <~ 3; MNRAS nebula cluster; MNRAS 380, 541–550 472, 321–327 377, 1717–1725 Irwin, J.; Irwin, M.; Aigrain, S.; Hodgkin, S.; Hebb, L.; Kausch, W.; Gitti, M.; Erben, T.; Schindler, S.; Koekemoer, A. M.; Aussel, H.; Calzetti, D.; Capak, P.; Moraux, E.; The Monitor project: data processing ARCRAIDER. – I. Detailed optical and X-ray analy- Giavalisco, M.; Kneib, J.-P.; Leauthaud, A.; Le and light curve production; MNRAS 375, sis of the cooling flow cluster Z3146; A&A 471, Fèvre, O.; McCracken, H. J.; Massey, R.; Mo- 1449–1462 31–50 basher, B.; Rhodes, J.; Scoville, N.; Shopbell, P. Hultzsch, P. J. N.; Puls, J.; Méndez, R. H.; Pauldrach, Kawakita, H.; Jehin, E.; Manfroid, J.; Hutsemékers, L.; The COSMOS Survey: Hubble Space Tele- A. W. A.; Kudritzki, R.-P.; Hoffmann, T. L.; D.; Nuclear spin temperature of ammonia in scope Advanced Camera for Surveys Observa- McCarthy, J. K.; Central stars of planetary nebu- Comet 9P/Tempel 1 before and after the Deep Im- tions and Data Processing; ApJS 172, 196–202 lae in the Galactic bulge; A&A 467, 1253–1264 pact event; Icar 187, 272–275 Korn, A. J.; Grundahl, F.; Richard, O.; Mashonkina, Jablonka, P.; Gorgas, J.; Goudfrooij, P.; Stellar Kellerer, A.; Petr-Gotzens, M. G.; Kervella, P.; Coudé L.; Barklem, P. S.; Collet, R.; Gustafsson, B.; population gradients in bulges along the Hubble Du Foresto, V.; Interferometric observations of Piskunov, N.; Atomic Diffusion and Mixing in Old sequence. – II. Relations with galaxy properties; the multiple stellar system δ Velorum; A&A 469, Stars. – I. Very Large Telescope FLAMES-UVES A&A 474, 763–776 633–637 Observations of Stars in NGC 6397; ApJ 671, Jahnke, K.; Wisotzki, L.; Courbin, F.; Letawe, G.; Kendall, T. R.; Jones, H. R. A.; Pinfield, D. J.; Pokorny, 402–419 Spatial decomposition of on-nucleus spectra of R. S.; Folkes, S.; Weights, D.; Jenkins, J. S.; Kóspál, Á.; Ábrahám, P.; Prusti, T.; Acosta-Pulido, J.; quasar host galaxies; MNRAS 378, 23–40 Mauron, N.; New nearby, bright southern ultracool Hony, S.; Moór, A.; Siebenmorgen, R.; The out- Janson, M.; Brandner, W.; Lenzen, R.; Close, L.; dwarfs; MNRAS 374, 445–454 burst of the eruptive young star OO Serpentis be- Nielsen, E.; Hartung, M.; Henning, T.; Bouy, H.; Kervella, P.; Interferometric observations of η Carinae tween 1995 and 2006; A&A 470, 211–219 Improved age constraints for the AB Doradus with VINCI/VLTI; A&A 464, 1045–1047 Kotilainen, J. K.; Falomo, R.; Labita, M.; Treves, A.; quadruple system. The binary nature of AB Do- Kervella, P.; Thévenin, F.; Deep imaging survey of the Uslenghi, M.; The Nuclear to Host Galaxy Relation radus B; A&A 462, 615–620 environment of α Centauri. – II. CCD imaging with of High-Redshift Quasars; ApJ 660, 1039–1050 Janson, M.; Brandner, W.; Henning, T.; Lenzen, R.; the NTT-SUSI2 camera; A&A 464, 373–375 Kouwenhoven, M. B. N.; Brown, A. G. A.; Kaper, L.; McArthur, B.; Benedict, G. F.; Reffert, S.; Nielsen, Kervella, P.; Domiciano de Souza, A.; The environ- A brown dwarf desert for intermediate mass stars E.; Close, L.; Biller, B.; Kellner, S.; Günther, E.; ment of the fast rotating star Achernar. High- in Scorpius OB2?; A&A 464, 581–599 Hatzes, A.; Masciadri, E.; Geissler, K.; Hartung, resolution thermal infrared imaging with VISIR in Kouwenhoven, M. B. N.; Brown, A. G. A.; Portegies M.; NACO-SDI Direct Imaging Search for the BURST mode; A&A 474, L49–L52 Zwart, S. F.; Kaper, L.; The primordial binary pop- Exoplanet e Eri b; AJ 133, 2442–2456 ulation. – II. Recovering the binary population for Jeffers, S. V.; Donati, J.-F.; Collier Cameron, A.; intermediate mass stars in Scorpius OB2; A&A Magnetic activity on AB Doradus: temporal evolu- 474, 77–104 tion of star-spots and differential rotation from Kovtyukh, V. V.; High-precision effective tempera- 1988 to 1994; MNRAS 375, 567–583 tures of 161 FGK supergiants from line-depth ra-

Joergens, V.; Müller, A.; 16–20 MJup Radial Velocity tios; MNRAS 378, 617–624 Companion Orbiting the Brown Dwarf Candidate Cha Hα 8; ApJ 666, L113–L116

108 ESO Annual Report 2007 Kraus, M.; Borges Fernandes, M.; de Araújo, F. X.; Landstreet, J. D.; Bagnulo, S.; Andretta, V.; Fossati, Levan, A. J.; Jakobsson, P.; Hurkett, C.; Tanvir, N. R.; On the hydrogen neutral outflowing disks of B[e] L.; Mason, E.; Silaj, J.; Wade, G. A.; Searching for Gorosabel, J.; Vreeswijk, P.; Rol, E.; Chapman, R.; supergiants; A&A 463, 627–634 links between magnetic fields and stellar evolu- Gehrels, N.; O’Brien, P. T.; Osborne, J. P.; Priddey, Kravtsov, V.; Alcaíno, G.; Marconi, G.; Alvarado, F.; tion: II. The evolution of magnetic fields as re- R. S.; Kouveliotou, C.; Starling, R.; vanden Berk, Multi-color photometry of the Galactic globular vealed by observations of Ap stars in open clus- D.; Wiersema, K.; A case of mistaken identity? cluster M75 = NGC 6864. A new sensitive metal- ters and associations; A&A 470, 685–698 GRB 060912A and the nature of the long-short licity indicator and the position of the horizontal Lanzoni, B.; Dalessandro, E.; Ferraro, F. R.; Mancini, GRB divide; MNRAS 378, 1439–1446 branch in UV; A&A 469, 529–537 C.; Beccari, G.; Rood, R. T.; Mapelli, M.; Levshakov, S. A.; Molaro, P.; Lopez, S.; D’Odorico, Kriek, M.; van Dokkum, P. G.; Franx, M.; Illingworth, Sigurdsson, S.; The Blue Straggler Population of S.; Centurión, M.; Bonifacio, P.; Agafonova, I. I.; G. D.; Coppi, P.; Förster Schreiber, N. M.; the Globular Cluster M5; ApJ 663, 267–276 Reimers, D.; A new measure of Δα/α at redshift Gawiser, E.; Labbé, I.; Lira, P.; Marchesini, D.; Lanzoni, B.; Sanna, N.; Ferraro, F. R.; Valenti, E.; z = 1.84 from very high resolution spectra of Quadri, R.; Rudnick, G.; Taylor, E. N.; Urry, C. M.; Beccari, G.; Schiavon, R. P.; Rood, R. T.; Mapelli, Q 1101–264; A&A 466, 1077–1082 van der Werf, P. P.; The Origin of Line Emission M.; Sigurdsson, S.; A Panchromatic Study of the Leyder, J.-C.; Walter, R.; Lazos, M.; Masetti, N.; in Massive z ~ 2.3 Galaxies: Evidence for Cosmic Globular Cluster NGC 1904. – I. The Blue Strag- Produit, N.; Hard X-ray flares in IGR J08408–4503 Downsizing of AGN Host Galaxies; ApJ 669, gler Population; ApJ 663, 1040–1048 unveil clumpy stellar winds; A&A 465, L35–L38 776–790 Lanzoni, B.; Dalessandro, E.; Ferraro, F. R.; Miocchi, Lilly, S. J.; Le Fèvre, O.; Renzini, A.; Zamorani, G.; Krisciunas, K.; Garnavich, P. M.; Stanishev, V.; P.; Valenti, E.; Rood, R. T.; The Surface Density Scodeggio, M.; Contini, T.; Carollo, C. M.; Suntzeff, N. B.; Prieto, J. L.; Espinoza, J.; Profile of NGC 6388: A Good Candidate for Hasinger, G.; Kneib, J.-P.; Iovino, A.; Le Brun, V.; Gonzalez, D.; Salvo, M. E.; Elias de la Rosa, N.; Harboring an Intermediate-Mass Black Hole; ApJ Maier, C.; Mainieri, V.; Mignoli, M.; Silverman, J.; Smartt, S. J.; Maund, J. R.; Kudritzki, R.-P.; The 668, L139–L142 Tasca, L. A. M.; Bolzonella, M.; Bongiorno, A.; Type Ia Supernova 2004S, a Clone of SN 2001el, Lanzoni, B.; Dalessandro, E.; Perina, S.; Ferraro, F. Bottini, D.; Capak, P.; Caputi, K.; Cimatti, A.; and the Optimal Photometric Bands for Extinction R.; Rood, R. T.; Sollima, A.; The Surprising Exter- Cucciati, O.; Daddi, E.; Feldmann, R.; Franzetti, P.; Estimation; AJ 133, 58–72 nal Upturn of the Blue Straggler Radial Distribu- Garilli, B.; Guzzo, L.; Ilbert, O.; Kampczyk, P.; Krumpe, M.; Lamer, G.; Schwope, A. D.; Wagner, S.; tion in M55; ApJ 670, 1065–1073 Kovac, K.,; Lamareille, F.; Leauthaud, A.; Borgne, Zamorani, G.; Mignoli, M.; Staubert, R.; Wisotzki, Lazorenko, P. F.; Mayor, M.; Dominik, M.; Pepe, F.; J.-F. Le; McCracken, H. J.; Marinoni, C.; Pello, R.; L.; Hasinger, G.; The XMM-Newton survey in the Segransan, D.; Udry, S.; High-precision astrome- Ricciardelli, E.; Scarlata, C.; Vergani, D.; Sanders, Marano field. I. The X-ray data and optical follow- try on the VLT/FORS1 at time scales of few days; D. B.; Schinnerer, E.; Scoville, N.; Taniguchi, Y.; up; A&A 466, 41–61 A&A 471, 1057–1067 Arnouts, S.; Aussel, H.; Bardelli, S.; Brusa, M.; Küpcü Yoldas¸, A.; Salvato, M.; Greiner, J.; Pierini, D.; Leão, I. C.; de Laverny, P.; Chesneau, O.; Mékarnia, Cappi, A.; Ciliegi, P.; Finoguenov, A.; Foucaud, S.; Pian, E.; Rau, A.; The host galaxy of GRB 011121: D.; de Medeiros, J. R.; A snapshot of the inner Franceschini, R.; Halliday, C.; Impey, C.; Knobel, morphology and spectral energy distribution; A&A dusty regions of a R CrB-type variable; A&A 466, C.; Koekemoer, A.; Kurk, J.; Maccagni, D.; 463, 893–902 L1–L4 Maddox, S.; Marano, B.; Marconi, G.; Meneux, B.; Kurk, J. D.; Walter, F.; Fan, X.; Jiang, L.; Riechers, D. Leauthaud, A.; Massey, R.; Kneib, J.-P.; Rhodes, J.; Mobasher, B.; Moreau, C.; Peacock, J. A.; A.; Rix, H.-W.; Pentericci, L.; Strauss, M. A.; Carilli, Johnston, D. E.; Capak, P.; Heymans, C.; Ellis, R. Porciani, C.; Pozzetti, L.; Scaramella, R.; C.; Wagner, S.; Black Hole Masses and Enrich- S.; Koekemoer, A. M.; Le Fèvre, O.; Mellier, Y.; Ré- Schiminovich, D.; Shopbell, P.; Smail, I.; ment of z ~ 6 SDSS Quasars; ApJ 669, 32–44 frégier, A.; Robin, A. C.; Scoville, N.; Tasca, L.; Thompson, D.; Tresse, L.; Vettolani, G.; Zanichelli, Kurtz, D. W.; Elkin, V. G.; Mathys, G.; The detection Taylor, J. E.; Van Waerbeke, L.; Weak Gravitational A.; Zucca, E.; zCOSMOS: A Large VLT/VIMOS of the very low amplitude 16.2-min pulsation in in- Lensing with COSMOS: Galaxy Selection and Redshift Survey Covering 0 < z < 3 in the dividual lines of first ionization stage of rare earth Shape Measurements; ApJS 172, 219–238 COSMOS Field; ApJS 172, 70–85 elements in the roAp star ßCrB; MNRAS 380, Lecureur, A.; Hill, V.; Zoccali, M.; Barbuy, B.; Gómez, Limousin, M.; Richard, J.; Jullo, E.; Kneib, J.-P.; Fort, 741–748 A.; Minniti, D.; Ortolani, S.; Renzini, A.; Oxygen, B.; Soucail, G.; Elíasdóttir, Á.; Natarajan, P.; Ellis, Kurtev, R.; Borissova, J.; Georgiev, L.; Ortolani, S.; sodium, magnesium, and aluminium as tracers of R. S.; Smail, I.; Czoske, O.; Smith, G. P.; Hudelot, Ivanov, V. D.; Obscured clusters. – I. GLIMPSE the galactic bulge formation; A&A 465, 799–814 P.; Bardeau, S.; Ebeling, H.; Egami, E.; Knudsen, 30 – A young Milky Way star cluster hosting Wolf- Lee, T.-H.; Stanghellini, L.; Ferrario, L.; K. K.; Combining Strong and Weak Gravitational Rayet stars; A&A 475, 209–216 Wickramasinghe, D.; High-Resolution Spectra of Lensing in Abell 1689; ApJ 668, 643–666 Kurtz, D. W.; Elkin, V. G.; Mathys, G.; van Wyk, F.; On Bright Central Stars of Bipolar Planetary Nebulae Lin, Z. Y.; Weiler, M.; Rauer, H.; Ip, W. H.; Photometry the nature of the upper atmospheric variability in and the Question of Magnetic Shaping; AJ 133, and imaging of comet C/2004 Q2 (Machholz) at the rapidly oscillating Ap star HD 134214; MNRAS 987–999 Lulin and La Silla; A&A 469, 771–776 381, 1301–1312 Lee, H.; Zucker, D. B.; Grebel, E. K.; Interstellar Linder, N.; Rauw, G.; Sana, H.; De Becker, M.; Labbé, I.; Franx, M.; Rudnick, G.; Schreiber, N. M. F.; medium oxygen abundances of dwarf irregular Gosset, E.; The Struve-Sahade effect in the opti- van Dokkum, P. G.; Moorwood, A.; Rix, H.-W.; galaxies in Centaurus A and nearby groups; cal spectra of O-type binaries. – I. Main-sequence Röttgering, H.; Trujillo, I.; van der Werf, P.; The MNRAS 376, 820–840 systems; A&A 474, 193–204 Color-Magnitude Distribution of Field Galaxies to Lefever, K.; Puls, J.; Aerts, C.; Statistical properties Driver, S. P.; Allen, P. D.; Liske, J.; Graham, A. W.; z ~ 3: The Evolution and Modeling of the Blue Se- of a sample of periodically variable B-type super- The Millennium Galaxy Catalogue: The Luminosity quence; ApJ 665, 944–972 giants. Evidence for opacity-driven gravity-mode Functions of Bulges and Disks and Their Implied Labiano, A.; Barthel, P. D.; O’Dea, C. P.; de Vries, W. oscillations; A&A 463, 1093–1109 Stellar Mass Densities; ApJ 657, L85–L88 H.; Pérez, I.; Baum, S. A.; GPS radio sources: new Leipski, C.; Haas, M.; Meusinger, H.; Siebenmorgen, De Propris, R.; Conselice, C. J.; Liske, J.; Driver, S. optical observations and an updated master list; R.; Chini, R.; Drass, H.; Albrecht, M.; Wilkes, B. J.; P.; Patton, D. R.; Graham, A. W.; Allen, P. D.; The A&A 463, 97–104 Huchra, J. P.; Ott, S.; Cesarsky, C.; Cutri, R.; Nar- Millennium Galaxy Catalogue: The Connection Lachaume, R.; Preibisch, T.; Driebe, T.; Weigelt, G.; row-line AGN in the ISO-2MASS survey; A&A 464, between Close Pairs and Asymmetry; Implications Resolving the B[e] star Hen 3-1191 at 10 μm with 895–901 for the Galaxy Merger Rate; ApJ 666, 212–221 VLTI/MIDI; A&A 469, 587–593 Leipski, C.; Haas, M.; Siebenmorgen, R.; Meusinger, Liu, Y. J.; Zhao, G.; Shi, J. R.; Pietrzyn´ski, G.; Gieren, Lacy, J. H.; Jaffe, D. T.; Zhu, Q.; Richter, M. J.; Bitner, H.; Albrecht, M.; Cesarsky, C.; Chini, R.; Cutri, R.; W.; The abundances of nearby red clump giants; M. A.; Greathouse, T. K.; Volk, K.; Geballe, T. R.; Drass, H.; Huchra, J. P.; Ott, S.; Wilkes, B. J.; The MNRAS 382, 553–566 Mehringer, D. M.; W51 IRS 2: A Massive Jet reddest ISO-2MASS quasar; A&A 473, 121–128 Lo Curto, G.; Mignani, R. P.; Perna, R.; Israel, G. L.; Emerging from a Molecular Cloud into an H ii Re- Lemasle, B.; François, P.; Bono, G.; Mottini, M.; Deep VLT infrared observations of X-ray dim iso- gion; ApJ 658, L45–L49 Primas, F.; Romaniello, M.; Detailed chemical lated neutron stars; A&A 473, 539–543 Lagos, P.; Telles, E.; Melnick, J.; Narrow-band Hß composition of Galactic Cepheids. A determina- images of star-formation regions in H ii galaxies; tion of the Galactic abundance gradient in the A&A 476, 89–96 8–12 kpc region; A&A 467, 283–294 Letawe, G.; Magain, P.; Courbin, F.; Jablonka, P.; Jahnke, K.; Meylan, G.; Wisotzki, L.; On-axis spectroscopy of the host galaxies of 20 optically luminous quasars at z ~ 0.3; MNRAS 378, 83–108

ESO Annual Report 2007 109 Lodieu, N.; Pinfield, D. J.; Leggett, S. K.; Jameson, Malbet, F.; Benisty, M.; de Wit, W.-J.; Kraus, S.; Margutti, R.; Chincarini, G.; Covino, S.; Tagliaferri, G.; R. F.; Mortlock, D. J.; Warren, S. J.; Burningham, Meilland, A.; Millour, F.; Tatulli, E.; Berger, J.-P.; Campana, S.; Della Valle, M.; Filippenko, A. V.; B.; Lucas, P. W.; Chiu, K.; Liu, M. C.; Venemans, Chesneau, O.; Hofmann, K.-H.; Isella, A.; Natta, Fiore, F.; Foley, R.; Fugazza, D.; Giommi, P.; B. P.; McMahon, R. G.; Allard, F.; Baraffe, I.; Y A.; Petrov, R. G.; Preibisch, T.; Stee, P.; Testi, L.; Malesani, D.; Moretti, A.; Stella, L.; The host gal- Navascués, D. B.; Carraro, G.; Casewell, S. L.; Weigelt, G.; Antonelli, P.; Beckmann, U.; Bresson, axy of GRB 031203: a new spectroscopic study; Chabrier, G.; Chappelle, R. J.; Clarke, F.; Day- Y.; Chelli, A.; Dugué, M.; Duvert, G.; Gennari, S.; A&A 474, 815–826 Jones, A. C.; Deacon, N. R.; Dobbie, P. D.; Folkes, Glück, L.; Kern, P.; Lagarde, S.; Le Coarer, E.; Lisi, Marilli, E.; Frasca, A.; Covino, E.; Alcalá, J. M.; S. L.; Hambly, N. C.; Hewett, P. C.; Hodgkin, S. T.; F.; Perraut, K.; Puget, P.; Rantakyrö, F.; Robbe- Catalano, S.; Fernández, M.; Arellano Ferro, A.; Jones, H. R. A.; Kendall, T. R.; Magazzù, A.; Dubois, S.; Roussel, A.; Zins, G.; Accardo, M.; Rubio-Herrera, E.; Spezzi, L.; Rotational periods Martín, E. L.; McCaughrean, M. J.; Nakajima, T.; Acke, B.; Agabi, K.; Altariba, E.; Arezki, B.; Aristidi, of solar-mass young stars in Orion; A&A 463, Pavlenko, Y.; Tamura, M.; Tinney, C. G.; Zapatero E.; Baffa, C.; Behrend, J.; Blöcker, T.; Bonhomme, 1081–1091 Osorio, M. R.; Eight new T4.5–T7.5 dwarfs discov- S.; Busoni, S.; Cassaing, F.; Clausse, J.-M.; Colin, Maris, M.; Carraro, G.; Parisi, M. G.; Light curves and ered in the UKIDSS Large Area Survey Data Re- J.; Connot, C.; Delboulbé, A.; Domiciano de colours of the faint Uranian irregular satellites lease 1; MNRAS 379, 1423–1430 Souza, A.; Driebe, T.; Feautrier, P.; Ferruzzi, D.; Sycorax, Prospero, Stephano, Setebos, and Londish, D.; Croom, S. M.; Heidt, J.; Boyle, B. J.; Forveille, T.; Fossat, E.; Foy, R.; Fraix-Burnet, D.; Trinculo; A&A 472, 311–319 Sadler, E. M.; Whiting, M.; Rector, T. A.; Pursimo, Gallardo, A.; Giani, E.; Gil, C.; Glentzlin, A.; Marquart, T.; Fathi, K.; Ã-Stlin, G.; Bergvall, N.; T.; Chynoweth, K.; The 2QZ BL Lac survey – II; Heiden, M.; Heininger, M.; Hernandez Utrera, O.; Cumming, R. J.; Amram, P.; Star-gas decoupling MNRAS 374, 556–578 Kamm, D.; Kiekebusch, M.; Le Contel, D.; Le and a non-rotating stellar core in He 2–10. Integral López-Sánchez, Á. R.; Esteban, C.; García-Rojas, J.; Contel, J.-M.; Lesourd, T.; Lopez, B.; Lopez, M.; field spectroscopy with FLAMES/ARGUS; A&A Peimbert, M.; Rodríguez, M.; The Localized Magnard, Y.; Marconi, A.; Mars, G.; Martinot-La- 474, L9–L12 Chemical Pollution in NGC 5253 Revisited: Results garde, G.; Mathias, P.; Mège, P.; Monin, J.-L.; Martayan, C.; Frémat, Y.; Hubert, A.-M.; Floquet, M.; from Deep Echelle Spectrophotometry; ApJ 656, Mouillet, D.; Mourard, D.; Nussbaum, E.; Ohnaka, Zorec, J.; Neiner, C.; Effects of metallicity, star- 168–185 K.; Pacheco, J.; Perrier, C.; Rabbia, Y.; Rebattu, formation conditions, and evolution in B and Be Lopez, S.; Ellison, S.; D’Odorico, S.; Kim, T.-S.; S.; Reynaud, F.; Richichi, A.; Robini, A.; stars. – II. Small Magellanic Cloud, field of Clues to the nature of high-redshift O v i absorption Sacchettini, M.; Schertl, D.; Schöller, M.; NGC 330; A&A 462, 683–694 systems from their lack of small-scale structure; Solscheid, W.; Spang, A.; Stefanini, P.; Tallon, M.; Martins, F.; Genzel, R.; Hillier, D. J.; Eisenhauer, F.; A&A 469, 61–74 Tallon-Bosc, I.; Tasso, D.; Vakili, F.; von der Lühe, Paumard, T.; Gillessen, S.; Ott, T.; Trippe, S.; Stel- Lopes de Oliveira, R.; Motch, C.; Smith, M. A.; O.; Valtier, J.-C.; Vannier, M.; Ventura, N.; Disk and lar and wind properties of massive stars in the Negueruela, I.; Torrejón, J. M.; On the X-ray and wind interaction in the young stellar object MWC central parsec of the Galaxy; A&A 468, 233–254 optical properties of the Be star HD 110432: a very 297 spatially resolved with AMBER/VLTI; A&A Martin-Zaïdi, C.; Lagage, P.-O.; Pantin, E.; Habart, E.; hard-thermal X-ray emitter; A&A 474, 983–996 464, 43–53 Detection of Warm Molecular Hydrogen in Lorin, O.; Rousselot, P.; Search for cometary activity Malesani, D.; Covino, S.; D’Avanzo, P.; D’Elia, V.; the Circumstellar Disk around the Herbig Ae Star

in three Centaurs [(60558) Echeclus, 2000 FZ53 Fugazza, D.; Piranomonte, S.; Ballo, L.; Campana, HD 97048; ApJ 666, L117–L120 and 2000 GM137] and two trans-Neptunian objects S.; Stella, L.; Tagliaferri, G.; Antonelli, L. A.; Martayan, C.; Floquet, M.; Hubert, A. M.; Gutiérrez- [(29981) 1999 TD10 and (28978) Ixion]; MNRAS Chincarini, G.; Della Valle, M.; Goldoni, P.; Gui- Soto, J.; Fabregat, J.; Neiner, C.; Mekkas, M.; 376, 881–889 dorzi, C.; Israel, G. L.; Lazzati, D.; Melandri, A.; Be stars and binaries in the field of the SMC open Lovis, C.; Pepe, F.; A new list of thorium and argon Pellizza, L. J.; Romano, P.; Stratta, G.; Vergani, S. cluster NGC 330 with VLT-FLAMES; A&A 472, spectral lines in the visible; A&A 468, 1115–1121 D.; Multicolor observations of the afterglow of the 577–586 Lovis, C.; Mayor, M.; Planets around evolved inter- short/hard GRB 050724; A&A 473, 77–84 Mashonkina, L.; Korn, A. J.; Przybilla, N.; A non-LTE mediate-mass stars. – I. Two substellar Maness, H.; Martins, F.; Trippe, S.; Genzel, R.; study of neutral and singly-ionized calcium in late- companions in the open clusters NGC 2423 and Graham, J. R.; Sheehy, C.; Salaris, M.; Gillessen, type stars; A&A 461, 261–275 NGC 4349; A&A 472, 657–664 S.; Alexander, T.; Paumard, T.; Ott, T.; Abuter, R.; Mason, E.; Wickramasinghe, D.; Howell, S. B.; Lowry, S. C.; Fitzsimmons, A.; Pravec, P.; Eisenhauer, F.; Evidence for a Long-standing Top- Szkody, P.; First detection of Zeeman absorption Vokrouhlický, D.; Boehnhardt, H.; Taylor, P. A.; heavy Initial Mass Function in the Central Parsec lines in the polar VV Puppis. Observations of low Margot, J.-L.; Galád, A.; Irwin, M.; Irwin, J.; of the Galaxy; ApJ 669, 1024–1041 activity states; A&A 467, 277–281 Kusnirák, P.; Direct Detection of the Asteroidal Manfroid, J.; Hutsemékers, D.; Jehin, E.; Cochran, A. Massey, R.; Rhodes, J.; Ellis, R.; Scoville, N.; YORP Effect; Sci 316, 272 L.; Arpigny, C.; Jackson, W. M.; Meech, K. J.; Leauthaud, A.; Finoguenov, A.; Capak, P.; Bacon, Lynch, R. S.; Charlton, J. C.; Physical Properties of Schulz, R.; Zucconi, J.-M.; The impact and rota- D.; Aussel, H.; Kneib, J.-P.; Koekemoer, A.; Mc- Weak Mg ii Absorbers at z ~ 2; ApJ 666, 64–78 tional light curves of Comet 9P/Tempel 1; Icar 187, Cracken, H.; Mobasher, B.; Pires, S.; Refregier, A.; Mainieri, V.; Hasinger, G.; Cappelluti, N.; Brusa, M.; 144–155 Sasaki, S.; Starck, J.-L.; Taniguchi, Y.; Taylor, A.; Brunner, H.; Civano, F.; Comastri, A.; Elvis, M.; Mannucci, F.; Buttery, H.; Maiolino, R.; Marconi, A.; Taylor, J.; Dark matter maps reveal cosmic scaf- Finoguenov, A.; Fiore, F.; Gilli, R.; Lehmann, I.; Pozzetti, L.; Evidence for strong evolution of the folding; Natur 445, 286–290 Silverman, J.; Tasca, L.; Vignali, C.; Zamorani, G.; cosmic star formation density at high redshifts; Massi, F.; de Luca, M.; Elia, D.; Giannini, T.; Schinnerer, E.; Impey, C.; Trump, J.; Lilly, S.; A&A 461, 423–431 Lorenzetti, D.; Nisini, B.; Star formation in the Vela Maier, C.; Griffiths, R. E.; Miyaji, T.; Capak, P.; Marchesini, D.; van Dokkum, P.; Quadri, R.; Rudnick, molecular ridge. Large scale mapping of cloud D Koekemoer, A.; Scoville, N.; Shopbell, P.; G.; Franx, M.; Lira, P.; Wuyts, S.; Gawiser, E.; in the mm continuum; A&A 466, 1013–1023 Taniguchi, Y.; The XMM-Newton Wide-Field Sur- Christlein, D.; Toft, S.; The Rest-Frame Optical Lu- Massey, P.; Levesque, E. M.; Olsen, K. A. G.; Plez, vey in the COSMOS Field. – IV. X-Ray Spectral minosity Functions of Galaxies at 2 <= z <= 3.5; ApJ B.; Skiff, B. A.; HV 11423: The Coolest Supergiant Properties of Active Galactic Nuclei; ApJS 172, 656, 42–65 in the SMC; ApJ 660, 301–310 368–382 Marcolino, W. L. F.; Hillier, D. J.; de Araujo, F. X.; Massey, R.; Rhodes, J.; Leauthaud, A.; Capak, P.; Maiolo, B.; Strafella, F.; Campeggio, L.; Elia, D.; Pereira, C. B.; Detailed Far-Ultraviolet to Optical Ellis, R.; Koekemoer, A.; Réfrégier, A.; Scoville, N.; Aiello, S.; Optical and Near-IR Imaging of the Dark Analysis of Four [WR] Stars; ApJ 654, 1068–1086 Taylor, J. E.; Albert, J.; Bergé, J.; Heymans, C.; Globule CB 52; ApJ 661, 926–937 Marchenko, S. V.; Foellmi, C.; Moffat, A. F. J.; Johnston, D.; Kneib, J.-P.; Mellier, Y.; Mobasher, Martins, F.; Bouret, J.-C.; Depagne, E.; Spectros- B.; Semboloni, E.; Shopbell, P.; Tasca, L.; Van copy of SMC Wolf-Rayet Stars Suggests that Waerbeke, L.; COSMOS: Three-dimensional Wind Clumping Does Not Depend on Ambient Weak Lensing and the Growth of Structure; ApJS Metallicity; ApJ 656, L77–L80 172, 239–253 Maret, S.; Bergin, E. A.; Lada, C. J.; Using Chemistry to Unveil the Kinematics of Starless Cores: Com- plex Radial Motions in Barnard 68; ApJ 670, L25–L28

110 ESO Annual Report 2007 Mathys, G.; Kurtz, D. W.; Elkin, V. G.; Pulsation in the Meilland, A.; Millour, F.; Stee, P.; Domiciano de Merlin, F.; Guilbert, A.; Dumas, C.; Barucci, M. A.; presence of a strong magnetic field: the roAp star Souza, A.; Petrov, R. G.; Mourard, D.; Jankov, S.; de Bergh, C.; Vernazza, P.; Properties of the icy

HD 166473; MNRAS 380, 181–198 Robbe-Dubois, S.; Spang, A.; Aristidi, E.; An- surface of the TNO 136108 (2003 EL61); A&A 466, Matsuura, M.; Speck, A. K.; Smith, M. D.; Zijlstra, A. tonelli, P.; Beckmann, U.; Bresson, Y.; Chelli, A.; 1185 –1188 A.; Viti, S.; Lowe, K. T. E.; Redman, M.; Wareing, Dugué, M.; Duvert, G.; Gennari, S.; Glück, L.; Mermilliod, J.-C.; Mayor, M.; Red giants in open C. J.; Lagadec, E.; VLT/near-infrared integral field Kern, P.; Lagarde, S.; Le Coarer, E.; Lisi, F.; clusters. – XII. Six old open clusters NGC 2112, spectrometer observations of molecular hydrogen Malbet, F.; Perraut, K.; Puget, P.; Rantakyrö, F.; 2204, 2243, 2420, 2506, 2682; A&A 470, 919–926 lines in the knots of the planetary nebula NGC 7293 Roussel, A.; Tatulli, E.; Weigelt, G.; Zins, G.; Mermilliod, J.-C.; Andersen, J.; Latham, D. W.; (the Helix Nebula); MNRAS 382, 1447–1459 Accardo, M.; Acke, B.; Agabi, K.; Altariba, E.; Mayor, M.; Red giants in open clusters. – XIII. Or- Mattila, S.; Väisänen, P.; Farrah, D.; Efstathiou, A.; Arezki, B.; Baffa, C.; Behrend, J.; Blöcker, T.; bital elements of 156 spectroscopic binaries; A&A Meikle, W. P. S.; Dahlen, T.; Fransson, C.; Lira, P.; Bonhomme, S.; Busoni, S.; Cassaing, F.; Clausse, 473, 829–845 Lundqvist, P.; Östlin, G.; Ryder, S.; Sollerman, J.; J.-M.; Colin, J.; Connot, C.; Delboulbé, A.; Driebe, Messineo, M.; Petr-Gotzens, M. G.; Schuller, F.; Adaptive Optics Discovery of Supernova 2004ip T.; Feautrier, P.; Ferruzzi, D.; Forveille, T.; Fossat, Menten, K. M.; Habing, H. J.; Kissler-Patig, M.; in the Nuclear Regions of the Luminous Infrared E.; Foy, R.; Fraix-Burnet, D.; Gallardo, A.; Giani, E.; Modigliani, A.; Reunanen, J.; Integral-field spec- Galaxy IRAS 18293–3413; ApJ 659, L9–L12 Gil, C.; Glentzlin, A.; Heiden, M.; Heininger, M.; troscopy of the Galactic cluster [DBS2003]8. Maturi, M.; Schirmer, M.; Meneghetti, M.; Bartelmann, Hernandez Utrera, O.; Hofmann, K.-H.; Kamm, D.; Discovery of an ultra-compact H ii region and its M.; Moscardini, L.; Searching dark-matter halos in Kiekebusch, M.; Kraus, S.; Le Contel, D.; Le ionizing star in the bright rimmed cloud SFO49; the GaBoDS survey; A&A 462, 473–479 Contel, J.-M.; Lesourd, T.; Lopez, B.; Lopez, M.; A&A 472, 471–482 Maund, J. R.; Wheeler, J. C.; Patat, F.; Baade, D.; Magnard, Y.; Marconi, A.; Mars, G.; Martinot-La- Meyer, L.; Schödel, R.; Eckart, A.; Duschl, W. J.; Wang, L.; Höflich, P.; Spectropolarimetry of the garde, G.; Mathias, P.; Mège, P.; Monin, J.-L.; Karas, V.; Dovcˇiak, M.; On the orientation of the Type Ib/c SN 2005bf; MNRAS 381, 201–210 Mouillet, D.; Nussbaum, E.; Ohnaka, K.; Pacheco, Sagittarius A system; A&A 473, 707–710 Maund, J. R.; Wheeler, J. C.; Patat, F.; Baade, D.; J.; Perrier, C.; Rabbia, Y.; Rebattu, S.; Reynaud, Meynadier, F.; Heydari-Malayeri, M.; Low-excitation Wang, L.; Höflich, P.; Spectropolarimetry of SN F.; Richichi, A.; Robini, A.; Sacchettini, M.; Schertl, blobs in the Magellanic Clouds; A&A 461, 565–569 2006aj at 9.6 days; A&A 475, L1–L4 D.; Schöller, M.; Solscheid, W.; Stefanini, P.; Michielsen, D.; Koleva, M.; Prugniel, P.; Zeilinger, W. Maund, J. R.; Wheeler, J. C.; Patat, F.; Wang, L.; Tallon, M.; Tallon-Bosc, I.; Tasso, D.; Testi, L.; W.; De Rijcke, S.; Dejonghe, H.; Pasquali, A.; Baade, D.; Höflich, P. A.; Spectropolarimetry Vakili, F.; von der Lühe, O.; Valtier, J.-C.; Vannier, Ferreras, I.; Debattista, V. P.; Toward a Solution of the Type IIb Supernova 2001ig; ApJ 671, M.; Ventura, N.; An asymmetry detected in the for the Ca ii Triplet Puzzle: Results from Dwarf El- 1944–1958 disk of κ Canis Majoris with AMBER/VLTI; A&A liptical Galaxies; ApJ 670, L101–L104 Mauron, N.; Gigoyan, K. S.; Kendall, T. R.; The 464, 73–79 Mieske, S.; Hilker, M.; Jordán, A.; Infante, L.; properties of carbon stars found in the Byurakan Meisenheimer, K.; Tristram, K. R. W.; Jaffe, W.; Kissler-Patig, M.; A search for ultra-compact and the Hamburg/ESO surveys; A&A 463, Israel, F.; Neumayer, N.; Raban, D.; Röttgering, H.; dwarf galaxies in the Centaurus galaxy cluster; 969–974 Cotton, W. D.; Graser, U.; Henning, T.; Leinert, C.; A&A 472, 111–119 Maxted, P. F. L.; O’Donoghue, D.; Morales-Rueda, Lopez, B.; Perrin, G.; Prieto, A.; Resolving the Mignano, A.; Miralles, J.-M.; da Costa, L.; Olsen, L. L.; Napiwotzki, R.; Smalley, B.; The mass and ra- innermost parsec of Centaurus A at mid-infrared F.; Prandoni, I.; Arnouts, S.; Benoist, C.; Madejsky, dius of the M-dwarf in the short-period eclipsing wavelengths; A&A 471, 453–465 R.; Slijkhuis, R.; Zaggia, S.; ESO imaging survey: binary RR Caeli; MNRAS 376, 919–928 Mekkaden, M. V.; Muneer, S.; Raveendran, A. V.; optical deep public survey; A&A 462, 553–563 Mazure, A.; Adami, C.; Pierre, M.; Le Fèvre, O.; Photometric, spectroscopic and polarimetric vari- Mignani, R. P.; Bagnulo, S.; Dyks, J.; Lo Curto, G.; Arnouts, S.; Duc, P. A.; Ilbert, O.; Lebrun, V.; Me- ability of the weak-emission T Tauri star HD 288313; Słowikowska, A.; The optical polarisation of the neux, B.; Pacaud, F.; Surdej, J.; Valtchanov, I.; MNRAS 378, 1079–1088 Vela pulsar revisited; A&A 467, 1157–1162 Structure detection in the D1 CFHTLS deep field Melo, C.; Santos, N. C.; Gieren, W.; Pietrzynski, G.; Mignani, R. P.; Perna, R.; Rea, N.; Israel, G. L.; using accurate photometric redshifts: a bench- Ruiz, M. T.; Sousa, S. G.; Bouchy, F.; Lovis, C.; Mereghetti, S.; Curto, G. Lo.; VLT/NACO obser mark; A&A 467, 49–62 Mayor, M.; Pepe, F.; Queloz, D.; da Silva, R.; vations of the high-magnetic field radio pulsar Mazzali, P. A.; Foley, R. J.; Deng, J.; Patat, F.; Pian, Udry, S.; A new Neptune-mass planet orbiting PSR J1119-6127; A&A 471, 265–270 E.; Baade, D.; Bloom, J. S.; Filippenko, A. V.; HD 219828; A&A 467, 721–727 Mignani, R. P.; Zharikov, S.; Caraveo, P. A.; The Perley, D. A.; Valenti, S.; Wang, L.; Kawabata, K.; Memola, E.; Caccianiga, A.; Cocchia, F.; Della Ceca, optical spectrum of the Vela pulsar; A&A 473, Maeda, K.; Nomoto, K.; Keck and European R.; Maccacaro, T.; Severgnini, P.; Fyfe, D. J.; 891–896 Southern Observatory Very Large Telescope View Mateos, S.; Watson, M. G.; Lamer, G.; Searching Mignani, R. P.; de Luca, A.; Zaggia, S.; Sester, D.; of the Symmetry of the Ejecta of the XRF/SN for absorbed AGN in the 2XMM-Newton pre-re- Pellizzoni, A.; Mereghetti, S.; Caraveo, P. A.; VLT 2006aj; ApJ 661, 892–898 lease EPIC Serendipitous Source Catalogue; A&A observations of the central compact object in the McCracken, H. J.; Peacock, J. A.; Guzzo, L.; Capak, 465, 759–764 Vela Jr. supernova remnant; A&A 473, 883–889 P.; Porciani, C.; Scoville, N.; Aussel, H.; Mengel, S.; Tacconi-Garman, L. E.; Medium resolu- Miknaitis, G.; Pignata, G.; Rest, A.; Wood-Vasey, W. Finoguenov, A.; James, J. B.; Kitzbichler, M. G.; tion 2.3 μm spectroscopy of the massive Galactic M.; Blondin, S.; Challis, P.; Smith, R. C.; Stubbs, Koekemoer, A.; Leauthaud, A.; Le Fèvre, O.; open cluster Westerlund 1; A&A 466, 151–155 C. W.; Suntzeff, N. B.; Foley, R. J.; Matheson, T.; Massey, R.; Mellier, Y.; Mobasher, B.; Norberg, P.; Menut, J.-L.; Gendron, E.; Schartmann, M.; Tuthill, Tonry, J. L.; Aguilera, C.; Blackman, J. W.; Becker, Rhodes, J.; Sanders, D. B.; Sasaki, S. S.; P.; Lopez, B.; Danchi, W. C.; Wolf, S.; Lagrange, A. C.; Clocchiatti, A.; Covarrubias, R.; Davis, T. Taniguchi, Y.; Thompson, D. J.; White, S. D. M.; A.-M.; Flament, S.; Rouan, D.; Clénet, Y.; Berruyer, M.; Filippenko, A. V.; Garg, A.; Garnavich, P. M.; El-Zant, A.; The Angular Correlations of Galaxies N.; The carbon star IRC+10216: linking the com- Hicken, M.; Jha, S.; Krisciunas, K.; Kirshner, R. P.; in the COSMOS Field; ApJS 172, 314–319 plex inner region with its spherical large-scale Leibundgut, B.; Li, W.; Miceli, A.; Narayan, G.; McDonald, I.; van Loon, J. T.; Dust, pulsation, structures; MNRAS 376, L6–L10 Prieto, J. L.; Riess, A. G.; Salvo, M. E.; Schmidt, chromospheres and their rôle in driving mass loss Mérand, A.; Aufdenberg, J. P.; Kervella, P.; du B. P.; Sollerman, J.; Spyromilio, J.; Zenteno, A.; from red giants in Galactic globular clusters; A&A Foresto, V. C.; ten Brummelaar, T. A.; McAlister, H. The ESSENCE Supernova Survey: Survey Optimi- 476, 1261–1282 A.; Sturmann, L.; Sturmann, J.; Turner, N. H.; Ex- zation, Observations, and Supernova Photometry; McNamara, D. H.; Clementini, G.; Marconi, M.; A δ tended Envelopes around Galactic Cepheids. ApJ 666, 674–693 Scuti Distance to the Large Magellanic Cloud; AJ – III. Y Ophiuchi and α Persei from Near-Infrared 133, 2752–2763 Interferometry with CHARA/FLUOR; ApJ 664, Meilland, A.; Stee, P.; Vannier, M.; Millour, F.; 1093–1101 Domiciano de Souza, A.; Malbet, F.; Martayan, C.; Merín, B.; Augereau, J.-C.; van Dishoeck, E. F.; Paresce, F.; Petrov, R. G.; Richichi, A.; Spang, A.; Kessler-Silacci, J.; Dullemond, C. P.; Blake, G. A.; First direct detection of a Keplerian rotating disk Lahuis, F.; Brown, J. M.; Geers, V. C.; Pontoppidan, around the Be star α Arae using AMBER/VLTI; K. M.; Comerón, F.; Frasca, A.; Guieu, S.; Alcalá, A&A 464, 59–71 J. M.; Boogert, A. C. A.; Evans II, N. J.; D’Alessio, P.; Mundy, L. G.; Chapman, N.; Abundant Crystal- line Silicates in the Disk of a Very Low Mass Star; ApJ 661, 361–367

ESO Annual Report 2007 111 Millour, F.; Petrov, R. G.; Chesneau, O.; Bonneau, D.; Monaco, L.; Bellazzini, M.; Bonifacio, P.; Buzzoni, A.; Narayanan, A.; Misawa, T.; Charlton, J. C.; Kim, Dessart, L.; Bechet, C.; Tallon-Bosc, I.; Tallon, M.; Ferraro, F. R.; Marconi, G.; Sbordone, L.; Zaggia, T.-S.; A Survey of Weak Mg ii Absorbers at Thiébaut, E.; Vakili, F.; Malbet, F.; Mourard, D.; An- S.; High-resolution spectroscopy of RGB stars in 0.4 < z < 2.4; ApJ 660, 1093–1105 tonelli, P.; Beckmann, U.; Bresson, Y.; Chelli, A.; the Sagittarius streams. – I. Radial velocities and Nardetto, N.; Mourard, D.; Mathias, P.; Fokin, A.; Dugué, M.; Duvert, G.; Gennari, S.; Glück, L.; chemical abundances; A&A 464, 201–209 Gillet, D.; High-resolution spectroscopy for Kern, P.; Lagarde, S.; Le Coarer, E.; Lisi, F.; Moni Bidin, C.; Moehler, S.; Piotto, G.; Momany, Y.; Cepheids distance determination. – II. A period- Perraut, K.; Puget, P.; Rantakyrö, F.; Robbe- Recio-Blanco, A.; Spectroscopy of horizontal projection factor relation; A&A 471, 661–669 Dubois, S.; Roussel, A.; Tatulli, E.; Weigelt, G.; branch stars in NGC 6752. Anomalous results on Negrão, A.; Hirtzig, M.; Coustenis, A.; Gendron, E.; Zins, G.; Accardo, M.; Acke, B.; Agabi, K.; Al- atmospheric parameters and masses; A&A 474, Drossart, P.; Rannou, P.; Combes, M.; Boudon, V.; tariba, E.; Arezki, B.; Aristidi, E.; Baffa, C.; Be- 505–514 The 2-μm spectroscopy of Huygens probe landing hrend, J.; Blöcker, T.; Bonhomme, S.; Busoni, S.; Moraux, E.; Bouvier, J.; Stauffer, J. R.; Navascués, D. site on Titan with Very Large Telescope/Nasmyth Cassaing, F.; Clausse, J.-M.; Colin, J.; Connot, C.; Barrado Y.; Cuillandre, J.-C.; The lower mass Adaptive Optics System Near-Infrared Imager and Delboulbé, A.; Domiciano de Souza, A.; Driebe, T.; function of the young open cluster Blanco 1: from Spectrograph; JGRE 112

Feautrier, P.; Ferruzzi, D.; Forveille, T.; Fossat, E.; 30 MJup to 3 M0; A&A 471, 499–513 Negueruela, I.; Schurch, M. P. E.; A search for Foy, R.; Fraix-Burnet, D.; Gallardo, A.; Giani, E.; Morganti, R.; Holt, J.; Saripalli, L.; Oosterloo, T. A.; counterparts to massive X-ray binaries using Gil, C.; Glentzlin, A.; Heiden, M.; Tadhunter, C. N.; IC 5063: AGN driven outflow of photometric catalogues; A&A 461, 631–639 Heininger, M.; Hernandez Utrera, O.; Hofmann, warm and cold gas; A&A 476, 735–743 Nesvadba, N. P. H.; Lehnert, M. D.; Genzel, R.; K.-H.; Kamm, D.; Kiekebusch, M.; Kraus, S.; Le Mottram, J. C.; Hoare, M. G.; Lumsden, S. L.; Eisenhauer, F.; Baker, A. J.; Seitz, S.; Davies, R.; Contel, D.; Le Contel, J.-M.; Lesourd, T.; Lopez, Oudmaijer, R. D.; Urquhart, J. S.; Sheret, T. L.; Lutz, D.; Tacconi, L.; Tecza, M.; Bender, R.; B.; Lopez, M.; Magnard, Y.; Marconi, A.; Mars, G.; Clarke, A. J.; Allsopp, J.; The RMS survey: mid-in- Abuter, R.; Intense Star Formation and Feedback Martinot-Lagarde, G.; Mathias, P.; Mège, P.; frared observations of candidate massive YSOs in at High Redshift: Spatially Resolved Properties of Monin, J.-L.; Mouillet, D.; Nussbaum, E.; Ohnaka, the southern hemisphere; A&A 476, 1019–1111 the z = 2.6 Submillimeter Galaxy SMM K.; Pacheco, J.; Perrier, C.; Rabbia, Y.; Rebattu, Mshar, A. C.; Charlton, J. C.; Lynch, R. S.; Churchill, J14011+0252; ApJ 657, 725–737 S.; Reynaud, F.; Richichi, A.; Robini, A.; Sacchettini, C.; Kim, T.-S.; The Kinematic Evolution of Strong Nesvadba, N. P. H.; Lehnert, M. D.; De Breuck, C.; M.; Schertl, D.; Schöller, M.; Solscheid, W.; Mgii Absorbers; ApJ 669, 135–157 Gilbert, A.; van Breugel, W.; Compact radio Spang, A.; Stee, P.; Stefanini, P.; Tasso, D.; Testi, Mucciarelli, P.; Zampieri, L.; Treves, A.; Turolla, R.; sources and jet-driven AGN feedback in the early L.; von der Lühe, O.; Valtier, J.-C.; Vannier, M.; Falomo, R.; X-Ray and Optical Variability of the Ul- universe: constraints from integral-field spectros- Ventura, N.; Direct constraint on the distance of traluminous X-Ray Source NGC 1313 X-2; ApJ copy; A&A 475, 145–153 γ2 Velorum from AMBER/VLTI observations; A&A 658, 999–1005 Neumayer, N.; Cappellari, M.; Reunanen, J.; Rix, 464, 107–118 Mugrauer, M.; Neuhäuser, R.; Mazeh, T.; The multi- H.-W.; van der Werf, P. P.; de Zeeuw, P. T.; Davies, Minniti, D.; Fernández, J. M.; Díaz, R. F.; Udalski, A.; plicity of exoplanet host stars. Spectroscopic R. I.; The Central Parsecs of Centaurus A: High- Pietrzynski, G.; Gieren, W.; Rojo, P.; Ruíz, M. T.; confirmation of the companions GJ 3021 B and excitation Gas, a Molecular Disk, and the Mass of Zoccali, M.; Millimagnitude Photometry for Transit- HD 27442 B, one new planet host triple-star sys- the Black Hole; ApJ 671, 1329–1344 ing Extrasolar Planetary Candidates. – III. Accu- tem, and global statistics; A&A 469, 755–770 Nielbock, M.; Chini, R.; Hoffmeister, V. H.; rate Radius and Period for OGLE-TR-111-b; ApJ Mugrauer, M.; Seifahrt, A.; Neuhäuser, R.; The multi- Scheyda, C. M.; Steinacker, J.; Nürnberger, D.; 660, 858–862 plicity of planet host stars – new low-mass Siebenmorgen, R.; The Morphology of M17-UC1: Mobasher, B.; Capak, P.; Scoville, N. Z.; Dahlen, T.; companions to planet host stars; MNRAS 378, A Disk Candidate Surrounding a Hypercompact Salvato, M.; Aussel, H.; Thompson, D. J.; 1328–1334 H ii Region; ApJ 656, L81–L84 Feldmann, R.; Tasca, L.; Lefevre, O.; Lilly, S.; Mundell, C. G.; Melandri, A.; Guidorzi, C.; Kobayashi, Nieppola, E.; Tornikoski, M.; Lähteenmäki, A.; Carollo, C. M.; Kartaltepe, J. S.; McCracken, H.; S.; Steele, I. A.; Malesani, D.; Amati, L.; D’Avanzo, Valtaoja, E.; Hakala, T.; Hovatta, T.; Kotiranta, M.; Mould, J.; Renzini, A.; Sanders, D. B.; Shopbell, P. P.; Bersier, D. F.; Gomboc, A.; Rol, E.; Bode, M. F.; Nummila, S.; Ojala, T.; Parviainen, M.; Ranta, M.; L.; Taniguchi, Y.; Ajiki, M.; Shioya, Y.; Contini, T.; Carter, D.; Mottram, C. J.; Monfardini, A.; Smith, Saloranta, P.-M.; Torniainen, I.; Tröller, M.; 37 GHz Giavalisco, M.; Ilbert, O.; Iovino, A.; Le Brun, V.; R. J.; Malhotra, S.; Wang, J.; Bannister, N.; Observations of a Large Sample of BL Lacertae Mainieri, V.; Mignoli, M.; Scodeggio, M.; Photo- O’Brien, P. T.; Tanvir, N. R.; The Remarkable After- Objects; AJ 133, 1947–1953 metric Redshifts of Galaxies in COSMOS; ApJS glow of GRB 061007: Implications for Optical Nieva, M. F.; Przybilla, N.; Hydrogen and helium 172, 117–131 Flashes and GRB Fireballs; ApJ 660, 489–495 line formation in OB dwarfs and giants. A hybrid Moehler, S.; Dreizler, S.; Lanz, T.; Bono, G.; Sweigart, Muñoz, D. J.; Mardones, D.; Garay, G.; Rebolledo, non-LTE approach; A&A 467, 295–309 A. V.; Calamida, A.; Monelli, M.; Nonino, M.; The D.; Brooks, K.; Bontemps, S.; Massive Clumps Nigoche-Netro, A.; Moles, M.; Ruelas-Mayorga, A.; hottest horizontal-branch stars in ω Centauri. Late in the NGC 6334 Star-forming Region; ApJ 668, Franco-Balderas, A.; Kjørgaard, P.; Structural hot flasher vs. helium enrichment; A&A 475, L5–L8 906–917 properties of isolated early-type galaxies. The de- Mohanty, S.; Jayawardhana, R.; Huélamo, N.; Murphy, M. T.; Curran, S. J.; Webb, J. K.; Ménager, pendence of scaling relations on environment; Mamajek, E.; The Planetary Mass Companion H.; Zych, B. J.; The connection between metallic- A&A 472, 773–784 2MASS 1207–3932B: Temperature, Mass, and Evi- ity and metal-line kinematics in (sub-)damped Lyα Nikolic´, S.; Garay, G.; Rubio, M.; Johansson, L. E. B.; dence for an Edge-on Disk; ApJ 657, 1064–1091 systems; MNRAS 376, 673–681 CO and CS in the Magellanic Clouds: a χ2-analysis Mokiem, M. R.; de Koter, A.; Evans, C. J.; Puls, J.; Murphy, M. T.; Tzanavaris, P.; Webb, J. K.; Lovis, C.; of multitransitional data based on the MEP radia- Smartt, S. J.; Crowther, P. A.; Herrero, A.; Langer, Selection of ThAr lines for wavelength calibration tive transfer model; A&A 471, 561–571 N.; Lennon, D. J.; Najarro, F.; Villamariz, M. R.; of echelle spectra and implications for variations Nilsson, K. K.; Møller, P.; Möller, O.; Fynbo, J. P. U.; Vink, J. S.; The VLT-FLAMES survey of massive in the fine-structure constant; MNRAS 378, Michałowski, M. J.; Watson, D.; Ledoux, C.; Ro- stars: wind properties and evolution of hot mas- 221–230 sati, P.; Pedersen, K.; Grove, L. F.; A multi-wave- sive stars in the Large Magellanic Cloud; A&A Mužic´, K.; Eckart, A.; Schödel, R.; Meyer, L.; Zensus, length study of z = 3.15 Lyman-α emitters in the 465, 1003–1019 A.; First proper motions of thin dust filaments at GOODS South Field; A&A 471, 71–82 Moll, S. L.; Mengel, S.; de Grijs, R.; Smith, L. J.; the Galactic center; A&A 469, 993–1002 Nissen, H. D.; Gustafsson, M.; Lemaire, J. L.; Clénet, Crowther, P. A.; Cluster and nebular properties Naef, D.; Mayor, M.; Benz, W.; Bouchy, F.; Lo Curto, Y.; Rouan, D.; Field, D.; Observations of spatial of the central star-forming region of NGC 1140; G.; Lovis, C.; Moutou, C.; Pepe, F.; Queloz, D.; and velocity structure in the Orion molecular MNRAS 382, 1877–1888 Santos, N. C.; Udry, S.; The HARPS search for cloud; A&A 466, 949–968 Momany, Y.; Held, E. V.; Saviane, I.; Zaggia, S.; Rizzi, southern extra-solar planets. – IX. Exoplanets or- Nissen, P. E.; Akerman, C.; Asplund, M.; Fabbian, D.; L.; Gullieuszik, M.; The blue plume population biting HD 100777, HD 190647, and HD 221287; Kerber, F.; Kaufl, H. U.; Pettini, M.; Sulphur and in dwarf spheroidal galaxies. Genuine blue strag- A&A 470, 721–726 zinc abundances in Galactic halo stars revisited; glers or young stellar population?; A&A 468, A&A 469, 319–330 973–978 Noël, N. E. D.; Gallart, C.; Stellar Populations in the Outskirts of the Small Magellanic Cloud: No Outer Edge Yet; ApJ 665, L23–L26

112 ESO Annual Report 2007 Noll, S.; Pierini, D.; Pannella, M.; Savaglio, S.; Page, M. J.; Lehmann, I.; Boller, T.; Watson, M. G.; Pavlenko, Y. V.; Jones, H. R. A.; Martín, E. L.; Presence of dust with a UV bump in massive, Dwelly, T.; Hess, S.; Matute, I.; Loaring, N. S.; Guenther, E.; Kenworthy, M. A.; Zapatero Osorio, star-forming galaxies at 1 < z < 2.5; A&A 472, Rosen, S.; Ziaeepour, H.; Schwope, A.; Lamer, G.; M. R.; Lithium in LP944–20; MNRAS 380, 455–469 Carrera, F. J.; Tedds, J.; Della Ceca, R.; Severgnini, 1285–1296 Norris, J. E.; Christlieb, N.; Korn, A. J.; Eriksson, K.; P.; McMahon, R. G.; Yuan, W.; The XMM-SSC Peña, M.; Richer, M. G.; Stasin´ska, G.; A catalog of Bessell, M. S.; Beers, T. C.; Wisotzki, L.; Reimers, survey of hard-spectrum XMM-Newton sources planetary nebula candidates and H ii regions in D.; HE 0557–4840: Ultra-Metal-Poor and Carbon- – I. Optically bright sources; MNRAS 378, NGC 3109; A&A 466, 75–82 Rich; ApJ 670, 774–788 1335–1355 Peña, M.; Stasin´ska, G.; Richer, M. G.; The chemical Noterdaeme, P.; Petitjean, P.; Srianand, R.; Ledoux, Paizis, A.; Nowak, M. A.; Chaty, S.; Rodriguez, J.; composition of planetary nebulae and H ii regions C.; Le Petit, F.; Physical conditions in the neutral Courvoisier, T. J.-L.; Del Santo, M.; Ebisawa, K.; in NGC 3109; A&A 476, 745–758 interstellar medium at z = 2.43 toward Q 2348–011; Farinelli, R.; Ubertini, P.; Wilms, J.; Unveiling the Pentericci, L.; Grazian, A.; Fontana, A.; Salimbeni, A&A 469, 425–436 Nature of IGR J17497–2821 Using X-Ray and S.; Santini, P.; de Santis, C.; Gallozzi, S.; Giallongo, Noterdaeme, P.; Ledoux, C.; Petitjean, P.; Le Petit, F.; Near-Infrared Observations; ApJ 657, L109–L112 E.; Physical properties of z ~ 4 LBGs: differences Srianand, R.; Smette, A.; Excitation mechanisms Palla, F.; Randich, S.; Pavlenko, Y. V.; Flaccomio, E.; between galaxies with and without Lyα emission; in newly discovered H2-bearing damped Lyman-α Pallavicini, R.; Old Stars in Young Clusters: Lith- A&A 471, 433–438 clouds: systems with low molecular fractions; A&A ium-depleted Low-Mass Stars of the Orion Nebula Pepe, F.; Correia, A. C. M.; Mayor, M.; Tamuz, O.; 474, 393–407 Cluster; ApJ 659, L41–L44 Couetdic, J.; Benz, W.; Bertaux, J.-L.; Bouchy, F.; Nowak, N.; Saglia, R. P.; Thomas, J.; Bender, R.; Palmeri, P.; Quinet, P.; Biémont, É.; Yushchenko, A. Laskar, J.; Lovis, C.; Naef, D.; Queloz, D.; Santos, Pannella, M.; Gebhardt, K.; Davies, R. I.; The su- V.; Jorissen, A.; van Eck, S.; Radiative decay N. C.; Sivan, J.-P.; Sosnowska, D.; Udry, S.; The permassive black hole in NGC 4486a detected of the 4d5(6S)5p z5,7Po states in Tc ii: comparison HARPS search for southern extra-solar planets. with SINFONI at the Very Large Telescope; along the homologous and isoelectronic se- – VIII. μ Arae, a system with four planets; A&A 462, MNRAS 379, 909–914 quences. Application to astrophysics; MNRAS 769–776 Nürnberger, D. E. A.; Chini, R.; Eisenhauer, F.; 374, 63–71 Pérez-Beaupuits, J. P.; Aalto, S.; Gerebro, H.; Kissler-Patig, M.; Modigliani, A.; Siebenmorgen, Paltani, S.; Le Fèvre, O.; Ilbert, O.; Arnouts, S.; HNC, HCN and CN in Seyfert galaxies; A&A 476, R.; Sterzik, M. F.; Szeifert, T.; Formation of a Bardelli, S.; Tresse, L.; Zamorani, G.; Zucca, E.; 177–192 massive protostar through disk accretion. Bottini, D.; Garilli, B.; Le Brun, V.; Maccagni, D.; Pérez-Torres, M. A.; Mattila, S.; Alberdi, A.; Colina, L.; – II. SINFONI integral field spectroscopy of the Picat, J.-P.; Scaramella, R.; Scodeggio, M.; Torrelles, J. M.; Väisänen, P.; Ryder, S.; Panagia, M17 silhouette disk and discovery of the associ- Vettolani, G.; Zanichelli, A.; Adami, C.; Bolzonella, N.; Wilson, A.; Radio Detection of Supernova

ated H2 jet; A&A 465, 931–936 M.; Cappi, A.; Charlot, S.; Ciliegi, P.; Contini, T.; 2004ip in the Circumnuclear Region of the Lumi- Ohnaka, K.; Driebe, T.; Weigelt, G.; Wittkowski, M.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Guzzo, nous Infrared Galaxy IRAS 18293–3413; ApJ 671, Temporal variations of the outer atmosphere and L.; Iovino, A.; McCracken, H. J.; Marano, B.; L21–L24 the dust shell of the carbon-rich Mira variable V Marinoni, C.; Mazure, A.; Meneux, B.; Merighi, R.; Péroux, C.; Dessauges-Zavadsky, M.; D’Odorico, S.; Ophiuchi probed with VLTI/MIDI; A&A 466, Pellò, R.; Pollo, A.; Pozzetti, L.; Radovich, M.; Kim, T.-S.; McMahon, R. G.; A homogeneous 1099–1110 Bondi, M.; Bongiorno, A.; Brinchmann, J.; sample of sub-damped Lyman systems – IV. Glo- Origlia, L.; Rood, R. T.; Fabbri, S.; Ferraro, F. R.; Fusi Cucciati, O.; de La Torre, S.; Lamareille, F.; Mellier, bal metallicity evolution; MNRAS 382, 177–193 Pecci, F.; Rich, R. M.; The First Empirical Mass- Y.; Merluzzi, P.; Temporin, S.; Vergani, D.; Walcher, Perrin, G.; Verhoelst, T.; Ridgway, S. T.; Cami, J.; Loss Law for Population II Giants; ApJ 667, C. J.; The VIMOS VLT deep survey. The ultraviolet Nguyen, Q. N.; Chesneau, O.; Lopez, B.; Leinert, L85–L88 galaxy luminosity function and luminosity density C.; Richichi, A.; The molecular and dusty compo- Orio, M.; Zezas, A.; Munari, U.; Siviero, A.; at 3 ≤ z ≤ 4; A&A 463, 873–882 sition of Betelgeuse’s inner circumstellar environ- Tepedelenlioglu, E.; Two SMC Symbiotic Stars Pancino, E.; Galfo, A.; Ferraro, F. R.; Bellazzini, M.; ment; A&A 474, 599–608 Undergoing Steady Hydrogen Burning; ApJ 661, The Rotation of Subpopulations in ω Centauri; Persi, P.; Tapia, M.; Gòmez, M.; Whitney, B. A.; 1105 –1111 ApJ 661, L155–L158 Marenzi, A. R.; Roth, M.; ISO-Cha I 192: A New Orton, G. S.; Encrenaz, T.; Leyrat, C.; Puetter, R.; Pasquini, L.; Bonifacio, P.; Randich, S.; Galli, D.; Embedded Eruptive Variable in the Chamaeleon I Friedson, A. J.; Evidence for methane escape and Gratton, R. G.; Wolff, B.; Beryllium abundance in Dark Cloud; AJ 133, 1690–1697 strong seasonal and dynamical perturbations of turn-off stars of NGC 6752; A&A 464, 601–607 Phillips, M. M.; Li, W.; Frieman, J. A.; Blinnikov, S. I.; Neptune’s atmospheric temperatures; A&A 473, Pastorello, A.; Mazzali, P. A.; Pignata, G.; Benetti, S.; DePoy, D.; Prieto, J. L.; Milne, P.; Contreras, C.; L5–L8 Cappellaro, E.; Filippenko, A. V.; Li, W.; Meikle, W. Folatelli, G.; Morrell, N.; Hamuy, M.; Suntzeff, N. Östlin, G.; Cumming, R. J.; Bergvall, N.; Dynamical P. S.; Arkharov, A. A.; Blanc, G.; Bufano, F.; B.; Roth, M.; González, S.; Krzeminski, W.; masses of two young globular clusters in the blue Derekas, A.; Dolci, M.; Elias-Rosa, N.; Foley, R. J.; Filippenko, A. V.; Freedman, W. L.; Chornock, R.; compact galaxy ESO 338–IG04; A&A 461, Ganeshalingam, M.; Harutyunyan, A.; Kiss, L. L.; Jha, S.; Madore, B. F.; Persson, S. E.; Burns, C. 471–483 Kotak, R.; Larionov, V. M.; Lucey, J. R.; Napoleone, R.; Wyatt, P.; Murphy, D.; Foley, R. J.; Ovaldsen, J.-E.; Jaunsen, A. O.; Fynbo, J. P. U.; N.; Navasardyan, H.; Patat, F.; Rich, J.; Ryder, S. Ganeshalingam, M.; Serduke, F. J. D.; Krisciunas, Hjorth, J.; Thöne, C. C.; Féron, C.; Xu, D.; Selj, J. D.; Salvo, M.; Schmidt, B. P.; Stanishev, V.; K.; Bassett, B.; Becker, A.; Dilday, B.; Eastman, J.; H.; Teuber, J.; A Search for Host Galaxies of 24 Székely, P.; Taubenberger, S.; Temporin, S.; Tu- Garnavich, P. M.; Holtzman, J.; Kessler, R.; Gamma-Ray Bursts; ApJ 662, 294–303 ratto, M.; Hillebrandt, W.; ESC and KAIT observa- Lampeitl, H.; Marriner, J.; Frank, S.; Marshall, J. Pacaud, F.; Pierre, M.; Adami, C.; Altieri, B.; Andreon, tions of the transitional Type Ia SN 2004eo; L.; Miknaitis, G.; Sako, M.; Schneider, D. P.; van S.; Chiappetti, L.; Detal, A.; Duc, P.-A.; Galaz, G.; MNRAS 377, 1531–1552 der Heyden, K.; Yasuda, N.; The Peculiar SN Gueguen, A.; Le Fèvre, J.-P.; Hertling, G.; Patat, F.; Chandra, P.; Chevalier, R.; Justham, S.; 2005hk: Do Some Type Ia Supernovae Explode Libbrecht, C.; Melin, J.-B.; Ponman, T. J.; Quintana, Podsiadlowski, P.; Wolf, C.; Gal-Yam, A.; Pasquini, as Deflagrations?; PASP 119, 360–387 H.; Refregier, A.; Sprimont, P.-G.; Surdej, J.; L.; Crawford, I. A.; Mazzali, P. A.; Pauldrach, A. W. Piatti, A. E.; Clariá, J. J.; Mermilliod, J.-C.; Parisi, M. Valtchanov, I.; Willis, J. P.; Alloin, D.; Birkinshaw, A.; Nomoto, K.; Benetti, S.; Cappellaro, E.; C.; Ahumada, A. V.; CCD BVI photometry and M.; Bremer, M. N.; Garcet, O.; Jean, C.; Jones, L. Elias-Rosa, N.; Hillebrandt, W.; Leonard, D. C.; Coravel observations of stars in the open cluster R.; Le Fèvre, O.; Maccagni, D.; Mazure, A.; Proust, Pastorello, A.; Renzini, A.; Sabbadin, F.; Simon, J. NGC 2489; MNRAS 377, 1737–1746 D.; Röttgering, H. J. A.; Trinchieri, G.; The XMM- D.; Turatto, M.; Detection of Circumstellar Material Piatti, A. E.; Sarajedini, A.; Geisler, D.; Gallart, C.; LSS survey: the Class 1 cluster sample over the in a Normal Type Ia Supernova; Sci 317, 924 Wischnjewsky, M.; Two newly identified, relatively initial 5 deg2 and its cosmological modelling; Patat, F.; Benetti, S.; Justham, S.; Mazzali, P. A.; old star clusters in the Small Magellanic Cloud; MNRAS 382, 1289–1308 Pasquini, L.; Cappellaro, E.; Della Valle, M.; MNRAS 381, L84–L88 Padovani, P.; Giommi, P.; Landt, H.; Perlman, E. S.; Podsiadlowski, P.; Turatto, M.; Gal-Yam, A.; The Deep X-Ray Radio Blazar Survey. – III. Radio Simon, J. D.; Upper limit for circumstellar gas Number Counts, Evolutionary Properties, and Lu- around the type Ia SN 2000cx; A&A 474, 931–936 minosity Function of Blazars; ApJ 662, 182–198 Paunzen, E.; Netopil, M.; Zwintz, K.; Investigating star formation in the young open cluster NGC 6383; A&A 462, 157–162

ESO Annual Report 2007 113 Piatti, A. E.; Sarajedini, A.; Geisler, D.; Gallart, C.; Prisinzano, L.; Randich, S.; Lithium abundances in Reda, F. M.; Proctor, R. N.; Forbes, D. A.; Hau, G. K. Wischnjewsky, M.; Five young star clusters in the the old open cluster NGC 3960 from VLT/FLAMES T.; Larsen, S. S.; The spatially resolved stellar outer region of the Small Magellanic Cloud; observations; A&A 475, 539–547 populations of isolated early-type galaxies; MNRAS 382, 1203–1212 Prochaska, J. X.; Chen, H.-W.; Dessauges-Zavadsky, MNRAS 377, 1772–1784 Piranomonte, S.; Perri, M.; Giommi, P.; Landt, H.; M.; Bloom, J. S.; Probing the Interstellar Medium Régulo, C.; Roca Cortés, T.; Stellar p-modes oscil Padovani, P.; The sedentary survey of extreme near Star-forming Regions with Gamma-Ray Burst lation measurements in solar-like star signals: α high-energy peaked BL Lacs. – III. Results from Afterglow Spectroscopy: Gas, Metals, and Dust; Centauri A as an example; A&A 469, 233–237 optical spectroscopy; A&A 470, 787–809 ApJ 666, 267–280 Reid, M. J.; Menten, K. M.; Trippe, S.; Ott, T.; Genzel, Pirogov, L.; Zinchenko, I.; Caselli, P.; Johansson, L. Puech, M.; Hammer, F.; Lehnert, M. D.; Flores, H.; R.; The Position of Sagittarius A. – III. Motion of E. B.; Chemical differentiation in regions of 3D spectroscopy with VLT/GIRAFFE. – IV. Angular the Stellar Cusp; ApJ 659, 378–388 high-mass star formation. CS, dust, and N2H+ in momentum and dynamical support of intermedi- Reiners, A.; Schmitt, J. H. M. M.; Liefke, C.; Rapid southern sources; A&A 461, 523–535 ate redshift galaxies; A&A 466, 83–92 magnetic flux variability on the flare star CN Le- Pirzkal, N.; Malhotra, S.; Rhoads, J. E.; Xu, C.; Puech, M.; Hammer, F.; Flores, H.; Neichel, B.; Yang, onis; A&A 466, L13–L16 Optical-to-Mid-Infrared Observations of Lyα Gal- Y.; Rodrigues, M.; First detection of a minor Reiners, A.; The narrowest M-dwarf line profiles and axies at z ~ 5 in the Hubble Ultra Deep Field: A merger at z ~ 0.6; A&A 476, L21–L24 the rotation-activity connection at very slow rota- Young and Low-Mass Population; ApJ 667, 49–59 Puzia, T. H.; Mobasher, B.; Goudfrooij, P.; Evidence tion; A&A 467, 259–268 Platais, I.; Melo, C.; Mermilliod, J.-C.; Kozhurina- for the Evolution of Young Early-Type Galaxies in Reiners, A.; Seifahrt, A.; Käufl, H. U.; Siebenmorgen, Platais, V.; Fulbright, J. P.; Méndez, R. A.; Altmann, the GOODS/CDF-S Field; AJ 134, 1337–1347 R.; Smette, A.; Spectral-type dependent rotational M.; Sperauskas, J.; WIYN open cluster study. Raiteri, C. M.; Villata, M.; Capetti, A.; Heidt, J.; braking and strong magnetic flux in three compo- – XXVI. Improved kinematic membership and Arnaboldi, M.; Magazzù, A.; Spectroscopic moni- nents of the late-M multiple system LHS 1070; spectroscopy of IC 2391; A&A 461, 509–522 toring of the BL Lac object AO 0235+164; A&A A&A 471, L5–L8 Pohlen, M.; Zaroubi, S.; Peletier, R. F.; Dettmar, R.-J.; 464, 871–878 Reiners, A.; Homeier, D.; Hauschildt, P. H.; Allard, F.; On the three-dimensional structure of edge-on Rajagopal, J.; Menut, J.-L.; Wallace, D.; Danchi, W. A high resolution spectral atlas of brown dwarfs; disc galaxies; MNRAS 378, 594–616 C.; Chesneau, O.; Lopez, B.; Monnier, J. D.; A&A 473, 245–255 Pompei, E.; Dahlem, M.; Iovino, A.; Optical and radio Ireland, M.; Tuthill, P. G.; Mid-Infrared Interferom- Reiners, A.; Seifahrt, A.; Stassun, K. G.; Melo, C.; survey of southern compact groups of galaxies. etry of Dust around Massive Evolved Stars; ApJ Mathieu, R. D.; Detection of Strong Activity in – I. Pilot study of six groups; A&A 473, 399–409 671, 2017–2027 the Eclipsing Binary Brown Dwarf 2MASS Poncelet, A.; Doucet, C.; Perrin, G.; Sol, H.; Lagage, Ramella, M.; Biviano, A.; Pisani, A.; Varela, J.; J05352184–0546085: A Possible Explanation for P. O.; An original interferometric study of Bettoni, D.; Couch, W. J.; D’Onofrio, M.; Dressler, the Temperature Reversal; ApJ 671, L149–L152 NGC 1068 with VISIR BURST mode images; A&A A.; Fasano, G.; Kjørgaard, P.; Moles, M.; Pignatelli, Reipurth, B.; Aspin, C.; Beck, T.; Brogan, C.; 472, 823–831 E.; Poggianti, B. M.; Substructures in WINGS Connelley, M. S.; Herbig, G. H.; V733 Cep Pontoppidan, K. M.; Dullemond, C. P.; Blake, G. A.; clusters; A&A 470, 39–51 (Persson’s Star): A New FU Orionis Object in Ce- Evans II, N. J.; Geers, V. C.; Harvey, P. M.; Ramírez, I.; Allende Prieto, C.; Lambert, D. L.; pheus; AJ 133, 1000–1011 Spiesman, W.; Modeling Spitzer Observations Oxygen abundances in nearby stars. Clues to the Rejkuba, M.; Dubath, P.; Minniti, D.; Meylan, G.; of VV Ser. – II. An Extended Quantum-heated formation and evolution of the Galactic disk; A&A Bright globular clusters in NGC 5128: the missing Nebula and a Disk Shadow; ApJ 656, 991–1000 465, 271–289 link between young massive clusters and evolved Pont, F.; Moutou, C.; Gillon, M.; Udalski, A.; Bouchy, Randich, S.; Primas, F.; Pasquini, L.; Sestito, P.; massive objects; A&A 469, 147–162 F.; Fernandes, J. M.; Gieren, W.; Mayor, M.; Mazeh, Pallavicini, R.; Tracing mixing in stars: new beryl- Reunanen, J.; Tacconi-Garman, L. E.; Ivanov, V. D.; T.; Minniti, D.; Melo, C.; Naef, D.; Pietrzynski, G.; lium observations of the open clusters NGC 2516, VLT/SINFONI integral field spectroscopy of the Queloz, D.; Ruiz, M. T.; Santos, N. C.; Udry, S.; Hyades, and M67; A&A 469, 163–172 Super-antennae; MNRAS 382, 951–959 The “666” collaboration on OGLE transits. Ratzka, T.; Leinert, C.; Henning, T.; Bouwman, J.; Reyniers, M.; Abia, C.; van Winckel, H.; Lloyd Evans, – I. Accurate radius of the planets OGLE-TR-10b Dullemond, C. P.; Jaffe, W.; High spatial resolution T.; Decin, L.; Eriksson, K.; Pollard, K. R.; AGB nu- and OGLE-TR-56b with VLT deconvolution pho- mid-infrared observations of the low-mass young cleosynthesis in the Large Magellanic Cloud. De- tometry; A&A 465, 1069–1074 star TW Hydrae; A&A 471, 173–185 tailed abundance analysis of the RV Tauri star Pozzi, F.; Vignali, C.; Comastri, A.; Pozzetti, L.; Rauw, G.; Manfroid, J.; Gosset, E.; Nazé, Y.; Sana, MACHO 47.2496.8; A&A 461, 641–650 Mignoli, M.; Gruppioni, C.; Zamorani, G.; Lari, C.; H.; De Becker, M.; Foellmi, C.; Moffat, A. F. J.; Reyniers, M.; van Winckel, H.; First detection of Civano, F.; Brusa, M.; Fiore, F.; Maiolino, R.; La Early-type stars in the core of the young open photospheric depletion in the Large Magellanic Franca, F.; The HELLAS2XMM survey. – X. The cluster Westerlund 2; A&A 463, 981–991 Cloud; A&A 463, L1–L4 bolometric output of luminous obscured quasars: Ravikumar, C. D.; Puech, M.; Flores, H.; Proust, D.; Reyniers, M.; van de Steene, G. C.; van Hoof, P. A. The Spitzer perspective; A&A 468, 603–612 Hammer, F.; Lehnert, M.; Rawat, A.; Amram, P.; M.; van Winckel, H.; IRAS 08281-4850 and Pozzetti, L.; Bolzonella, M.; Lamareille, F.; Zamorani, Balkowski, C.; Burgarella, D.; Cassata, P.; Ce- IRAS 14325-6428: two A-type post-AGB stars G.; Franzetti, P.; Le Fèvre, O.; Iovino, A.; Temporin, sarsky, C.; Cimatti, A.; Combes, F.; Daddi, E.; with s-process enrichment; A&A 471, 247–254 S.; Ilbert, O.; Arnouts, S.; Charlot, S.; Brinchmann, Dannerbauer, H.; di Serego Alighieri, S.; Elbaz, D.; Rhodes, J. D.; Massey, R. J.; Albert, J.; Collins, N.; J.; Zucca, E.; Tresse, L.; Scodeggio, M.; Guzzo, Guiderdoni, B.; Kembhavi, A.; Liang, Y. C.; Ellis, R. S.; Heymans, C.; Gardner, J. P.; Kneib, L.; Bottini, D.; Garilli, B.; Le Brun, V.; Maccagni, D.; Pozzetti, L.; Vergani, D.; Vernet, J.; Wozniak, H.; J.-P.; Koekemoer, A.; Leauthaud, A.; Mellier, Y.; Picat, J. P.; Scaramella, R.; Vettolani, G.; Zheng, X. Z.; New spectroscopic redshifts from Refregier, A.; Taylor, J. E.; Van Waerbeke, L.; The Zanichelli, A.; Adami, C.; Bardelli, S.; Cappi, A.; the CDFS and a test of the cosmological relevance Stability of the Point-Spread Function of the Ad- Ciliegi, P.; Contini, T.; Foucaud, S.; Gavignaud, I.; of the GOODS-South field; A&A 465, 1099–1108 vanced Camera for Surveys on the Hubble Space McCracken, H. J.; Marano, B.; Marinoni, C.; Rawat, A.; Kembhavi, A. K.; Hammer, F.; Flores, H.; Telescope and Implications for Weak Mazure, A.; Meneux, B.; Merighi, R.; Paltani, S.; Barway, S.; Unravelling the morphologies of Gravitational Lensing; ApJS 172, 203–218 Pellò, R.; Pollo, A.; Radovich, M.; Bondi, M.; luminous compact galaxies using the HST/ACS Richard, J.; Kneib, J.-P.; Jullo, E.; Covone, G.; Bongiorno, A.; Cucciati, O.; de La Torre, S.; GOODS survey; A&A 469, 483–501 Limousin, M.; Ellis, R.; Stark, D.; Bundy, K.; Gregorini, L.; Mellier, Y.; Merluzzi, P.; Vergani, D.; Rea, N.; Torres, M. A. P.; Jonker, P. G.; Mignani, R. Czoske, O.; Ebeling, H.; Soucail, G.; A Statistical Walcher, C. J.; The VIMOS VLT Deep Survey. The P.; Zane, S.; Burgay, M.; Kaplan, D. L.; Turolla, R.; Study of Multiply Imaged Systems in the Lensing assembly history of the stellar mass in galaxies: Israel, G. L.; Steeghs, D.; Accurate X-ray position Cluster Abell 68; ApJ 662, 781–796 from the young to the old universe; A&A 474, and multiwavelength observations of the isolated Rizzi, L.; Tully, R. B.; Makarov, D.; Makarova, L.; 443–459 neutron star RBS1774; MNRAS 379, 1484–1490 Dolphin, A. E.; Sakai, S.; Shaya, E. J.; Tip of the Prause, N.; Reimers, D.; Fechner, C.; Janknecht, E.; Recio-Blanco, A.; de Laverny, P.; The extra-mixing Red Giant Branch Distances. – II. Zero-Point The baryon density at z = 0.9–1.9. Tracing the efficiency in very low metallicity RGB stars; A&A Calibration; ApJ 661, 815–829 warm-hot intergalactic medium with broad Lyman 461, L13–L16 Rizzi, L.; Held, E. V.; Saviane, I.; Tully, R. B.; α absorption; A&A 470, 67–72 Gullieuszik, M.; The distance to the Fornax dwarf Prisinzano, L.; Damiani, F.; Micela, G.; Pillitteri, I.; spheroidal galaxy; MNRAS 380, 1255–1260 VLT/Flames observations of the star forming region NGC 6530; A&A 462, 123–138

114 ESO Annual Report 2007 Robin, A. C.; Rich, R. M.; Aussel, H.; Capak, P.; Ryabchikova, T.; Sachkov, M.; Kochukhov, O.; Scarpa, R.; Marconi, G.; Gilmozzi, R.; Carraro, G.; Tasca, L. A. M.; Jahnke, K.; Kakazu, Y.; Kneib, Lyashko, D.; Pulsation tomography of rapidly os- Using globular clusters to test gravity in the weak J.-P.; Koekemoer, A.; Leauthaud, A. C.; Lilly, S.; cillating Ap stars. Resolving the third dimension in acceleration regime: NGC 7099; A&A 462, L9–L12 Mobasher, B.; Scoville, N.; Taniguchi, Y.; peculiar pulsating stellar atmospheres; A&A 473, Schaerer, D.; Hempel, A.; Egami, E.; Pelló, R.; Thompson, D. J.; The Stellar Content of the 907–922 Richard, J.; Le Borgne, J.-F.; Kneib, J.-P.; Wise, COSMOS Field as Derived from Morphological Sacco, G. G.; Randich, S.; Franciosini, E.; Pallavicini, M.; Boone, F.; EROs found behind lensing clus- and SED-based Star/Galaxy Separation; ApJS R.; Palla, F.; Lithium-depleted stars in the young σ ters. – I. Stellar populations and dust properties 172, 545–559 Orionis cluster; A&A 462, L23–L26 of optical dropout EROs and comparison with re- Rocca-Volmerange, B.; de Lapparent, V.; Seymour, Sacuto, S.; Chesneau, O.; Vannier, M.; Cruzalèbes, lated objects; A&A 469, 47–60 N.; Fioc, M.; The 12 μm ISO-ESO-Sculptor and P.; A compact dust shell in the symbiotic system Scharwächter, J.; Eckart, A.; Pfalzner, S.; Saviane, I.; 24 μm Spitzer faint counts reveal a population of HM Sagittae; A&A 465, 469–480 Zuther, J.; The nearby QSO host I Zw 1: the stellar ULIRGs as dusty massive ellipticals. Evolution by Safi-Harb, S.; Ribó, M.; Butt, Y.; Matheson, H.; disk and adjacent objects; A&A 469, 913–923 types and cosmic star formation; A&A 475, Negueruela, I.; Lu, F.; Jia, S.; Chen, Y.; A Multi- Schaye, J.; Carswell, R. F.; Kim, T.-S.; A large popu- 801–812 wavelength Study of 1WGA J1346.5–6255: A New lation of metal-rich, compact, intergalactic CIV ab- Rodighiero, G.; Cimatti, A.; Franceschini, A.; Brusa, γ Cas Analog Unrelated to the Background Super- sorbers – evidence for poor small-scale metal M.; Fritz, J.; Bolzonella, M.; Unveiling the oldest nova Remnant G309.2–00.6; ApJ 659, 407–418 mixing; MNRAS 379, 1169–1194 and most massive galaxies at very high redshift; Salaris, M.; Held, E. V.; Ortolani, S.; Gullieuszik, M.; Schirmer, M.; Erben, T.; Hetterscheidt, M.; Schneider, A&A 470, 21–37 Momany, Y.; Deep near-infrared photometry of the P.; GaBoDS: the Garching-Bonn Deep Survey. Rodríguez-Gil, P.; Schmidtobreick, L.; Gänsicke, B. T.; globular cluster 47 Tucanae. Reconciling theory – IX. A sample of 158 shear-selected mass con- Spectroscopic search for new SW Sextantis stars and observations; A&A 476, 243–253 centration candidates; A&A 462, 875–887 in the 3–4 h orbital period range – I; MNRAS 374, Salinas, R.; Richtler, T.; Romanowsky, A. J.; West, M. Schmidtobreick, L.; Tappert, C.; Horst, H.; Saviane, 1359–1376 J.; Schuberth, Y.; The star pile in Abell 545; A&A I.; Lidman, C.; The emission line galaxy TV Re- Roelofs, G. H. A.; Groot, P. J.; Nelemans, G.; Marsh, 475, 507–512 ticuli. Evidence for an ultraluminous supernova; T. R.; Steeghs, D.; On the orbital periods of Sana, H.; Rauw, G.; Gosset, E.; Constraining the A&A 461, 943–947 the AM CVn stars HP Librae and V803 Centauri; Fundamental Parameters of the O-Type Binary Schödel, R.; Eckart, A.; Mužic´, K.; Meyer, L.; MNRAS 379, 176–182 CPD –41 7733; ApJ 659, 1582–1591 Viehmann, T.; Bower, G. C.; The possibility of de- Roelofs, G. H. A.; Groot, P. J.; Steeghs, D.; Marsh, T. Sanders, D. B.; Salvato, M.; Aussel, H.; Ilbert, O.; tecting Sagittarius A at 8.6 μm from sensitive im- R.; Nelemans, G.; The long-period AM CVn Scoville, N.; Surace, J. A.; Frayer, D. T.; Sheth, K.; aging of the Galactic center; A&A 462, L1–L4 star SDSS J155252.48+320150.9; MNRAS 382, Helou, G.; Brooke, T.; Bhattacharya, B.; Yan, L.; Scholz, A.; Jayawardhana, R.; Wood, K.; Meeus, G.; 1643–1647 Kartaltepe, J. S.; Barnes, J. E.; Blain, A. W.; Stelzer, B.; Walker, C.; O’Sullivan, M.; Evolution Rol, E.; van der Horst, A.; Wiersema, K.; Patel, S. K.; Calzetti, D.; Capak, P.; Carilli, C.; Carollo, C. M.; of Brown Dwarf Disks: A Spitzer Survey in Upper Levan, A.; Nysewander, M.; Kouveliotou, C.; Wi- Comastri, A.; Daddi, E.; Ellis, R. S.; Elvis, M.; Fall, Scorpius; ApJ 660, 1517–1531 jers, R. A. M. J.; Tanvir, N.; Reichart, D.; Fruchter, S. M.; Franceschini, A.; Giavalisco, M.; Hasinger, Schödel, R.; Eckart, A.; Alexander, T.; Merritt, D.; A. S.; Graham, J.; Ovaldsen, J.-E.; G.; Impey, C.; Koekemoer, A.; Le Fèvre, O.; Lilly, Genzel, R.; Sternberg, A.; Meyer, L.; Kul, F.; Jaunsen, A. O.; Jonker, P.; van Ham, W.; Hjorth, S.; Liu, M. C.; McCracken, H. J.; Mobasher, B.; Moultaka, J.; Ott, T.; Straubmeier, C.; The struc- J.; Starling, R. L. C.; O’Brien, P. T.; Fynbo, J.; Renzini, A.; Rich, M.; Schinnerer, E.; Shopbell, P. ture of the nuclear stellar cluster of the Milky Way; Burrows, D. N.; Strom, R.; GRB 051022: Physical L.; Taniguchi, Y.; Thompson, D. J.; Urry, C. M.; A&A 469, 125–146 Parameters and Extinction of a Prototype Dark Williams, J. P.; S-COSMOS: The Spitzer Legacy Schöier, F. L.; Bast, J.; Olofsson, H.; Lindqvist, M.; Burst; ApJ 669, 1098–1106 Survey of the Hubble Space Telescope ACS 2 The abundance of SiS in circumstellar envelopes Román-Zúñiga, C. G.; Lada, C. J.; Muench, A.; deg2 COSMOS Field I: Survey Strategy and First around AGB stars; A&A 473, 871–882 Alves, J. F.; The Infrared Extinction Law at Ex- Analysis; ApJS 172, 86–98 Schröder, A. C.; Mamon, G. A.; Kraan-Korteweg, R. treme Depth in a Dark Cloud Core; ApJ 664, Santander-García, M.; Corradi, R. L. M.; Whitelock, C.; Woudt, P. A.; The highly obscured region 357–362 P. A.; Munari, U.; Mampaso, A.; Marang, F.; Boffi, around PKS 1343–601. – I. Galactic interstellar Ruiz-Velasco, A. E.; Swan, H.; Troja, E.; Malesani, D.; F.; Livio, M.; HST and VLT observations of the extinctions using DENIS galaxy colours; A&A 466, Fynbo, J. P. U.; Starling, R. L. C.; Xu, D.; Aharonian, symbiotic star Hen 2–147. Its nebular dynamics, its 481–499 F.; Akerlof, C.; Andersen, M. I.; Ashley, M. C. B.; Mira variable and its distance; A&A 465, 481–491 Schurch, M. P. E.; Coe, M. J.; McGowan, K. E.; Barthelmy, S. D.; Bersier, D.; Castro Cerón, J. M.; Santos, N. C.; Mayor, M.; Bouchy, F.; Pepe, F.; McBride, V. A.; Buckley, D. A. H.; Galache, J. L.; Castro-Tirado, A. J.; Gehrels, N.; Gög˘üs¸, E.; Queloz, D.; Udry, S.; The HARPS search for Corbet, R. H. D.; Still, M.; Vaisanen, P.; Kniazev, Gorosabel, J.; Guidorzi, C.; Güver, T.; Hjorth, J.; southern extra-solar planets. – XII. A giant planet A.; Nordsieck, K.; Optical follow-up of new Small Horns, D.; Huang, K. Y.; Jakobsson, P.; Jensen, B. orbiting the metal-poor star HD 171028; A&A 474, Magellanic Cloud wing Be/X-ray binaries; MNRAS L.; Kızılog˘lu, Ü.; Kouveliotou, C.; Krimm, H. A.; 647–651 381, 1561–1568 Ledoux, C.; Levan, A. J.; Marsh, T.; McKay, T.; Sargent, M. T.; Carollo, C. M.; Lilly, S. J.; Scarlata, C.; Scoville, N.; Aussel, H.; Brusa, M.; Capak, P.; Carollo, Melandri, A.; Milvang-Jensen, B.; Mundell, C. G.; Feldmann, R.; Kampczyk, P.; Koekemoer, A. M.; C. M.; Elvis, M.; Giavalisco, M.; Guzzo, L.; Hasinger, O’Brien, P. T.; Özel, M.; Phillips, A.; Quimby, R.; Scoville, N.; Kneib, J.-P.; Leauthaud, A.; Massey, G.; Impey, C.; Kneib, J.-P.; LeFevre, O.; Lilly, S. J.; Rowell, G.; Rujopakarn, W.; Rykoff, E. S.; R.; Rhodes, J.; Tasca, L. A. M.; Capak, P.; Mc- Mobasher, B.; Renzini, A.; Rich, R. M.; Sanders, Schaefer, B. E.; Sollerman, J.; Tanvir, N. R.; Cracken, H. J.; Porciani, C.; Renzini, A.; D. B.; Schinnerer, E.; Schminovich, D.; Shopbell, Thöne, C. C.; Urata, Y.; Vestrand, W. T.; Vreeswijk, Taniguchi, Y.; Thompson, D. J.; Sheth, K.; The Ev- P.; Taniguchi, Y.; Tyson, N. D.; The Cosmic Evolu- P. M.; Watson, D.; Wheeler, J. C.; Wijers, R. A. M. olution of the Number Density of Large Disk Gal- tion Survey (COSMOS): Overview; ApJS 172, 1–8 J.; Wren, J.; Yost, S. A.; Yuan, F.; Zhai, M.; Zheng, axies in COSMOS; ApJS 172, 434–455 Scoville, N.; Aussel, H.; Benson, A.; Blain, A.; Calzetti, W. K.; Detection of GRB 060927 at z = 5.47: Impli- Saripalli, L.; Mack, K.-H.; A search for molecular D.; Capak, P.; Ellis, R. S.; El-Zant, A.; Finoguenov, cations for the Use of Gamma-Ray Bursts as gas in restarting radio galaxies; MNRAS 376, A.; Giavalisco, M.; Guzzo, L.; Hasinger, G.; Koda, Probes of the End of the Dark Ages; ApJ 669, 1–9 1385–1392 J.; Le Fèvre, O.; Massey, R.; McCracken, H. J.; Russell, D. M.; Fender, R. P.; Jonker, P. G.; Evidence Saviane, I.; Jerjen, H.; NGC 5011C: An Overlooked Mobasher, B.; Renzini, A.; Rhodes, J.; Salvato, M.; for a jet contribution to the optical/infrared Dwarf Galaxy in the Centaurus A Group; AJ 133, Sanders, D. B.; Sasaki, S. S.; Schinnerer, E.; light of neutron star X-ray binaries; MNRAS 379, 1756–1762 Sheth, K.; Shopbell, P. L.; Taniguchi, Y.; Taylor, J. 1108 –1116 Sbordone, L.; Bonifacio, P.; Buonanno, R.; Marconi, E.; Thompson, D. J.; Large Structures and Galaxy Ryabchikova, T.; Sachkov, M.; Weiss, W. W.; Kallinger, G.; Monaco, L.; Zaggia, S.; The exotic chemical Evolution in COSMOS at z < 1.1; ApJS 172, T.; Kochukhov, O.; Bagnulo, S.; Ilyin, I.; Landstreet, composition of the Sagittarius dwarf spheroidal 150–181 J. D.; Leone, F.; Lo Curto, G.; Lüftinger, T.; Lyashko, galaxy; A&A 465, 815–824 Seabroke, G. M.; Gilmore, G.; Revisiting the relations: D.; Magazzù, A.; Pulsation in the atmosphere of Galactic thin disc age-velocity dispersion relation; the roAp star HD 24712. – I. Spectroscopic obser- MNRAS 380, 1348–1368 vations and radial velocity measurements; A&A Seifahrt, A.; Neuhäuser, R.; Hauschildt, P. H.; Near- 462, 1103–1112 infrared integral-field spectroscopy of the companion to GQ Lupi; A&A 463, 309–313

ESO Annual Report 2007 115 Selvelli, P.; Danziger, J.; Bonifacio, P.; The HeII Fowler Sollerman, J.; Fynbo, J. P. U.; Gorosabel, J.; Halpern, Stratta, G.; D’Avanzo, P.; Piranomonte, S.; Cutini, S.; lines and the O iii and N iii Bowen fluorescence J. P.; Hjorth, J.; Jakobsson, P.; Mirabal, N.; Preger, B.; Perri, M.; Conciatore, M. L.; Covino, S.; lines in the symbiotic nova RR Telescopii; A&A Watson, D.; Xu, D.; Castro-Tirado, A. J.; Féron, C.; Stella, L.; Guetta, D.; Marshall, F. E.; Holland, S. 464, 715–734 Jaunsen, A. O.; Jelínek, M.; Jensen, B. L.; Kann, T.; Stamatikos, M.; Guidorzi, C.; Mangano, V.; An- Sestito, P.; Randich, S.; Bragaglia, A.; Element D. A.; Ovaldsen, J. E.; Pozanenko, A.; Stritzinger, tonelli, L. A.; Burrows, D.; Campana, S.; Capalbi, abundances in the metal-rich open cluster M.; Thöne, C. C.; de Ugarte Postigo, A.; Guziy, S.; M.; Chincarini, G.; Cusumano, G.; D’Elia, V.; NGC 6253; A&A 465, 185–196 Ibrahimov, M.; Järvinen, S. P.; Levan, A.; Evans, P. A.; Fiore, F.; Fugazza, D.; Giommi, P.; Setiawan, J.; Weise, P.; Henning, T.; Launhardt, R.; Rumyantsev, V.; Tanvir, N.; The nature of the X-ray Osborne, J. P.; La Parola, V.; Mineo, T.; Moretti, Müller, A.; Rodmann, J.; Evidence for a Planetary flash of August 24 2005. Photometric evidence for A.; Page, K. L.; Romano, P.; Tagliaferri, G.; A study Companion around a Nearby Young Star; ApJ an on-axis z = 0.83 burst with continuous energy of the prompt and afterglow emission of the short 660, L145–L148 injection and an associated supernova?; A&A 466, GRB 061201; A&A 474, 827–835 Seymour, N.; Rocca-Volmerange, B.; de Lapparent, 839–846 Stritzinger, M.; Sollerman, J.; Late-time emission of V.; A 12 μm ISOCAM survey of the ESO-Sculptor Sollima, A.; Ferraro, F. R.; Bellazzini, M.; The mass type Ia supernovae: optical and near-infrared ob- field. Data reduction and analysis; A&A 475, function of ω Centauri down to 0.15 Msolar; servations of SN 2001el; A&A 470, L1–L4 791–799 MNRAS 381, 1575–1582 Stroeer, A.; Heber, U.; Lisker, T.; Napiwotzki, R.; Shahbaz, T.; Watson, C. A.; The rotational broadening Southworth, J.; Clausen, J. V.; Absolute dimensions Dreizler, S.; Christlieb, N.; Reimers, D.; Hot of V395 Carinae. Implications on the compact ob- of eclipsing binaries. – XXIV. The Be star system subdwarfs from the ESO supernova Ia progenitor ject’s mass; A&A 474, 969–973 DW Carinae, a member of the open cluster survey. – II. Atmospheric parameters of subdwarf Sikkema, G.; Carter, D.; Peletier, R. F.; Balcells, M.; Collinder 228; A&A 461, 1077–1093 O stars; A&A 462, 269–280 Del Burgo, C.; Valentijn, E. A.; HST/ACS observa- Spezzi, L.; Alcalá, J. M.; Frasca, A.; Covino, E.; Sudilovsky, V.; Savaglio, S.; Vreeswijk, P.; Ledoux, tions of shell galaxies: inner shells, shell colours Gandolfi, D.; A WFI survey in the Chamaeleon II C.; Smette, A.; Greiner, J.; Intervening Metal Sys- and dust; A&A 467, 1011–1024 dark cloud; A&A 470, 281–294 tems in GRB and QSO Sight Lines: The Mg ii and Simon, P.; Hetterscheidt, M.; Schirmer, M.; Erben, T.; Srianand, R.; Gupta, N.; Petitjean, P.; Multiwavelength C iv Question; ApJ 669, 741–748 Schneider, P.; Wolf, C.; Meisenheimer, K.; GaBoDS: investigation of a near-solar metallicity sub-DLA Sulentic, J. W.; Bachev, R.; Marziani, P.; Negrete, C. The Garching-Bonn Deep Survey. – VI. Probing at zabs = 1.3647 towards PKS0237–233; MNRAS A.; Dultzin, D.; C iv λ1549 as an Eigenvector 1 Pa- galaxy bias using weak gravitational lensing; A&A 375, 584–594 rameter for Active Galactic Nuclei; ApJ 666, 461, 861–879 Stark, D. P.; Bunker, A. J.; Ellis, R. S.; Eyles, L. P.; 757–777 Simon, J. D.; Bolatto, A. D.; Whitney, B. A.; Robitaille, Lacy, M.; A New Measurement of the Stellar Mass Swinbank, A. M.; Bower, R. G.; Smith, Graham P.; T. P.; Shah, R. Y.; Makovoz, D.; Stanimirovic´, S.; Density at z ~ 5: Implications for the Sources of Wilman, R. J.; Smail, Ian; Ellis, R. S.; Morris, S. L.; Barbá, R. H.; Rubio, M.; The Spitzer Survey of the Cosmic Reionization; ApJ 659, 84–97 Kneib, J.-P.; Resolved spectroscopy of a gravita- Small Magellanic Cloud: Discovery of Embedded Stello, D.; Bruntt, H.; Kjeldsen, H.; Bedding, T. R.; tionally lensed L Lyman-break galaxy at z ~ 5; Protostars in the H ii Region NGC 346; ApJ 669, Arentoft, T.; Gilliland, R. L.; Nuspl, J.; Kim, S.-L.; MNRAS 376, 479–491 327–336 Kang, Y. B.; Koo, J.-R.; Lee, J.-A.; Sterken, C.; Sziládi, K.; Vinkó, J.; Poretti, E.; Szabados, L.; Kun, Sluse, D.; Claeskens, J.-F.; Hutsemékers, D.; Surdej, Lee, C.-U.; Jensen, H. R.; Jacob, A. P.; Szabó, R.; M.; New homogeneous iron abundances of dou- J.; Multi-wavelength study of the gravitational lens Frandsen, S.; Csubry, Z.; Dind, Z. E.; Bouzid, M. ble-mode Cepheids from high-resolution echelle system RXS J1131-1231. – III. Long slit spectros- Y.; Dall, T. H.; Kiss, L. L.; Multisite campaign on spectroscopy; A&A 473, 579–587 copy: micro-lensing probes the QSO structure; the open cluster M67 – II. Evidence for solar-like Tachihara, K.; Rengel, M.; Nakajima, Y.; Yamaguchi, A&A 468, 885–901 oscillations in red giant stars; MNRAS 377, N.; André, P.; Neuhäuser, R.; Onishi, T.; Fukui, Y.; Smiljanic, R.; Porto de Mello, G. F.; da Silva, L.; 584–594 Mizuno, A.; Gas and Dust Condensations and a Abundance analysis of barium and mild barium Stelzer, B.; Scholz, A.; Jayawardhana, R.; Emission Peculiar Class 0 Object in the Lupus 3 Star-Form- stars; A&A 468, 679–693 Line Variability of the Accreting Young Brown ing Cloud; ApJ 659, 1382–1393 Smith, N.; Bally, J.; Walawender, J.; And in the Dwarf 2MASSW J1207334–393254: From Hours Tajer, M.; Polletta, M.; Chiappetti, L.; Maraschi, L.; Darkness Bind Them: Equatorial Rings, B[e] Su- to Years; ApJ 671, 842–852 Trinchieri, G.; Maccagni, D.; Andreon, S.; Garcet, pergiants, and the Waists of Bipolar Nebulae; AJ Stempels, H. C.; Gahm, G. F.; Petrov, P. P.; Periodic O.; Surdej, J.; Pierre, M.; Le Fèvre, O.; Franceschini, 134, 846–859 radial velocity variations in RU Lupi; A&A 461, A.; Lonsdale, C. J.; Surace, J. A.; Shupe, D. L.; Smoker, J. V.; Hunter, I.; Kalberla, P. M. W.; Keenan, 253–259 Fang, F.; Rowan-Robinson, M.; Smith, H. E.; F. P.; Morras, R.; Hanuschik, R.; Thompson, H. M. Sterken, C.; Vogt, N.; Schreiber, M. R.; Uemura, M.; Tresse, L.; Obscured and unobscured AGN popu- A.; Silva, D.; Bajaja, E.; Poppel, W. G. L.; Arnal, M.; Tuvikene, T.; WX Ceti: a closer look at its lations in a hard-X-ray selected sample of the Observations towards early-type stars in the ESO- behaviour in quiescence and outburst; A&A 463, XMDS survey; A&A 467, 73–91 POP Survey – II. Searches for intermediate- and 1053–1060 Takahashi, M. I.; Shioya, Y.; Taniguchi, Y.; Murayama, high-velocity clouds; MNRAS 378, 947–954 Stratta, G.; Basa, S.; Butler, N.; Atteia, J. L.; Gendre, T.; Ajiki, M.; Sasaki, S. S.; Koizumi, O.; Nagao, T.; Smolcˇic´, V.; Schinnerer, E.; Finoguenov, A.; Sakelliou, B.; Pélangeon, A.; Malacrino, F.; Mellier, Y.; Kann, Scoville, N. Z.; Mobasher, B.; Aussel, H.; Capak, I.; Carilli, C. L.; Botzler, C. S.; Brusa, M.; Scoville, D. A.; Klose, S.; Zeh, A.; Masetti, N.; Palazzi, E.; P.; Carilli, C.; Ellis, R. S.; Garilli, B.; Giavalisco, M.; N.; Ajiki, M.; Capak, P.; Guzzo, L.; Hasinger, G.; Gorosabel, J.; Castro-Tirado, A. J.; de Ugarte Guzzo, L.; Hasinger, G.; Impey, C.; Kitzbichler, M. Impey, C.; Jahnke, K.; Kartaltepe, J. S.; Mc- Postigo, A.; Jelinek, M.; Cepa, J.; Castañeda, H.; G.; Koekemoer, A.; Le Fèvre, O.; Lilly, S. J.; Cracken, H. J.; Mobasher, B.; Murayama, T.; Sas- Martínez-Delgado, D.; Boër, M.; Braga, J.; Crew, Maccagni, D.; Renzini, A.; Rich, M.; Sanders, D. aki, S. S.; Shioya, Y.; Taniguchi, Y.; Trump, J. R.; A G.; Donaghy, T. Q.; Dezalay, J.-P.; Doty, J.; B.; Schinnerer, E.; Scodeggio, M.; Shopbell, P.; Wide-Angle Tail Radio Galaxy in the Fenimore, E. E.; Galassi, M.; Graziani, C.; Jernigan, Smolcˇic´, V.; Tribiano, S.; Ideue, Y.; Mihara, S.; The COSMOS Field: Evidence for Cluster Formation; J. G.; Kawai, N.; Lamb, D. Q.; Levine, A.; [Oii] λ3727 Luminosity Function and Star Forma- ApJS 172, 295–313 Manchanda, R. K.; Martel, F.; Matsuoka, M.; tion Rate at z ~ 1.2 in the COSMOS 2 Square De- Snellen, I. A. G.; Covino, E.; K-band transit and Nakagawa, Y.; Olive, J.-F.; Pizzichini, G.; Prigozhin, gree Field and the Subaru Deep Field; ApJS 172, secondary eclipse photometry of exoplanet G.; Ricker, G.; Sakamoto, T.; Shirasaki, Y.; Sugita, 456–467 OGLE-TR-113b; MNRAS 375, 307–312 S.; Suzuki, M.; Takagishi, K.; Tamagawa, T.; Tanaka, M.; Kodama, T.; Kajisawa, M.; Bower, R.; Snijders, L.; Kewley, L. J.; van der Werf, P. P.; Vanderspek, R.; Villasenor, J.; Woosley, S. E.; Demarco, R.; Finoguenov, A.; Lidman, C.; Rosati, Mid-Infrared Diagnostics of Starburst Galaxies: Yamauchi, M.; Yoshida, A.; X-ray flashes or soft P.; A deficit of faint red galaxies in the possible Clumpy, Dense Structures in Star-Forming Re- gamma-ray bursts?. The case of the likely distant large-scale structures around the RDCS gions in the Antennae (NGC 4038/4039); ApJ 669, XRF 040912; A&A 461, 485–492 J1252.9–2927 cluster at z = 1.24; MNRAS 377, 269–288 1206–1214 Sollima, A.; Ferraro, F. R.; Bellazzini, M.; Origlia, L.; Tapken, C.; Appenzeller, I.; Noll, S.; Richling, S.; Straniero, O.; Pancino, E.; Deep FORS1 Observa- Heidt, J.; Meinköhn, E.; Mehlert, D.; Lyα emission tions of the Double Main Sequence of ω Centauri; in high-redshift galaxies; A&A 467, 63–72 ApJ 654, 915–922

116 ESO Annual Report 2007 Tappert, C.; Gänsicke, B. T.; Schmidtobreick, L.; Thöne, C. C.; Greiner, J.; Savaglio, S.; Jehin, E.; Trundle, C.; Dufton, P. L.; Hunter, I.; Evans, C. J.; Aungwerojwit, A.; Mennickent, R. E.; Koester, D.; ISM Studies of GRB 030329 with High-Resolution Lennon, D. J.; Smartt, S. J.; Ryans, R. S. I.; The The pre-cataclysmic variable, LTT 560; A&A 474, Spectroscopy; ApJ 671, 628–636 VLT-FLAMES survey of massive stars: evolution of 205–211 Tillich, A.; Heber, U.; O’Toole, S. J.; Østensen, R.; surface N abundances and effective temperature Tappert, C.; Gänsicke, B. T.; Schmidtobreick, L.; Schuh, S.; The Multi-Site Spectroscopic Tele- scales in the Galaxy and Magellanic Clouds; A&A Mennickent, R. E.; Navarrete, F. P.; K-band spec- scope Campaign. – II. Effective temperature and 471, 625–643 troscopy of pre-cataclysmic variables; A&A 475, gravity variations in the multi-periodic pulsating Tubiana, C.; Duffard, R.; Barrera, L.; Boehnhardt, H.; 575–583 subdwarf B star PG 1605+072; A&A 473, 219–228 Photometric and spectroscopic observations of

Tatulli, E.; Isella, A.; Natta, A.; Testi, L.; Marconi, A.; Tisserand, P.; Le Guillou, L.; Afonso, C.; Albert, J. N.; (132524) 2002 JF56: fly-by target of the New Hori- Malbet, F.; Stee, P.; Petrov, R. G.; Millour, F.; Chelli, Andersen, J.; Ansari, R.; Aubourg, É.; Bareyre, P.; zons mission; A&A 463, 1197–1199 A.; Duvert, G.; Antonelli, P.; Beckmann, U.; Beaulieu, J. P.; Charlot, X.; Coutures, C.; Ferlet, Tumlinson, J.; Prochaska, J. X.; Chen, H.-W.; Bresson, Y.; Dugué, M.; Gennari, S.; Glück, L.; R.; Fouqué, P.; Glicenstein, J. F.; Goldman, B.; Dessauges-Zavadsky, M.; Bloom, J. S.; Missing Kern, P.; Lagarde, S.; Le Coarer, E.; Lisi, F.; Perraut, Gould, A.; Graff, D.; Gros, M.; Haissinski, J.; Ha- Molecular Hydrogen and the Physical Conditions K.; Puget, P.; Rantakyrö, F.; Robbe-Dubois, S.; madache, C.; de Kat, J.; Lasserre, T.; Lesquoy, É.; of GRB Host Galaxies; ApJ 668, 667–673 Roussel, A.; Weigelt, G.; Zins, G.; Accardo, M.; Loup, C.; Magneville, C.; Marquette, J. B.; Mau- Tzanavaris, P.; Murphy, M. T.; Webb, J. K.; Flambaum, Acke, B.; Agabi, K.; Altariba, E.; Arezki, B.; Aristidi, rice, É.; Maury, A.; Milsztajn, A.; Moniez, M.; Pal- V. V.; Curran, S. J.; Probing variations in funda- E.; Baffa, C.; Behrend, J.; Blöcker, T.; Bonhomme, anque-Delabrouille, N.; Perdereau, O.; Rahal, Y. mental constants with radio and optical quasar S.; Busoni, S.; Cassaing, F.; Clausse, J.-M.; Colin, R.; Rich, J.; Spiro, M.; Vidal-Madjar, A.; Vigroux, absorption-line observations; MNRAS 374, J.; Connot, C.; Delboulbé, A.; Domiciano de L.; Zylberajch, S.; The EROS-2 Collaboration; 634–646 Souza, A.; Driebe, T.; Feautrier, P.; Ferruzzi, D.; Limits on the Macho content of the Galactic Halo Udry, S.; Bonfils, X.; Delfosse, X.; Forveille, T.; Mayor, Forveille, T.; Fossat, E.; Foy, R.; Fraix-Burnet, D.; from the EROS-2 Survey of the Magellanic Clouds; M.; Perrier, C.; Bouchy, F.; Lovis, C.; Pepe, F.; Gallardo, A.; Giani, E.; Gil, C.; Glentzlin, A.; Heiden, A&A 469, 387–404 Queloz, D.; Bertaux, J.-L.; The HARPS search for M.; Heininger, M.; Hernandez Utrera, O.; Hofmann, Toft, S.; van Dokkum, P.; Franx, M.; Labbe, I.; Förster southern extra-solar planets. – XI. Super-Earths

K.-H.; Kamm, D.; Kiekebusch, M.; Kraus, S.; Le Schreiber, N. M.; Wuyts, S.; Webb, T.; Rudnick, (5 and 8 M⊕) in a 3-planet system; A&A 469, Contel, D.; Le Contel, J.-M.; Lesourd, T.; Lopez, G.; Zirm, A.; Kriek, M.; van der Werf, P.; Blakeslee, L43–L47 B.; Lopez, M.; Magnard, Y.; Mars, G.; Martinot-La- J. P.; Illingworth, G.; Rix, H.-W.; Papovich, C.; Urquhart, J. S.; Thompson, M. A.; Morgan, L. K.; garde, G.; Mathias, P.; Mège, P.; Monin, J.-L.; Moorwood, A.; Hubble Space Telescope and Pestalozzi, M. R.; White, Glenn J.; Muna, D. N.; A Mouillet, D.; Mourard, D.; Nussbaum, E.; Ohnaka, Spitzer Imaging of Red and Blue Galaxies at tale of two cores: triggered massive star formation K.; Pacheco, J.; Perrier, C.; Rabbia, Y.; Rebattu, z ~ 2.5: A Correlation between Size and Star For- in the bright-rimmed cloud SFO 75; A&A 467, S.; Reynaud, F.; Richichi, A.; Robini, A.; Sacchettini, mation Activity from Compact Quiescent Galaxies 1125 –1137 M.; Schertl, D.; Schöller, M.; Solscheid, W.; to Extended Star-forming Galaxies; ApJ 671, Uttenthaler, S.; Hron, J.; Lebzelter, T.; Busso, M.; Spang, A.; Stefanini, P.; Tallon, M.; Tallon-Bosc, I.; 285–302 Schultheis, M.; Käufl, H. U.; Technetium and the Tasso, D.; Vakili, F.; von der Lühe, O.; Valtier, J.-C.; Tokovinin, A.; Sarazin, M.; Smette, A.; Testing turbu- third dredge up in AGB stars. – II. Bulge stars; Vannier, M.; Ventura, N.; Constraining the wind lence model at metric scales with mid-infrared A&A 463, 251–259 launching region in Herbig Ae stars: AMBER/VLTI VISIR images at the VLT; MNRAS 378, 701–708 Uttenthaler, S.; Lebzelter, T.; Palmerini, S.; Busso, spectroscopy of HD 104237; A&A 464, 55–58 Tozzi, G. P.; Boehnhardt, H.; Kolokolova, L.; Bonev, M.; Aringer, B.; Lederer, M. T.; Low-mass lithium- Tautvaišiene˙, G.; Geisler, D.; Wallerstein, G.; T.; Pompei, E.; Bagnulo, S.; Ageorges, N.; Barrera, rich AGB stars in the Galactic bulge: evidence for Borissova, J.; Bizyaev, D.; Pagel, B. E. J.; L.; Hainaut, O.; Käufl, H. U.; Kerber, F.; Locurto, cool bottom processing?; A&A 471, L41–L45 Charbonnel, C.; Smith, V.; First Stellar Abundances G.; Marco, O.; Pantin, E.; Rauer, H.; Saviane, I.; Valcheva, A. T.; Ivanov, V. D.; Ovcharov, E. P.; in the Dwarf Irregular Galaxy IC 1613; AJ 134, Sterken, C.; Weiler, M.; Dust observations of Nedialkov, P. L.; Carbon stars and C/M ratio in the 2318–2327 Comet 9P/Tempel 1 at the time of the Deep Im- WLM dwarf irregular galaxy; A&A 466, 501–507 Taylor, P. A.; Margot, J.-L.; Vokrouhlický, D.; Scheeres, pact; A&A 476, 979–988 Valenti, E.; Ferraro, F. R.; Origlia, L.; Near-Infrared D. J.; Pravec, P.; Lowry, S. C.; Fitzsimmons, A.; Tresse, L.; Ilbert, O.; Zucca, E.; Zamorani, G.; Properties of 24 Globular Clusters in the Galactic Nolan, M. C.; Ostro, S. J.; Benner, L. A. M.; Bardelli, S.; Arnouts, S.; Paltani, S.; Pozzetti, L.; Bulge; AJ 133, 1287–1301 Giorgini, J. D.; Magri, C.; Spin Rate of Asteroid Bottini, D.; Garilli, B.; Le Brun, V.; Le Fèvre, O.; van Hoof, P. A. M.; Hajduk, M.; Zijlstra, Albert A.; (54509) 2000 PH5 Increasing Due to the YORP Maccagni, D.; Picat, J.-P.; Scaramella, R.; Herwig, F.; Evans, A.; van de Steene, G. C.; Effect; Sci 316, 274– Scodeggio, M.; Vettolani, G.; Zanichelli, A.; Adami, Kimeswenger, S.; Kerber, F.; Eyres, S. P. S.; The Tejos, N.; Lopez, S.; Prochaska, J. X.; Chen, H.-W.; C.; Arnaboldi, M.; Bolzonella, M.; Cappi, A.; onset of photoionization in Sakurai’s Object Dessauges-Zavadsky, M.; On the Incidence of C iv Charlot, S.; Ciliegi, P.; Contini, T.; Foucaud, S.; (V4334 Sagittarii); A&A 471, L9–L12 Absorbers Along the Sight Lines to Gamma-Ray Franzetti, P.; Gavignaud, I.; Guzzo, L.; Iovino, A.; van der Meer, A.; Kaper, L.; van Kerkwijk, M. H.; Bursts; ApJ 671, 622–627 McCracken, H. J.; Marano, B.; Marinoni, C.; Heemskerk, M. H. M.; van den Heuvel, E. P. J.; Testa, V.; Marconi, M.; Musella, I.; Ripepi, V.; Dall’Ora, Mazure, A.; Meneux, B.; Merighi, R.; Pellò, R.; Determination of the mass of the neutron star in M.; Ferraro, F. R.; Mucciarelli, A.; Mateo, M.; Côté, Pollo, A.; Radovich, M.; Bondi, M.; Bongiorno, A.; SMC X-1, LMC X-4, and Cen X-3 with VLT/UVES; P.; Infrared photometry of Cepheids in the LMC Busarello, G.; Cucciati, O.; Lamareille, F.; Mathez, A&A 473, 523–538 clusters NGC 1866 and NGC 2031; A&A 462, G.; Mellier, Y.; Merluzzi, P.; Ripepi, V.; The cosmic Vaz, L. P. R.; Andersen, J.; Claret, A.; Absolute 599–605 star formation rate evolution from z = 5 to z = 0 dimensions of eclipsing binaries. – XXV. U Testor, G.; Lemaire, J. L.; Kristensen, L. E.; Field, D.; from the VIMOS VLT deep survey; A&A 472, Ophiuchi and the evolution and composition of

Diana, S.; VLT/NACO near-infrared imaging and 403–419 5 M0 stars; A&A 469, 285–296 spectroscopy of N159-5 in the LMC H ii complex Trippe, S.; Paumard, T.; Ott, T.; Gillessen, S.; Venemans, B. P.; Röttgering, H. J. A.; Miley, G. K.; N159; A&A 469, 459–469 Eisenhauer, F.; Martins, F.; Genzel, R.; A polarized van Breugel, W. J. M.; de Breuck, C.; Kurk, J. D.; Thatte, N.; Abuter, R.; Tecza, M.; Nielsen, E. L.; infrared flare from Sagittarius A and the signatures Pentericci, L.; Stanford, S. A.; Overzier, R. A.; Clarke, F. J.; Close, L. M.; Very high contrast of orbiting plasma hotspots; MNRAS 375, 764–772 Croft, S.; Ford, H.; Protoclusters associated with integral field spectroscopy of AB Doradus C: Tristram, K. R. W.; Meisenheimer, K.; Jaffe, W.; z > 2 radio galaxies . – I. Characteristics of high 9-mag contrast at 0.2 arcsec without a corona- Schartmann, M.; Rix, H.-W.; Leinert, C.; Morel, S.; redshift protoclusters; A&A 461, 823–845 graph using spectral deconvolution; MNRAS 378, Wittkowski, M.; Röttgering, H.; Perrin, G.; Lopez, Venemans, B. P.; McMahon, R. G.; Warren, S. J.; 1229–1236 B.; Raban, D.; Cotton, W. D.; Graser, U.; Paresce, Gonzalez-Solares, E. A.; Hewett, P. C.; Mortlock, Thompson, H. M. A.; Keenan, F. P.; Dufton, P. L.; F.; Henning, T.; Resolving the complex structure of D. J.; Dye, S.; Sharp, R. G.; The discovery of the Ryans, R. S. I.; Smoker, J. V.; Lambert, D. L.; the dust torus in the active nucleus of the Circinus first luminous z ~ 6 quasar in the UKIDSS Large Zijlstra, A. A.; Iron abundances of B-type post-as- galaxy; A&A 474, 837–850 Area Survey; MNRAS 376, L76–L80 ymptotic giant branch stars in globular clusters: Vergani, D.; Pizzella, A.; Corsini, E. M.; van Driel, W.; Barnard29 in M13 and ROA5701 in ωCen; MNRAS Buson, L. M.; Dettmar, R.-J.; Bertola, F.; 378, 1619–1632 NGC 5719/13: interacting spirals forming a counter-rotating stellar disc; A&A 463, 883–892

ESO Annual Report 2007 117 Verhoelst, T.; van Aarle, E.; Acke, B.; Direct diameter Wang, W.; Liu, X.-W.; Elemental abundances of Wittkowski, M.; Boboltz, D. A.; Ohnaka, K.; Driebe, measurement of a star filling its Roche lobe. The Galactic bulge planetary nebulae from optical re- T.; Scholz, M.; The Mira variable S Orionis: rela- semi-detached binary SS Leporis spatially re- combination lines; MNRAS 381, 669–701 tionships between the photosphere, molecular solved with VINCI/VLTI; A&A 470, L21–L24 Warren, S. J.; Mortlock, D. J.; Leggett, S. K.; Pinfield, layer, dust shell, and SiO maser shell at 4 epochs; Verma, A.; Lehnert, M. D.; Förster S., Natascha M.; D. J.; Homeier, D.; Dye, S.; Jameson, R. F.; Lo- A&A 470, 191–210 Bremer, M. N.; Douglas, L.; Lyman-break galaxies dieu, N.; Lucas, P. W.; Adamson, A. J.; Allard, F.; Wood-Vasey, W. M.; Miknaitis, G.; Stubbs, C. W.; at z ~ 5 – I. First significant stellar mass assembly Barrado Y Navascués, D.; Casali, M.; Chiu, K.; Jha, S.; Riess, A. G.; Garnavich, P. M.; Kirshner, in galaxies that are not simply z ~ 3 LBGs at Hambly, N. C.; Hewett, P. C.; Hirst, P.; Irwin, M. J.; R. P.; Aguilera, C.; Becker, A. C.; Blackman, J. W.; higher redshift; MNRAS 377, 1024–1042 Lawrence, A.; Liu, M. C.; Martín, E. L.; Smart, R. Blondin, S.; Challis, P.; Clocchiatti, A.; Conley, A.; Vernazza, P.; Rossi, A.; Birlan, M.; Fulchignoni, M.; L.; Valdivielso, L.; Venemans, B. P.; A very cool Covarrubias, R.; Davis, T. M.; Filippenko, A. V.; Nedelcu, A.; Dotto, E.; 832 Karin: Absence of ro- brown dwarf in UKIDSS DR1; MNRAS 381, Foley, R. J.; Garg, A.; Hicken, M.; Krisciunas, K.; tational spectral variations; Icar 191, 330–336 1400–1412 Leibundgut, B.; Li, W.; Matheson, T.; Miceli, A.; Villar-Martín, M.; Humphrey, A.; De Breuck, C.; Weigelt, G.; Kraus, S.; Driebe, T.; Petrov, R. G.; Narayan, G.; Pignata, G.; Prieto, J. L.; Rest, A.; Fosbury, R.; Binette, L.; Vernet, J.; Lyα excess in Hofmann, K.-H.; Millour, F.; Chesneau, O.; Schertl, Salvo, M. E.; Schmidt, B. P.; Smith, R. C.; high-redshift radio galaxies: a signature of star D.; Malbet, F.; Hillier, J. D.; Gull, T.; Davidson, K.; Sollerman, J.; Spyromilio, J.; Tonry, J. L.; Suntzeff, formation; MNRAS 375, 1299–1310 Domiciano de Souza, A.; Antonelli, P.; Beckmann, N. B.; Zenteno, A.; Observational Constraints on Villar-Martín, M.; Sánchez, S. F.; Humphrey, A.; U.; Bresson, Y.; Chelli, A.; Dugué, M.; Duvert, G.; the Nature of Dark Energy: First Cosmological Re- Dijkstra, M.; di Serego Alighieri, S.; De Breuck, C.; Gennari, S.; Glück, L.; Kern, P.; Lagarde, S.; Le sults from the ESSENCE Supernova Survey; ApJ González Delgado, R.; VIMOS-VLT spectroscopy Coarer, E.; Lisi, F.; Perraut, K.; Puget, P.; 666, 694–715 of the giant Lyα nebulae associated with three Rantakyrö, F.; Robbe-Dubois, S.; Roussel, A.; Worseck, G.; Fechner, C.; Wisotzki, L.; Dall’Aglio, A.; z ~ 2.5 radio galaxies; MNRAS 378, 416–428 Tatulli, E.; Zins, G.; Accardo, M.; Acke, B.; Agabi, The transverse proximity effect in spectral hard- Villanova, S.; Piotto, G.; King, I. R.; Anderson, J.; K.; Altariba, E.; Arezki, B.; Aristidi, E.; Baffa, C.; ness on the line of sight towards HE 2347–4342; Bedin, L. R.; Gratton, R. G.; Cassisi, S.; Momany, Behrend, J.; Blöcker, T.; Bonhomme, S.; Busoni, A&A 473, 805–818 Y.; Bellini, A.; Cool, A. M.; Recio-Blanco, A.; S.; Cassaing, F.; Clausse, J.-M.; Colin, J.; Connot, Wuyts, S.; Labbé, I.; Franx, M.; Rudnick, G.; van Renzini, A.; The Multiplicity of the Subgiant C.; Delboulbé, A.; Feautrier, P.; Ferruzzi, D.; Dokkum, P. G.; Fazio, G. G.; Förster Schreiber, N. Branch of ω Centauri: Evidence for Prolonged Forveille, T.; Fossat, E.; Foy, R.; Fraix-Burnet, D.; M.; Huang, J.; Moorwood, A. F. M.; Rix, H.-W.; Star Formation; ApJ 663, 296–314 Gallardo, A.; Giani, E.; Gil, C.; Glentzlin, A.; Röttgering, H.; van der Werf, P.; What Do We Vink, J. S.; Constraining GRB progenitor models by Heiden, M.; Heininger, M.; Hernandez Utrera, O.; Learn from IRAC Observations of Galaxies at probing Wolf-Rayet wind geometries in the Large Kamm, D.; Kiekebusch, M.; Le Contel, D.; Le 2 < z < 3.5?; ApJ 655, 51–65 Magellanic Cloud; A&A 469, 707–711 Contel, J.-M.; Lesourd, T.; Lopez, B.; Lopez, M.; Yakut, K.; Aerts, C.; Morel, T.; The early-type close von Hippel, T.; Thompson, S. E.; Discovery of Magnard, Y.; Marconi, A.; Mars, G.; Martinot-La- binary CV Velorum revisited; A&A 467, 647–655 Photospheric Calcium Line-Strength Variations in garde, G.; Mathias, P.; Mège, P.; Monin, J.-L.; Yun, J. L.; Torrelles, J. M.; Santos, N. C.; A “diamond- the DAZd White Dwarf G29-38; ApJ 661, 477–481 Mouillet, D.; Mourard, D.; Nussbaum, E.; Ohnaka, ring” star: the unusual morphology of a young Voss, B.; Koester, D.; Napiwotzki, R.; Christlieb, N.; K.; Pacheco, J.; Perrier, C.; Rabbia, Y.; Rebattu, (multiple?) object; A&A 470, 231–237 Reimers, D.; High-resolution UVES/VLT spectra of S.; Reynaud, F.; Richichi, A.; Robini, A.; Yun, J. L.; López-Sepulcre, A.; Torrelles, J. M.; A new white dwarfs observed for the ESO SN Ia progeni- Sacchettini, M.; Schöller, M.; Solscheid, W.; young stellar cluster embedded in a molecular tor survey. – II. DB and DBA stars; A&A 470, Spang, A.; Stee, P.; Stefanini, P.; Tallon, M.; cloud in the far outer Galaxy; A&A 471, 573–578 1079–1088 Tallon-Bosc, I.; Tasso, D.; Testi, L.; Vakili, F.; von Zamanov, R. K.; Bode, M. F.; Melo, C. H. F.; Bachev, Vreeswijk, P. M.; Ledoux, C.; Smette, A.; Ellison, S. der Lühe, O.; Valtier, J.-C.; Vannier, M.; Ventura, R.; Gomboc, A.; Stateva, I. K.; Porter, J. M.; L.; Jaunsen, A. O.; Andersen, M. I.; Fruchter, A. N.; Weis, K.; Wittkowski, M.; Near-infrared inter- Pritchard, J.; Rotational velocities of the giants in S.; Fynbo, J. P. U.; Hjorth, J.; Kaufer, A.; Møller, P.; ferometry of η Carinae with spectral resolutions of symbiotic stars – II. Are S-type symbiotics syn- Petitjean, P.; Savaglio, S.; Wijers, R. A. M. J.; 1500 and 12 000 using AMBER/VLTI; A&A 464, chronized?; MNRAS 380, 1053–1063 Rapid-response mode VLT/UVES spectroscopy 87–106 Zavagno, A.; Pomarès, M.; Deharveng, L.; Hosokawa, of GRB 060418. Conclusive evidence for UV Weiler, M.; Rauer, H.; Knollenberg, J.; Sterken, C.; T.; Russeil, D.; Caplan, J.; Triggered star formation pumping from the time evolution of Fe ii and Ni ii The gas production of Comet 9P/Tempel 1 around on the borders of the Galactic H ii region RCW excited- and metastable-level populations; A&A the Deep Impact date; Icar 190, 423–431 120; A&A 472, 835–846 468, 83–96 Welty, D. E.; Monitoring the Variable Interstellar Zepf, S. E.; Maccarone, T. J.; Bergond, G.; Kundu, Vucˇkovic´, M.; Aerts, C.; Östensen, R.; Nelemans, G.; Absorption toward HD 219188 with Hubble Space A.; Rhode, K. L.; Salzer, J. J.; [O iii] λ5007 Emis- Hu, H.; Jeffery, C. S.; Dhillon, V. S.; Marsh, T. R.; Telescope STIS; ApJ 668, 1012–1027 sion from the Black Hole X-Ray Binary in an The binary properties of the pulsating subdwarf B Werner, K.; Rauch, T.; Kruk, J. W.; Identification of NGC 4472 Globular Cluster; ApJ 669, L69–L72 eclipsing binary PG 1336–018 (NY Virginis); A&A N e viii lines in H-deficient (pre-) white dwarfs: a Zhang, J. S.; Henkel, C.; Mauersberger, R.; Chin, 471, 605–615 new tool to constrain the temperature of the hot- Y.-N.; Menten, K. M.; Tieftrunk, A. R.; Belloche, A.; Wade, G. A.; Bagnulo, S.; Drouin, D.; Landstreet, J. test stars; A&A 474, 591–597 The interaction of young massive stars with their D.; Monin, D.; A search for strong, ordered mag- Whelan, E. T.; Ray, T. P.; Randich, S.; Bacciotti, F.; environment. A millimeter and submillimeter line netic fields in Herbig Ae/Be stars; MNRAS 376, Jayawardhana, R.; Testi, L.; Natta, A.; Mohanty, study of NGC 6334 FIR II; A&A 465, 887–898 1145 –1161 S.; Discovery of a Bipolar Outflow from Zuther, J.; Iserlohe, C.; Pott, J.-U.; Bertram, T.;

Wallerstein, G.; Sandstrom, K.; Gredel, R.; A 2MASSW J1207334–393254, a 24 MJup Brown Fischer, S.; Voges, W.; Hasinger, G.; Eckart, A.; Preliminary Investigation of the Diffuse Interstellar Dwarf; ApJ 659, L45–L48 Mrk 609: resolving the circumnuclear structure Line at 8621 Å; PASP 119, 1268–1277 Wiersema, K.; Savaglio, S.; Vreeswijk, P. M.; Ellison, with near-infrared integral field spectroscopy; A&A Walter, R.; Lubin´ski, P.; Paltani, S.; Produit, N.; Zurita, S. L.; Ledoux, C.; Yoon, S.-C.; Møller, P.; 466, 451–466 J.; Kuulkers, E.; Beckmann, V.; Gehrels, N.; Sollerman, J.; Fynbo, J. P. U.; Pian, E.; Starling, R. Zych, B. J.; Murphy, M. T.; Pettini, M.; Hewett, P. C.; Blecha, A.; Carrier, F.; Cherix, M.; IGR J17497-2821: L. C.; Wijers, R. A. M. J.; The nature of the dwarf Ryan-Weber, E. V.; Ellison, S. L.; The host galaxies a new X-ray nova; A&A 461, L17–L20 starforming galaxy associated with GRB 060218/ of strong Ca ii quasar absorption systems at Wang, L.; Baade, D.; Patat, F.; Spectropolarimetric SN 2006aj; A&A 464, 529–539 z < 0.5; MNRAS 379, 1409–1422 Diagnostics of Thermonuclear Supernova Explo- Willott, Chris J.; Delorme, P.; Omont, A.; Bergeron, sions; Sci 315, 212 J.; Delfosse, X.; Forveille, T.; Albert, L.; Reylé, C.; Hill, G. J.; Gully-Santiago, M.; Vinten, P.; Crampton, D.; Hutchings, J. B.; Schade, D.; Simard, L.; Sawicki, M.; Beelen, A.; Cox, P.; Four Quasars above Redshift 6 Discovered by the Canada- France High-z Quasar Survey; AJ 134, 2435–2450

118 ESO Annual Report 2007 Additional peer-reviewed publications by ESO Scientists

Ganguly, R.; Brotherton, M. S.; Arav, N.; Heap, S. R.; Snel, R. C.; Mangum, J. G.; Baars, J. W. M.; Study Christensen, L.; Wisotzki, L.; Roth, M. M.; Sánchez, Wisotzki, L.; Aldcroft, T. L.; Alloin, D.; Behar, E.; of the Dynamics of Large Reflector Antennas with S. F.; Kelz, A.; Jahnke, K.; An integral field spec- Canalizo, G.; Crenshaw, D. M.; de Kool, M.; Accelerometers; arXiv 0710, 4254 troscopic survey for high redshift damped Lyman-α Chambers, K.; Cecil, G.; Chatzichristou, E.; Baars, J. W. M.; Lucas, R.; Mangum, J. G.; Lopez- galaxies; A&A 468, 587–601 Everett, J.; Gabel, J.; Gaskell, C. M.; Galliano, E.; Perez, J. A.; Near-Field Radio Holography of Kendall, T. R.; Tamura, M.; Tinney, C. G.; Martín, E. Green, R. F.; Hall, P. B.; Hines, D. C.; Junkkarinen, Large Reflector Antennas; arXiv 0710, 4244 L.; Ishii, M.; Pinfield, D. J.; Lucas, P. W.; Jones, H. V. T.; Kaastra, J. S.; Kaiser, Mary E.; Kazanas, D.; Catala, C.; Alecian, E.; Donati, J.-F.; Wade, G. A.; R. A.; Leggett, S. K.; Dye, S.; Hewett, P. C.; Allard, Konigl, A.; Korista, K. T.; Kriss, G. A.; Laor, A.; Landstreet, J. D.; Böhm, T.; Bouret, J.-C.; Bagnulo, F.; Baraffe, I.; Barrado Y Navascués, D.; Carraro, Leighly, K. M.; Mathur, S.; Ogle, P.; Proga, D.; S.; Folsom, C.; Silvester, J.; The magnetic field of G.; Casewell, S. L.; Chabrier, G.; Chappelle, R. J.; Sabra, B.; Sivron, R.; Snedden, S.; Telfer, R.; the pre-main sequence Herbig Ae star HD 190073; Clarke, F.; Day-Jones, A.; Deacon, N.; Dobbie, P. Vestergaard, M.; Hubble Space Telescope Ultravi- A&A 462, 293–301 D.; Folkes, S.; Hambly, N. C.; Hodgkin, S. T.; Na- olet Spectroscopy of 14 Low-Redshift Quasars; Balestra, I.; Tozzi, P.; Ettori, S.; Rosati, P.; Borgani, kajima, T.; Jameson, R. F.; Lodieu, N.; Magazzù, AJ 133, 479–486 S.; Mainieri, V.; Norman, C.; Viola, M.; Tracing the A.; McCaughrean, M. J.; Pavlenko, Y. V.; Tadashi, Alloin, D.; Kneib, J.-P.; Guilloteau, S.; Bremer, M.; evolution in the iron content of the intra-cluster N.; Zapatero Osorio, M. R.; Two T dwarfs from the Dust and molecular content of the lensed quasar, medium; A&A 462, 429–442 UKIDSS early data release; A&A 466, 1059–1064 MG0751+2716, at z = 3.2; A&A 470, 53–60 Sarajedini, A.; Bedin, L. R.; Chaboyer, B.; Dotter, A.; Comerón, F.; Pasquali, A.; A very massive runaway Lutz, D.; Sturm, E.; Tacconi, L. J.; Valiante, E.; Siegel, M.; Anderson, J.; Aparicio, A.; King, I.; Ma- star from Cygnus OB2; A&A 467, L23–L27 Schweitzer, M.; Netzer, H.; Maiolino, R.; Andreani, jewski, S.; Marín-Franch, A.; Piotto, G.; Reid, I. N.; Schneider, N.; Simon, R.; Bontemps, S.; Comerón, P.; Shemmer, O.; Veilleux, S.; PAH Emission and Rosenberg, A.; The ACS Survey of Galactic Glob- F. ; Motte, F.; A multiwavelength study of the S106 Star Formation in the Host of the z ~ 2.56 Clover- ular Clusters. – I. Overview and Clusters without region. – III. The S106 molecular cloud as part of leaf QSO; ApJ 661, L25–L28 Previous Hubble Space Telescope Photometry; the Cygnus X cloud complex; A&A 474, 873–882 Kawakatu, N.; Andreani, P.; Granato, G. L.; Danese, AJ 133, 1658–1672 Conn, B C.; Lane, R. R.; Lewis, G. F.; Gil-Merino, R.; L.; Exploring Supermassive Black Hole Growth Piotto, G.; Bedin, L. R.; Anderson, J.; King, I. R.; Irwin, Mike J.; Ibata, R. A.; Martin, N. F.; Bellazzini, with ALMA; ApJ 663, 924–932 Cassisi, S.; Milone, A. P.; Villanova, S.; Pietrinferni, M.; Sharp, R.; Tuntsov, A. V.; Ferguson, A. M. N.; Williams, B. F.; Ciardullo, R.; Durrell, P. R.; Feldmeier, A.; Renzini, A.; A Triple Main Sequence in the The AAT/WFI survey of the Monoceros Ring and J. J.; Sigurdsson, S.; Vinciguerra, M.; Jacoby, G. Globular Cluster NGC 2808; ApJ 661, L53–L56 Canis Major dwarf galaxy – I. From l = (193–276)°; H.; von Hippel, T.; Ferguson, H. C.; Tanvir, N. R.; Wirström, E. S.; Bergman, P.; Hjalmarson, Å.; MNRAS 376, 939–959 Arnaboldi, M.; Gerhard, O.; Aguerri, J. A. L.; Nummelin, A.; A search for pre-biotic molecules in Seymour, N.; Stern, D.; De Breuck, C.; Vernet, J.; Freeman, K. C.; Virgo’s Intracluster Globular hot cores; A&A 473, 177–180 Rettura, A.; Dickinson, M.; Dey, A.; Eisenhardt, P.; Clusters as Seen by the Advanced Camera for Olofsson, A. O. H.; Persson, C. M.; Koning, N.; Fosbury, R.; Lacy, M.; McCarthy, P.; Miley, G.; Surveys; ApJ 654, 835–843 Bergman, P.; Bernath, P. F.; Black, J. H.; Frisk, U.; Rocca-Volmerange, B.; Röttgering, H.; Stanford, Williams, B. F.; Ciardullo, R.; Durrell, P. R.; Vinciguerra, Geppert, W.; Hasegawa, T. I.; Hjalmarson, Å.; S. A.; Teplitz, H.; van Breugel, W.; Zirm, A.; The M.; Feldmeier, J. J.; Jacoby, G. H.; Sigurdsson, S.; Kwok, S.; Larsson, B.; Lecacheux, A.; Nummelin, Massive Hosts of Radio Galaxies across Cosmic von Hippel, T.; Ferguson, H. C.; Tanvir, N. R.; A.; Olberg, M.; Sandqvist, A.; Wirström, E. S.; A Time; ApJS 171, 353–375 Arnaboldi, M.; Gerhard, O.; Aguerri, J. A. L.; spectral line survey of Orion KL in the bands Greve, T. R.; Stern, D.; Ivison, R. J.; De Breuck, C.; Freeman, K.; The Metallicity Distribution of 486–492 and 541–577 GHz with the Odin satellite. Kovács, A.; Bertoldi, F.; Wide-field mid-infrared Intracluster Stars in Virgo; ApJ 656, 756–769 – I. The observational data; A&A 476, 791–806 and millimetre imaging of the high-redshift radio Durrell, P. R.; Williams, B. F.; Ciardullo, R.; Feldmeier, Persson, C. M.; Olofsson, A. O. H.; Koning, N.; galaxy, 4C41.17; MNRAS 382, 48–66 J. J.; von Hippel, T.; Sigurdsson, S.; Jacoby, G. H.; Bergman, P.; Bernath, P.; Black, J. H.; Frisk, U.; Garay, G.; Rodríguez, L. F.; de Gregorio-Monsalvo, I.; Ferguson, H. C.; Tanvir, N. R.; Arnaboldi, M.; Geppert, W.; Hasegawa, T. I.; Hjalmarson, Å.; Very Large Array Observations of Candidate High- Gerhard, O.; Aguerri, J. A. L.; Freeman, K.; Kwok, S.; Larsson, B.; Lecacheux, A.; Nummelin, Mass Protostellar Objects at 7 Millimeters; AJ 134, Vinciguerra, M.; The Resolved Stellar Populations A.; Olberg, M.; Sandqvist, A.; Wirström, E. S.; A 906–911 of a Dwarf Spheroidal Galaxy in the Virgo Cluster; spectral line survey of Orion KL in the bands De Silva, G. M.; Freeman, K. C.; Bland-Hawthorn, J.; ApJ 656, 746–755 486–492 and 541–577 GHz with the Odin satellite. Asplund, M.; Bessell, M. S.; Chemically Tagging Gerhard, O.; Arnaboldi, M.; Freeman, K. C.; Okamura, – II. Data analysis; A&A 476, 807–827 the HR 1614 Moving Group; AJ 133, 694–704 S.; Kashikawa, N.; Yasuda, N.; The kinematics of Bono, G.; Caputo, F.; di Criscienzo, M.; RR Lyrae Hao, H.; Stanek, K. Z.; Dobrzycki, A.; Matheson, T.; intracluster planetary nebulae and the on-going stars in Galactic globular clusters. – VI. The pe- Bentz, M. C.; Kuraszkiewicz, J.; Garnavich, P. M.; subcluster merger in the Coma cluster core; A&A riod-amplitude relation; A&A 476, 779–790 Howk, J. C.; Calkins, M. L.; Worthey, G.; Modjaz, 468, 815–822 Piatek, S.; Pryor, C.; Bristow, P.; Olszewski, E. W.; M.; Serven, J.; Strongly Variable z = 1.48 Fe ii Douglas, N. G.; Napolitano, N. R.; Romanowsky, A. Harris, H. C.; Mateo, M.; Minniti, D.; Tinney, C. G.; and Mg ii Absorption in the Spectra of z = 4.05 J.; Coccato, L.; Kuijken, K.; Merrifield, M. R.; Proper Motions of Dwarf Spheroidal Galaxies from GRB 060206; ApJ 659, L99–L102 Arnaboldi, M.; Gerhard, O.; Freeman, K. C.; Hubble Space Telescope Imaging. – V. Final Stanek, K. Z.; Dai, X.; Prieto, J. L.; An, D.; Garnavich, Merrett, H. R.; Noordermeer, E.; Capaccioli, M.; Measurement for Fornax; AJ 133, 818–844 P. M.; Calkins, M. L.; Serven, J.; Worthey, G.; Hao, The PN.S Elliptical Galaxy Survey: Data Reduction, Casali, M.; Adamson, A.; Alves de Oliveira, C.; H.; Dobrzycki, A.; Howk, C.; Matheson, T.; “Anom- Planetary Nebula Catalog, and Basic Dynamics Almaini, O.; Burch, K.; Chuter, T.; Elliot, J.; Folger, alous” Optical Gamma-Ray Burst Afterglows Are for NGC 3379; ApJ 664, 257–276 M.; Foucaud, S.; Hambly, N.; Hastie, M.; Henry, Common: Two z ~ 4 Bursts, GRB 060206 and Murante, G.; Giovalli, M.; Gerhard, O.; Arnaboldi, M.; D.; Hirst, P.; Irwin, M.; Ives, D.; Lawrence, A.; GRB 060210; ApJ 654, L21–L24 Borgani, S.; Dolag, K.; The importance of mergers Laidlaw, K.; Lee, D.; Lewis, J.; Lunney, D.; McLay, Dobrzycki, A.; Nikolajuk, M.; Bechtold, J.; Ebeling, for the origin of intracluster stars in cosmological S.; Montgomery, D.; Pickup, A.; Read, M.; Rees, H.; Czerny, B.; Róz˙an´ska, A.; Absorption spec- simulations of galaxy clusters; MNRAS 377, 2–16 N.; Robson, I.; Sekiguchi, K.; Vick, A.; Warren, S.; trum of the quasar HS1603+3820. – I. Observa- Woodward, B.; The UKIRT wide-field camera; tions and data analysis; A&A 476, 1205–1217 A&A 467, 777–784 Guimarães, R.; Petitjean, P.; Rollinde, E.; de Carvalho, R. R.; Djorgovski, S. G.; Srianand, R.; Aghaee, A.; Castro, S.; Evidence for overdensity around

zem > 4 quasars from the proximity effect; MNRAS 377, 657–666

ESO Annual Report 2007 119 Döllinger, M. P.; Hatzes, A. P.; Pasquini, L.; Guenther, Hubrig, S.; North, P.; Schöller, M.; Evolution of mag- Martinez, P.; Boccaletti, A.; Kasper, M.; Baudoz, P.; E. W.; Hartmann, M.; Girardi, L.; Esposito, M.; netic fields in stars across the upper main se- Cavarroc, C.; Optimization of apodized pupil Lyot Discovery of a planet around the K giant star 4 quence: II. Observed distribution of the magnetic coronagraph for ELTs; A&A 474, 671–678 Ursae Majoris; A&A 472, 649–652 field geometry; AN 328, 475 Kellerer, A.; Tokovinin, A.; Atmospheric coherence Spencer, J. R.; Stern, S. A.; Cheng, A. F.; Weaver, H. Zavala, R. T.; Adelman, S. J.; Hummel, C. A.; Gulliver, times in interferometry: definition and measure- A.; Reuter, D. C.; Retherford, K.; Lunsford, A.; A. F.; Caliskan, H.; Armstrong, J. T.; Hutter, D. J.; ment; A&A 461, 775–781 Moore, J. M.; Abramov, O.; Lopes, R. M. C.; Perry, Johnston, K. J.; Pauls, T. A.; The Mercury-Manga- Rauch, T.; Ziegler, M.; Werner, K.; Kruk, J. W.; J. E.; Kamp, L.; Showalter, M.; Jessup, K. L.; nese Binary Star φ Herculis: Detection and Prop- Oliveira, C. M.; Vande Putte, D.; Mignani, R. P.; Marchis, F.; Schenk, P. M.; Dumas, C.; Io Volcan- erties of the Secondary and Revision of the Kerber, F.; High-resolution FUSE and HST ultravi- ism Seen by New Horizons: A Major Eruption of Elemental Abundances of the Primary; ApJ 655, olet spectroscopy of the white dwarf central star the Tvashtar Volcano; Sci 318, 240 1046–1057 of Sh 2-216; A&A 470, 317–329 Conrad, A. R.; Dumas, C.; Merline, W. J.; Drummond, Mei, S.; Blakeslee, J. P.; Côté, P.; Tonry, J. L.; West, Hajduk, M.; Zijlstra, Albert A.; van Hoof, P. A. M.; J. D.; Campbell, R. D.; Goodrich, R. W.; Le M. J.; Ferrarese, L.; Jordán, A.; Peng, E. W.; An- Lopez, J. A.; Drew, J. E.; Evans, A.; Eyres, S. P. S.; Mignant, D.; Chaffee, F. H.; Fusco, T.; Kwok, S. H.; thony, A.; Merritt, D.; The ACS Virgo Cluster Sur- Gesicki, K.; Greimel, R.; Kerber, F.; Kimeswenger, Knight, R. I.; Direct measurement of the size, vey. – XIII. SBF Distance Catalog and the Three- S.; Richer, M. G.; The enigma of the oldest ‘nova’: shape, and pole of 511 Davida with Keck AO in a dimensional Structure of the Virgo Cluster; ApJ the central star and nebula of CK Vul; MNRAS single night; Icar 191, 616–627 655, 144–162 378, 1298–1308 Schrabback, T.; Erben, T.; Simon, P.; Miralles, J.-M.; Jordán, A.; Blakeslee, J. P.; Côté, P.; Ferrarese, L.; Gerardy, C. L.; Meikle, W. P. S.; Kotak, R.; Höflich, P.; Schneider, P.; Heymans, C.; Eifler, T.; Fosbury, R. Infante, L.; Mei, S.; Merritt, D.; Peng, E. W.; Tonry, Farrah, D.; Filippenko, A. V.; Foley, R. J.; Lundqvist, A. E.; Freudling, W.; Hetterscheidt, M.; Hildebrandt, J. L.; West, M. J.; The ACS Fornax Cluster Survey. P.; Mattila, S.; Pozzo, M.; Sollerman, J.; Van Dyk, H.; Pirzkal, N.; Cosmic shear analysis of archival – I. Introduction to the Survey and Data Reduction S. D.; Wheeler, J. C.; Signatures of Delayed Deto- HST/ACS data. – I. Comparison of early ACS pure Procedures; ApJS 169, 213–224 nation, Asymmetry, and Electron Capture in the parallel data to the HST/GEMS survey; A&A 468, Sivakoff, G. R.; Jordán, A.; Sarazin, C. L.; Blakeslee, Mid-Infrared Spectra of Supernovae 2003hv and 823–847 J. P.; Côté, P.; Ferrarese, L.; Juett, A. M.; Mei, S.; 2005df; ApJ 661, 995–1012 Cescutti, G.; Matteucci, F.; François, P.; Chiappini, Peng, E. W.; The Low-Mass X-Ray Binary and Stanishev, V.; Goobar, A.; Benetti, S.; Kotak, R.; C.; Abundance gradients in the Milky Way for α el- Globular Cluster Connection in Virgo Cluster Pignata, G.; Navasardyan, H.; Mazzali, P.; ements, iron peak elements, barium, lanthanum, Early-Type Galaxies: Optical Properties; ApJ 660, Amanullah, R.; Garavini, G.; Nobili, S.; Qiu, Y.; and europium; A&A 462, 943–951 1246–1263 Elias-Rosa, N.; Ruiz-Lapuente, P.; Mendez, J.; Kamp, I.; Freudling, W.; Chengalur, Jayaram N.; H i Jordán, A.; McLaughlin, D. E.; Côté, P.; Ferrarese, L.; Meikle, P.; Patat, F.; Pastorello, A.; Altavilla, G.; 21 cm Emission as a Tracer of Gas During the Ev- Peng, E. W.; Mei, S.; Villegas, D.; Merritt, D.; Gustafsson, M.; Harutyunyan, A.; Iijima, T.; olution from Protoplanetary to Debris Disks; ApJ Tonry, J. L.; West, M. J.; The ACS Virgo Cluster Jakobsson, P.; Kichizhieva, M. V.; Lundqvist, P.; 660, 469–478 Survey. – XII. The Luminosity Function of Globular Mattila, S.; Melinder, J.; Pavlenko, E. P.; Pavlyuk, Bastian, N.; Ercolano, B.; Gieles, M.; Rosolowsky, E.; Clusters in Early-Type Galaxies; ApJS 171, 101–145 N. N.; Sollerman, J.; Tsvetkov, D. Y.; Turatto, M.; Scheepmaker, R. A.; Gutermuth, R.; Efremov, Y.; Hardcastle, M. J.; Kraft, R. P.; Sivakoff, G. R.; Hillebrandt, W.; SN 2003du: 480 days in the life of Hierarchical star formation in M33: fundamental Goodger, J. L.; Croston, J. H.; Jordán, A.; Evans, a normal type Ia supernova; A&A 469, 645–661 properties of the star-forming regions; MNRAS D. A.; Worrall, D. M.; Birkinshaw, M.; Pastorello, A.; Taubenberger, S.; Elias-Rosa, N.; 379, 1302–1312 Raychaudhury, S.; Brassington, N. J.; Forman, W. Mazzali, P. A.; Pignata, G.; Cappellaro, E.; Smith, L. J.; Bastian, N.; Konstantopoulos, I. S.; R.; Harris, W. E.; Jones, C.; Juett, A. M.; Murray, Garavini, G.; Nobili, S.; Anupama, G. C.; Bayliss, Gallagher III, J. S.; Gieles, M.; de Grijs, R.; Larsen, S. S.; Nulsen, P. E. J.; Sarazin, C. L.; Woodley, K. D. D. R.; Benetti, S.; Bufano, F.; Chakradhari, N. S. S.; O’Connell, R. W.; Westmoquette, M. S.; The A.; New Results on Particle Acceleration in K.; Kotak, R.; Goobar, A.; Navasardyan, H.; Patat, Young Cluster Population of M82 Region B; ApJ the Centaurus A Jet and Counterjet from a Deep F.; Sahu, D. K.; Salvo, M.; Schmidt, B. P.; 667, L145–L149 Chandra Observation; ApJ 670, L81–L84 Stanishev, V.; Turatto, M.; Hillebrandt, W.; ESC Gieles, M.; Lamers, H. J. G. L. M.; Portegies Zwart, Donahue, M.; Jordán, A.; Baum, S. A.; Côté, P.; observations of SN 2005cf – I. Photometric evolu- S. F.; On the Interpretation of the Age Distribution Ferrarese, L.; Goudfrooij, P.; Macchetto, D.; tion of a normal Type Ia supernova; MNRAS 376, of Star Clusters in the Small Magellanic Cloud; Malhotra, S.; O’Dea, C. P.; Pringle, J. E.; Rhoads, 1301–1316 ApJ 668, 268–274 J. E.; Sparks, W. B.; Voit, G. M.; Infrared Emission Peletier, R. F.; Falcón-Barroso, J.; Bacon, R.; Gilmour, R.; Gray, M. E.; Almaini, O.; Best, P.; Wolf, from the Nearby Cool Core Cluster Abell 2597; Cappellari, M.; Davies, R. L.; de Zeeuw, P. T.; Em- C.; Meisenheimer, K.; Papovich, C.; Bell, E.; Envi- ApJ 670, 231–236 sellem, E.; Ganda, K.; Krajnovic´, D.; ronmental dependence of active galactic nuclei Côté, P.; Ferrarese, L.; Jordán, A.; Blakeslee, J. P.; Kuntschner, H.; McDermid, R. M.; Sarzi, M.; van activity in the supercluster A901/2; MNRAS 380, Chen, C.-W.; Infante, L.; Merritt, D.; Mei, S.; Peng, de Ven, G.; The SAURON project – XI. Stellar 1467–1487 E. W.; Tonry, J. L.; West, A. A.; West, M. J.; The populations from absorption-line strength maps Gilmozzi, R.; Selvelli, P.; The secrets of T Pyxidis. ACS Fornax Cluster Survey. – II. The Central of 24 early-type spirals; MNRAS 379, 445–468 – I. UV observations; A&A 461, 593–603 Brightness Profiles of Early-Type Galaxies: A Cappellari, M.; Emsellem, E.; Bacon, R.; Bureau, M.; Richards, A. M. S.; Muxlow, T. W. B.; Beswick, R.; Characteristic Radius on Nuclear Scales and the Davies, R. L.; de Zeeuw, P. T.; Falcón-Barroso, J.; Allen, M. G.; Benson, K.; Dickson, R. C.; Garrett, Transition from Central Luminosity Deficit to Ex- Krajnovic´, D.; Kuntschner, H.; McDermid, R. M.; M. A.; Garrington, S. T.; Gonzalez-Solarez, E.; cess; ApJ 671, 1456–1465 Peletier, R. F.; Sarzi, M.; van den Bosch, R. C. E.; Harrison, P. A.; Holloway, A. J.; Kettenis, M. M.; Kainulainen, J.; Juvela, M.; Alves, J.; Determination van de Ven, G.; The SAURON project – X. The or- Laing, R. A.; Richards, E. A.; Thrall, H.; van of the mass function of extra-galactic GMCs via bital anisotropy of elliptical and lenticular galaxies: Langevelde, H. J.; Walton, N. A.; Wilkinson, P. N.; NIR color maps. Testing the method in a disk-like revisiting the (V/σ, ε) diagram with integral-field Winstanley, N.; Using VO tools to investigate geometry; A&A 468, 581–585 stellar kinematics; MNRAS 379, 418–444 distant radio starbursts hosting obscured AGN in Emsellem, E.; Cappellari, M.; Krajnovic´, D.; van de the HDF(N) region; A&A 472, 805–822 Ven, G.; Bacon, R.; Bureau, M.; Davies, R. L.; de Evstigneeva, E. A.; Gregg, M. D.; Drinkwater, M. J.; Zeeuw, P. T.; Falcón-Barroso, J.; Kuntschner, H.; Hilker, M.; Internal Properties of Ultracompact McDermid, R.; Peletier, R. F.; Sarzi, M.; The Dwarf Galaxies in the Virgo Cluster; AJ 133, SAURON project – IX. A kinematic classification 1722–1740 for early-type galaxies; MNRAS 379, 401–417 Briquet, M.; Hubrig, S.; De Cat, P.; Aerts, C.; North, P.; Schöller, M.; On the co-existence of chemically peculiar Bp stars, slowly pulsating B stars and constant B stars in the same part of the HR diagram; A&A 466, 269–276

120 ESO Annual Report 2007 Ganda, K.; Peletier, R. F.; McDermid, R. M.; Falcón- Finoguenov, A.; Guzzo, L.; Hasinger, G.; Scoville, N. Dhillon, V. S.; Marsh, T. R.; Stevenson, M. J.; Barroso, J.; de Zeeuw, P. T.; Bacon, R.; Cappellari, Z.; Aussel, H.; Böhringer, H.; Brusa, M.; Capak, P.; Atkinson, D. C.; Kerry, P.; Peacocke, P. T.; Vick, A. M.; Davies, R. L.; Emsellem, E.; Krajnovic´, D.; Cappelluti, N.; Comastri, A.; Giodini, S.; Griffiths, J. A.; Beard, S. M.; Ives, D. J.; Lunney, D. W.; Kuntschner, H.; Sarzi, M.; van de Ven, G.; Absorp- R. E.; Impey, C.; Koekemoer, A. M.; Kneib, J.-P.; McLay, S. A.; Tierney, C. J.; Kelly, J.; Littlefair, S. tion-line strengths of 18 late-type spiral galaxies Leauthaud, A.; Le Fèvre, O.; Lilly, S.; Mainieri, V.; P.; Nicholson, R.; Pashley, R.; Harlaftis, E. T.; observed with SAURON; MNRAS 380, 506–540 Massey, R.; McCracken, H. J.; Mobasher, B.; Mu- O’Brien, K.; ULTRACAM: an ultrafast, triple-beam Worrall, D. M.; Birkinshaw, M.; Laing, R. A.; Cotton, rayama, T.; Peacock, J. A.; Sakelliou, I.; CCD camera for high-speed astrophysics; W. D.; Bridle, A. H.; The inner jet of radio galaxy Schinnerer, E.; Silverman, J. D.; Smolcˇic´, V.; MNRAS 378, 825–840 NGC 315 as observed with Chandra and the Very Taniguchi, Y.; Tasca, L.; Taylor, J. E.; Trump, J. R.; Giommi, P.; Massaro, E.; Padovani, P.; Perri, M.; Large Array; MNRAS 380, 2–14 Zamorani, G.; The XMM-Newton Wide-Field Sur- Cavazzuti, E.; Turriziani, S.; Tosti, G.; Davis, T. M.; Mörtsell, E.; Sollerman, J.; Becker, A. vey in the COSMOS Field: Statistical Properties of Colafrancesco, S.; Tagliaferri, G.; Chincarini, G.; C.; Blondin, S.; Challis, P.; Clocchiatti, A.; Clusters of Galaxies; ApJS 172, 182–195 Burrows, D. N.; McMath Chester, M.; Gehrels, N.; Filippenko, A. V.; Foley, R. J.; Garnavich, P. M.; Mieske, S.; Hilker, M.; Infante, L.; Mendes de Oliveira, ROXA J081009.9+384757.0: a 1047 erg s-1 blazar Jha, S.; Krisciunas, K.; Kirshner, R. P.; Leibundgut, C.; The early-type dwarf galaxy population of the with hard X-ray synchrotron peak or a new type of B.; Li, W.; Matheson, T.; Miknaitis, G.; Pignata, G.; Fornax cluster; A&A 463, 503–512 radio loud AGN?; A&A 468, 97–101 Rest, A.; Riess, A. G.; Schmidt, B. P.; Smith, R. C.; Mieske, S.; Baumgardt, H.; On the efficiency of field Parker, L. C.; Hoekstra, H.; Hudson, M. J.; van Spyromilio, J.; Stubbs, C. W.; Suntzeff, N. B.; star capture by star clusters; A&A 475, 851–857 Waerbeke, L.; Mellier, Y.; The Masses and Shapes Tonry, J. L.; Wood-Vasey, W. M.; Zenteno, A.; Combi, J. A.; Bronfman, L.; Mirabel, I. F.; New of Dark Matter Halos from Galaxy-Galaxy Lensing Scrutinizing Exotic Cosmological Models Using evidence on the origin of the microquasar in the CFHT Legacy Survey; ApJ 669, 21–31 ESSENCE Supernova Data Combined with Other GRO J1655–40; A&A 467, 597–602 Murphy, M. T.; Udem, T.; Holzwarth, R.; Sizmann, Cosmological Probes; ApJ 666, 716–725 Dhawan, V.; Mirabel, I. F.; Ribó, M.; Rodrigues, I.; A . ; Pasquini, L.; Araujo-Hauck, C.; Dekker, H.; Beuther, H.; Leurini, S.; Schilke, P.; Wyrowski, F.; Kinematics of Black Hole X-Ray Binary D’Odorico, S.; Fischer, M.; Hänsch, T. W.; Menten, K. M.; Zhang, Q.; Interferometric multi- GRS 1915+105; ApJ 668, 430–434 Manescau, A.; High-precision wavelength cali wavelength (sub)millimeter continuum study of the Mora, M. D.; Larsen, S. S.; Kissler-Patig, M.; Imaging bration of astronomical spectrographs with laser young high-mass protocluster IRAS 05358+3543; of star clusters in unperturbed spiral galaxies with frequency combs; MNRAS 380, 839–847 A&A 466, 1065–1076 the Advanced Camera for Surveys. – I. The low lu- Pasquini, L.; Döllinger, M. P.; Weiss, A.; Girardi, L.; Beuther, H.; Zhang, Q.; Bergin, E. A.; Sridharan, T. minosity galaxy NGC 45; A&A 464, 495–505 Chavero, C.; Hatzes, A. P.; da Silva, L.; Setiawan, K.; Hunter, T. R.; Leurini, S.; Dust and gas emis- Nilsson, K. K.; Orsi, A.; Lacey, C. G.; Baugh, C. M.; J.; Evolved stars suggest an external origin of the sion in the prototypical hot core G29.96–0.02 at Thommes, E.; Narrow-band surveys for very high enhanced metallicity in planet-hosting stars; A&A sub-arcsecond resolution; A&A 468, 1045–1056 redshift Lyman-α emitters; A&A 474, 385–392 473, 979–982 Leurini, S.; Beuther, H.; Schilke, P.; Wyrowski, F.; Ptak, A.; Mobasher, B.; Hornschemeier, A.; Bauer, F.; Simon, J. D.; Gal-Yam, A.; Penprase, B. E.; Li, W.; Zhang, Q.; Menten, K. M.; Multi-line (sub)millime- Norman, C.; X-Ray Luminosity Functions of Nor- Quimby, R. M.; Silverman, J. M.; Prieto, C. A.; tre observations of the high-mass proto cluster mal Galaxies in the Great Observatories Origins Wheeler, J. C.; Filippenko, A. V.; Martinez, I. T.; IRAS 05358+3543; A&A 475, 925–939 Deep Survey; ApJ 667, 826–858 Beeler, D. J.; Patat, F.; Constraints on Circumstel- Melbourne, J.; Dawson, K. S.; Koo, D. C.; Max, C.; Weidner, C.; Kroupa, P.; Nürnberger, D. E. A.; Sterzik, lar Material around the Type Ia Supernova 2007af; Larkin, J. E.; Wright, S. A.; Steinbring, E.; Barczys, M. F.; On the infant weight loss of low- to interme- ApJ 671, L25–L28 M.; Aldering, G.; Barbary, K.; Doi, M.; Fadeyev, V.; diate-mass star clusters; MNRAS 376, 1879–1885 Khare, P.; Kulkarni, V. P.; Péroux, C.; York, D. G.; Goldhaber, G.; Hattori, T.; Ihara, Y.; Kashikawa, Shepherd, D. S.; Povich, M. S.; Whitney, B. A.; Lauroesch, J. T.; Meiring, J. D.; The nature of N.; Konishi, K.; Kowalski, M.; Kuznetsova, N.; Robitaille, T. P.; Nürnberger, D. E. A.; Bronfman, damped Lyman α and sub-damped Lyman α ab- Lidman, C.; Morokuma, T.; Perlmutter, S.; Rubin, L.; Stark, D. P.; Indebetouw, R.; Meade, M. R.; Ba- sorbers; A&A 464, 487–493 D.; Schlegel, D. J.; Spadafora, A. L.; Takanashi, bler, B. L.; Molecular Outflows and a Mid- Meiring, J. D.; Lauroesch, J. T.; Kulkarni, V. P.; N.; Yasuda, N.; Rest-Frame R-band Light Curve Infrared Census of the Massive Star Formation Péroux, C.; Khare, P.; York, D. G.; Crotts, A. P. S.; of a z ~ 1.3 Supernova Obtained with Keck Laser Region Associated with IRAS 18507+0121; ApJ New abundance determinations in z < 1.5 QSO Adaptive Optics; AJ 133, 2709–2715 669, 464–482 absorbers: seven sub-DLAs and one DLA; Alves, J.; Lombardi, M.; Lada, C. J.; The mass Larsson, B.; Liseau, R.; Pagani, L.; Bergman, P.; MNRAS 376, 557–572 function of dense molecular cores and the origin Bernath, P.; Biver, N.; Black, J. H.; Booth, R. S.; Kulkarni, V. P.; Khare, P.; Péroux, C.; York, D. G.; of the IMF; A&A 462, L17–L21 Buat, V.; Crovisier, J.; Curry, C. L.; Dahlgren, M.; Lauroesch, J. T.; Meiring, J. D.; The Role of Sub- Kuhlen, M.; Diemand, J.; Madau, P.; The Shapes, Encrenaz, P. J.; Falgarone, E.; Feldman, P. A.; Damped Lyα Absorbers in the Cosmic Evolution Orientation, and Alignment of Galactic Dark Fich, M.; Florén, H. G.; Fredrixon, M.; Frisk, U.; of Metals; ApJ 661, 88–94 Matter Subhalos; ApJ 671, 1135–1146 Gahm, G. F.; Gerin, M.; Hagström, M.; Harju, J.; Bouché, N.; Lehnert, M. D.; Aguirre, A.; Péroux, C.; Magliocchetti, M.; Brüggen, M.; The interplay Hasegawa, T.; Hjalmarson, Å.; Johansson, L. E. Bergeron, J.; The missing metals problem – III. between radio galaxies and cluster environment; B.; Justtanont, K.; Klotz, A.; Kyrölä, E.; Kwok, S.; How many metals are expelled from galaxies?; MNRAS 379, 260–274 Lecacheux, A.; Liljeström, T.; Llewellyn, E. J.; MNRAS 378, 525–540 Hasinger, G.; Cappelluti, N.; Brunner, H.; Brusa, M.; Lundin, S.; Mégie, G.; Mitchell, G. F.; Murtagh, D.; Comastri, A.; Elvis, M.; Finoguenov, A.; Fiore, F.; Nordh, L. H.; Nyman, L.-Å.; Olberg, M.; Olofsson, Franceschini, A.; Gilli, R.; Griffiths, R. E.; Lehmann, A. O. H.; Olofsson, G.; Olofsson, H.; Persson, G.; I.; Mainieri, V.; Matt, G.; Matute, I.; Miyaji, T.; Mo- Plume, R.; Rickman, H.; Ristorcelli, I.; Rydbeck, lendi, S.; Paltani, S.; Sanders, D. B.; Scoville, N.; G.; Sandqvist, A. A.; Schéele, F. V.; Serra, G.; Tresse, L.; Urry, C. M.; Vettolani, P.; Zamorani, G.; Torchinsky, S.; Tothill, N. F.; Volk, K.; Wiklind, T.; The XMM-Newton Wide-Field Survey in the COS- Wilson, C. D.; Winnberg, A.; Witt, G.; Molecular MOS Field. – I. Survey Description; ApJS 172, oxygen in the ρ Ophiuchi cloud; A&A 466, 29–37 999–1003 Tafoya, D.; Gómez, Y.; Anglada, G.; Loinard, L.; Torrelles, J. M.; Miranda, L. F.; Osorio, M.; Franco- Hernández, R.; Nyman, L.-Å.; Nakashima, J.; Deguchi, S.; Detection of HCO+ Emission toward the Planetary Nebula K3-35; AJ 133, 364–369

ESO Annual Report 2007 121 Popesso, P.; Biviano, A.; Böhringer, H.; Romaniello, Mouhcine, M.; Rejkuba, M.; Ibata, R.; The stellar halo Busso, G.; Cassisi, S.; Piotto, G.; Castellani, M.; M.; RASS-SDSS galaxy cluster survey. – VII. On of the edge-on galaxy NGC 891; MNRAS 381, Romaniello, M.; Catelan, M.; Djorgovski, S. G.; the cluster mass-to-light ratio and the halo occu- 873–880 Recio Blanco, A.; Renzini, A.; Rich, M. R.; pation distribution; A&A 464, 451–464 Scoville, N.; Abraham, R. G.; Aussel, H.; Barnes, J. Sweigart, A. V.; Zoccali, M.; The peculiar horizon- Elbaz, D.; Daddi, E.; Le Borgne, D.; Dickinson, M.; E.; Benson, A.; Blain, A. W.; Calzetti, D.; Comastri, tal branch morphology of the Galactic globular Alexander, D. M.; Chary, R.-R.; Starck, J.-L.; A.; Capak, P.; Carilli, C.; Carlstrom, J. E.; Carollo, clusters NGC 6388 and NGC 6441: new insights Brandt, W. N.; Kitzbichler, M.; MacDonald, E.; C. M.; Colbert, J.; Daddi, E.; Ellis, R. S.; Elvis, M.; from UV observations; A&A 474, 105–119 Nonino, M.; Popesso, P.; Stern, D.; Vanzella, E.; Ewald, S. P.; Fall, M.; Franceschini, A.; Giavalisco, Wang, J. X.; Jiang, P.; Zheng, Z. Y.; Tozzi, P.; Norman, The reversal of the star formation-density relation M.; Green, W.; Griffiths, R. E.; Guzzo, L.; Hasinger, C.; Giacconi, R.; Gilli, R.; Hasinger, G.; Kewley, L.; in the distant universe; A&A 468, 33–48 G.; Impey, C.; Kneib, J.-P.; Koda, J.; Koekemoer, Mainieri, V.; Nonino, M.; Rosati, P.; Streblyanska, Popesso, P.; Biviano, A.; Romaniello, M.; Böhringer, A.; Lefevre, O.; Lilly, S.; Liu, C. T.; McCracken, H. A.; Szokoly, G.; Zirm, A.; Zheng, W.; Most Hard-X- H.; RASS-SDSS galaxy cluster survey. – VI. The J.; Massey, R.; Mellier, Y.; Miyazaki, S.; Mobasher, Ray-Selected Quasars in the Chandra Deep Fields dependence of the cluster SFR on the cluster glo- B.; Mould, J.; Norman, C.; Refregier, A.; Renzini, are Obscured; ApJ 657, 95–101 bal properties; A&A 461, 411–421 A.; Rhodes, J.; Rich, M.; Sanders, D. B.; De Propris, R.; Stanford, S. A.; Eisenhardt, P. R.; Popesso, P.; Biviano, A.; Böhringer, H.; Romaniello, Schiminovich, D.; Schinnerer, E.; Scodeggio, M.; Holden, Brad P.; Rosati, P.; The Rest-Frame K- M.; RASS-SDSS galaxy cluster survey. – V. The X- Sheth, K.; Shopbell, P. L.; Taniguchi, Y.; Tyson, N. Band Luminosity Function of Galaxies in Clusters ray-underluminous Abell clusters; A&A 461, D.; Urry, C. M.; Van Waerbeke, L.; Vettolani, P.; to z = 1.3; AJ 133, 2209–2215 397–410 White, S. D. M.; Yan, L.; COSMOS: Hubble Space Böhringer, H.; Schuecker, P.; Pratt, G. W.; Arnaud, Krips, M.; Eckart, A.; Krichbaum, T. P.; Pott, J.-U.; Telescope Observations; ApJS 172, 38–45 M.; Ponman, T. J.; Croston, J. H.; Borgani, S.; Leon, S.; Neri, R.; García-Burillo, S.; Combes, F.; Taniguchi, Y.; Scoville, N.; Murayama, T.; Sanders, D. Bower, R. G.; Briel, U. G.; Collins, C. A.; Donahue, Boone, F.; Baker, A. J.; Tacconi, L. J.; Schinnerer, B.; Mobasher, B.; Aussel, H.; Capak, P.; Ajiki, M.; M.; Forman, W. R.; Finoguenov, A.; Geller, M. J.; E.; Hunt, L. K.; NUclei of GAlaxies. – V. Radio Miyazaki, S.; Komiyama, Y.; Shioya, Y.; Nagao, T.; Guzzo, L.; Henry, J. P.; Kneissl, R.; Mohr, J. J.; emission in 7 NUGA sources; A&A 464, 553–563 Sasaki, S. S.; Koda, J.; Carilli, C.; Giavalisco, M.; Matsushita, K.; Mullis, C. R.; Ohashi, T.; Pedersen, Randall, S. K.; Green, E. M.; van Grootel, V.; Fontaine, Guzzo, L.; Hasinger, G.; Impey, C.; LeFevre, O.; K.; Pierini, D.; Quintana, H.; Raychaudhury, S.; G.; Charpinet, S.; Lesser, M.; Brassard, P.; Lilly, S.; Renzini, A.; Rich, M.; Schinnerer, E.; Reiprich, T. H.; Romer, A. K.; Rosati, P.; Sabirli, K.; Sugimoto, T.; Chayer, P.; Fay, A.; Wroblewski, P.; Shopbell, P.; Kaifu, N.; Karoji, H.; Arimoto, N.; Temple, R. F.; Viana, P. T. P.; Vikhlinin, A.; Voit, G. Daniel, M.; Story, S.; Fitzgerald, T.; Observations Okamura, S.; Ohta, K.; The Cosmic Evolution M.; Zhang, Y.-Y.; The representative XMM-Newton and asteroseismic analysis of the rapidly pulsating Survey (COSMOS): Subaru Observations of the cluster structure survey (REXCESS) of an X-ray lu- hot B subdwarf PG 0911+456; A&A 476, HST Cosmos Field; ApJS 172, 9–28 minosity selected galaxy cluster sample; A&A 1317–1329 Capak, P.; Aussel, H.; Ajiki, M.; McCracken, H. J.; 469, 363–377 Petrov, R. G.; Malbet, F.; Weigelt, G.; Antonelli, P.; Mobasher, B.; Scoville, N.; Shopbell, P.; Taniguchi, Gouliermis, D. A.; Henning, T.; Brandner, W.; Dolphin, Beckmann, U.; Bresson, Y.; Chelli, A.; Dugué, M.; Y.; Thompson, D.; Tribiano, S.; Sasaki, S.; Blain, A. E.; Rosa, M.; Brandl, B.; Discovery of the Pre- Duvert, G.; Gennari, S.; Glück, L.; Kern, P.; La- A. W.; Brusa, M.; Carilli, C.; Comastri, A.; Carollo, Main-Sequence Population of the Stellar Associa- garde, S.; Le Coarer, E.; Lisi, F.; Millour, F.; C. M.; Cassata, P.; Colbert, J.; Ellis, R. S.; Elvis, tion LH 95 in the Large Magellanic Cloud with Perraut, K.; Puget, P.; Rantakyrö, F.; Robbe- M.; Giavalisco, M.; Green, W.; Guzzo, L.; Hasinger, Hubble Space Telescope Advanced Camera for Dubois, S.; Roussel, A.; Salinari, P.; Tatulli, E.; G.; Ilbert, O.; Impey, C.; Jahnke, K.; Kartaltepe, J.; Surveys Observations; ApJ 665, L27–L30 Zins, G.; Accardo, M.; Acke, B.; Agabi, K.; Al- Kneib, J.-P.; Koda, J.; Koekemoer, A.; Komiyama, Rzepecki, J.; Lombardi, M.; Rosati, P.; Bignamini, A.; tariba, E.; Arezki, B.; Aristidi, E.; Baffa, C.; Be- Y.; Leauthaud, A.; Lefevre, O.; Lilly, S.; Liu, C.; Tozzi, P.; Strong lensing analysis of the cluster hrend, J.; Blöcker, T.; Bonhomme, S.; Busoni, S.; Massey, R.; Miyazaki, S.; Murayama, T.; Nagao, T.; RCS0224-0002 at z = 0.77; A&A 471, 743–752 Cassaing, F.; Clausse, J.-M.; Colin, J.; Connot, C.; Peacock, J. A.; Pickles, A.; Porciani, C.; Renzini, Sana, H.; Rauw, G.; Sung, H.; Gosset, E.; Vreux, Delboulbé, A.; Domiciano de Souza, A.; Driebe, T.; A.; Rhodes, J.; Rich, M.; Salvato, M.; Sanders, D. J.-M.; An XMM-Newton view of the young open Feautrier, P.; Ferruzzi, D.; Forveille, T.; Fossat, E.; B.; Scarlata, C.; Schiminovich, D.; Schinnerer, E.; cluster NGC 6231 – III. Optically faint X-ray Foy, R.; Fraix-Burnet, D.; Gallardo, A.; Giani, E.; Scodeggio, M.; Sheth, K.; Shioya, Y.; Tasca, L. A. sources; MNRAS 377, 945–956 Gil, C.; Glentzlin, A.; Heiden, M.; M.; Taylor, J. E.; Yan, L.; Zamorani, G.; The First De Becker, M.; Rauw, G.; Pittard, J. M.; Sana, H.; Heininger, M.; Hernandez Utrera, O.; Hofmann, Release COSMOS Optical and Near-IR Data and Stevens, I. R.; Romero, G. E.; INTEGRAL-ISGRI K.-H.; Kamm, D.; Kiekebusch, M.; Kraus, S.; Le Catalog; ApJS 172, 99–116 observations of the Cygnus OB2 region. Search- Contel, D.; Le Contel, J.-M.; Lesourd, T.; Lopez, Sasaki, S. S.; Taniguchi, Y.; Scoville, N.; Mobasher, ing for hard X-ray point sources in a region con- B.; Lopez, M.; Magnard, Y.; Marconi, A.; Mars, G.; B.; Aussel, H.; Sanders, D. B.; Koekemoer, A.; taining several non-thermal emitting massive Martinot-Lagarde, G.; Mathias, P.; Mège, P.; Ajiki, M.; Komiyama, Y.; Miyazaki, S.; Kaifu, N.; stars; A&A 472, 905–910 Monin, J.-L.; Mouillet, D.; Mourard, D.; Nussbaum, Karoji, H.; Okamura, S.; Arimoto, N.; Ohta, K.; Leon, S.; Eckart, A.; Laine, S.; Kotilainen, J. K.; E.; Ohnaka, K.; Pacheco, J.; Perrier, C.; Rabbia, Shioya, Y.; Murayama, T.; Nagao, T.; Koda, J.; Schinnerer, E.; Lee, S.-W.; Krips, M.; Reunanen, Y.; Rebattu, S.; Reynaud, F.; Richichi, A.; Robini, Hainline, L.; Renzini, A.; Giavalisco, M.; Le Fèvre, J.; Scharwächter, J.; Nuclear starburst-driven evo- A.; Sacchettini, M.; Schertl, D.; Schöller, M.; O.; Impey, C.; Elvis, M.; Lilly, S.; Rich, M.; lution of the central region in NGC 6764; A&A 473, Solscheid, W.; Spang, A.; Stee, P.; Stefanini, P.; Schinnerer, E.; Sheth, K.; A Potential Galaxy 747–759 Tallon, M.; Tallon-Bosc, I.; Tasso, D.; Testi, L.; Threshing System in the COSMOS Field; ApJS Siebenmorgen, R.; Krügel, E.; Dust in starburst Vakili, F.; von der Lühe, O.; Valtier, J.-C.; Vannier, 172, 511–517 nuclei and ULIRGs. SED models for observers; M.; Ventura, N.; AMBER, the near-infrared A&A 461, 445–453 spectro-interferometric three-telescope VLTI in- Stanke, T.; Williams, J. P.; Molecular CO Outflows in strument; A&A 464, 1–12 the L1641-N Cluster: Kneading a Cloud Core; AJ Dünner, R.; Reisenegger, A.; Meza, A.; Araya, P. A.; 133, 1307–1320 Quintana, H.; Redshift-space limits of bound structures; MNRAS 376, 1577–1587 Soto, M.; Minniti, D.; Rejkuba, M.; Spectroscopic and light curve characterization of bulge microlensing events; A&A 466, 157–164

122 ESO Annual Report 2007 Molinari, E.; Vergani, S. D.; Malesani, D.; Covino, S.; Pastorello, A.; Smartt, S. J.; Mattila, S.; Eldridge, J. Meurer, G. R.; Tsvetanov, Z. I.; Gronwall, C.; Capak, D’Avanzo, P.; Chincarini, G.; Zerbi, F. M.; Antonelli, J.; Young, D.; Itagaki, K.; Yamaoka, H.; P.; Blakeslee, J. P.; Benítez, N.; Ford, H. C.; L. A.; Conconi, P.; Testa, V.; Tosti, G.; Vitali, F.; Navasardyan, H.; Valenti, S.; Patat, F.; Agnoletto, Illingworth, G. D.; Bradley, L. D.; Pirzkal, N.; D’Alessio, F.; Malaspina, G.; Nicastro, L.; Palazzi, I.; Augusteijn, T.; Benetti, S.; Cappellaro, E.; Boles, Walsh, J.; Bouwens, R. J.; Srinivasan, S.; Auto- E.; Guetta, D.; Campana, S.; Goldoni, P.; Masetti, T.; Bonnet-Bidaud, J.-M.; Botticella, M. T.; Bufano, mated Selection and Characterization of Emis- N.; Meurs, E. J. A.; Monfardini, A.; Norci, L.; Pian, F.; Cao, C.; Deng, J.; Dennefeld, M.; Elias-Rosa, sion-Line Sources in Advanced Camera for E.; Piranomonte, S.; Rizzuto, D.; Stefanon, M.; N.; Harutyunyan, A.; Keenan, F. P.; Iijima, T.; Surveys Wide Field Camera Grism Data; AJ 134, Stella, L.; Tagliaferri, G.; Ward, P. A.; Ihle, G.; Lorenzi, V.; Mazzali, P. A.; Meng, X.; Nakano, S.; 77–95 Gonzalez, L.; Pizarro, A.; Sinclaire, P.; Valenzuela, Nielsen, T. B.; Smoker, J. V.; Stanishev, V.; Turatto, Bania, T. M.; Balser, D. S.; Rood, R. T.; Wilson, T. L.; J.; REM observations of GRB 060418 and M.; Xu, D.; Zampieri, L.; A giant outburst two years LaRocque, Jennifer M.; 3He in the Milky Way Inter- GRB 060607A: the onset of the afterglow and before the core-collapse of a massive star; Natur stellar Medium: Ionization Structure; ApJ 664, the initial fireball Lorentz factor determination; 447, 829–832 915–927 A&A 469, L13–L16 Rich, R. M.; Origlia, L.; Valenti, E.; The First Detailed Wold, M.; Brotherton, M. S.; Shang, Z.; The Tanaka, M.; Hoshi, T.; Kodama, T.; Kashikawa, N.; A Abundances for M Giants in the Inner Bulge from dependence of quasar variability on black hole huge filamentary structure at z = 0.55 and star Infrared Spectroscopy; ApJ 665, L119–L122 mass; MNRAS 375, 989–999 formation histories of galaxies at z < 1; MNRAS Robbe-Dubois, S.; Lagarde, S.; Petrov, R. G.; Lisi, F.; de Diego, J. A.; Binette, L.; Ogle, P.; Andersen, A. C.; 379, 1546–1556 Beckmann, U.; Antonelli, P.; Bresson, Y.; Martinot- Haro-Corzo, S.; Wold, M.; Quasar 3C 298: a test- Koyama, Y.; Kodama, T.; Tanaka, M.; Shimasaku, K.; Lagarde, G.; Roussel, A.; Salinari, P.; Vannier, M.; case for meteoritic nanodiamond 3.5 μm emis- Okamura, S.; Dependence of the build-up of the Chelli, A.; Dugué, M.; Duvert, G.; Gennari, S.; sion; A&A 467, L7–L10 colour-magnitude relation on cluster richness at Glück, L.; Kern, P.; Le Coarer, E.; Malbet, F.; Wold, M.; Lacy, M.; Armus, L.; The influence of AGN z ~ 0.8; MNRAS 382, 1719–1728 Millour, F.; Perraut, K.; Puget, P.; Rantakyrö, F.; nuclear parameters on the FRI/FRII dichotomy; Vig, S.; Testi, L.; Walmsley, M.; Molinari, S.; Carey, S.; Tatulli, E.; Weigelt, G.; Zins, G.; Accardo, M.; Acke, A&A 470, 531–538 Noriega-Crespo, A.; IRAS 18511+0146: a proto B.; Agabi, K.; Altariba, E.; Arezki, B.; Aristidi, E.; Meyer, M. J.; Zwaan, M. A.; Webster, R. L.; Brown, Herbig Ae/Be cluster?; A&A 470, 977–989 Baffa, C.; Behrend, J.; Blöcker, T.; Bonhomme, S.; M. J. I.; Staveley-Smith, L.; The Weak Clustering Zirm, A. W.; van der Wel, A.; Franx, M.; Labbé, I.; Busoni, S.; Cassaing, F.; Clausse, J.-M.; Colin, J.; of Gas-rich Galaxies; ApJ 654, 702–713 Trujillo, I.; van Dokkum, P.; Toft, S.; Daddi, E.; Connot, C.; Delage, L.; Delboulbé, A.; Domiciano Oey, M. S.; Meurer, G. R.; Yelda, S.; Furst, E. J.; Rudnick, G.; Rix, H.-W.; Röttgering, H. J. A.; van de Souza, A.; Driebe, T.; Feautrier, P.; Ferruzzi, D.; Caballero-Nieves, S. M.; Hanish, D. J.; Levesque, der Werf, P.; NICMOS Imaging of DRGs in the Forveille, T.; Fossat, E.; Foy, R.; Fraix-Burnet, D.; E. M.; Thilker, D. A.; Walth, G. L.; Bland-Hawthorn, HDF-S: A Relation between Star Formation and Gallardo, A.; Giani, E.; Gil, C.; Glentzlin, A.; J.; Dopita, M. A.; Ferguson, H. C.; Heckman, T. Size at z ~ 2.5; ApJ 656, 66–72 Heiden, M.; Heininger, M.; Hernandez Utrera, O.; M.; Doyle, M. T.; Drinkwater, M. J.; Freeman, K. Quadri, R.; Marchesini, D.; van Dokkum, P.; Gawiser, Hofmann, K.-H.; Kamm, D.; Kiekebusch, M.; C.; Kennicutt, R. C., Jr.; Kilborn, V. A.; Knezek, P. E.; Franx, M.; Lira, P.; Rudnick, G.; Urry, C. M.; Kraus, S.; Le Contel, D.; Le Contel, J.-M.; Le- M.; Koribalski, B.; Meyer, M.; Putman, M. E.; Maza, J.; Kriek, M.; Barrientos, L. F.; Blanc, G. A.; sourd, T.; Lopez, B.; Lopez, M.; Magnard, Y.; Mar- Ryan-Weber, E. V.; Smith, R. C.; Staveley-Smith, Castander, F. J.; Christlein, D.; Coppi, P. S.; Hall, coni, A.; Mars, G.; Mathias, P.; Mège, P.; Monin, L.; Webster, R. L.; Werk, J.; Zwaan, M. A.; The P. B.; Herrera, D.; Infante, L.; Taylor, E. N.; Treister, J.-L.; Mouillet, D.; Mourard, D.; Nussbaum, E.; Survey for Ionization in Neutral Gas Galaxies. E.; Willis, J. P.; The Multiwavelength Survey by Ohnaka, K.; Pacheco, J.; Perrier, C.; Rabbia, Y.; – III. Diffuse, Warm Ionized Medium and Escape Yale-Chile (MUSYC): Deep Near-Infrared Imaging Rebattu, S.; Reynaud, F.; Richichi, A.; Robini, A.; of Ionizing Radiation; ApJ 661, 801–814 and the Selection of Distant Galaxies; AJ 134, Sacchettini, M.; Schertl, D.; Schöller, M.; 1103 –1117 Solscheid, W.; Spang, A.; Stee, P.; Stefanini, P.; Gronwall, C.; Ciardullo, R.; Hickey, T.; Gawiser, E.; Tallon, M.; Tallon-Bosc, I.; Tasso, D.; Testi, L.; Feldmeier, J. J.; van Dokkum, P. G.; Urry, C. M.; Vakili, F.; von der Lühe, O.; Valtier, J.-C.; Ventura, Herrera, D.; Lehmer, B. D.; Infante, L.; Orsi, A.; N.; Optical configuration and analysis of the Marchesini, D.; Blanc, G. A.; Francke, H.; Lira, P.; AMBER/VLTI instrument; A&A 464, 13–27 Treister, E.; Lyα Emission-Line Galaxies at z = 3.1 Tatulli, E.; Millour, F.; Chelli, A.; Duvert, G.; Acke, B.; in the Extended Chandra Deep Field-South; ApJ Hernandez Utrera, O.; Hofmann, K.-H.; Kraus, S.; 667, 79–91 Malbet, F.; Mège, P.; Petrov, R. G.; Vannier, M.; Gawiser, E.; Francke, H.; Lai, K.; Schawinski, K.; Zins, G.; Antonelli, P.; Beckmann, U.; Bresson, Y.; Gronwall, C.; Ciardullo, R.; Quadri, R.; Orsi, A.; Dugué, M.; Gennari, S.; Glück, L.; Kern, P.; La- Barrientos, L. F.; Blanc, G. A.; Fazio, G.; garde, S.; Le Coarer, E.; Lisi, F.; Perraut, K.; Feldmeier, J. J.; Huang, J.-s.; Infante, L.; Lira, P.; Puget, P.; Rantakyrö, F.; Robbe-Dubois, S.; Padilla, N.; Taylor, E. N.; Treister, E.; Urry, C. M.; Roussel, A.; Weigelt, G.; Accardo, M.; Agabi, K.; van Dokkum, P. G.; Virani, S. N.; Lyα-Emitting Altariba, E.; Arezki, B.; Aristidi, E.; Baffa, C.; Galaxies at z = 3.1: L Progenitors Experiencing Behrend, J.; Blöcker, T.; Bonhomme, S.; Busoni, Rapid Star Formation; ApJ 671, 278–284 S.; Cassaing, F.; Clausse, J.-M.; Colin, J.; Connot, C.; Delboulbé, A.; Domiciano de Souza, A.; Driebe, T.; Feautrier, P.; Ferruzzi, D.; Forveille, T.; Fossat, E.; Foy, R.; Fraix-Burnet, D.; Gallardo, A.; Giani, E.; Gil, C.; Glentzlin, A.; Heiden, M.; Heininger, M.; Kamm, D.; Kiekebusch, M.; Le Contel, D.; Le Contel, J.-M.; Lesourd, T.; Lopez, B.; Lopez, M.; Magnard, Y.; Marconi, A.; Mars, G.; Martinot-Lagarde, G.; Mathias, P.; Monin, J.-L.; Mouillet, D.; Mourard, D.; Nussbaum, E.; Ohnaka, K.; Pacheco, J.; Perrier, C.; Rabbia, Y.; Rebattu, S.; Reynaud, F.; Richichi, A.; Robini, A.; Sacchettini, M.; Schertl, D.; Schöller, M.; Solscheid, W.; Spang, A.; Stee, P.; Stefanini, P.; Tallon, M.; Tallon-Bosc, I.; Tasso, D.; Testi, L.; Vakili, F.; von der Lühe, O.; Valtier, J.-C.; Ventura, N.; Interfer ometric data reduction with AMBER/VLTI. Princi- ple, estimators, and illustration; A&A 464, 29–42

ESO Annual Report 2007 123 ESO Europe Guest House Front cover: The extended tail of Comet McNaught Rey Gustavo Adolfo 4634 was captured at Paranal by Hans Hermann Heyer on the evening of 18 January 2007. In the foreground, Headquarters Las Condes one can distinguish one of the VLT Unit Telescope Karl-Schwarzschild-Straße 2 Santiago de Chile and two Auxiliary Telescopes. 85748 Garching bei München Chile Germany Phone +5622084254 Back cover: A 30-min VLT/NACO K-band exposure Phone +49 89 320 06-0 Fax +5622289333 has been combined with archive HST/ACS B- and Fax +49893202362 I-band images to produce a three-colour image of www.eso.org Antofagasta Office the ‘Bird’ interacting galaxy system. The NACO im- Avenida Balmaceda 2536 age has allowed Finnish astronomer Petri Väisänen and his colleagues to identify, in addition to the two Office 504 previously known galaxies, a third, clearly separate ESO Chile Edificio ‘Don Guillermo’ component, an irregular, yet fairly massive galaxy Antofagasta that seems to form stars at a frantic rate. Santiago Office Chile Alonso de Córdova 3107 Phone +56 55 26 00 32 Vitacura Fax +56 55 26 00 81 Casilla 19001 Santiago de Chile 19 Chile ESO is a partner in the international Phone +56 2463 3100 ALMA project Fax +56 2463 3101 ALMA Office Santiago La Silla Paranal Observatory El Golf 40, Piso 18 La Silla Site Las Condes IV Región Santiago de Chile Chile Chile Phone +56 2 464 4100 Phone +56 24676100 Fax +56 2 464 4101 Fax +56 24676101

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