KAPTEYN ASTRONOMICAL INSTITUTE 2003

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KAPTEYN ASTRONOMICAL INSTITUTE

University of Groningen

ANNUAL REPORT

2003

Groningen, May 2004

Cover: Multi-wavelength image of the nearby starburst galaxy NGC 253. The deep optical image is made by David Malin, the blue shows the bright optical disk as seen in the Digitized Sky Survey, the red is soft X-ray emission from ROSAT, and the green contours are neutral hydrogen from the Compact Array. (Boomsma, Oosterloo, Fraternali, Van der Hulst and Sancisi). Neutral hydrogen is now detected up to more than 10 kpc from the plane of the galaxy. This gas has probably been dragged up by the superwind produced by the central starburst.

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CONTENTS 1. FOREWORD............................................................................................ 1 2. EDUCATION............................................................................................ 7 3. RESEARCH ............................................................................................11

3.1 History of astronomy...............................................................................11 3.2 Stars .......................................................................................................11 3.3 Circumstellar Matter, Interstellar Medium, and Star Formation...............12 3.4 Structure and Dynamics of Galaxies.......................................................16 3.5 Quasars and Active Galaxies .................................................................32 3.6 Clusters, High-Redshift Galaxies and Large Scale Structure .................36 3.7 Computing at the Kapteyn Astronomical Institute ...................................43 3.8 Instrumentation.......................................................................................47

APPENDIX I : PUBLICATIONS 2003 ...............................................................55 I.1 Papers in scientific journals, books..........................................................55 I.2 Conference papers ..................................................................................62 I.3 Dissertations............................................................................................71 I.4 Reports, popular articles..........................................................................71

APPENDIX II : Participation in scientific meetings............................................73 APPENDIX III : Visits to institutes abroad.........................................................83

III.1 Work visits .............................................................................................83 III.2 Observing trips.......................................................................................85

APPENDIX IV : Colloquia, popular lectures......................................................87 IV.1 Colloquia given outside Groningen........................................................87 IV.2 Popular lectures ....................................................................................89

APPENDIX V : Colloquia in Groningen.............................................................91 APPENDIX VI : Visiting scientists in Groningen ...............................................97 APPENDIX VII Memberships, etc.....................................................................99 APPENDIX VIII : Personnel (Dec. 31, 2003) ..................................................105 APPENDIX IX : Organisation of the Kapteyn Astronomical Institute...............107 APPENDIX X : Telephone numbers and electronic mail addresses ...............109 APPENDIX XI : Address .................................................................................113

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1. FOREWORD

General

This annual report follows the usual format. The staff of the Kapteyn Astronomical Institute is responsible for the educational program in astronomy at Groningen University and for the astronomical research, including instrumentation development. The Institute has a close collaboration with the Groningen laboratory of the Netherlands Foundation for Space Research (SRON). Also, it is part of the Netherlands Research School for Astronomy (NOVA), which has been awarded extra funding in the “bonus-incentives scheme” (known as the “dieptestrategie”) for top research schools in the Netherlands. Ken Freeman was appointed the Blaauw visiting professor for 2003. Due to personal circumstances having to do with the fire in Canberra that also destroyed a large part of the Mount Stromlo Observatory, he was not able to spent an extended period at the Institute. He will visit again in the course of 2004. Ken did give the Blaauw lecture on "Globular Clusters: Cannonballs of the Cosmos" on November 19, 2003. On May 1 the permanent staff of the Institute held a retreat in Kloosterburen, discussing for a full day aspects of the future of the Institute. In this particular case the discussions focussed on a changes in the educational system at the universities. Education

In 2003 the new bachelor/master curriculum in astronomy entered its second year. This five-year curriculum, with a three-year bachelor and a two-year master program follows to a large extent the five-year curriculum which started in 1999. The new curriculum is slowly stabilising, though at the horizon ideas develop to introduce a major/minor system within the framework of a general bachelor degree in natural science and technology. Development of astronomy major and minor programs is slowly beginning. Our new staff member Reynier Peletier has taken over the effort to design a curriculum for students interested in instrumentation. This is being done in collaboration with SRON and ASTRON and the applied physics group of Groningen University. The program is designed to be attractive to both (applied) physics and astronomy students. This master “stream” will probably be named “Advanced Instrumentation and Space Research Technology”. In 2003 nine new students in astronomy arrived. The total number of students at the end of 2003 was 47. Six students received a masters degree. The staff of the Kapteyn Institute taught 15 courses.

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NOVA

The Netherlands Research School for Astronomy (NOVA), has in 1998 been awarded extra funding in the "bonus-incentives scheme" (in Dutch "dieptestrategie") for top research schools in the Netherlands. Part of this program involves instrumentation developments; of these the major contributions to the OmegaCam wide-field Camera for the VLT Survey Telescope (VST) on Paranal, Chile and receiver development for the Atacame Large Millimeter Array (ALMA), also to be erected in Chile, are for the main part carried out at the Kapteyn Astronomical Institute and the Groningen laboratory of the Netherlands Foundation for Space Research (SRON). Progress during 2003 has been significant and is described in the report. Important to note is that the ALMA consortium won a contract for 4 MEuro from the European Southern Observatory (ESO) to produce 8 prototype receivers for Band 9. Possibly this may eventually lead to a contract for the full set of 64 receivers plus spares. The other part of the NOVA program concerns positions for Ph.D. students and postdocs, overlap appointments in the permanent staff a few years before a retirement and colloquia (see below). Research schools that involve more than one university has one of these as administrative principal partner ("penvoerder" or "pen-holder"), which acts on behalf of all the participating universities. At the founding of NOVA in 1992 it was decided that this would rotate every recognition period of five years between the participating universities, first Leiden and then Amsterdam. Since September 2002 this "pen-holdership" resides in Groningen for five years. In 2003 the important point of the extension of the funds of the bonus incentives scheme funds (2005–2009) was on the agenda. Although the program was approved for a full 10 years, funding had only been allocated up to mid-2005, the rest depending on a mid-term evaluation. For this a detailed "Self-evaluation of Phase 1 and Plans for Phase 2" had to be prepared. The plans for Phase 2 were based on the Strategic Plan "Astronomy in the Nether-lands; strategy for 2001–2010", that was drawn up by the astronomical commu-nity in 2001. The NOVA Instrument Steering Committee (ISC) made a final selection of proposals that had been solicited for instruments to be funded out of Phase 2. On this basis and after further discussions within the NOVA Board and senior astronomers the final document was produced. Before submitting to Netherlands Foundation for Research in the Netherlands (NWO) this document was put before the International Advisory Board (IAB). This committee is chaired by John Bahcall (Princeton). The membership can be found in appendix IX. The IAB submitted a very positive report on the self-evaluation and fully endorsed the program for the second phase. NWO asked a committee under Reinder van Duijnen (former chairman of NWO) to advise on the NOVA document and those of the other five top research schools. The Board of NOW advised the Minister on the basis of this and around the turn of the year the Minister decided to continue all six schools. Although a request was put in for a correction for inflation and for a ramp-down after the end of the period, and although both had been taken over by the NWO Board, the Minister did not provide additional funds over and above what was foreseen at the start of the scheme. In 2004 the final plans for Phase 2 will have to be defined and adapted

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to the funding provided. Also we have to look seriously and urgently in how to continue after the end of Phase 2. During 2003 the role of national coordinator of NOVA Network I (Formation and evolution of galaxies: from high redshift to the present) passed from Koen Kuijken (who in the mean time had moved to Leiden) to Thijs van der Hulst. Research

The main part of this Annual Report concerns a description of the research carried out at the Kapteyn Astronomical Institute. As can be seen from the appendices the work at the Institute resulted in 2004 in (co-)authorship of 86 published papers in refereed journals, 72 contributions to printed conference proceedings and 6 Ph.D. theses. In this year staff members gave 38 invited reviews and contributions at international meetings and 42 colloquia at other institutes. The number of foreign researchers visiting Groningen was 59. The last few years I presented a table with numbers of published refereed papers according to the areas of astronomy and the observing facilities used. This is done again for 2003 in the following table. Again there is a wide range in both categories. Area Papers Facility Papers General 4 Radio 27 Solar System - (Sub)millimeter/farIR 4 Star Formation/ISM/CSM 29 Optical/near IR 22 Galaxies 21 Space 13 Active Galactic Nuclei 15 Theory/interpretation 16 Large Scale Structure/ Cosmology

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Lensing 7 NOVA supports so-called NOVA colloquium speakers. These are senior scientists from abroad who are invited to visit the Netherlands and give colloquia at some or all of the NOVA participating institutes. In 2003 these were George Helou (Caltech), Tom Abel (Pen State), John Lattanzio (Monash), Craig Sarazin (Virginia), Ortwin Gerhard (Basle), Giuseppe Bono (Rome), Dave Sanders (Hawaii), David Spergel (Princeton) and Andy Fabian (Cambridge). Staff

Two new staff members arrived during 2003, namely Amina Helmi and Reynier Peletier. They are appointed on NOVA financed "overlap" positions, where future vacancies due to retirement can be filled a number of years earlier. Reynier's appointment is on a position as "instrumentation oriented" astro-nomer, which means that he will spend part of his time being involved with instrumentation projects in optical or near-infrared astronomy. During 2003 the Institute staff selected three more appointments on vacancies in the permanent staff and these offers were accepted by the candidates con-cerned. These were Leon Koopmans, Saleem Zaroubi and Marc Verheijen. The appointments were effected early in 2004.

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New appointments on the staff are done in the new so-called "tenure track" system of the Faculty of Mathematics and Natural Sciences (see www.fwn.rug.nl/pobc/careersciences.pdf and .../annexuk.pdf). Such appoint-ments ensure that promising young staff have a clear career path with well-defined evaluations that lead up in case of excellent performance to a full professorship after a period of about 10 or 11 years (assuming that they come in after one of two postdoc periods after their Ph.D.). After 6 years they already will get an "adjunct professorship" for a period of 5 years that will allow them to formally act as promotor at Ph.D. ceremonies. At the end of these 5 years they will be evaluated and if successfull promoted to full professor. Persons that come in a bit more senior into the system start at a somewhat more advanced level. We now have eight staff members that were appointed in the last few years in this system: Eline Tolstoy, Scott Trager, Marco Spaans, Amina Helmi, Reynier Peletier, Leon Koopmans, Saleem Zaroubi and Marc Verheijen. During 2003 staff that is already present could opt for being evaluated and channeled into the system if appropriate. Peter Barthel, Xander Tielens (who was appointed on a special chair) and Rien van de Weijgaert participated successfully in that exercise. Early 2004 Peter and Xander were appointed as full professor and Rien as adjunct professor. At the same time Xander, who was partly employed by SRON, came for 100% on the pay-roll of the University. The Foundation for Research in Astronomy (ASTRON) proposed to sponsor a special professorship in instrumentation in astronomy. This was accepted by the Faculty and the University's Governing Board; the appointment of Jan Willem Pel on this professorship took place during 2004. The Institute also has a number of unpayed appointments. During 2003 Wolfgang Wild and Frank Helmich were appointed on this at the level of respectively UHD (roughly associate professor) and UD (assistant professor). Both work for SRON. Such appointments were extended for Harvey Butcher (ASTRON, full professor), Peter Roelfsema (SRON; UD) and Russ Taylor (SRON; UD). The Faculty also provided a grant in order to support visits over the summer months for Jacqueline van Gorkom over the next 10 years. Jacqueline, who is affiliated with Columbia University in New York, already spent about half a year at the Institute as part of a sabbatical leave. Bernard J.T. Jones was appointed senior visiting scientist on an unpaid position; he will make short visits a few times per year. With the new appointments comes an end to an understaffing of the Institute for a significant period. The distribution of ages of the scientific staff has become very even now. At the end of 2003 the distribution was as follows (decimals correspond to part time appointments): Ages 30-34 35-39 40-44 45-49 50-54 55-59 60-64 Staff 4 2 3 1 3 2.3 2.3 Amina Helmi successfully proposed for a so-called VIDI grant from NWO. This prestigious grant is given to excellent young researchers to support their research for a number of years. As a final part of the restructuring of the scientific staff appointments and the tenure-track system, the Faculty decided to create three special named professorships to appoint three professors from

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within the Faculty. These were selected as having "exceptional scientific capabilities and accomplishments". The undersigned was selected as one of these and was appointed as Jacobus C. Kapteyn professor in astronomy in December 2003. Along with this appointment comes an annual grant of 50 kEuro to support research. In the area of postdocs, one left in 2003 (Annette Ferguson), while also four new appointments were made (Philip Heraudeau, Nicola Napolitano, Isabel Perez Martin and Neil Nagar). Neil’s appointment was on a VENI grant from NWO. Six graduate students defended their theses and obtained their Ph.D. in 2003: Henrik Spoon, Mercedes Filho, Stephanie Cazaux, Cesar Gonzalez Garcia, Hans Klöckner and Michiel Kregel). Electronic versions (in PDF format) of these theses are available via the Web-site of the Institute. Seven new Ph.D. students started (or continued after one or more initial years elsewhere) in Groningen during the year: Mirela Obric, Giuseppina Battaglia, Kambiz Fathi, Dieter Poelman, Gert Sikkema, Katia Ganda and Benne Holwerda. The total number of Ph.D. students at the end of 2003 was 20. They are funded through various channels: 2 on the regular Institute budget, 9 on other University appointments, 3 Ubbo Emmius grants, 1 NOVA, 4 NWO and 1 on external funds (including the European Union). The descendents of the late professor Pieter van Rhijn, second director of the Kapteyn Astronomical Laboratory, donated a drawing of van Rhijn. This has been placed in the Kapteyn Room along with paintings of Kapteyn and Adriaan Blaauw. Finally I note that due to illness in the secretariat the completion of this Annual Report is significantly delayed compared to other years; this shows the vulnerability of a limited secretarial support. Many staff members have contributed to this Annual Report, but I am parti-cularly grateful to Gineke Alberts and Jackie Zwegers-Morris for their work on its preparation. Groningen, August 2004 Pieter C. van der Kruit Director

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2. EDUCATION

Astronomy Students

Per 31 December 2003, 23 older-year students were registered with Astronomy as their principal subject. There were 8 older-year ‘Physics and Astronomy’ students registered with Astronomy as their principal subject; The table below lists the number of students in the past 11 years:

Year: number of students per 31 December 1993 49 1994 43 1995 50 1996 50 1997 52 1998 49 1999 59 2000 62 2001 56 2002 52 2003 39

The number of students is declining slightly the last couple of years. The fact that in the year 2000 Physics and Astronomy were joined to form “Physics and Astronomy” is probably the cause of this; Astronomy is not as visible as it was in the past. In total there are only 4 women among the 31 older-year students. The analysis of students in year and achievement (as of 31–12–2003) is as follows:

next exam: number of students: per year: propedeuse 17 of which 8 1st year’s 4 2nd 2 3rd 1 4th 1 5th 1 6th + more bachelor 0 of which 0 2nd year’s doctoraal 22 of which 2 3rd 3 4th 10 5th 7 6th + more

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The table below gives some statistics (as of 31–12–2003) concerning the progress of students since 1985: Year 85 86 87 88 89 90 91 92 93 94 95 96 97 98 99 00 01 02 03 No 1st year (31 Dec) 14 6 5 13 7 10 13 9 9 10 18 14 14 10 22 15 16 11 8 Influx after the propedeuse 1 2 1 0 1 3 4 2 2 0 4 0 1 1 0 1 0 0 0 No. of females 4 0 0 0 0 3 1 1 1 5 1 2 1 1 6 3 3 2 3 Gained propedeuse 8 5 3 10 6 8 11 7 6 8 15 7 8 8 13 7 3 - - Propedeuse in 12 months 5 0 0 5 0 1 3 3 1 3 8 4 4 4 8 1 3 - - Doctorandus degree 6 3 3 8 3 5 6 5 5 5 8 4 6 1 - - - - - Ph.D. Study 3 1 1 5 2 3 4 5 1 5 5 4 5 1 - - - - - Stopped/switched 9 5 3 5 4 8 11 6 6 5 13 10 7 6 11 12 12 7 0 • Based on a period of 17 years (from 1985 through 2001), 61% of the

students gain their propedeuse, and 27% do so within the first year of their study. Although few students get their propedeuse within the first year, many students complete their propedeuse during the second year, whilst following the second year courses at the same time.

• 59% of the total number of students during the years from 1985 to 2001 terminated their studies without obtaining a doctorandus degree. The majority left during the first year, indicating that the difficulty factor and the workload of the astronomy study is often underestimated by beginning students. There are also a small number of students who decide to switch to physics after the first year. This number is more or less compensated by the number of 2nd and 3rd year students who switch over from physics to astronomy.

• A high percentage of the doctorandi (66% during the years '85–'98) continue with a Ph.D.-study.

Examinations

The following examinations were taken in 2003:

Propedeuse: S. Höcük, M.H.D. van der Wiel Finals: D. Bodewits, W.F. Frieswijk, E.A.M. Westra,

S.J. Wijnholds, P. Kamphuis, E.M. Helmich

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Study supervision and information

The organisation, the innovation of the curriculum, the registration of progress achieved, study supervision and study information are taken care of by J.M. van der Hulst (director of education) G. de Vries (coordinator), M.A.M. van de Weijgaert (student counsellor till 1–10–2003), M.C. Spaans (student counsellor from 1–10–2003) and M.G. Alberts (department secretariat). The education coordinating staff is also responsible for supplying information to prospective students during the University Open Days, the introduction of first year students, providing job information at secondary schools, and organising the Science Week. There is a mentor system for first year students. During the first term, the new students hold regular meetings together under the leadership of two third-year students. In this way, problems can be quickly detected and effective commu-nication with the coordinator can be established. Individual discussions be-tween students and the coordinator take place regularly. Meetings of the Education Committee were held twice per term during 2003. Courses

In 2003 the following courses were given: 2nd and 3rd term courses 2002/2003: The Evolving Universe P.D. Barthel, R. Boomsma Introductory Astronomy 2A M.A.M. van de Weijgaert Introductory Astronomy 2B M.A.M. van de Weijgaert Astrophysics A J.-P. Macquart Recent research E. Tolstoy Observing Techniques in Astronomy II A.G. de Bruyn Dynamics of Galaxies and Stellar Systems

R.H. Sanders

Statistical methods R.F. van Shipman Forming and Evolution of Galaxies S.C. Trager The Interstellar Medium A.G.G.M. Tielens Computer course M.G.R. Vogelaar 1st semester courses 2003/2004: Astrophysics B M.C. Spaans Observing Techniques in Astronomy I N. Douglas, J.W. Pel, R.F. Peletier Galaxies A. Helmi Introductory Astronomy 1A J.M. van der Hulst Introductory Astronomy 1B J.M. van der Hulst Stellar Atmospheres A.G.G.M. Tielens Active Galaxies P.D. Barthel High Energy Astrophysics R.H. Sanders In Utrecht interacademical courses were given on the theme “History of Astro-nomy” during the first months of 2003.

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3. RESEARCH

3.1 History of astronomy

Adriaan Blaauw contributed brief biographies to the Biographical Encyclopedia of Astronomers, he wrote the prefatory chapter for Annual Review Astronomy & Astrophysics 2004, and did occasional refereeing for Astronomy & Astro-physics.

3.2 Stars

Late phases of stellar evolution Together with Meakin and Bieging (Univ. Arizona), Latter (Spitzer Science Center), Hora (Harvard), and Hony, Kemper, de Koter, Waters (Univ. Amster-dam), Tielens has investigated mass loss during the late phases of evolution of solar-type stars. NICMOS/HST observations have revealed new structures in the morphology of the enigmatic object, OH 231.8+4.2. In particular, the jets in this object show a complex behavior, including splitting and curvature, which is ill understood by present models. Likely, this object represents a very early phase in the post-Asymptotic Giant Branch evolution of low mass stars. The post-AGB object, HD 56126, is the prototype of a class of objects collectively known as 21 micron sources because their infrared spectra are dominated by a prominent emission feature at 21 microns. These objects represent a class of low metallicity, population II stars of about 1 Solar mass which are currently evolving from the AGB phase to the Planetary Nebula phase. Analysis of their spectra show the presence of a rich inventory of carbonaceous compounds including Hydrogenated Amorphous Carbon, Polycyclic Aromatic Hydrocarbon, Titanium Carbide and Magnesium Sulfide. CO observations from J = 2 → 1 up to 7 → 6 for a sample of Asymptotic Giant Branch stars – using SEST and the JCMT – have shown time-variations in mass loss history of such stars. The time-scales involved, a few hundred years, are similar to those required to explain spatial structure in the envelopes of post-AGB objects, such as the egg nebula.

Blue halo and RR Lyr stars as distance indicators of high-velocity clouds The determination of distances to high-velocity clouds (HVCs) requires high-resolution spectra of halo stars lying at different distances, projected on HVCs; the presence or absence of CaII absorption lines at the appropriate Doppler shift provides an upper or lower limit to the HVC's distance. Together with Morrison and Harding (Case Western Reserve Univ., Cleveland) and Helmi, van Woerden and Wakker (Univ. of Wisconsin, Madison) have undertaken a

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search for distant blue stars in the Galactic Halo with the Wide-Field Camera on the Isaac Newton Telescope at La Palma. Observations have been taken in several fields containing bright HVC cores; the program continues. RR Lyrae stars are also suitable during maximum phase, when their spectra are relatively free of contamination by stellar atmospheric lines. Unfortunately, catalogue data are often not accurate enough to predict epochs of maximum phase. In collaboration with van Woerden and Peletier, Vermaas has under-taken a redetermination of epochs of maximum of RR Lyrae stars. Around 1 July 2003, six nights on the 1-meter Jacobus Kapteyn Telescope (La Palma) were available for the project. Three-colour photometric observations were obtained for twenty stars lying projected on the high-velocity complexes M, C and GP. Each observation consisted of brief integrations (of order 100 seconds) in V, B and R. Careful planning made it possible to obtain, for each of the twenty program stars, 10–12 observations well-spread in phase. The obser-vations of the stars projected on Complex GP have been fully reduced. They show that the light-curve coverage obtained was good enough to allow determination of epochs of maximum to an accuracy of order 15 minutes or better. Further work will thus provide reliable epochs of maximum for several RR Lyrae stars at different distances, projected on Complexes M, C and GP; this will allow effective planning of future high-resolution spectroscopy aimed at the determination of the distances of these HVCs.

3.3 Circumstellar Matter, Interstellar Medium, and Star Formation

PAHs as carriers of diffuse interstellar bands Spaans, Ruiterkamp (Leiden Observatory), Cox (Amsterdam), Foing (ESTEC) and Ehrenfreund (Amsterdam) have investigated the properties and nature of the carrier(s) of diffuse interstellar bands (DIBs), which have so far resisted unambiguous identification. Polycyclic aromatic hydrocarbons (PAHs) are believed to be a good candidate for the carrier molecule(s). In this light, diffuse and translucent clouds with extinctions of 0.1 to 4.0 mag have been modelled and the charge state fractions of different PAHs calculated as a function of depth for various densities, electron abundances, temperatures and strengths of the impinging UV radiation field, as well as internal symmetry groups of the PAH molecules. Together with laboratory data on the wavelengths and strengths of electronic transitions for a large set of PAH molecules, the compu-tation of electronic spectra, that can be compared to observations, was possible. Good agreement was found for the translucent line of sight toward HD 147889 and it was concluded that small PAHs, with less than NC = 50 carbon atoms, provide a good fit to the observations of HD 147889 given the depen-dence of PAH ionization potentials and electronic band strengths on NC.

PDRs in starburst galaxies Photon-dominated regions (PDRs) are regions in the ISM where the radiation field of nearby stars completely determines the temperature and chemical

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composition of interstellar gas. As such, PDRs are direct manifestations of the energy balance of interstellar gas and their study allows one to determine how the ISM survives the presence of the stars that it forms. UV and X-ray photons from nearby sources heat, through photo-electric emission from dust grains, (partially) ionize and dissociate the gas. Fine-structure lines of [OI] and [CII] as well as molecular emission of, e.g., CO and H2O provides cooling. PDRs are bright sources of infrared dust emission because the bulk of the impinging FUV (6–13.6 eV) flux is absorbed by dust grains and re-radiated at longer wave-lengths. Detailed models have been constructed of PDRs by Spaans and Meijerink (Leiden Observatory) that allow for an arbitrary radiation field, from hard X-rays to the optical, and complex geometries. These models are relevant to the lumi-nous centers of starburst galaxies like NGC 253, NGC 1068 and M82, and are necessary to interpret existing ground-based observations of atomic and molecular lines as well as future data from Herschel, SOFIA and ALMA.

H2 formation in the early universe Cazaux and Spaans have developed a model for the formation of molecular hydrogen at high redshift. Molecular hydrogen is believed to be the dominant coolant at redshifts above 5–10 and to facilitate the formation of pop III stars (with masses of the order of 100 M�). These primordial stars are thought to be instrumental in the re-ionization of the universe. It is found that the injection of dust by population III objects leads to positive feedback on the ambient star formation rate through the enhancement of the H2 production on dust grain surfaces. For redshifts above 20, the cosmic microwave background causes dust grains to be too warm, and H2 formation on dust grains is suppressed. For redshifts between 0 and 6, and for a dust abundance as low as 10-3 in solar units, cold dust grains with temperatures of the order of 10–30 K compete favo-rably with H2 formation in the gas phase through the H- route. This suggests a strong interplay between the ambient cooling of primordial gas and the radiation field produced by the first stars.

Population III stars and the reionization epoch In a collaboration with Spaans, Kamphuis investigated the problem of feedback of population III stars in the reionization epoch. Feedback is one of the most important problems in reionization. This paper explores the feedback of UV radiation on the molecular hydrogen in a proto-stellar gas cloud. The fate of molecular hydrogen in UV radiation fields is one of the biggest feedback problems because molecular hydrogen is the only coolant in the primordial gas below 10,000 K. Because of this molecular hydrogen determines the collapse of gas clouds during the reionization epoch. A simulation is done where a proto-stellar cloud without metals is subjected to a population III star radiation field, and its density of molecular hydrogen is examined after irradiation. It is found that the very first stars provide a negative feedback to stars forming later. And thus stretch the epoch of reionization. It is found that, without considering fragmentation, the population III stars form as isolated objects in regions with a radius of 10±2 pc.

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Cloud/intercloud phases in the interstellar medium Much of the interstellar medium in disk galaxies is in the form of neutral atomic hydrogen, HI. This gas can be in thermal and pressure equilibrium in two dis-tinct phases, a cold cloud phase and a warm intercloud phase. In collaboration with Wolfire (Univ. Maryland), McKee (UC Berkeley), and Hollenbach (NASA ARC), Tielens has investigated the stability of these phases in the Milky Way. The results show that a multiphase equilibrium exists from the inner galaxy all the way out to some 18 kpc. The high surface brightness of HII regions at infrared and radio wavelengths makes them ultimately suitable for the study of the properties of the interstellar medium. In collaboration with Martín-Hernández (Observatoire de Geneve), and Bik, Kapers, de Koter (Amsterdam), Tielens has exploited this character-istic to measure the properties of the interstellar medium. High resolution, ISAAC observations of the cometary ultracompact HII region, G29.96–0.02 have revealed a rich line spectrum at sub-arcsecond resolution. Analysis shows rapid velocity variations near the head of the nebula, which is inconsistent with current models for the dynamical evolution of such regions. Analysis of all the available data for this object shows that the central star of this HII region has a spectral type in the range O5–O6V. Radio observations with the Australian Telescope Compact Array of a sample of southern HII regions in combination with infrared spectroscopy using the Short Wavelength Spectrometer on board of the Infrared Space Observatory have been used to derive the abundance gradient in the Milky Way. Furthermore, these observations show that the degree of ionization of these nebulae is correlated with their metal content.

Chemistry in regions of star formation In collaboration with Ceccarelli (Observatoire de Grenoble), Caux and Parise (CESR, Toulouse), Castet (Observatoire de Bordeaux) and Pontoppidan and van Dishoeck (Leiden), Tielens has continued his studies of the chemistry in regions of star formation. This study has focused on the composition of inter-stellar ices around low mass protostars. Specifically, a survey of the infrared solid CO absorption feature in the spectra of protostars obtained with ISAAC on the VLT has revealed that most of the CO in the solid phase is not well mixed in with other ice molecules such as H2O but rather forms a pure solid CO phase. Likely, this reflects the accretion history of species during the collapse phase of the star formation process. Submillimeter studies of the prototypical low mass protostar, IRAS 16293–2422, using the 30meter IRAM telescope have revealed the presence of a rich array of complex species in the warm gas associated with this object. The organic inventory of the Hore Core around this protostar contains abundant amounts of formic acid, acetaldehyde, methyl formate, dimethyl ether, acetic acid, methyl cyanide, ethyl cyanide, and propyne. These species are thought to reflect the rich chemistry possible when solid ices – in particular methanol ice – evaporates into the gas phase when a newly formed star heats its environment.

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Physics and chemistry of gas in planetary nebulae Bernard Salas in collaboration with Pottasch, Wesselius and Beintema (SRON, Groningen), have derived accurate chemical abundances and physical condi-tions of several planetary nebulae (PNe) using ISO data. In collaboration with Marigo (Univ. Padova), these abundances have been compared with detailed nucleosynthetic model calculations appropriate for the AGB evolution in order to better understand the nucleosynthesis history of the progenitor star. The results indicate that it is possible to distinguish between PNe that have experienced only the third dredge-up during the AGB phase and those that also have experienced hot bottom burning. Moreover it has been possible to explain quantitatively both the N/H-He/H correlation and the N/H-C/H anti-correlation. Together with Tielens they are also investigating the infrared emission line spectra of Photo-Dissociation Regions (PDRs) in the immediate vicinity of PNe to derive physical conditions. In order to interpret the observations, we compare the measured line intensities with those predicted by theoretical models. Preli-minary results indicate that photo-dissociation rather than shocks is the main driving force responsible for the atomic lines in the PNe that have been studied. In collaboration with Méndez (SRON, Utrecht) they have started a project to study PNe BD+30 3639 and NGC 6543 using the XMM-Newton observatory. These PNe are especially interesting because chemical studies of the ionized gas reveal that the nebula is hydrogen rich while the central stars are hydrogen poor. This chemical transition still remains a puzzle but is probably produced by the interaction of the mass loss from the central star and the nebular material which emits in the X-ray region of the spectrum.

The temperature of the warm neutral medium in the Milky Way Kanekar, Subrahmanyan (ATNF), Chengalur (NCRA-TIFR) and Safouris (ATNF) used high spectral resolution ATCA 21cm absorption studies to detect the Galactic warm neutral medium (WNM) in absorption against two extra-galactic radio sources. All four detected WNM components were found to have kinetic temperatures in the thermally unstable range 500 < Tk < 5000 K; this suggests that thermal equilibrium has not been reached throughout the WNM.

Structure of Infrared Dark Clouds Frieswijk graduated in March 2003 on the structure of Infrared Dark Clouds under supervision of Shipman. Both the Midcourse Space Experiment (MSX) and the ISOGAL project observed isolated regions of extremely high extinction in the Galactic Plane. These so-called Infrared Dark Clouds are seen in silhouette against the bright diffuse emission of the galactic background. IRDCs are often completely opaque at wavelengths between 7–100 micron and may well represent the high mass equivalents of Bok Globules. However, their temperature and density variations, and their connection to star formation has yet to be established. In his master’s thesis Frieswijk describes the use of star counts and infrared colors of background stars to determine the extinction around Infrared Dark Clouds. In particular he looks at two regions, Cygnus and W51, where he estimates the mass contained in the inner parts. These

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estimates support the idea that the IRDCs are the possible progenitors of high mass stars. From April to October Frieswijk worked for SRON. During this period they created a database of high resolution re-processed and defringed AOT1 ISO observations. The data are available at http://www.iso.vilspa.esa.es. In January 2004 he started as an AIO under the supervision of Shipman, Spaans and Tielens. He will continue his work on Infrared Dark Clouds.

3.4 Structure and Dynamics of Galaxies

Substructures in the Galaxy: probing its formation and its dark matter halo Helmi, Navarro and Freeman (Mt. Stromlo) have reanalyzed the group of stars associated kinematically with Arcturus (Eggen, 1971), and confirm that they constitute a peculiar grouping of metal poor stars with similar apocentric radius, common angular momentum, and distinct metal abundance patterns. These properties are consistent with those expected for a group of stars originating from the debris of a disrupted satellite. The Arcturus group stands out clearly in the compilations of metal poor stars in the solar neighborhood. Validating the extragalactic origin of the Arcturus stream would lend support to the prevalence of accretion events envisioned in hierarchical models of galaxy formation, and would suggest that early mergers may have contributed a substantial fraction of the old and metal deficient stars in the Galactic disk. It has been recently claimed that the confined structure of the debris from the Sagittarius dwarf implies that the dark matter halo of our Galaxy should be nearly spherical, in strong contrast with predictions from cold dark matter (CDM) simulations, where dark halos are found to have typical density axis ratios of 0.6–0.8. Helmi uses numerical simulations to show that the Sagittarius streams discovered thus far are too young dynamically to be sensitive to the shape of the dark halo of the Milky Way. The data presently available are entirely consistent with a Galactic dark matter halo that could either be oblate or prolate, with minor to major density axis ratios c/a as low as 0.6 within the region probed by the orbit of the Sagittarius dwarf (Figure 1).

Microlensing in the Andromeda Galaxy The nature and distribution of dark matter in galaxies is still an unsolved mystery in astronomy. The microlensing results towards the Magellanic Clouds indicate that at most 20 percent of the Galactic dark matter can be in compact objects. The Andromeda galaxy (M31), being the nearest large spiral galaxy to the Milky Way, provides a way of studying another dark matter halo, indepen-dent of our own Milky Way halo. Because of the high inclination of M31 a micro-lensing halo will induce a clear signal in the spatial distribution of the micro-lensing events. The MEGA (Microlensing Exploration of the Galaxy and Andromeda) collabo-ration, consisting of J.T.A. de Jong, K.H. Kuijken (Leiden), A.P.S. Crotts, R.R. Uglesich, D. Alves, P. Czjernes (Columbia University), P.D. Sackett (Mt. Stromlo), W.J. Sutherland (IoA, Cambridge), E.A. Baltz (Stanford), G. Gyuk

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Figure 1: The different panels show the sky distribution of particles in numerical simulations of the disruption of the Sgr dwarf in potentials with varying degrees of flattening for the dark halo of the Galaxy. The different shades represent sets of particles which have become unbound more than 6.5 Gyr ago (dark grey), more than 3 Gyr but less than 6.5 Gyr ago (light grey), and less than 3 Gyr ago (black). In the top left panel, the different detections of debris from Sgr are shown. Direct comparison of the first panel with any of our numerical experiments suggests that the observations are tracing only the most recently formed streams of Sgr (black dots in the different panels). Such streams are too young dynami-cally to have experienced the effects of a flattened halo, be it prolate or oblate, and therefore remain quite coherent even when the minor-to-major density axis ratios c/a are as low as 0.6 within the region probed by the orbit of Sgr.

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(Chicago), L.M. Widrow (Queens) is performing a survey of two large fields in M31, using special techniques to detect microlensing of unresolved stars. Several telescopes are being used for several years, among which the Isaac Newton Telescope (INT) on La Palma. In 2003 de Jong continued to work on the analysis of the INT data. At the end of 2003 the first results, based on a two-year data set were published. The sample of 14 candidate microlensing events is suggestive of the presence of a microlensing halo, but for a more significant signal the full dataset is needed. In the figure the two INT fields and the positions of the microlensing candidates are indicated.

Figure 2: The Layout of the two MEGA fields at the Isaac Newton Tele-scope and the positions of the 14 detected candidate microlensing events. Events MEGA-ML-7 and MEGA-ML-11 correspond to the events PA-99-N2 and PA-00-S4 reported previously by the POINT-AGAPE group. The positions of the two other events reported by POINT-AGAPE are indi-cated with the open circles.

Metallicity distribution of stars in dwarf galaxies In 2003, Cole began the major effort of improving the empirical calibration of the calcium triplet line strength to metallicity, for red giants of all ages and abundances. This followed from continuing work on the chemical evolution of the Large Magellanic Cloud, undertaken with Smecker-Hane (UC Irvine) and Gallagher (Wisconsin). With the new calibration produced by Cole et al. in hand, new projects to measure the metallicity distributions of old stars in dwarf irregular galaxies across the Local Group were begun. The first data were

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taken from Paranal in August 2003 on the galaxies IC 1613, NGC 6822, Phoenix, and WLM, in collaboration with Tolstoy and Irwin (Cambridge). Cole initiated a new program in collaboration with Grebel (Basel) to characterize the age-metallicity relation of the Small Magellanic Cloud. Much of the year was spent reducing the large number of spectra obtained in December 2002 for stars in the LMC bar; with these data, Cole is positioned to measure the metallicity distribution and chemical evolution of the LMC's dominant popu-lation, and to measure the abundance gradient in this galaxy.

Nearby dwarf spheroidal galaxies Tolstoy has continued her work on galaxy formation and evolution with parti-cular interest in the resolved stellar populations of nearby dwarf galaxies. At the beginning of 2003 she was granted an ESO Large Programme “Dwarf galaxies: remnants of galaxy formation and corner stones for understanding galaxy evolution” with VLT/FLAMES multi-fibre spectrograph to study the detailed properties of many hundreds of individual stars in three nearby dwarf spheroi-dal galaxies. According to current structure formation scenarios, dwarf galaxies are the fundamental building blocks of galactic evolution. The surviving systems thereby provide a unique laboratory for detailed study of the generic galactic assembly process and the chemo-dynamical evolution of the low-mass end of the galaxy distribution. VLT/FLAMES provides us with an unparalleled oppor-tunity to make ground-breaking detailed abundance and kinematic measure-ments for large numbers of stars in a sample of Galactic dwarf spheroidal systems (dSphs). This will make possible for the first time: a detailed and complete determination of the combined star formation and chemical enrichment histories of these systems; an accurate assessment of their dyna-mical state and the role of dark matter in their development; the role of dSphs in the assembly of large galactic systems; when and in which type of environ-ments dSphs first formed stars; how this relates to the re-ionization of the Universe; and how the diversity of the star formation histories in these systems arose. This project involves Helmi, two graduate Kapteyn students (Letarte and Battaglia), a post-doc (Cole) and a group of international collaborators: V. Hill, P. Jablonka and P. Francois (Paris-Meudon); F. Primas, A. Kaufer and T. Szeifert (ESO); M. Irwin (Cambridge), K. Venn (Macalester), M. Shetrone (Texas), T. Abel (Penn State) N. Arimoto (NOAJ) and K. Sadakane (Osaka Kyoiku Univ). Results from a painstaking VLT/UVES study of a sample of 15 individual red giant branch stars in four dwarf spheroidals which served as a precursor to the FLAMES programme was published this year. This study concluded that these stars have significantly different abundance patterns to stars found in globular clusters or anywhere in our Galaxy. Making it hard to reconcile these results with the standard paradigm that big galaxies such as the Milky Way are made up of the merging small systems such as dwarf galaxies.

The DART (Dwarf Abundance and Radial-velocity Team) project According to current structure formation scenarios, dwarf galaxies are the fundamental building blocks of galactic evolution. The surviving systems thereby provide a unique laboratory for detailed study of the generic galactic assembly process and the chemo-dynamical evolution of the low-mass end of

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the galaxy distribution In 2003, Letarte worked with Tolstoy on the first phases of the DART (Dwarf Abundance and Radial-velocity Team) project, the obser-ving strategy (with Irwin (Cambridge)), the planing of the observations and the observations themselves. The instrument used, FLAMES, provides an un-paralleled opportunity to make ground-breaking detailed abundance and kine-matic measurements for large numbers of stars in a sample of Galactic dwarf spheroidal systems. Pre-imaging was done by Letarte, high and low-resolution spectroscopy was done by Hill and by Jablonka (both Observatoire de Paris-Meudon) and Letarte. High-resolution measurements were made for a complete samples of red giant branch stars in the inner regions of Sculptor and Fornax, and low-resolution for the outer fields of these two galaxies.

Analysis of the Colour-Magnitude diagrams of IC 1613 Tolstoy continued her work on the analysis of Colour-Magnitude diagrams from HST/WFPC2 data with, among others, Skillman (Minnesota), Cole and Dolphin (NOAO). A study was published of nearby dwarf galaxy IC1613 based on deep imaging with HST. They were able to determine the star formation history back to 8–10 Gyr ago based on main sequence turnoff photometry. It is possible that they are able to see the effects of reionisation on the star formation of these small systems. After a very early start it seems that star formation stops in these systems, perhaps due to increased ionizing radiation, only resuming again when levels fall sufficiently 6–8 Gyr ago.

Variable stars in nearby galaxies Tolstoy was also involved in several papers looking for variable stars in nearby galaxies. There have been a number of papers led by Dolphin (NOAO) which are able to use of our carefully planned HST/WFPC2 observations to use the multiple epochs needed to build up a deep Colour-Magnitude Diagram to search for short period variable stars which can be used as distance indicators as well as providing useful information about the star formation history and metallicity evolution of a stellar population. In Sextans A 82 short-period variable stars were identified. All the periodic variables appear to be short-period Cepheids These objects have been used, along with measurements of the red giant branch tip and red clump, to measure a true distance modulus to Sextans A of (m-M)0 = 25.61±0.07, corresponding to a distance of 1.32±0.04 Mpc. Comparing distances calculated by these techniques, they found that short-period Cepheids (P < 2 days) are accurate distance indicators for objects at or below the metallicity of the Small Magellanic Cloud. They also compared the relative distances produced by other distance indicators and concluded that calibrations of RR Lyrae stars, the RGB tip, and the red clump are self-consistent, but that there appears to be a small dependence of long-period Cepheid distances on metallicity.

Cepheid variable stars in M83 Tolstoy contributed to a VLT/FORS study of Cepheid variable stars in M83 to determine an accurate distance with Thim, Saha and Dolphin (NOAO),

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Tammann, Labhardt (Basel) and Sandage (OCIW). This new distance, together with the previously measured HST/WFPC Cepheid distance to nearby NGC 5253 suggests that these galaxies are so close as to have interacted in the past. Together they are the major members in the group around M83 and the new distance to the group of (m–M)0 = 28.28±0.10 (4.5±0.2 Mpc), together with its mean recession velocity of vLG = 249±42 km s-1 reveals that M83 fits onto the local mean Hubble flow line of the velocity-distance relation (with H0 = 60) with no significant deviation, supporting earlier conclusions that the local velocity expansion field is remarkably cold on a scale of 10 Mpc, contrary to the predictions of the simplest cold dark matter model for large-scale structure.

Studies of super-giants in nearby dwarf irregular galaxies using VLT/UVES Tolstoy worked with Venn (Macalester) and Kaufer (ESO) on detailed abun-dance studies of super-giants in nearby dwarf irregular galaxies using VLT/ UVES. They finished studies of two stars in WLM and three in Sextans A. With-in both galaxies the abundances were consistent between the stars measured. In WLM a metallicity, [Fe/H] = –0.38±0.20 (±0.29) was measured. Two indepen-dent spectroscopic analyses of the HII regions in WLM yielded [O/H] = –0.89. This is the first time that a significant difference between stellar and nebular oxygen abundances has been found, and currently, there is no simple expla-nation for this difference. The two stars observered are massive young (<10 Myr) super-giants with distances that clearly place them in WLM. In the case of Sextans A the mean iron group abundance was determined from the three A-supergiant stars to be [(FeII,CrII)/H] = –0.99±0.04±0.06. This is the first deter-mination of the present-day iron group abundances in Sextans A. These three stars now represent the most metal-poor massive stars for which detailed abundance analyses have been carried out. The �/Fe abundance ratio is [�(MgI)/FeII,CrII]= –0.11±0.02 ±0.10, which is consistent with the solar ratio consistent with the results from analyses in other Local Group dwarf irregular galaxies but in stark contrast with the high [�/Fe] results from metal-poor stars in the Galaxy.

Multi-slit observations of individual red giant branch stars Tolstoy has worked with Fraternali (ASTRON/Dwingeloo) and Irwin (Cambridge) on VLT/FORS2 multi-slit observations of individual red giant branch stars in the distant Tucana dwarf spheroidal. This is a Local Group galaxy for which very little information has been available. They measured for the first time an accurate optical radial velocity, v(opt) = +182 km/s, and with 15 individual stellar velocities they see tentative signs of rotation (see Figure 3), and estimate the velocity dispersion to be 12 km/s. This result rules out the direct association of HI seen near the system by Oosterloo et al. 1996, at velo-cities closer to 150 km/s, probably belonging to the Magellanic stream. From our FORS2 spectra they also have Ca II triplet metallicities, which suggest a low metallicity system, albeit with a fairly large disperion, similar to the Sculptor dwarf spheroidal. Their data are consistent with the intriguing scenario that Tucana was once a “normal” dwarf spheroidal galaxy in the halo of our Galaxy which was ejected at some point in the past (around 4–8 Gyr ago), which is

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perhaps the point at which it lost all its HI gas, as it currently has no measureable ISM and has not formed stars for 6–8 Gyr.

Figure 3: This is a 20 arcmin by 7 arcmin image from the DSS centred on the Tucana dwarf spheroidal. North is up and East is to the left. The crosses represent stars for which they have measured optical velocities of individual stars with FORS2/MXU on the VLT. The green crosses are those at systemic velocity (182 km/s), the red crosses are at velocities greater than systemic and the blue crosses less than systemic. There is intriguing evidence for rotation, although the number of stars is too small to be certain. More details will be published in Fraternali et al. 2004, in preparation.

Structure, kinematics and stellar populations of galactic bulges Peletier continued with his work to study the structure, kinematics and stellar populations of galactic bulges. This is in collaboration with Balcells and Vazdekis (IAC) and Falcon-Barroso (Leiden). Falcon-Barroso presented his PhD thesis in January in Nottingham under supervision of Peletier. They showed that bulges show a tight relation between the Ca triplet line strength and the central velocity dispersion, an indicator of the galaxy mass. What is particularly surprising is that larger galaxies have small Ca triplet values. At present there are several effects which can explain this relation, but none is very well understools (Falcon-Barroso et al. 2003a). A paper was also publish-ed on the minor axis kinematics of bulges. It seems that several bulges, also of very early-type show flat velocity dispersion profiles, indicative of bar-like structures (Falcon-Barroso et al. 2003b). Balcells et al. (2003) studied the surface brightness profiles of bulges. They showed that when you look in detail,

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bulges that obey the r1/4 law are extremely rare. Also, bulges often seem to have a central point source, or a small exponential component (such as a central disk) in the center. An important part of Peletier's work was his involvement in the development on new stellar population models for galaxies, mainly together with Vazdekis (IAC). The series of papers studying the red region of the Ca II IR triplet was finished with the stellar population model paper (Vazdekis et al. 2003), presenting high-resolution spectra in the red for various ages and metallicities. At present the work is being continued in the optical region between 3500 and 7500 Angstrom. Peletier, Vazdekis and collaborators (Gorgas, Sanchez-Blazquez and Cenarro, Madrid; Jimenez, currently in Granada, and Selam, Ankara) have observed a new large library at 2 A resolution between 2000 and 2002, and are currently making a next version of the stellar population models. To work on this Sanchez-Blazquez will come to Groningen from January to August 2004. Peletier is member of the SAURON collaboration, a group of people mainly from Leiden, Lyon and Oxford who use the SAURON instrument, built by this group, at the WHT in La Palma to study nearby galaxies. In 2003 the observations of the SAURON survey, a representative sample of 72 ellipticals and early-type spirals, were finished, and the analysis continued. The group studied kinematics of gas and stars, as well as stellar populations in 2 dimen-sions in these galaxies. The Leiden group uses these for detailed dynamical models, while Peletier, Fathi and collaborators analyse the motion of the gas and the absorption line strengths. A paper on NGC 7332 by Falcon-Barroso et al. was submitted to MNRAS. Here it was shown that the galaxy contains a significant amount of ionized gas, which apparently is moving in a very dis-orderly way, maybe due to an interaction with the nearby galaxy NGC 7339.

High velocity HI in external galaxies Boomsma has continued his thesis project (with van der Hulst, Sancisi, Fraternali and Oosterloo (Dwingeloo)) on the vertical structure and kinematics of HI gas in spiral galaxies. Two galaxies have been studied in detail: NGC 6946 and NGC 253. He has finished the reduction of sensitive HI observations of the nearby, almost face-on spiral galaxy NGC 6946. In the direction of the inner disk of this galaxy large complexes of kinematically anomalous HI have been detected as well as many HI holes. Both are believed to be caused by the massive star formation in the disk. HI holes and anomalous gas complexes have also been found in the outer parts of NGC 6946, where star formation does not seem to be playing a significant role. These may, therefore, have been produced by other mechanisms such as the collision with infalling gas clouds. Furthermore, Boomsma has finished the reduction and analysis of 21 cm data of the southern spiral galaxy NGC 253. This starburst galaxy also shows HI peculiar features and plumes of gas which apparently extend vertically up to 8 kpc from the plane. This may be related to the starburst taking place in the central regions of the galaxy. Another remarkable aspect shown by the data is the unusually small size of the HI disk of NGC 253 as compared to the stellar disk. Barbieri (Milano), Fraternali and Oosterloo (Dwingeloo), Sancisi, and Bertin (Milano) have studied the distribution of mass and the presence of HI (ano-

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malous velocities) in the halo of the spiral galaxy NGC 4559. They have used HI line observations obtained with the Westerbork radiotelescope. The HI picture obtained from these observations is similar to that of NGC 2403 as derived by Fraternali et al. in recent years. NGC 4559 is kinematically lopsided and shows an asymmetriic distribution also in the halo gas.

Luminous and dark matter in spiral galaxies Battaglia, Fraternali, Oosterloo and Sancisi have completed their study of the HI distribution and dynamics of NGC 5055. This galaxy shows a very large, symmetric warp and a decline of 25 km/s in the rotation curve, both occurring at about R25. A firm lower limit is derived for the disk mass-to-light ratio in a model with an isothermal halo. This galaxy also shows a peculiar dynamical beha-viour: at about R25 the systemic velocity changes. A striking geometrical and kinematical symmetrization of the system is obtained by allowing the centre and the systemic velocity to vary. Furthermore, also in NGC 5055 the observations show the presence of HI with anomalous kinematics.

Galaxy dynamics and dark matter Milgrom (Weizman Inst.) and Sanders considered the findings of Romanowsky et al. (Science, 301, 1696) concerning the apparent absence of dark matter in ordinary elliptical galaxies based upon planetary nebula kinematics. In the con-text of modified Newtonian dynamics (MOND), this result is understandable because these galaxies are high surface density objects with mean accelerations considerably larger than the acceleration constant of MOND. These findings continue, and are now extreme examples of, the trend predicted by MOND: the mass discrepancy sets in at larger and larger scaled radii in galaxies with larger mean surface densities.

Planetary Nebulae (PNe) as mass tracers in galaxies Napolitano has been appointed in January 2003 as a two years Marie Curie Fellow. The aim of this project is to study kinematics and mass distribution in the outskirts of early-type galaxies by means of discrete radial velocity fields of PNe as measured by the dedicated instrument called Planetary Nebula Spectrograph (PN.S). This project is leaded from other staff members of this Institute (Kuijken and Douglas) within an international consortium. Napolitano has been involved both in observational runs (March and October) at the WHT in La Palma, and data reduction and analysis, and galaxy modeling. He has given an important contribution to the work done on the publication of preliminary PN.S data both in elliptical galaxies (Science) and M31 galaxy (MNRAS), focussing in particular on the issues of PNe identification and reliability of kinematical and mass estimates.

Dark Matter properties in early-type galaxies Napolitano has been also interested in a statistical study of Dark Matter proper-ties in early-type galaxies, collecting and re-interpreting archive data and looking for correlations with structural properties of these galaxies. The prelimi-

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nary results show the presence of a dichotomy in DM properties as well as in luminous properties of the sample investigated. This result has been presented as poster contribution at the IAU Symposium 220 in Sydney. Napolitano has also accomplished a project started before his appointment at Kapteyn Institute on the study of the physical properties of the Intracluster Planetary Nebulae in N-body cosmological simulations, published in Astrophys. J. in March 2003. He his still continuing the collaboration with an international team which is carrying out an observational project on the search of PNe in the intracluster medium of nearby cluster and groups and the investigation of their physical and dynamical properties.

The mass distribution in early type disk galaxies Noordermeer has continued his PhD work on the mass distribution in early type disk galaxies, under supervision of Van der Hulst, and in collaboration with Sancisi, Van Albada and Swaters (Baltimore). They study early-type disk galaxies in the WHISP database, with morphological type between Sa and Sb. Rotation curves are derived from the HI data and additional optical spectra. They are found to rise extremely quickly in the center; often they decline significantly in the outer parts. The more recent part of this work has been focused on carefully modelling the contribution of the different mass components in these galaxies to the observed rotation curves. The stellar light distribution is decomposed in a spheroidal bulge and a flat disk component, taking into account their respective 3D density distributions and different stellar populations. The bulge dominates the mass distribution in the inner regions and is responsible for the steep rise in rotation velocity in the center; its mass-to-light ratio is tightly constrained by the observed rotation curve. The stellar disk is needed to explain the rotation curve at intermediate radii, whereas the rotation velocities in the outer regions can only be explained by the presence of a substantial amount of dark matter. The neutral gas is found to have little or no dynamical impact in these systems. There is a degeneracy between the contributions of the stellar disk and the dark matter, but these early-type disks are certainly not as dark matter dominated as most late-type and dwarf galaxies.

Accreting small companion galaxies or HI clouds Van der Hulst and Sancisi reobserved two galaxies with the upgraded WSRT to verify that these are examples of objects in the process of accreting small companion galaxies or HI clouds. One is NGC 3359 which has a small com-panion which now clearly shows distortions and an HI connection with the main galaxy. The other is the edge-on galaxy NGC 4565, which is warped, but shows clear signs of extra-planar gas in the central regions, disconnected with the warp, but possibly accreted from a small companion galaxy NGP9 F378–0021557. In these cases the amount of HI involved in the accretion is less than 0.5% of the HI mass of the parent galaxies. Similar amount of gas, possibly associated with accretion events can be found in other nearby galaxies studied recently: NGC 2403, NGC 6946, NGC 891 (Fraternali, Boomsma, Oosterloo, Sancisi).

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The central regions of spiral galaxies Sancisi and Swaters (Baltimore) have continued their study of the luminous and dark matter in the central parts of spiral galaxies. Sancisi (see contribution at IAU Symp. 220 (Sydney, 2003)) has emphasized the close coupling between the luminous matter and the dark matter in the central regions of spiral galaxies (including LSBs and low-luminosity systems).

Chemo-dynamical evolution of dwarf galaxies in the Local Group In June 2003 Battaglia started her PhD research on “Chemo-dynamical evolution of dwarf galaxies in the Local Group” with Tolstoy and Helmi. During 2003 Battaglia has been working on a project with Helmi, using data from the “Spaghetti” Survey. This survey of Milky Way halo stars includes Field Horizon-thal Branch (FHB) stars, turn-off stars, globular clusters and halo giants, which are detectable out to 100 kpc from the galactic centre. The large distances of the detected stars from the centre give a very good opportunity to derive the velocity dispersion of the Milky Way and to compare it with the velocity dispersion predicted from several models. The observed velocity dispersion is consistent with a costant value of about 130 km/s out to approximately 50–60 kpc from the centre and then it shows a decline of 80 km/s out to the last measured point at about 120 kpc.

Stellar kinematics of edge-on galaxy disks During 2003 Kregel has finished his PhD research on the structure and kinematics of edge-on spiral galaxy disks. In this period he collaborated with van der Kruit, de Blok (ATNF, Sydney) and Freeman (MSSO, Canberra). A structural analysis of the stellar thin disks of 34 edge-on spirals in the I-band has revealed a remarkable relation between the disk flattening, disk face-on central surface brightness and the galaxy dynamical mass-to-light ratio. Appa-rently, the three dimensional disk shape is intimately tied to the prominence of the dark matter halo. Dynamical modeling of the stellar disk structure and kinematics and the rotation curves of 15 of these edge-on spirals shows that the almost all of their disks are submaximal, with an average disk contribution to the galaxy rotation curve of 53±15 percent (1� scatter). Seven spirals have either a boxy- or peanut-shaped bulge, strongly suggesting that the sub-maximal nature of disks is independent of barredness. The stellar disk velocity dispersion shows an increase with the galaxy maximum rotational velocity, confirming the work of Bottema (1993). Moreover, the scatter in this relation correlates with disk flattening, central surface brightness and the dynamical mass-to-light ratio. The findings are in general accordance with the collapse theory of disk galaxy formation, suggesting that the disks of spirals of intermediate- to late-type Hubble type have emerged from the hierarchical merging process largely unscratched.

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Cold dust opacities from counts of background objects The PhD project of Holwerda, in collaboration with van der Kruit and Allen (STScI, Baltimore), is to determine the dust opacities of nearby spiral galaxies using the number of background field galaxies detected through the foreground galaxy in HST/WFPC2 archival data. The numbers of field galaxies are compared with those of simulations. These are the original field with an appropriately dimmed Hubble deep field added, thus calibrating for crowding and confusion on the numbers. The goal is to have radial extinction profiles for spiral hubble types (Sa-Sc) to compare with HI and stellar profiles. In addition the opacity of typical regions in spiral disks will be obtained (arm, inter-arm and outside regions). In the third year of the project, the bulk of the field galaxy identification was done on the sample of 33 HST/WFPc2 pointing on 30 spiral disks. The cali-bration of several error and uncertainty factors was finalized. Several possibi-lities to segment the foreground images into areas with similar characteristics were explored: radial distance from the foreground galaxy center, arm, inter-arm or outer region masks and 2 MASS surface brightness masks. A first paper, describing in full the updated technique was written in 2003, illustrated by two example galaxies. It will be submitted early 2004. Initial results were presented at the AAS 2003 winter meeting in Seattle. Radial profiles for three examples were presented on a poster at the IAU in Sidney. A poster exploring the differences in radial extinction profiles between Hubble types was presented at the 2004 winter AAS meeting.

Statistical studies of extinction in galaxies Choloniewski and Valentijn completed and published a new statistical method to determine the extinction in galaxies. The method uses exclusively the obser-ved surface brightness in galaxies, and determines from that the extinction along the line of sight. In a first paper the method is presented, while in a second paper the method is applied to the Galaxy, using the surface photo-metry of the ESO-LV catalogue. Valentijn further investigated the application of the method to self-calibrate photometrically single, one square degree, OmegaCAM images containing typically 100.000 galaxies.

Hydroxyl maser emission in ULIG galaxies Extragalactic Megamaser emission from the hydroxyl and the water molecules was first detected in the early eighties. They revealed a new class of maser emission with unexpected isotropic luminosities of many magnitudes higher than their Galactic counterparts. Galaxies that display this exceptional and so called Megamaser emission show enhanced core activity in the form of a nuclear starburst or an active galactic nucleus. During the completion phase of the PhD thesis of Klöckner, in collaboration with van der Hulst, Baan and Garrett (Dwingeloo), a trust-able sample of 75 OH Megamaser galaxies has been build. Based on this sample, the general properties of OH Megamaser galaxies in the optical, infrared- and radio-bands have been evaluated. It has been found that most of the host galaxies show

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warm infrared colours associated with a 60 K dusty environment and that the dominant power source in most of these sources is driven by prominent star formation in the nucleus. Furthermore, a model of infrared pumping has been developed in order to investigate the infrared pumping mechanism. The investi-gation of the maser- to infrared-photon efficiency showed that most of the extra-galactic OH Megamaser emission is caused by an unsaturated maser process. In addition, the evolution of OH Megamaser galaxies has been compared with galaxies showing enhanced infrared emission. In general, the evolution of OH Megamaser galaxies is best described by a Schechter luminosity function, but shows significant differences with respect to the infrared sampled galaxies. Furthermore, a program has been developed in order to study extragalactic Megamaser emission with respect to the geometric distribution of maser clouds in the circumnuclear region. To reproduce the typical line characteristics of extragalactic hydroxyl Megamaser emission a Monte-Carlo approach has been used and the influence to the synthesized spectrum of various cloud distri-butions has been evaluated. The model indicates that significant changes in the spectral pattern can be associated with cloud size, opening angle, background continuum emission and different kinematics, which has been discussed for a prototype circumnuclear structure of 450 pc in size. Furthermore, the method used in the program to calculate the integrated maser emission provides strong evidence to the nature of extragalactic hydroxyl emission itself, that most of the extragalactic maser emission can be explained by an unsaturated maser process.

A search for the lowest mass galaxies Current cosmological models predict existence of more small galaxies then is observed. Recent work adressing this discrepancy suggests that the small galaxies contain relatively smaller amount of luminous matter then larger gala-xies. In that case statistics based on the luminous matter do not represent sta-tistical properties of the mass. To investigate this possibility Kova�, Oosterloo and van der Hulst started a project (in November 2002) to reveal existence of small faint galaxies with HI masses below 107 M� via an HI survey of a region in the nearby Universe. Given the low average density of galaxies in the field, it would require more then one year of continous observing with large radio tele-scopes to obtain reliable statistics. They proposed to survey a region of about 100 square degrees covering the CVnI/II groups. By observing this nearby, mild over-density region meaningful statistics can be obtained in a reasonable amount of observing time. Also, the CVn region is unique because it is the only region where for distances of a few Mpc recessional velocities can still be converted into a distance and used for the determination of HI masses. WSRT observations of about 30 × 12 hrs have been performed for this project. Reduction and calibration pipelines have been written (Oosterloo), which have been implemented and these observations have been partially reduced (Kova�). Many galaxies over a wide range of HI masses have been detected so far, using additional computer programs (created by Oosterloo and Kova�). Analysis of the data shows that observing procedure meets the requirements for the proposed survey. At this stage of data reduction, two candidates with HI

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masses ~106 M� have been detected for which there are no known optical counterparts.

Dark matter in the inner parts of barred galaxies Testing the dark matter distribution in the inner parts of galaxies is crucial to determine the cosmological scenarios in which the universe has evolved. Perez Martin in collaboration with Freeman and Fux (MSSO, Canberra) have carried out a project to test whether the luminous stellar mass of spiral galaxies domi-nates the potential gradient in the inner parts. For this purpose the galaxy dyna-mics of a sample of barred spiral galaxies has been modelled by running an SPH code on the luminous underlying matter distribution of the sample galaxies. The results obtained indicate that the gravitational field in the inner parts is mostly provided by the stellar luminous component and favours the maximum disk assumption. Fast rotating bars seem to be needed in order to fit the data. This result agrees with the few direct measurements obtained of the bar pattern speed on galaxies. These results have been submitted for publi-cation.

The origin of the hot metal-poor gas in NGC 1291 The X-ray faint source NGC 1291 posses low-metallicity hot gas at its center while having metal-rich stellar bulge component. This scenario is hard to reconcile with the stellar origin that it is usually found to be the cause of the hot gas enrichment. VLT observations were awarded to Perez Martin, Freeman (MSSO, Canberra) to test the possibility of this hot gas being heated by a dynamical process by obtaining the metallicities of the ionised gas HII regions located in the ring. We find that these regions show metallicities much larger than the ones obtained for the hot gas. This result rules out the dynamical heating as a the heating source in NGC 1291. These results have been sub-mitted to a scientific journal for publication.

Galaxy dynamics using planetary nebulae Douglas, Napolitano, and Kuijken continued their work on galaxy dynamics based on data taken with the PN.Spectrograph, which was described in some detail in the Annual Report 2002. The instrument, built and run by an inter-national consortium with the “hub” currently in Groningen, uses “counter-dispersed imaging” (a type of slitless spectroscopy) to detect Planetary nebulae and measure their radial velocities in one step. Data taken with the PN.S, now in its third year of operation at the William Herschel Telescope, have begun to reach “critical mass” with approximately 100 Planetary Nebulae detected in three galaxies, NGC 821, NGC 3379, and NGC 4494. The radial velocities of the Planetary Nebulae, measured with an accuracy of about 20 km-1, allow them to estimate the velocity dispersion in the outer halos of these galaxies, extending the results of conventional stellar spectroscopy by a factor of 2–3 in radius. One of the galaxy fields is shown in Figure 4.

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Figure 4: Planetary Nebulae in the normal elliptical galaxy NGC 3379. A few hours of observing with the PN Spectrograph (and several months of careful data reduction) yielded over a hundred Planetary Nebulae velo-cities. Previous analysis of about one third of this number by Ciardullo et al. (1993) had already indicated that the dynamics of this galaxy were consistent with the absence of a dark halo. With the larger sample we were able to strengthen this statement (see Figure 5). Their finding is that in all three cases the velocity dispersion appears to decline, a result more compatible with a constant mass-to-light ratio galaxy than one dominated in the outer parts by a dark halo. Note that this finding would not have been established on the basis of the integrated light spectroscopy (solid points in Figure 5). These inevitably controversial findings were published in Science. Another highlight was the completion of a catalogue of Planetary Nebulae in M31, based on observations carried out in October 2002. This was done in collaboration with a consortium led by Evans (Cambridge). For an instrument designed to take long (typically half-hour) integrations on a single field encom-passing a single galaxy, M31 was a challenging observation, since the galaxy covers a vast area of sky and required some 20 fields per night, each of about 15 minutes integration time. The result is a vast mosaic in which over 2,600 Planetary Nebulae velocities have been measured. The very size of M31, which makes slit spectroscopy difficult, is one of the motivations for studying it with the PN Spectrograph.

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Figure 5: Equivalent circular velocity derived for the elliptical galaxy NGC 3379, enabling a comparison with the "flat rotation curve" of a typical spiral galaxy. The family of curves is parameterised by the mass-to-light ratio. Most elliptical galaxies studied to date have a flat circular velocity curve as well, indicating a rise in mass-to-light ratio towards larger radius, consistent with the presence of an extended dark matter halo. However in the case of NGC 3379 the velocity curve corresponds approximately to a constant mass-to-light ratio of between 5 and 8, with the acceptable fit indicated by the shaded area. If confirmed by future data, this would rule out the presence of a massive centrally concentrated dark halo. Similar results were obtained for NGC 821 and NGC 4494. They searched the PNe population for kinematic outliers and found about 20 such objects. Their positions and velocities suggested that they might connect the previously identified “Southern Stream” (Ibata et al., 2001) with a feature known as the Northern Spur, as indeed suggested by Ferguson et al. (2002). They were able to suggest an orbit consistent with the known properties of M31 and able to make the sharp turn required to connect the two features, a result published in the Letters section of the MNRAS (Merrett et al., 2003).

Strong gravitational lensing Together with Noordermeer, Möller investigated the possibilities of observing and reconstructing the rotation curves of gravitationally lensed arcs. Using simulations, the properties of strongly lensed velocity fields were investigated.

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A routine was developed to fit a mass model of a cluster to the observed arcs and reconstruct the integrated light profile of a lensed galaxy as well as its velocity field. The kinematic information can be used to differentiate between degenerate cluster mass models. Even with relatively simple arc systems the source can be reconstructed with sufficient accuracy to derive a rotation curve of the lensed galaxy. In this way rotation curves of galaxies at redshifts z > 1 can be measured.

Dynamics of early-type galaxies Fathi's research interest lies in galactic structure and dynamics, studying formation mechanisms and evolution processes of galaxies from observations of their present dynamical state and structure, complemented by theoretical modeling. Fathi is an associate member of the SAURON project, dedicated to studying the intrinsic shape and dynamical properties of early-type spiral galaxies. The main aim of the SAURON project is to map the kinemtics and line-strengths of a large number of early-type galaxies to large radii, of which 1/3rd are early type spiral galaxies. Based on Schoenmakers, Franx & de Zeeuw (1997), Kambiz makes use of Fourier decomposition of the SAURON velocity fields. SAURON provides high quality velocity maps for the central regions of the sample galaxies, which provide full kinematic signatures of the underlying potential. Although, the kinematic features are primarily dominated by circular rotation in the plane of the disk, thorough investigations reveal somewhat strong deviations corresponding to higher order perturbations in the potential, or to potentials that deviate from axisymmetry. The velocity maps show very prominent kinemtical effects of non-axisymmetric components, the under-standing of which is imperative for developing current galaxy formation and evolution theories. Also this kind of study has the potential of increasing of our understanding of fuelling of active galactic nuclei.

3.5 Quasars and Active Galaxies

Radio properties of LINER galaxies Barthel is collaborating with Ho (Carnegie Observatories) and Filho (Bologna) in a study of the radio properties of LINER galaxies, objects displaying a mild form of nuclear activity. High resolution radio observations (VLA, MERLIN, VLBA, and EVN) are being employed to assess accretion driven energy production in galaxies, which is likely to be widespread. Radio data are being supplemented with X-ray as well as optical data. A collaborative effort with Peletier, de Zeeuw (Leiden) and the SAURON group finds an intriguing corre-lation between accretion and circumnuclear gas properties.

Low redshift QSO’s Low redshift QSOs are being investigated by Barthel and co-workers, targeting the interrelation between accretion driven energy production and host galaxy

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star formation. Radio and optical imaging is being combined with molecular gas spectroscopy: More JCMT data have been acquired supporting the truth of an AGN-star formation symbiosis.

Extremely high redshift QSO’s The search for extremely high redshift QSOs, being conducted in a collaborative effort with Neeser (Munich) and Maza (Santiago), is continuing. Near-infrared photometry has been conducted to weed the candidate sample (eliminate brown dwarf stars). VLT spectroscopy of the remaining faint ultra-distant QSO candidates in the 3 square degree field will be conducted in 2004.

Orientation of quasars and radio galaxies Barthel and van Bemmel (STScI) are continuing their study of the far-IR proper-ties of radio-loud active galaxies. IRAS and ISO data will be supplemented with data to be obtained with the Japanese ASTRO-F mission: Barthel is taking part in a British-Groningen consortium collaborating with the Japanese Space Agency JAXA. Spitzer (formerly SIRTF) observations will also be sought. Data using the new VISIR infrared instruent on the VLT will be obtained in 2004. Studies of the host galaxies of compact powerful radio sources, constraining evolutionary models for these objects, are being continued, in collaboration with de Vries (Livermore), O'Dea (STScI), Hunstead (Sydney), and graduate student Labiano (Baltimore/Groningen). Spectropolarimetric investigations of radio galaxies and quasars, conducted in a collaborative effort with Cohen and Barth (Pasadena), Goodrich (Keck) and van Bemmel, using the Keck-II telescope, are being continued. The data are being analysed addressing unification as well as evolutionary (growth) aspects. Barthel is spending an increasing amount of his time on the Herschel Mission, ESA's far-IR and submm space telescope. This 3.5m telescope, with planned launch in February 2007, will open up the Universe in the 200–600 micron domain. As one of the Mission Scientists in the Herschel Science Team, Barthel deals with the interface between the Agency, the (3) Herschel Instrument Teams, and the users-to-be. Planning of the first phase of the Mission is now at order.

Ultra-compact sources and inhomogeneous media Macquart and de Bruyn's ongoing investigations of the intra-day variable quasar J1819+3845 continue yielding a stream of surprises. Foremost among these is the discovery of the presence of diffractive scintillation; this is the first time this phenomenon has been observed in a quasar, and it implies that a component of source possesses the remarkably high brightness temperature of 1015 K. This emission is very difficult to understand in terms of incoherent syn-chrotron radiation, which should radiate below the inverse Compton limit (1012 K). Macquart and de Bruyn are also charting the intrinsically evolving micro-arcsecond structure of this source using a novel technique called Scintillation Earth Orbit Synthesis. The remainder of Macquart's work this year concentrated on various theoretical problems related to the propagation of radiation through inhomogeneous

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media. This included the development of a model to explain the spectral line variations observed in some radio sources, and a treatment of the effects of multi-path propagation on the gravitational lensing of gravitational radiation. The latter has several implications for the detectability of gravitational radiation with current and next generation gravitational radiation detectors such as LIGO and LISA. Macquart also continued work with Melrose (Sydney) and Rickett (UC San Diego) on various theoretical problems related to the scintillation of the intra-day variable radio sources.

Rotation Measure synthesis De Bruyn and Brentjens have applied Rotation-Measure synthesis to 92 cm radio observations that were obtained in December 2002 with the WSRT. RM-synthesis was suggested by Burn (1966). De Bruyn applied it for the first time in 1996 on a test observation of a pulsar. In RM synthesis one derotates the Q-U vectors of many channelmaps to correct for the effect of Faraday rotation. After derotation, all channel maps are averaged to yield a high signal-to-noise map of emission at a certain Faraday depth. By repeating this procedure for many assumed Faraday depths, one obtains a RM-cube. This cube shows the emission as a function of both sky position and Faraday depth. The technique enables them to study weak, heavily Faraday rotated emission as found in galaxy clusters. They have discovered previously unknown, large-scale structures in the Perseus cluster at radio frequencies between 310 and 380 MHz. One of the structures they found resembles a giant, flattened bubble. It measures approximately 1 by 0.5 Mpc. This may be an example of the mag-netized AGN bubbles proposed by Ensslin and Gopal-Krishna (2001). Parallel to this bubble runs a long straight feature that could be caused by a shock in the Perseus-Pisces supercluster. These results have been presented at IAU JD 10 in Sydney, Australia and at a cooling flow conference in Charlottesville, USA (Brentjens & de Bruyn, 2003). They have conducted new observations of the Perseus cluster in December in order to exclude a galactic origin of the emission they detected.

HI and galaxy evolution Van Gorkom continues her work on gas and galaxy evolution and its environ-mental dependence. She is analyzing a VLA HI survey of clusters in the local universe with Bravo-Alfaro (Guanajuato), Dwarakanath (NRAO & RRI, Bangalore), Guhathakurta (UCSC), Poggianti (Padova), Schiminovich (Caltech), Valluri (Chicago), Verheijen (Potsdam), Wilcots (Wisconsin) and Zabludoff (Arizona). This survey is aimed at probing statistically the evolution of galaxies as they move from the low density outer parts to the dense inner parts of the clusters. Six clusters have been imaged in HI out to two Abell radii. The HI detection rate varies enormously from cluster to cluster with as most probable cause the dynamical state of the ICM. An analysis of the star formation rate in A2670 by Lugt strengthens this conclusion, the merging of subclumps seems to enhance the SFR. Kenney (Yale University), van Gorkom and Vollmer (Univ. of Strassbourg) are performing a new HI survey of selected galaxies in the Virgo cluster which will be ten times more sensitive than the previous surveys done almost 20 years

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ago. The survey is aimed at studying in detail the processes that affect galaxy evolution in a cluster environment. The data will be used to constrain hydro-dynamical simulations of galaxy evolution in clusters. The first galaxy observed as part of this survey, NGC 4522, displays all the characteristics of an ongoing ICM-ISM interaction, yet the simple scenarios to explain the observations don't work. The galaxy is located far from the center of the cluster, where the esti-mated ram pressure, based on ROSAT images, would be too low by almost an order of magnitude. The most likely explanation is that the effective ram-pressure is locally much higher due to bulk motions and shocks in the intracluster medium. NGC 4522 sits just between the M49 group and Virgo proper and there is evidence from the temperature structure of the ICM that the merging of the group with the cluster has started. Van Gorkom, de Bruyn and Brentjens have started a deep HI survey with the WSRT of selected regions in the Perseus cluster. The goal is also here to compare the HI properties of galaxies in subgroups falling into the cluster with those that already reside in the very center.

Accreting black holes Nagar, with collaborators Wilson, Falcke and others, continued his work on the demographics and properties of accreting black holes in nearby galaxies by studying their radio nuclei at highest resolution. The completed radio survey of the nearest 500 bright galaxies show that >25–50% harbor accreting black holes. The sub-parsec radio jets in several of these nuclei have been quasi-simultaneously monitored with HST and VLBA and found to be highly dynamic, with sub-relativistic outflow speeds. A similar radio study has now targeted a large sample of Ultraluminous InfraRed Galaxies or ULIRGs. Initial results show a high incidence of AGNs and follow up milli-arcsec resolution radio imaging is now in progress. Another major focus of Nagar's research has been the radio search for multiple or binary black holes in merging galaxy systems. Several samples of merging galaxies are being observed at milli-arcsec resolution in order to identify single or multiple accreting black holes through their associated high brightness temperature radio cores. Nagar was co-I on several other AGN-related projects. The two most notable of these were the following: the finding that the Iron abundance in quasars is relatively constant over the redshift range 1 to 6.5. This implies galaxy assem-bly as early as redshift 9. A continuing study of the precessing accretion disk in NGC 1097 as traced by its double-peaked broad H� emission. The 10 years of data on the variable profile is well fit by a precessing accretion disk. Interestingly, we found that line broadened as its luminosity decreased i.e. a quasi- reverberation effect.

Origin and evolution of nearby radio galaxies Emonts has continued his PhD project under supervision of Morganti (ASTRON, Dwingeloo), van der Hulst, Oosterloo (ASTRON) and Tadhunter (Sheffield, UK). It involves studying nearby powerful radio galaxies for recent merger/interaction events and relating this to the on-set of radio and starburst activity in these systems. In a continuously growing HI study to trace and date

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long-lived merger/interaction signatures around different types of nearby radio galaxies they detect massive HI disks that are settled at scales of up to 180 kpc around a number of compact radio sources, which are hosted by early type galaxies (normally considered to be gas-poor). This in contrast to the more extended FR-I radio sources in our sample, which show no such amounts of HI. The relatively young age of the compact radio sources suggests that the radio activity starts late in the lifetime of the merger. In extensive collaboration with the group of Tadhunter and Wills in Sheffield, optical long-slit spectra have been obtained for already 75% of this HI sample in order to trace and date recent starburst events in these galaxies and compare this with the age of the merger as well as the on-set of the radio activity. Eventually they aim to study the possibility of an evolutionary connection between powerful radio galaxies and e.g. ULIRGs and “normal” early type galaxies.

Fast outflows of neutral gas in powerful radio galaxies Morganti, Oosterloo, Emonts, Tadhunter and van der Hulst study recently dis-covered fast outflows of HI gas from the central regions of several nearby powerful radio galaxies. One of these radio galaxies is 3C 293, where they detect a 1000 km/s broad, blue-shifted central HI absorption (Astrophys. J., 593, L69–L72, 2003). With optical spectroscopy they detect a similar outflow of ionized gas in 3C 293 and analysis so far indicates that this outflow is most likely caused by the interaction of the inner few kpc radio lobes with sur-rounding ISM.

3.6 Clusters, High-Redshift Galaxies and Large Scale Structure

Weak gravitational lensing Christen started his PhD research on the Shapelet method applied to weak gravitational lensing, under the supervision of Kuijken and Möller. The first part of this project, based on the KSB (Kaiser, Squires and Broadhurst 1995) method, is almost accomplished. They are now able to locate galaxies, measure the ellipticities and to correct the point spread function to estimate the cosmic shear. They focus on distortion field measurements, mass map recon-struction and mass estimation. The procedure was validated using simulated images and reduced CFHT data. Meanwhile Möller developed a software package to allow the Shapelet decom-position of images and use Shapelet (Refregier 2003, Refregier & Bacon 2003) representations of stars and galaxies to correct for PSF anisotropy and measure the gravitational shear.

The Delaunay tessellation of the peculiar velocity field Romano-Diaz, Schaap and van de Weijgaert have applied the Delaunay Tessellations Field Estimator [DTFE] to calculate continuous full spatial-

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covering galaxy peculiar velocity fields from an irregularly distributed velocity field sample. The method interpolates velocities linearly along the whole space. Regions devoid of objects which represent a major problem for conventional techniques are fully sampled with this method as linear mini-universes in expansion. The method is fully adaptive and independent of the geometry of the point distribution. They have tested and compared this method with the conventional interpolation techniques and the results show that this method is superior to the common algorithms, especially at regions with poor sampling. Analyses of velocity related quantities, such as the velocity divergence, vorticity and shear, suggest that the DTFE-velocity method represents a major step forward for dynamical studies of the cosmic structure.

The velocity bulk flow and shear components inferred from the PSCz catalogue Romano-Diaz, van de Weijgaert and Branchini (Universita de Roma) have investigated the two main components of the large scale velocity field inferred from the IRAS-PSCz catalogue, the bulk flow and velocity shear. The modeling of the peculiar velocity field was performed by means of an implementation of the Least Action Principle, the Fast Action Minimization method [FAM]. Results indicates that the bulk flow estimates are in very good agreement with other measurements from different catalogues and techniques. The cumulative distri-butions of the velocity shear indicate that most of the contributions to it come from structures located within a volume of 20 Mpc/h around the Local Group. Structures located within 20 and 60 Mpc/h still deform the velocity ellipsoid considerably, and those located beyond 70 Mpc/h do not contribute to the velocity shear. The shear eigenvectors suggest that the Hydra-Centaurus supercluster is responsible for the largest stretching direction of the velocity ellipsoid, with an anti-apex direction pointing toward the Perseus-Pisces super-cluster. This eigenvector is roughly aligned with the bulk flow direction, implying that some of the structures responsible for the bulk flow motion, are also responsible for the velocity shear, i.e. the Hydra-Centaurus supercluster. The Coldness of the Local Supercluster Romano-Diaz, Schaap and van de Weijgaert have applied the Delaunay Tessellation Velocity Field Estimator to reconstruct volume-covering peculiar velocity fields of constrained N-body simulations of the Local Supercluster. These velocity fields have been used to compute in a volume-weighted fashion, the cosmic Mach number which is the ratio of the large-scale bulk flow over the small-scale velocity dispersion. The cosmic Mach number is a way to characterize the thermal state of the Local Supercluster. They found that the Local Group of galaxies is located in a rather cold region, with a very low velocity dispersion and mainly dominated by the bulk flow exerted by the Great Attractor region.

Cosmic dynamics and structure formation Scientific work of van de Weijgaert concentrated on the 1) development of an analytical model to describe the evolving hierarchy of voids in gravitational

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instability structure formation scenarios (with Sheth (Pittsburgh)), expanded in a numerical study (with Platen), 2) the application of the Delaunay Tessellation Field Estimator to analyze density and velocity fields in reconstructions of the Local Cosmic Neighbourhood (with Romano-Diaz and Schaap), 3) the develop-ment of the DTFE technique and its application to the 2dF galaxy redshift survey (with Schaap), 4) an investigation of the pattern recognition abilities of Delaunay Tessellations (with Jones), 5) a renewed and expanded formalism and code for constrained random fields, used to reconstruct cosmic environ-ments from observed cluster and galaxy positions (project with Aragon-Calvo and Arayo, collaboration with Boehringer), 6) a radio and optical study of galaxy spin alignments in and near the Perseus and Coma Supercluster (with Aragon and van der Hulst), 7) the formulation of a large wide-angle photometric survey of the Hercules and Horologium supercluster complexes (collaboration around Valentijn). Particular emphasis was put on the project involving the description of the cosmic foam as the result of a hierarchically evolving network of voids, an analytical and numerical study in collaboration with Sheth (Pittsburgh). The evolving void hierarchy is described by means of a Press-Schechter like excursion set formulation. In our void model, the fate of voids is ruled by two processes. The first process affects those voids which are embedded in larger underdense regions: the evolution is effectively one in which a larger void is made up by the mergers of smaller voids, and is analogous to how massive clusters form from the mergers of less massive progenitors. The second pro-cess is unique to voids, and occurs to voids which happen to be embedded within a larger scale overdensity: these voids get squeezed out of existence as the overdensity collapses around them. It is this second process which is responsible for the distinct void characteristics, involving a well-peaked void size distribution, in distinctcontrast to the distribution of virialized halo masses which does not have a small-scale cut-off. In the conventional description for the hierarchical evolution of halos, the excursion set formulation solves the cloud-in-cloud problem by studying the crossings of a random walk through the collapse density barrier. Halos are only counted as objects when they are are not embedded in larger halos. For voids a similar formulation requires study of a two-barrier problem: one barrier is required to account for voids-in-voids, and the other for voids-in-clouds. Thus, in our model, the void size distribution is a function of two parameters, one of which reflects the dynamics of void formation, and the other the formation of collapsed objects. This model leads to the finding that at any cosmic epoch the voids have a size distribution which is well-peaked about a characteristic void size which evolves self-similarly in time. The model provides a natural explanation for the formation and characteristics of the typical foamlike patterns in the observed galaxy distribution and in com-puter models of structure formation. In addition, the natural tendency of voids to peak around a characteristic size and expansion velocity provides an expla-nation for the fact that models based on Voronoi tessellations, a heuristic and geometric description of cellular patterns based upon a population of equal sized and equally fast expanding spherical voids, have demonstrrated to reproduce a multitude of clustering characteristics. At present, the study of void hierarchy is being expanded to yield more analytical results on issues such as environmental influences, the construction of void merging histories, and in particular adressing the issue of the formation of galaxies within the diluted void

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environments. Numerical investigation and testing of the model by means of N-body simulations is the topic of a current study with Platen, which will be expan-ded within a large program in collaboration with Sheth and Colberg (Pittsburgh). Schaap and van de Weijgaert have continued their efforts on the development of the Delaunay Tessellation Field Estimator technique. The DTFE is a highly versatile, self-adaptive and natural technique for multi-dimensional (linear) field reconstruction in which the Delaunay tetrahedra of the point process (e.g. N-body particle distribution, galaxy distribution) are used as multi-D interpolation intervals. Its potential has been underlined through its application to various test situations as well as the galaxy distributions in 2dFGRS and SDSS redshift survey slices. Its capacity to recover simultaneously a wealthy internal sub-structure as well as salient anisotropic features has culminated in striking visualizations of the cosmic web. A statistical analysis of uniform distributions has led to a characterization of its sampling and noise characteristics. It stressed a third major virtue of DTFE, its intrinsic capacity to suppress shot noise in undersampled regions. The product of DTFE being volume-covering and continuous volume-weighted density fields (or any other discretely sampled field), we are developing it as a tool towards computing autocorrelation functions and power spectra of the recovered fields. Together with Romano-Diaz, the DTFE has been applied in the context of producing volume-covering velocity fields. It has yielded promising results in rendering the flows in low-density areas as well as the flow pattern in and near features such as filaments and clusters. Being applied to representations of the local cosmic neighbour-hood, they are using these velocity field renderings towards a more balanced and less noise-ridden analysis of the localized velocity characteristics. On the basis of this application, the coldness of the local cosmic flow is being assessed within the context of a few cosmological scenarios.

Constraining the variation of fundamental constants using OH lines Kanekar and Chengalur (NCRA-TIFR) developed a new technique to estimate variations in the fine structure constant �, the ratio of electron mass to proton mass y and the proton g-factor gp, using redshifted 18cm OH lines. The method was applied to the z = 0.685 absorber towards B0218+357 to obtain the first simultaneous constraint on changes in these parameters. It was found that at least two of �, y and gp vary with time, unless there are velocity offsets between the clouds causing the OH, HCO+ and HI absorption. The technique was improved by the use of cm-wave “main” lines from other OH rotational states, resulting in a sensitivity increase by a factor of ~1000.

The influence of the environment on the evolution of galaxies Sikkema started a PHD project on the first of september under supervision of Peletier and Valentijn on "The influence of the environment on the evolution of galaxies". The project involves the analysis of galaxy properties in cluster environments using wide field data like WFI (data from the ESO archive) and later Omegacam data. However, currently he is working on the analysis of HST–ACS data of six shell galaxies (i.e. galaxies which show arc-like structure probably due to a small companion which has fallen in).

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Figure 6: Four mode (extended) excursion set formalism. Each row illu-Dstrates one of the four basic modes of hierarchical clustering: the cloud-in-cloud process, cloud-in-void process, void-in-void process and void-in-cloud process (from top to bottom). Each mode is illustrated using three frames. Leftmost panels show “random walks”: the local density pertur-bation �0(x) as a function of (mass) resolution scale Sm at an early time in an N-body simulation of cosmic structure formation. In each graph, the dashed horizontal lines indicate the collapse barrier �c and the shell-crossing void barrier �v. The two frames on the right show how the associated particle distribution evolves. Whereas halos within voids may be observable (second row depicts a halo within a larger void), voids within collapsed halos are not (last row depicts a small void which will be squeezed to small size as the surrounding halo collapses). It is this fact which makes the calculation of void sizes qualitatively different from that usually used to estimate the mass function of collapsed halos.

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1720 MHz OH Megamaser emission at z ~ 0.247 Kanekar, Chengalur (NCRA-TIFR) and Ghosh (NAIC) used the WSRT to detect the two 18 cm OH satellite lines (1720 MHz emission and 1612 MHz absorp-tion) from the z ~ 0.247 source PKS1413+135 (see Figure 7). The 1720 MHz isotropic luminosity is LOH = 354 L�, more than an order of magnitude larger than that of Arp 220, the only other known 1720 MHz megamaser. The satellite line profiles are conjugate, with the sum of optical depths consistent with noise; this implies that the lines arise in the same gas. The agreement between the line redshifts yields the constraint ��/� < 5.4 × 10-6 on changes in the fine structure constant �, from z ~ 0.247 to today.

Figure 7: WSRT satellite OH spectra towards PKS 1413+135. Here, OH optical depth � (×××× 103) is plotted against heliocentric velocity (relative to z = 0.24671). The two satellite lines are conjugate to each other, with the sum of the profiles consistent with noise.

HI and CO absorption in a z ~ 0.7645 gravitational lens Kanekar and Briggs (ANU, Canberra) detected HI absorption in a gravitational lens at z = 0.7645, towards PMN J0134–0931. The very high estimated HI column density suggests the presence of large amounts of dust in the lens,

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perhaps responsible for the extremely red colour of the background quasar. Galaxy models that assumed a single disk-like absorber were unable to account for the relative brightness and scatter broadening of the lens images, although they could roughly reproduce the observed 21cm profile. This sug-gests that the lens system is made up of multiple galaxies. Follow-up IRAM observations with Combes (Lerma) and Wiklind (STScI) resulted in the detect-ion of CO 2–1 absorption at the 21cm redshift; this is only the fifth detection of mm-wave absorption at cosmological distances.

Galaxies in the early universe Obric started her PhD research under the supervision of Spaans and van de Weijgaert to work on a project: "Formation and evolution of galaxies: Inter-preting observations of the young universe". During her first year she attended Interacademial courses in Utrecht on “The Early Universe” and a two-week summer school on cosmology in Cargese, France (NATO ASI Summer School: Frontiers of the Universe: Cosmology 2003). From March till June she super-vised a “werkcollege” in Astrophysics. In May/June 2003 she went observing for 8 days to the JK Telescope on La Palma, on behalf of Douglas and his colla-borators. She also started two projects. First one, which started in March, with Trager on "Impact of stellar populations on the Fundamental Plane tilt in multiple bands". This project is ongoing. The other one started with one-month work visit in October to Princeton University and SDSS collaborator, Zeljko Ivezic: "Multi-wavelength properties of galaxies observed by ROSAT, SDSS, 2MASS, IRAS, GB6, FIRST, NVSS and WENSS surveys". This project is in preparation for publication in MNRAS.

Stellar populations of galaxies near and far Trager's studies of the ages and compositions of the stars composing galaxies from times of roughly half the current age of the Universe to the present continued. Trager and Obric have begun a study to examine the impact of stellar population variations on the Fundamental Plane of early-type (elliptical and lenticular) galaxies in four nearby clusters of galaxies, based on data previously acquired by Trager at Las Campanas Observatory. Trager, Poggianti (Padova), Dressler (Carnegie), and Gonzalez-Garcia (Kapteyn/IAC) have just acquired deep spectroscopy and imaging of galaxies in Abell 550 (z = 0.125) with VIMOS on the VLT to extend this study to higher redshifts. Trager, van der Hulst, Oosterloo and Morganti (ASTRON), Sadler (Sydney) and van Gorkom (Columbia/Kapteyn) have begun a project to explore the HI and stellar population properties of E and S0 galaxies selected by their gas content from HIPASS (Southern Hemisphere) or by morphological peculiarities or lack thereof (Northern Hemisphere); Serra has been hired to pursue this project as his PhD research. Trager, Polko, and Somerville (STScI) are examining the stellar population parameters inferred from semi-analytic models of galaxy formation, both to calibrate the observed parameters of real galaxies and to probe deficiencies in galaxy models (particularly the chemical evolution prescriptions).

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Trager and Worthey (Washington State) are developing new stellar population models (in collaboration with Chaboyer (Dartmouth) and Baron (Oklahoma)) and new calibrating stellar libraries (in collaboration with Peletier, Sanchez-Blazquez (Kapteyn/Madrid), Rose (North Carolina), Vazdekis (IAC), Jorgas (Madrid), and others) to improve the accuracy and precision of stellar population age-dating techniques.

ISO survey and source counts Héraudeau and his collaborators have been working on the analysis of a survey performed with the Infrared Space Observatory (ISO) in the far infrared. Number counts at 90 microns have been compared to evolutionary scenarios and show a large excess above the no-evolution model. This confirms the strong evolution detected at shorter (15 µm) and longer (170 µm) wavelengths with ISO. A band-merged catalogue for the fields observed by ISO with obser-vations from the ultraviolet to the radio regime is in preparation. HI observations were obtained from Westerbork for one of these regions to map the foreground cirrus emission.

Galaxy counts Sanders has reconsidered the number counts of faint galaxies in the Hubble Deep Fields along with recent determinations of the distribution of these galaxies by redshift. The redshift distribution can break, to some extent, the de-generacy between cosmology and evolution which corrupts the use of number counts as a cosmological tool. Using a simple “minimalist” model for galaxy evolution, whereby galaxies brighten as a function of lookback time, it is found that the cosmology which is most consistent with both number counts and redshift distribution is none other than the “concordance” model with �� = 0.7 and �m = 0.3. This reinforces the conclusion that these numbers are robust in the context of FRW cosmology.

3.7 Computing at the Kapteyn Astronomical Institute

Hardware In 2003 the computer group succeeded to uniform the machinery by removing the last HP from the server park and by replacing the last Suns by Linux machines. Two isolated Suns are still running to provide FORTRAN function-ality that could not be found for Linux. Replacements for the last 8 X-terminals were ordered in December. The majority of the new client computers are towers. With towers there is more flexibility to deal with requests for disk space. Most of the monitors that were purchased were flat screens. Nowadays these screens are affordable and suitable for image processing. Hard disks caused a lot of inconvenience. This year there were a lot of complaints about slow disks, disks with lots of errors and even disks that failed to boot a system. Some of the complaints could be related to the long and

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warm summer, but anyhow, with the supplier, there was an agreement to try another brand. In November the migration of the Sun fileserver to a Linux machine was unavoidable, which caused a pile of problems that one can encounter while migrating a central machine from one operating system to another. Murphy’s Law applied perfectly: Anything that can go wrong, will go wrong. An internal report was written that describes the migration and in which the conclusions are drawn that client machines are too dependent on a central machine, that server machines are not independent enough and that redundancy of server machines is essential. To avoid unacceptable down time of the system in the future, the computer group focused in the last months of 2003 on upgrading the server machinery and on the development of knowledge about the internals of (server) services. On the other hand the migration path of clients to RedHat 9 was investigated. To enable automatic installation of patches and other software in a mixed environment (different RedHat distributions) a new update script was written.

Software System: A so-called ‘safe area’ with a central firewall was developed to experiment with new system tools that allow for more security and more efficiency. An important software component is LDAP (Lightweight Directory Access Protocol). LDAP will combine several systems that normally have to be maintained separately, such as UNIX authentication, services/protocols/hosts information and network address systems etc. Bottleneck of this development turned out to be scientific software installation on a new file server that operated within the safe area. A request for temporary manpower to speed up this process, was turned down by the financial manager of the faculty. With the migration of the old fileserver to a new Linux machine, this new fileserver was sacrificed and suspended the development for the safe area. However, the obtained LDAP knowledge is not lost, but can be applied directly to the existing environment. Cluster: The computer cluster for students is used to prepare the migration to the RedHat 9 Linux distribution. Two students made a list with problems and missing software not yet available on these re-installed machines. Database: Three new, web based database utilities were written. One program extracts photos of staff and guests and prints them on A3 for use on the institute’s photo board. Another program produces letters in the Kapteyn style and archives these letters in the institute database. For the S.O.S. (Studenten Overleg Sterrenkunde) the institute database is used to generate a list with research projects for students. The starting page can be found at the education page on the intranet or on the home page of the S.O.S. Windows: A separate machine, maintained by SRON and installed in the SRON domain, is used as the current (Windows) NT server. It is called ‘apphost’. The old NT server is not longer maintained. The use of ‘Crossover’ was advertised, which runs windows applications in Linux. It integrates in the KDE desktop and it is perfect for viewing operations like displaying Word, Excel or PowerPoint files. Spam: Spam is one of the most annoying abuses of Internet. Some users complain that they receive at least 250 spam mails per day. An experiment with

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a central ‘spam killer’ was successful. However the load on the machines that process mail became too high and the program was stopped. It will be activated as soon as possible; therefore a new stand alone mail server was bought which should be able to run all the mail related applications without problems. GIPSY: A new web based Linux application is written in cooperation with SRON. It retrieves data from the IRAS database. A Python binding for GIPSY was written which allows developers to write complete and complex GIPSY applications in Python. Even GUI’s, based on Ggi (GIPSY Graphical Interface), can be written in Python. A tutorial with many example programs can be found at: www.astro.rug.nl/~gipsy/python/recipes/pythonrep.php KPLOT, the Kapteyn object oriented plotting package for Python, was adopted for use in GIPSY. This project will be continued next year. An extensive tutorial and recipes book can be found at: http://www.astro.rug.nl/~kplot/DOC/ Backup: Our tape robot, used for backups, was broken and after repair it will get its place in a new backup scheme which will be implemented early 2004. For users a new backup machine was ordered with DVD-writer and dds3&dds4 tape drives. Digital learning environment: This year progress was made with the local version of a digital learning environment. A computer science student and an astronomy student are working on a digital learning environment in which the software manages distributed content in contrast to Nestor, which needs to keep the data in a central database. It is useful to create a system that is both flexible and user friendly. Any attempts to interest programmers working on the university wide project called the ‘webplatform’ at the ECCOO failed because of shortage of manpower. A provisional version of the software was presented at a workshop during the faculty’s ‘onderwijsdag’ at November 5th. Two other students are preparing a new set-up for the computer course. To balance the components of this course and to make the classification and weighting of the parts more flexible, they transform the subjects into modules. These modules will be used to test the new digital learning environment. Webplatform: This year finally part of our web pages were switched to the ‘Webplatform’. The Webplatform is a name for the new university system that manages the web pages of all departments using a central database and a content management system. Early this year a start was made to separate intranet- and Internet functionality. The intranet runs on our private web server and the Internet pages are uploaded to the Webplatform. These systems were coupled by developing a system that automatically uploads relevant data that needs to be visible in both systems (like lists with names and addresses). Faculty meetings for web managers were attended to participate in the process of tuning and adjusting web pages. Participants are disappointed that, already in the starting phase, there is a stagnation of the development of the Web-platform owing to money problems and organizational problems.

Organisation Central ICT management: On Thursday, October 13th there was a meeting with members of a project group that examines the possibilities to organize central ICT management to increase the level of ICT professionalism at the depart-ments. The meeting was organized and prepared, together with the Mathe-matics/Computer science department (IWI) and the goal was to inform the

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group about our machinery and ICT procedures which differ from other depart-ments. Also there was a need for information about the ideas of the people behind the centralization. Present for the project group were Kuné, Kammenga and Wind. For IWI, Botta and Paas and the Kapteyn Institute were represented by Vogelaar and van der Hulst. Both IWI and Kapteyn Institute share a history of use and development of scientific software running in a UNIX environment and it was agreed that this property should be the core of discussion. A different point of view was taken regarding centralization because there is a great deal of specialization and heavy dependence on UNIX. Also the project group’s enthusiasm for the front-office/back-office model for system management was not shared. Detailed minutes, made by the project group can be found at: www.astro.rug.nl/intranet/computing/bulletin/ CENTRALISATIE/ conckaptiwi.pdf An interesting item in the discussion was the maintenance of MS-Windows on machines used by the secretariat. Perhaps centralization can enhance support for these machines. The next step of the project group and the steering committee is awaitened. Faculty: Marike Peterzon left the ICT group at the faculty and was appointed by the ‘Rekencentrum’. Her job is taken over by Haijko Wind, but this is temporary and only for three days a week. He took the initiative to have a meeting with the computer group of the Kapteyn Instittute. Wind is also member of the project group described earlier so he already was informed about our institute and its (ICT) history. The meeting was useful and it was agreed thtat we would organize a site visit at the faculty in January 2004 to achieve better relations between the computer group of the Institute and the equivalent of the faculty. Local: After the Institute retreat in Kloosterburen it was concluded that further improvements of our interface with users shouldbe made. Trager was asked to organize user meetings and to filter the obvious wishes and remarks so that what remains can be used as action points for the computer group. The system seems to work for both users and the computer group. The system with ‘to-do’s’, howto’s and memo’s stored in a database works fine. Currently 89 howto’s exists and most 5000 page views for those pages. On top is the howto ‘how to mail a group’ with 792 page views.

Security Security award: October 22nd the computer group received the first annual security award in an official meeting at the Rekencentrum. The award was handed over by M. Kooyman, vice-chairman of the ‘College van Bestuur’. The contribution consisted of a detailed report of the problems with hackers and the process of learning about the vulnerabilities of computer systems and network. In this report a demonstratation was made that security contains many aspects which all need serious attention and that an increase on the level of security cannot be made overnight. The steps of the migration of clients machines to a ‘safe area’ protected by a firewall were described and also various tools and procedures to monitor the behaviour of machines and network. Honey pot course: Zwitser attended a course about honey-pots. Honey-pots are machines (in a honey-net) installed with standard software and connected to a special network which is monitored very carefully. The set-up is used to demonstrate that machines that are not up to date and protected by a firewall

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are hacked within days, sometimes within hours. One of the conclusions of this course was that probably a significant part of the machinery at the RUG is hacked, unnoticed by system managers, but common knowledge for a small but very active group of “exchangers” of games, music, images and movies.

Linux 103 Solaris 2 HP 0 MS-Windows 8 Distribution of platforms in 2003

3.8 Instrumentation

VISIR, the mid-infrared imager and spectrometer for the ESO-VLT In 2003 the VISIR project recovered from the technical problems that led to serious delays in the previous year. The extensive program of cold laboratory tests and calibrations was completed in November 2003 and the 'Preliminary Acceptance Europe' (PAE) process started in October. At the time of writing (early March 2004) the PAE milestone has been passed and the green light for transport of the instrument to the VLT has been given. Air transport of the fully integrated instrument and all periferal equipment (nearly 10 tons of sensitive hardware!) to Santiago de Chile is foreseen for the third week of March 2004. After post-transport checks and installation of VISIR in the cassegrain focus of the third 8-meter telescope ('Melipal'), the first commissioning run will start in the last week of April. A second run will follow later in the summer of 2004. As key members of the VISIR commissioning team Pel (P.I. for the VISIR spectrometer) and Peletier will participate in all parts of the commisioning and 'science verification' tests on Cerro Paranal. Provided that the commissioning plan works out successfully, VISIR can become available for the general user community in the fall of 2004. More details on VISIR can be found in previous annual reports and in the VISIR webpages at ASTRON (http://www.astron.nl/visir/).

MIRI, the mid-infrared instrument for the JWST MIRI is the mid-infrared imager/spectrometer for the James Webb Space Telescope (JWST), the 6.5-meter telescope that will replace 'Hubble' in 2011. The three JWST instruments NIRCAM, NIRSPEC and MIRI will operate in the visual and infrared (wavelengths 0.6 to 28 microns). Especially in the infrared, the combination of the large telescope aperture, diffraction-limited optics, low background (JWST will orbit around the L2 libration point, 1.5 million kilometers from the Earth) and highly improved detector performance will surpass the resolution and sensitivity of previous instruments by orders of magnitude.

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MIRI is being developed by a large international consortium of institutes in Europe and the USA. The European consortium members organized their own national funding, but they work under the supervision of ESA, which also acts as interface to NASA. In 2003 the composition of the European consortium changed significantly. Due to funding difficulties Italy had to withdraw, but Spain, Belgium, Switzerland and Denmark joined the existing European group (UK, Germany, France, Netherlands, Sweden, Ireland). The spectrometer subsystem of MIRI is responsibility of the UK/Netherlands /Germany collaboration, with smaller contributions from Sweden/Ireland. The Dutch MIRI budget of 9.4 MEuro is funded by NWO/NOVA with 'in kind' contributions from the university astronomical institutes and ASTRON. Overall PI for the spectrometer is G. Wright (ROE/ATC, Edinburgh). E. van Dishoeck (RUL) is Dutch co-PI and R. Jager (SRON) is NL project manager, stationed at ASTRON (Dwingeloo), where most of the hardware design and manufacture takes place. In Groningen Tielens and De Graauw are members of the NL MIRI science team and Pel is NL instrument scientist. In April 2003 MIRI entered the 'Phase B' detailed design phase. This is now well under way. The spectrometer optical design, a major contribution from TNO-TPD in Delft, is now frozen and most design choices in the opto-mechanical design (mainly ASTRON effort) have been made. Detailed design has started, ordering of components and manufacturing will follow soon. In August 2005 the 'verification model' of the spectrometer has to be ready for delivery to the Rutherford-Appleton Lab. in the UK for integration and testing. Delivery of the complete imager+spectrometer 'flight module' by the European consortium to NASA is planned for end 2007. For more details on the MIRI project see previous Annual Reports and the MIRI pages of the ASTRON website (http://www.astron.nl/miri).

Preparing Wide field Surveys with OmegaCAM Several meetings and workshops were held to discuss future observing programmes for the Guaranteed Time of OmegaCAM. At the Lorentz center in Leiden an international workshop was held, June 30 – July 2, 2003. Staff of the Kapteyn institute (Heraudeau, Trager, Valentijn, van de Weijgaert) presented an extensive observing programme of nearby superclusters, starting with a deep 10 square degree survey of the Hercules supercluster and extending this with a large 100 square degree survey of the Horologium supercluster. This multispectral study also involves X-ray XMM observations (Kaastra) and WSRT HI observations (Verheyen, van Gorkom). Within the framework of the EU RTN network SISCO (Spectroscopic and Imaging Surveys for Cosmology), in which OmegaCEN is participating, a new collaboration with Italian colleagues (Busarello, Merluzzi) at the Observatorio di Capodimonte has been initiated for the supercluster programme.

OmegaCEN The Kapteyn Institute hosts OmegaCEN, an Astronomical Data enter sup-porting WIDE-FIELD astronomical imaging. The center is building and supporting an advanced survey system: the VIRTUAL SURVEY TELESCOPE. OmegaCEN is an initiative of NOVA, supporting NOVA's instrumentation

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programme, in particular OmegaCAM. In 2003 the center has installed a new generation of hardware including several 2 Terabyte disk towers and computers used for own developed fileserver and Oracle database server. A new colla-boration with the RuG Rekencentrum HPC (High Performance Computing) was initiated, and OmegaCENs hardware was connected with glass-switches and glass fibres to the Linux parallel cluster at the Rekencentrum. Linux cluster, Oracle server, disk towers and local compute servers together with the users are connected in a peer-to-peer network. On 12 April the center celebrated its "first virtual light" when this new infrastructure was successfully charged with the Astro-Wise software which connects the user to this integrated archive, mass-storage, "everything overlooking database" and pipeline processing system. In this concept the user, by asking questions, triggers manipulations of the system, the result is not necessarily transferred to the user. The first light served as a proof of concept of a new approach to handling astronomical data, and was stimulating the whole team.

Figure 8: OmegaCEN team celebrates first virtual light http://www.astro.rug.nl/~omegacen/staff.html

Leading a European Wide field imaging data analysis system - Astro-Wise OmegaCEN is also leading the European Research and Technical Develop-ment program Astro-Wise. During the second year of Astro-Wise the project plan as outlined in the contract has been continued. Following the plan for Phase II of the project, a prototype of the AstroWise system has been imple-mented. An evaluation took place of the proto-type underlying pipeline, as

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delivered by WP1. At an AstroWise workshop in November at Groningen, "Developer and advanced user tutorials on Photometric Pipelines and quality control", this prototype was reviewed and a set of modification of class defini-tions was settled. Hardware for WP3 (disk storage) and WP4 (computers) have been implemented at various nodes. The central database systems have been put into operation (WP3) and a new preliminary version of the visualization tool has been delivered (WP2). The software development for the Astro-Wise project is well on schedule. At the JENAM (Joint European National Meeting) conference in Budapest Valentijn gave a invited presentation how to use the Astro-Wise system and the OmegaCAM camera for monitoring variable objects.

Figure 9: http://www.astro.rug.nl/~omegacen/Network-900p.jpg

OmegaCAM Due to delays with the delivery of the dewar and the detector system of OmegaCAM, made by ESO, and the VST (VLT Survey Telescope) the planned delivery of the OmegaCAM's calibration and data reduction system to ESO was shifted to the next year. The development of a new flatfielding technique was completed successfully. The OmegaCEN group tested the OmegaCAM software extensively on WFI@2.2m data and because of the delays with OmegaCAM decided to provide a full WFI@2.2m wide field imaging pipeline to its users. This pipeline is used for small scientific projects and also for Omega-CAM preparatory programmes aiming to settle secondary photometric standards. To this end, another observing campaign on the Wide-Field Camera on the Isaac Newton Telescope/La Palma was completed (Kuijken, Valentijn, Vermeij).

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The last observing run in this series allows the construction of one square degree standard star fields suitable for the calibration of the OmegaCAM instrument. The reduction of the data obtained in these runs is nearly complete.

Receiver development for ALMA – the Atacama Large Millimeter Array and the Champ multi-mixer array ALMA The two groups, which carry out the technical development work for the high frequency ALMA band 9 (602 to 720 GHz), are: at Kapteyn Institute/NOVA/ SRON in Groningen (A. Baryshev, R. Hesper, G. Gerlofsma, J. Adema, H. Schaeffer, B.D. Jackson, A. Koops), and at DIMES (Delft Institute of Micro-electronics and Submicron Technology) (T. Zijlstra, M. Kroug, T. Klapwijk). The work was funded by NOVA. A contract with ESO (European Southern Obser-vatory) is almost signed. ESO approved the funding for the European part of the ALMA project and several work packages were defined. The contract was changed from a prototype contract into a larger 8 pre-production contract. Our group presented a proposal, describing building and testing of the eight Band 9 receivers, to ESO. The project aims to build 64 antennas. Industrialization of the manufacturing process is needed. Most of the mechanical design work was outsourced to MECON in Doetinchem. Fine mechanical work was often done by WITEC in Ter Apel. The optical design remains within the group. Testing: Mixer testing was improved a lot: It is now fully automated. Testing can be completed within 2 hours, which used to be a few days with one person constantly present. After the cartridge is assembled it needs to be tested. The National Astronomical Observatory of Japan (NAOJ) supplied a test cryostat, which was installed in Groningen. For testing. For handling and measurement of fine mechanical components, a precision alignment and mounting set-up was procured. It still suffers a few imperfections, but can be used now. IF Bandwidth: Extending the IF bandwidth from 4-8 GHz to 4-12 GHz is almost completed. The most difficult part was the isolator, but the performance of the Pamtech version is now almost within spec. Junctions: These are the core of the receiver. They are produced in the Group of Teun Klapwijk in Delft. A few iterations have been made. A new batch of NiTiN junctions were received and tested. The performance appeared to be good. Mixer: A critical part is the mixer. It contains a few mechanical high precision components: Backpiece and horn. After close collaboration with industry the components needed, can now be ordered industrially. LO-Quintupler: A mixer has to be pumped by a local oscillator. The last stage of this LO is critical. A quintupler (multiplies the frequency 5 times to the 600-720 GHz range) is being developed. A fruitful collaboration with the NROA in the USA was realized on this topic, where the Band 9 group mainly helped in testing the units. Integrated optics/mirrors: It was decided that the mirrors should be made out of one aluminium block as possible and rely on CNC milling accuracy (see Figure 10). The reason for this is to minimize the amount of components and avoid elaborate aligning of mirrors. The concept was proved with two mirror system, with one coupling interface. The CNC quality appeared to be able to

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get close to optical quality. We could even make an ‘optical’ picture of the focussing quality with a HeNe laser: See Figure 11.

Figure 10: ALMA Integrated mirror concept.

Figure 11: ALMA ‘Optical’ focusing of sub-mm mirrors.

CHAMP The ALMA group is also involved in the CHAMP+ project. It requires manufacturing of two focal plane mixers arrays, each containing 7 mixers, for the frequency ranges 600–720 and 780–950 GHz. The Mixer design is largely

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similar to ALMA prototype and will be produced industrially as much as possible. This work is done in collaboration with MPI Bonn. The project is getting close to completion. Most components have been ordered. We have now entered the assembly phase.

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APPENDIX I : PUBLICATIONS 2003

I.1 Papers in scientific journals, books

Argo, M.K. et al. (including de Bruyn, A.G.), CLASS B0445+123: a new two-

image gravitational lens system, Mon. Not. Roy. Astron. Soc. 338, 957–961, 2003.

Bemmel, I.M. van, Dullemond, C.P., New radiative transfer models for

obscuring tori in active galaxies, Astron. Astrophys. 404, 1–19, 2003. Bernard-Salas, J., Pottasch, S.R., Beintema, D.A., Wesselius, P.R., Erratum:

The ISO-SWS spectrum of planetary nebula NGC 7027, Astron. Astrophys. 406, 175, 2003.

Bernard-Salas, J., Pottasch, S.R., Wesselius, P.R., Feibelman, W.A.,

Abundances of planetary nebulae BD+30 3639 and NGC 6543, Astron. Astrophys. 406, 165–174, 2003.

Biggs, A.D., et al. (including de Bruyn, A.G.), 0850+054: a new gravitational

lens system from CLASS, Mon. Not. Roy. Astron. Soc. 338, 1084–1088, 2003.

Bignall, H.E., Jauncey, D.L., Lovell, J.E.J., Tzioumis, A.K., Kedziora-Chudczer,

L., Macquart, J.-P., Tingay, S.J., Rayner, D.P., Clay, R.W., Rapid Variability and Annual Cycles in the Characteristic Timescale of the Scintillating Source PKS 1257-326, Astrophys. J. 585, 653–664, 2003.

Bottema, R., Simulations of normal spiral galaxies, Mon. Not. Roy. Astron.

Soc. 344, pp. 358-384, 2003. Browne, I.W.A. et al. (including de Bruyn, A.G., Koopmans, L.V.E.), The

cosmic lens all-sky survey – II. Gravitational lens candidate selection and follow-up, Mon. Not. Roy. Astron. Soc. 341, 13–32, 2003.

Cappellaro, E., Baruffolo, A., Cascone, E., Greggio, L., Kuijken, K., Bender, R.,

Muschielok, B., Iwert, O., Mitsch, W., Nicklas, H., Valentijn, E.A., OmegaCAM at the VLT Survey Telescope, Memorie della Societa Astronomica Italiana 74, p. 967, 2003.

Castro-Rodríguez, N., Aguerri, J.A.L., Arnaboldi, M., Gerhard, O., Freeman,

K.C., Napolitano, N.R., Capaccioli, M., Narrow band survey for intragroup light in the Leo HI cloud. Constraints on the galaxy background

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contamination in imaging surveys for intracluster planetary nebulae, Astron. Astrophys. 405, 803–812, 2003.

Cazaux, S., Tielens, A.G.G.M., Ceccarelli, C., Castets, A., Wakelam, V., Caux,

E., Parise, B., Teyssier, D., The hot core around the low-mass protostar IRAS 16293-2422: Scoundrels Rule!, Astrophys. J. 593, L51–55, 2003.

Ceccarelli, C., Maret, S., Tielens, A.G.G.M., Castets, A., Caux, E., Theoretical

H2CO emission from protostellar envelopes, Astron. Astrophys. 410, 587–595, 2003.

Chengalur, J.N., Kanekar, N., Widespread acetaldehyde near the Galactic

Centre, Astron. Astrophys. 403, L43–46, 2003. Chengalur, J.N., Kanekar, N., Constraining the variation of fundamental

constants using 18cm OH lines, Physical Review Letters 91, id. 241302, 2003.

Choloniewski, J., Valentijn, E.A., Extinction in the galaxy from surface

brightnesses of ESO-LV galaxies: Determination of AR/AB ratio, Acta Astro-nomica 53, 249–264, 2003.

Choloniewski, J., Valentijn, E.A., Extinction in the galaxy from surface

brightnesses of ESO-LV galaxies: Testing "standard" extinction maps, Acta Astronomica 53, 265–280, 2003.

Dennett-Thorpe, J., de Bruyn, A.G., Annual modulation in the scattering of

J1819+3845: Peculiar plasma velocity and anisotropy, Astron. Astrophys. 404, 113–132, 2003.

Dolphin, A.E., Saha, A., Skillman, E.D., Dohm-Palmer, R.C., Tolstoy, E., Cole,

A.A., Gallagher, J.S., Hoessel, J.G., Mateo, M., Deep Hubble Space telescope imaging of Sextans A. III. The star formation history, Astron. J. 126, 187–196, 2003.

Dolphin, A.E., Saha, A., Skillman, E.D., Dohm-Palmer, R.C., Tolstoy, E., Cole,

A.A., Gallagher, J.S., Hoessel, J.G., Mateo, M., Deep Hubble Space telescope Imaging of Sextans A. II. Cepheids and distance, Astron. J. 125, 1261–1290, 2003.

Dominik, C., Dullemond, C.P., Cami, J., van Winckel, H., The dust disk of HR

4049. Another brick in the wall, Astron. Astrophys. 397, 595–609, 2003. Filho, M.E., Barthel, P.D., Ho, L.C., Erratum: The Radio properties of

composite LINER/HII galaxies, Astrophys. J. Suppl. Series 144, 211, 2003. González-García, A.C., Albada, T.S. van, Mergers between elliptical galaxies

and the thickening of the Fundamental Plane, Mon. Not. Roy. Astron. Soc. 342, L36, 2003.

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Harwit, Martin, Spaans, Marco, Chemical composition of the Early Universe, Astrophys. J. 589, 53–57, 2003.

Haverkorn, M., Katgert, P., de Bruyn, A.G., Characteristics of the structure in

the Galactic polarized radio background at 350 MHz, Astron. Astrophys. 403, 1045–1057, 2003.

Haverkorn, M., Katgert, P., de Bruyn, A.G., Multi-frequency polarimetry of the

Galactic radio background around 350 MHz. I. A region in Auriga around l = 161 deg, b = 16 deg, Astron. Astrophys. 403, 1031–1044, 2003.

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Extinction in Spiral Disks, Bull. American Astron. Soc. (203rd Meeting of the American Astronomical Society) #114.04, 2003.

Hony, Sacha, Tielens, Xander, Waters, Rens, de Koter, Alex, Dust around C-

rich post-AGB objects, in: Astrophysics of Dust (ed. Adolf N. Witt), Estes Park, Colorado, May 2003, p. 60, 2003.

Hony, Sacha, Waters, Rens, Tielens, Xander, MgS grains around C-rich old

stars, in: Astrophysics of Dust (ed. Adolf N. Witt), Estes Park, Colorado, May 2003, p. 61, 2003.

Huygen, R., Boxhoorn, D., Roelfsema, P.R., Sym, N., Vandenbussche, B.,

Wieprecht, E., SWS CoCo: Lessons learned about Disturbed Multi-Platform

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Software Development and Configuration control, in: The Calibration legacy of the ISO Mission (eds. L. Metcalfe, A. Salama, S.B. Peschke and M.F. Kessler), Proc. ESA Conf. (Feb., 2001), ESA Publications Series, ES SP-481, 2003.

Jauncey, D.L., Bignall, H.E., Lovell, J.E.J., Kedziora-Chudczer, L., Tzioumis,

A.K., Macquart, J.-P., Rickett, B.J. Interstellar Scintillation and Radio Intra-Day Variability, in: Radio Astronomy at the Fringe (eds. J. Anton Zensus, Marshall H. Cohen and Eduardo Ros), ASP Conf. Proc. Vol. 300 (Nat. Radio Astron. Obs. (NRAO), Green Bank, USA), p. 199, San Francisco: Astron. Soc. of the Pacific, 2003.

Jong, J.T.A. de, Sackett, P., Kuijken, K., Uglesich, R., Crotts, A., Sutherland,

W., Microlensing in M31, preliminary lightcurves from MEGA, in: The Dark Universe: Matter, Energy and Gravity (ed. M. Livio), Poster Papers STScI Symp. (Baltimore, April 2001), p.18–21, 2003.

Keane, J.V., Pendleton, Y.V., Allamandola, L.J., Spoon, H.W.W., Tielens,

A.G.G.M., Carbonaceous material in dusty galactic nuclei, in: Astrophysics of Dust (ed. Adolf N. Witt), Estes Park, Colorado, May 2003, p. 44, 2003.

Kedziora-Chudczer, L., Rickett, B.J., Bignall, H.E., Jauncey, D.L., Lovell, J.E.J.,

Tzioumis, A.K., Macquart, J.-P., Seeing the cores of active galaxies in the sharpest detail, in: Radio Astronomy at the Fringe (eds. J. Anton Zensus, Marshall H. Cohen and Eduardo Ros), ASP Conf. Proc. Vol. 300 (Nat. Radio Astron. Obs. (NRAO), Green Bank, West Virginia, USA), p. 211, San Francisco: Astron. Soc. Of the Pacific, 2003.

Kemper, F., Tielens, A.G.G.M., The crystallinity of interstellar silicates, in:

Astrophysics of Dust (ed. Adolf N. Witt), Estes Park, Colorado, May 2003, p. 144, 2003.

Kraemer, K.E., Price, S.D., Sloan, G.C., Walker, H.J., Shipman, R.F., An atlas

of full-grating short wavelength spectrometer spectra: classification and processing, in: Exploiting the ISO Data Archive. Infrared Astronomy in the Internet Age (eds. C. Gry, S. Peschke, J. Matagne, P. Garcia-Lario, R. Lorente, & A. Salama) (Siguenza, Spain,June 2002), ESA Publ. Series, ESA SP-511, p. 63, 2003.

Kraft, S., Collon, M., Montella, J., Buis, E.J., Beijersbergen, M., Erd, C.,

Falkner, P., Schulz, R., Peacock, A., On the concepts of a highly integrated payload suite for use in future planetary missions: the example of the BepiColombo Mercury Planetary Orbiter, in: Low-Cost Planetary Missions (compiled by R.A. Harris), Proc. Fifth IAA International Conf. (Sept. 2003, Noordwijk, The Netherlands), ESA SP-542, pp. 219-226, ESA Publications Division, Noordwijk, the Netherlands, 2003.

Kuijken, K., The Mass of the Milky Way, in: The Mass of Galaxies at Low and

High Redshift, ESO Workshop Proc. (Venice, Italy, Oct. 2001), p. 1, 2003.

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Labbé, I., Franx, M., Rudnick, G., Moorwood, A., Förster Schreiber, N., Rix, H.-W., van Starkenburg, L., van Dokkum, P., van der Werf, P., Röttgering, H., Kuijken, K., Ultradeep Near-Infrared ISAAC Observations of the Hubble Deep Field South: Selecting High-Redshift Galaxies in the Rest-Frame Optical, in: The Mass of Galaxies at Low and High Redshift, ESO Workshop Proc. (Venice, Italy, Oct. 2001), p. 256, 2003.

Lagage, P.O., Pel, J.W., Damstra, S., Dubreuil, D., Durand, G.A., Elswijk, E.,

Galdemard, P., Jong, A.N. de, Kroes, G., Lyraud, C., Pantin, E., Pragt, J., Rio, Y., Schoenmaker, A.A., Characterization in the Laboratory of VISIR, the Mid-Infrared Imager and Spectrometer for the VLT, in: Instrument Design and Performance for Optical/Infrared Ground-Based Telescopes’ (eds. M. Iye, A. Moorwood), 2002 SPIE Conf. Proc. Vol. 4841, pp. 923–931, 2003.

Lahuis, F., Feuchtgruber, H., Golstein, H., Kester, D., Luinge, W., Shipman,

R.F., Wieprecht, E., SWS Signal Capture: from Flux to Signal, in: The Calibration legacy of the ISO Mission (eds. L. Metcalfe, A. Salama, S.B. Peschke and M.F. Kessler), Proc. ESA Conf. (Feb. 2001), ESA Publications Series, ESA SP-481, p. 387, 2003.

Lovell, J.E.J., Jauncey, D.L., Tzioumis, A.K., Bignall, H.E., Kedziora-Chudczer,

L., Macquart, J.-P., Rickett, B.J., The micro-arcsecond scintillation-induced variability (MASIV) VLA survey, in: Active Galactic Nuclei: from Central Engine to Host Galaxy (eds. S. Collin, F. Combes and I. Shlosman), ASP Conf. Series Vol. 290 (Meudon, France, July 2002), p. 347, San Francisco: Astron. Soc. of the Pacific, 2003.

Macquart, J.-P., Circular polarization in relativistic jets, New Astronomy

Reviews Vol. 47, pp. 609–612, 2003. Macquart, J.-P., de Bruyn, A.G.. Dennett-Thorpe, J., The micro-arcsecond

properties of J1819+385, in: Active Galactic Nuclei: from Central Engine to Host Galaxy (eds. S. Collin, F. Combes and I. Shlosman), ASP Conf. Series Vol. 290 (Meudon, France, July 2002), p. 349, San Francisco: Astron. Soc. of the Pacific, 2003.

Macquart, J.-P., Wu, K., Hannikainen, D.C., Sault, R.J., Jauncey, D.L.,

Similarities between circular polarization in galactic jet sources and AGN, Astrophys. Space Science Vol. 288, pp. 105–119, 2003.

Möller, O., Hewett, P., Blain, A., Detecting Disc-Like Structures in Early-Type

Galaxies with Lensing, in:The Mass of Galaxies at Low and High Redshift, ESO Workshop Proc. (Venice, Italy, Oct. 2001), p. 196, 2003.

Peeters, E., Tielens, A.G.G.M., Allamandola, L.J., Bauschlicher, C.W.,

Boogert, A.C.A., Hayward, T.L., Hudgins, D.M., Sandford, S.A., The detection of new dust-related IR emission features, in: Astrophysics of Dust (ed. Adolf N. Witt), Estes Park, Colorado, May 2003, p. 42, 2003.

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Peeters, E., van Diedenhoven, B., van Kerckhoven, C., Hony, S., Tielens, A.G.G.M., Allamandola, L.J., Hudgins, D.M., Bauschlicher, C.W., Profile variations of the 3 to 12 micron PAH features, in: Astrophysics of Dust (ed. Adolf N. Witt), Estes Park, Colorado, May 2003, p. 41, 2003.

Pihlström, Y.M., Baan, W.A., Darling, J., Klöckner, H.-R., OH Maser Disks and

Outflows in ULIRGs: VLBA Observations of two IRAS Galaxies, Bull. American Astron. Soc. (203rd Meeting of the American Astronomical Society) #146.02, 2003.

Pottasch, S.R., Beintema, D.A., Bernard Salas, J., Feibelman, W.A.,

Abundances in Planetary Nebulae: Including ISO Results, in: Planetary Nebulae; Their Evolution and Role in the Universe (eds. S. Kwok, M. Dopita, R. Sutherland), IAU Symp. 209 (Canberra, Australia, Nov. 2001), Publ. of the Astron. Soc. of the Pacific, p. 353, 2003.

Roelfsema, P.R. et al. (including Valentijn, E.A., Boxhoorn, D.R., Graauw, T.

de, Shipman, R.F.), The ISO SWS Calibration: Strategy and Lessons Learned, in: The Calibration legacy of the ISO Mission (eds. L. Metcalfe, A. Salama, S.B. Peschke and M.F. Kessler), Proc. ESA Conf. (Feb. 2001), ESA Publications Series, ES SP-481, p. 31, 2003.

Romanowsky, A.J., Douglas, N.G., Kuijken, K., Arnaboldi, M., Gerssen, J.,

Merrifield, M.R., Modern Techniques in Galaxy Kinematics: Results from Planetary Nebula Spectroscopy, in: Planetary Nebulae; Their Evolution and Role in the Universe (eds. S. Kwok, M. Dopita, R. Sutherland), IAU Symp. 209 (Canberra, Australia, Nov. 2001), Publ. Of the Astron. Soc. of the Pacific, p. 639, 2003.

Romanowsky, A.J., Douglas, N.G., Kuijken, K., Arnaboldi, M., Kissler-Patig,

M., Sharples, R.M., Zepf, S.E., Rhode, K.L., Dynamics of Stars and Globular Clusters in Galaxy Halos, in: Extragalactic Globular Cluster Systems (ed. M. Kissler-Patig), ESO Workshop Proc. (Garching, Germany, August 2002), p. 310, Springer-Verlag, 2003.

Romanowsky, A.J., Douglas, N.G., Kuijken, K., Merrifield, M.R., Arnaboldi,

M., Freeman, K.C., Taylor, K., Mass Distributions in Early-Type Galaxy Halos, in: The Mass of Galaxies at Low and High Redshift, ESO Workshop Proc. (Venice, Italy, Oct. 2001), p. 72, 2003.

Romanowsky, A.J., Douglas, N.G., Kuijken, K., Merrifield, M.R., Arnaboldi,

M., Merrett, H., Napolitano, N.R., Capaccioli, M., Freeman, K.C., Bergond, G., Sharples, R.M., Zepf, S.E., Rhode, K.L., Halo Tracers in Nearby Galaxies, Bull. American Astron. Soc. (203rd Meeting of the American Astronomical Society), #65.05, 2003.

Röttgering, H., de Bruyn, A.G., Fender, R.P., Kuijpers, J., van Haarlem, M.P.,

Johnston-Hollitt, M., Miley, G.K., LOFAR: a new radio telescope for low frequency radio observations: science and project status, in: Active Galactic Nuclei: from Central Engine to Host Galaxy (eds. S. Collin, F. Combes and

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I. Shlosman), ASP Conf. Series Vol. 290 (Meudon, France, July 2002), p. 349, San Francisco: Astron. Soc. of the Pacific, 2003.

Sanders, R.H., Modified Newtonian dynamics and its implications, in: The dark

universe: matter, energy and gravity (ed. Mario Livio), Proc. STScI Symp. Series Vol. 15 (Baltimore, April 2001), pp. 62-76, Cambridge University Press, Cambridge UK, 2003.

Sandford, S.A., et al (including Tielens, A.G.G.M.), Organics in the solar

system and the Astrobiology Explorer (ABE) mission, Bull. American Astron. Soc. (203rd Meeting of the American Astronomical Society), DPS meeting #35,, #41.09, 2003.

Schaap, W.E., and Weygaert, R. van de, Delaunay Recovery of Cosmic

Density and Velocity Probes, in: Statistical Challenges in Astronomy. Third Statistical Challenges in Modern Astronomy (SCMA III) Conf. (eds. E.D. Feigelson & G.J. Babu) (University Park, July 2001), pp. 483–484, New York: Springer-Verlag, 2003.

Setia Gunawan, D.Y.A., Chapman, J.M., Stevens, I.R., Rauw, G., Leitherer,

C., Radio continuum observations of massive stars in open cluster NGC 6231 and the Sco OB1 association, in: A Massive Star Odyssey: From Main Sequence to Supernova (eds. Karel van der Hucht, Artemio Herrero, and Esteban, César), Proc. IAU Symp. 212 (Lanzarote, Canary islands, Spain, June 2001), p. 230, San Francisco: Astron. Soc. of the Pacific, 2003.

Shipman, R.F., et al. (including Boxhoorn, D., Roelfsema, P., Valentijn, E.),

SWS In-flight Calibration, in: The Calibration legacy of the ISO Mission (eds. L. Metcalfe, A. Salama, S.B. Peschke and M.F. Kessler), Proc. ESA Conf. (Feb., 2001), ESA Publications Series, ES SP-481, p. 107, European Space Agency, 2003.

Shipman, R.F., Frieswijk, W., Helmich, F.P., Infrared Dark Clouds Toward

W51, in: Galactic Star Formation Across the Stellar Mass Spectrum (eds. James M. De Buizer and Nicole S. van der Bliek), Proc. IAO Chile (March 2002), ASP Conf. Series Vol. 287, pp. 252-256, San Francisco: Astron. Soc. of the Pacific, 2003.

Sterken, C., Fu, J.N., Brogt,E., BQ Ind: a double-mode SX Phoenicis star?, in:

Interplay of Periodic, Cyclic and Stochastic Variability in Selected Areas of the H-R Diagram (ed. C. Sterken), ASP Conf. Series Vol. 292, p.121, San Francisco: Astron. Soc. of the Pacific, 2003.

Tolstoy, E., Stellar populations in dwarf galaxies: A review of the contribution

of HST to our understanding of the nearby universe, in: A decade of Hubble Space Telescope science (eds. Mario Livio, Keith Noll, Massimo Stiavelli), Proc. STScI Symp. (Baltimore, MD, USA, April 11-14, 2000), STScI symp. series Vol. 14, pp. 128–152, Cambridge Univ. Press Cambridge UK, 2003.

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Tolstoy, E., Dwarf Galaxies: Important Clues to Galaxy Formation, in: Galaxy Evolution III: From Simple Approaches to Self-Consistent Models (eds. G. Hensler et al.), Conf. Proc., Astrophys. and Space Science Vol. 284, pp. 579–588, 2003.

Tolstoy, Eline, UVES Abundances of Stars in Nearby Galaxies: How Good are

Theoretical Isochrones? in: New Horizons in Globular Cluster Astronomy (eds. G. Piotto, G. Meylan, G. Djorgovski, & M. Riello), ASP Conf. Proc. Vol. 296 (Padua, June 2002), p. 234, San Francisco: Astron. Soc. of the Pacific 2003.

Vandenbussche,B., et al. (including Valentijn, E.A., Boxhoorn, D.R., Graauw

de, T.,Roelfsema, P., Shipman , R.F.), The Relative Spectral Response Calibration of the ISO-SWS, in: The Calibration legacy of the ISO Mission (eds. L. Metcalfe, A. Salama, S.B. Peschke and M.F. Kessler), Proc. ESA Conf. (Feb 5-9, 2001), ESA Publications Series, ESA SP-481, p. 455, European Space Agency, 2003.

Venn, K.A., Kaufer, A., Tolstoy, E., Kudritzki, R.-P., Przybilla, N., Smartt, S.J.,

Lennon, D.J., Chemical abundances of massive stars in Local Group galaxies, in: A Massive Star Odyssey: From Main Sequence to Supernova (eds. Karel van der Hucht, Artemio Herrero, and Esteban, César), IAU Symp. 212 (Lanzarote, Spain, June 2001), p. 30, San Francisco: Astron. Soc. of the Pacific, 2003.

Wells, M., Pel, J.W., Schoenmaker, A.A., Wright, G.S., Hastings, P., Design

for the 5-28 um NGST MIRI Spectroscopy Channel, in: Infrared Space Telescopes and Instruments (ed. J.C. Mather), 2002 SPIE Conf. Proc. 4850, pp. 504–516, 2003.

Weygaert, R. van de, Statistics of Galaxy Clustering - Commentary, in:

Statistical Challenges in Astronomy (eds E.D. Feigelson and G.J. Babu), p. 156, 2003.

Weygaert, R. van de, The cosmic foam: stochastic geometry and spatial

clustering across the universe, in: Statistical Challenges in Astronomy. Third Statistical Challenges in Modern Astronomy (SCMA III) Conf. (eds. E.D. Feigelson & G.J. Babu) (University Park, July 2001), pp. 175–196, New York: Springer-Verlag, 2003.

Wieprecht, E., et al. (including Boxhoorn, D., Roelfsema, P., Shipman, R.F.,

Valentijn, E.), The ISO SWS Data Analyses Software Systems, in: The Calibration legacy of the ISO Mission (eds. L. Metcalfe, A. Salama, S.B. Peschke and M.F. Kessler), Proc. ESA Conf. (Feb., 2001), ESA Publications Series, ESA SP-481, p. 285, European Space Agency, 2003.

Wright, G.S., Bortoletto, F., Bruce, C.F., Dishoeck, E. van, Karnik, A.R.,

Lagage, P.O., Larson, M.E., Lemke, D., Olofsson, G., Miller, E.A., Pel, J.W., Henning, T.F., Ray, T., Rodriguez, J., Walters, I., The NGST MIRI

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Instrument, in: Infrared Space Telescopes and Instruments (ed. J.C. Mather), 2002 SPIE Conf. Proc. 4850, pp. 493–503, 2003.

I.3 Dissertations

Beijersbergen, Marco, The Galaxy Population in the Coma Cluster, Promotor: Prof. Dr. J.M. van der Hulst, beoordelingscommissie: Prof. Dr. P.C. van der Kruit, Prof. Dr. R. Sancisi, Prof. Dr. F.H. Briggs, Proefschrift Faculteit Wiskunde en Natuurwetenschappen, Rijksuniversiteit Groningen (06-01-2003), 153 pgs., 2003.

Bernard-Salas, J., Physics and Chemistry of Gas in Planetary Nebulae

Promotor: Prof. Dr. A.G.G.M. Tielens, co-promotor: Dr. P.R. Wesselius, Proefschrift Faculteit Wiskunde en Natuurwetenschappen, Rijksuniversiteit Groningen, 175 pgs., 2003.

Filho, Mercedes E., Nuclear Activity in Nearby Galaxies, Promotor: Prof. Dr.

J.M. van der Hulst, co-promotores: Dr. P.D. Barthel, Dr. L.C. Ho, Proefschrift Faculteit Wiskunde en Natuurwetenschappen, Rijksuniversiteit Groningen (09-05-2003), 170 pgs., 2003.

González-García, A.C., Elliptical Galaxies: Merger Simulations & The

Fundamental Plane, Proefschrift Faculteit Wiskunde en Natuurweten-schappen, Rijksuniversiteit Groningen (28-03-2003), 195 pgs., 2003.

Kregel, Michiel, Structure and Kinematics of Edge-on Galaxy Disks, 1e

promotor: Prof. Dr. P.C. van der Kruit, 2e promotor: Prof. Dr. K.C. Freeman, Proefschrift Faculteit Wiskunde en Natuurwetenschappen, Rijksuniversiteit Groningen (17-11-2003), 211 pgs., 2003.

Spoon, Henrik Mid-Infrared Spectroscopy of Dusty Galactic Nuclei,

Proefschrift Faculteit Wiskunde en Natuurwetenschappen, Rijksuniversiteit Groningen (20-10-2003), 178 pgs., 2003.

I.4 Reports, popular articles

Barthel, P., Actieve stelsels in de achtertuin, Zenit, May, p. 201, 2003. Barthel, P.D. (eindred. Ned. Editie), De serie ESA/ESO Astronomische

Practica, verschenen op CD-Rom, 2003. Barthel, P.D., Three Dusty Beauties, ESO Press Release, Dec. 19 , 2003. Brentjens, M.A., LOFAR, een gloednieuwe radiotelescoop, Zenit, Sept, p. 378

2003.

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Comello, Georg, Rho Cassiopeiae - de hyperreus, in: Sterrengids 2004 (Matt Drummen en Jan Meeus), Stichting "De Koepel", in opdracht van de Koninklijke Nederlandse Vereniging voor Weer- en Sterrenkunde, p. 144–146, 2003.

Douglas, N.G., De Kleine Groene Reus, Zenit, July/August, 2003. Woerden, H. van, Harm Habing and the Outer Arm of the Milky Way, in: CD

Amicorum for Harm Habing, 2003.

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APPENDIX II : Participation in scientific meetings

201st Meeting of the American Astronomical Society (Seattle, USA; 6–9 Jan. ’03): B.W. Holwerda (poster: “Dust absorption in spiral galaxies from counts of background objects” – B.W. Holwerda, R.J. Allen, and P.C. van der Kruit). Winter School “Gravitational Lensing – a unique tool for cosmology” (Aussois, France; 5–11 Jan. ’03): F. Christen, K.H. Kuijken (inv. contr.: “Basics of Gravitational Lensing”), O. Möller (inv. review: “Weak lensing by groups and galaxies”). RAS Meeting (London, UK; 9–11 Jan. ’03): E. Tolstoy (Inv. review: “Nucleosynthesis and early chemical evolution in galaxies”). Dutch Astronomer’s Club Spring Meeting (Groningen; 10 Jan. ’03): A.M.N. Ferguson (“A giant stellar structure that surrounds the Milky Way”), Several staff members of the Kapteyn Institute. Workshop “Testing cosmological models with galaxy clusters” (Ringberg, Germany; 12–16 Jan. ’03): R. van de Weijgaert (inv. contr.: “Constraining and reconstructing cosmic large scale structure”). Aspen Winter Workshop “The Baryonic Universe” (Aspen, USA; 12–18 Jan. ’03): J.M. van der Hulst, A.M.N. Ferguson (inv. contr.: “Mining the fossil record in large disk galaxies”), N. Kanekar (talk: “Cold gas at high redshift”), E. Tolstoy (inv. contr.: “Abundance patterns in nearby dSph), S.C. Trager (inv. contr.: “The ages and abundances of early-type galaxies and globular clusters”). WAGOS Meeting (Grenoble, France; 6–9 Feb. ’03): S. Cazaux (talk: “Hot core in IRAS 16293”). Carnegie Observatories Centennial Symposium IV “Origin and Evolution of the Elements” (Pasadena, USA; 16–21 Feb. ’03): A.A. Cole (poster: “Abundance patterns of the LMC disk and bar” – A.A. Cole, T.A. Smecker-Hane, E. Tolstoy and J.S. Gallagher),

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E. Tolstoy (talk: “Stellar abundances in dwarf irregular galaxies – K. Venn, E. Tolstoy, A. Kaufer and R.-P. Kudritzki), S.C. Trager (inv. contr.: “Abundances from the integrated light of globular clusters and galaxies”). Dutch Astrophysical Days (Leiden, the Netherlands; 13–14 March ’03): P. Araya Melo, M.C. Spaans (“The first stars”), R. van de Weijgaert (“Hierarchical void evolution”). Workshop “Future Directions in AGB Research” on the occasion of the retirement of Harm Habing (Leiden, the Netherlands; 9–11 April ’03): A.A. Cole, J.M. van der Hulst, P.C. van der Kruit, B. Letarte, J.W. Pel, S.R. Pottasch, M. Spaans, A.G.G.M. Tielens (inv. review: “Dust formation of interstellar ices”) E. Valentijn, R. van de Weijgaert, H. van Woerden (“The appreciation of Harm Habing”). Grain Surface Chemistry Workshop (Lorentz Center, Leiden, the Nether-lands; 14–17 April ’03): A.G.G.M. Tielens (inv. review: “The formation of interstellar ices”) 14th International Symposium on Space TeraHertz Technology (Tucson, USA; 22–24 April ’03): A. Baryshev (talk.: “Influence of temperature variations on the stability of a submm wave receiver” – A. Baryshev, R. Hesper, G. Gerlofsma, M. Kroug and W. Wild), R. Hesper (poster: “Efficient side-band ratio measurement of a submm wave mixer using a Fourier transformspectrometer” – A. Baryshev, R. Hesper, G. Gerlofsma, M. Kroug and W. Wild). NNV Conference Fysica 2003 (Amsterdam, the Netherlands; 25 April ’03): R. van de Weijgaert (inv. contr. “Light over the Dark Lords of the Cosmos”). May Symposium STSCI (Baltimore, USA; 5–8 May ’03): B.W. Holwerda. 2nd International X-Ray Astronomy School (Wallops Island, Virginia, USA; 12–16 May ’03): A. Labiano Ortega. Conference “Dynamics and evolution of galaxies” (Rome, Italy; 18–21 May ’03): N.R. Napolitano (inv. contr.: “Dynamics of diffuse stellar population in clusters”).

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ESO Workshop “Large Programmes and Public Surveys + USM” (Garching, Germany; 18–23 May ’03): E.A. Valentijn (inv. contr.: “OmegaCAM”). Dinamica ed Evoluzione delle Galassie (Accademia Lincei, Rome, Italy; 19–20 May ’03): R. Sancisi (inv. contr.: “Luminous and dark matter in spiral galaxies”). 58e Nederlandse Astronomen Conferentie (Kleve, Germany; 21–23 May ’03): P.D. Barthel (“Sterrenkunde in het basis- en voortgezet onderwijs”), C. Boersma (poster: “Unravelling the density and temperature structure of W3 IRS 5”), M. Brentjens (talk: “LOFAR calibration strategy”) N.G. Douglas (talk: “Galaxy dynamics with the PN Spectrograph”), J.M. van der Hulst (talk: “Probing HI in the nearby Universe with the upgraded WSRT”), J.T.A. de Jong (talk: “Probing MACHOs in M31” – J.T.A. de Jong, K.H. Kuijken, A.P.S. Crotts et al.), N. Kanekar (talk: “21cm studies of damped Lyman � systems” – N. Kanekar and J.N. Chengalur), B. Letarte (poster: “Wide field photometry of local group dwarf galaxies” – B. Letarte, E. Tolstoy and M. Irwin), E. Loenen (poster: “Extragalactic megamaser Mrk 273: result of automated data reduction” – A.F. Loenen, H.-R. Klöckner and W.A. Baan), F. Lugt (poster: “Star formation in Abell 2670”), J.P. Macquart (talk: “High brightness temperature emission in J1819+3845” – J.P. Macquart and A.G. de Bruyn), C. Ormel (poster: “The Phoenix stellar population: HI cloud connection” – C.W. Ormel and E. Tolstoy), E. Platen (poster: “The abundances of Hubble 5” – E. Platen, J. Bernard Salas and S.R. Pottasch), A.Popping (poster: “Morphological aberrations in the SDSS Early Data Release” – A. Popping and Zs. Frei), E. Romano-Díaz (talk: “Bulk flows in our local Universe – E. Romano Díaz, E. Branchini, R. van de Weijgaert and Y. Hoffman), D. Seekles (poster: “Identifying lobsidedness in spiral galaxies”), S.C. Trager (talk: “Directly detecting galaxy evolution from starlight”). Symposium “The astrophysics of interstellar dust” (Estes Park, Colorado, USA; 26–30 May ’03): A.G.G.M. Tielens (SOC Member) (“Carbon-rich dust formation in the hydrogen deficient extreme environments of WC-type Wolf-Rayet stars” – Chiar, J.E., Tielens, A.G.G.M., Peeters, E.; “The detection of new dust-related IR emission features” – Peeters, E., Tielens, A.G.G.M. et al.; “Profile variations of the 3 to 12 micron PAH features” – Peeters, E., van Diedenhoven, B., van Kerckhoven, C., Hony, S., Tielens, A.G.G.M., et al.). Conference “First Stars II” (State College, USA; 28 May – 1 June ’03): E. Tolstoy (inv. review: “Extragalactic low metallicity stars”).

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Conference “The riddle of cooling flows in galaxies and clusters of galaxies’’ (Charlottesville, USA; 31 May–7 June ’03): M.A. Brentjens (“0.35 GHz radio observations of the Perseus cluster”). Guillermo Haro Workshop on AGN Surveys (Puebla, Mexico; 2 June ’03): N.M. Nagar (talk: “Binary black holes in merging galaxies”). Conference “Future directions in high resolution astronomy: a cele-bration of the 10th anniversary of the VLBA” (Socorro, New Mexico, USA; 9–12 June ’03): A. Labiano Ortega. SFA-2003 – Semaine de l’Astrophysique Francaise (Bordeaux, France; 16–21 June ’03): S. Cazaux (inv. contr.: “Molecular hydrogen formation in the interstellar medium” – Cazaux, S., Tielens, A.G.G.M; “The Hot Core towards the low mass protostar IRAS16293–2422” – Cazaux, S., Tielens, A.G.G.M., Ceccarelli, C., Castets, A.), Ph. Héraudeau (“Source counts at 90 micron with the European Large-Area ISO Survey (ELAIS)” – Héraudeau, P., Oliver, S., del Burgo, O., Kiss, C., Stickel, M., Tóth, V., Mueller, T.). “Multiwave Cosmology” Conference (Mykonos, Greece, 17–20 June ’03): R. van de Weijgaert (inv. contr.: “Much ado about nothing: a hierarchy of voids”). 3rd Cosmology Conference “Where cosmology and fundamental physics meet” (Marseille, France; 24 June ’03): R.H. Sanders (inv. contr.: “Are there alternatives to dark matter?”). Workshop “Emission Line Halos” (Leiden, 30 June ’03): B. Emonts “The neutral ISM in Starburst Galaxies” Workshop (Gothenburg, Sweden; 24–27 June ’03): B. Emonts (talk: “Fast outflow of HI in starburst radio galaxy 3C 293”). Workshop “OmegaCAM’s first survey” (Leiden, the Netherlands; 30 June –2 July ’03): D. Boxhoorn, F. Christen, Ph. Héraudeau, S.C. Trager (contr.: “Deep imaging of galaxy halos” – S.C. Trager and A. Helmi), E.A. Valentijn (inv. contr.: “Observing Superclusters with OmegaCAM” and “Observing with OmegaCAM”).

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“Star formation in the ISM” Workshop in honor of the 60th birthdays of Frank Shu, Chris McKee and David Hollenbach (Lake Tahoe, USA; 29 June – 3 July ’03): A.G.G.M. Tielens (inv. review: “PAH molecules in regions of star formation”). 5th Workshop on Galactic Chemodynamics (Melbourne, Australia; 9–11 July ’03): E. Tolstoy (inv. contr.: “Spheroidal galaxies: implications for galactic evolution”). 25th General Assembly of the IAU (Sydney, Australia; 13–26 July ‘03): R. Boomsma, N.G. Douglas, A.C. Gonzalez-Garcia, J.M. van der Hulst, P.C. van der Kruit, J.-P. Macquart, N. Napolitano, E. Tolstoy. IAU Symposium 217 “Recycling intergalactic and interstellar matter” (Sydney, Australia; 14–17 July ’03): R. Boomsma (poster: “High velocity HI in NGC 6946 and NGC 253” – R. Boomsma, J.M. van der Hulst, T.A. Oosterloo, R. Sancisi and F. Fraternali), J.M. van der Hulst (talk: “Evidence for gas accretion in galactic disks” – J.M. van der Hulst and R. Sancisi; poster: “Connection between damped Ly � systems and local galaxies” – M.A. Zwaan, J.M. van der Hulst et al.). IAU Symposium 220 “Dark matter in galaxies” (Sydney, Australia; 21–25 July ’03): N.G. Douglas (“Early-type Halo dynamics inferred using the PN Spectrograph” – N.G. Douglas, A.J. Romanowsky, N.R. Napolitano et al.; “Elliptical galaxies: darkly cloaked or scantily clad? – A.J. Romanowsky, N.G. Douglas, K.H. Kuijken, N.R. Napolitano et al. ; “Halo dynamics of early-type galaxies: models and implications” – A.J. Romanowsky, N.G. Douglas, M. Arnabold, K.H. Kuijken, N.R. Napolitano et al.), B.W. Holwerda (poster: “The opacity of spiral galaxies from counts of distant background galaxies” – B.W. Holwerda, R.A. Gonzalez, R.J. Allen and P.C. van der Kruit), N. Napolitano (“M/L ratios and structural parameters in early-type galaxies”), E. Noordermeer (talk: “The mass distribution in early-type disk galaxies” – E. Noordermeer, J.M. van der Hulst, R. Sancisi and T.S. van Albada), I. Pérez Martín (poster: “Gas flows and dark matter in the inner parts of barred galaxies” – I. Pérez Martín, K. Freeman and R. Fux). R. Sancisi (inv. contr.: “The visible matter-dark matter coupling”). IAU Joint Discussion #6 (Sydney, Australia; 17 July ’03): N.G. Douglas (“Dynamics of globular cluster systems in elliptical galaxies” – A.J. Romanowsky, N.G. Douglas, K.H. Kuijken, N.R. Napolitano et al.).

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IAU Joint Discussion #10 (Sydney, Australia; 10 July ’03): A.G. de Bruyn (inv. contr.: “WSRT 0.35 and 1.4 GHz observations of the Perseus cluster”). IAU Joint Discussion #15 (Sydney, Australia; July ’03): N. Kanekar (“Spin temperature in high redshift DLAs" – J.N. Chengalur, N. Kanekar), E. Tolstoy (inv. review: “Abundances in Local Group Galaxies” – E. Tolstoy and K. Venn; inv. talk: “Abundances of individual stars in Fornax globular clusters” – P. Jablonka, B. Letarte, V. Hill, E. Tolstoy, P. Francois). IAU Joint Discussion #18 “Quasar cores and jets” (Sydney, Australia; July ’03): J.P. Macquart (inv. contr.: “Microarcsecond structure in J1819+3845”). Dave Jauncey 65th Celebration (Parkes, Australia; 10 July ’03): A.G. de Bruyn (talk: “J1819+3845: 4 years of exciting discoveries”), J.P. Macquart (inv. contr.: “Diffractive scintillation in J1819+3845”). International SKA 2003 Conference (Geraldton, Australia; 27–31 July ’03): J.M. van der Hulst. Workshop “Cometary Dust in Astrophysics” (Crystal Mountain, Washington, USA; 10–15 Aug. ’03): A.G.G.M. Tielens (inv. review: “The destruction of interstellar dust”). Conference “Star and structure formation: from first light to the Milky Way” (Zürich, Switzerland; 18–22 Aug. ’03): J. van Gorkom, N. Kanekar, K. Kova� (poster: “Clustering of Lyman � galaxies at z=4.5” – K. Kova�, S. Malhotra and J.E. Rhoads), R. Sancisi (inv. contr.: “HI holes, HI halos and gas infall”), S.C. Trager. JENAM Conference (Budapest, Hungary; 27–31 Aug. ’03): A.G. de Bruyn (inv. review: “Variability in the extragalactic Radio Universe”), K. Fathi (“Central gas kinematics and dynamics in early-type spirals” – K. Fathi, R.F. Peletier, J. Falcón Barroso and E. Emsellem), E.A. Valentijn (inv. contr.: “Using the AstroWise for observing variable sources with OmegaCAM”). “New perspectives for post-Herschel Infrared Astronomy from space” Meeting (Madrid, Spain; 1–4 Sept. ’03): Th. de Graauw, F. Helmich (inv. contr.: “Space heterodyne interferometer mission” – Th. de Graauw, J. Cernicharo, A. Bos et al.), P. Roelfsema, P. Wesselius, W. Wild.

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SISCO Meeting (Naples, Italy; 4–5 Sept. ’03): Ph. Héraudeau, K.H. Kuijken (talk: “VST surveys”) E.A. Valentijn (talk: “Using AstroWise: a virtual survey system” and “Observing superclusters with OmegaCAM”). Summer School “Frontiers of the Universe – cosmology” (Cargese, Corsica, France; 8–20 Sept. ’03): M.A. Aragón Calvo, P. Araya Melo, M. Obri�, F. Simatupang. SAURON Workshop (Oxford, UK; 7–12 Sept. ‘03): K. Fathi, K. Ganda, R.F. Peletier. 2nd Aegean Summer School on the Early Universe (Ermoupoli, Greece; 20 Sept. – 1 Oct. ’03): R.H. Sanders (inv. contr.: “Observational cosmology”). 4th Cologne-Bonn-Zermatt Symposium on dense ISM in galaxies (Zermatt, Switzerland; 20–27 Sept. ’03): F. Helmich, N. Kanekar (talk: “HI at high redshift” – N. Kanekar and J.N. Chengalur), D. Poelman (poster: “Water emission from molecular clouds”), R. Shipman (poster: “Infrared dark clouds toward W51” – R. Shipman, F.P. Helmich, V. Ossenkopf and D. Teyssier), A.G.G.M. Tielens (inv. review: “Spectroscopy of interstellar PAH molecules”). HIFI Core Science Meeting (Zermatt, Switzerland; 20–21 Sept. ’03): M.C. Spaans. Conference “Stellar Populations 2003” (Garching, Germany; 5–10 Oct. ’03): A.A. Cole (poster: “Tracking the metallicity gradient of the LMC” – A.A. Cole, T.A. Smecker-Hane, E. Tolstoy and J.S. Gallagher), R.F. Peletier (inv. contr.: “Spectral index strengths”), I.Pérez Martín (poster: “M/L ratio determination from population synthesis models” – I. Pérez-Martín, K. Freeman and R. Fux), E. Tolstoy (inv. contr.: “The importance of complementing accurate stellar photometry with spectroscopy”), S.C. Trager (talk: “Old stellar populations in galaxy clusters” – S.C. Trager, S.M. Faber and A. Dressler). NOVA Fall School (Dwingeloo, the Netherlands; 6–10 October ’03): G. Battaglia, K. Ganda B. Holwerda, K. Kova�,

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A. Labiano, D. Poelman, G. Sikkema. Astrochemistry Symposium (Long Beach, Ca, USA; 13–17 Oct. ’03): A.G.G.M. Tielens (Inv. review: “Chemistry of interstellar dust and large molecules”). ESO Workshop “Multiwavelength mapping of galaxy evolution” (Venice, Italy; 13–16 Oct. ’03): R. Sancisi, S.C. Trager (inv. contr.: “Directly detecting galaxy evolution from starlight” – S.C. Trager, S.M. Faber and A. Dressler). LOFAR Science Meeting (Leiden; 30 Oct. ’03): J.M. van der Hulst, M.C. Spaans (inv. contr.: “Hydrogen recombination line masers with LOFAR”), R. van de Weijgaert. SKA Science Meeting (Lorenz Center, Leiden; 10–14 Nov. ’03): A.G. de Bruyn, J.M. van der Hulst (“Probing galaxy evolution with the Square Kilometre Array”), M.C. Spaans. ASTRO-WISE Workshop “Developer and advanced user tutorials on photometric pipelines and quality control” (Groningen, 17–20 Nov. ’03): K.G. Begeman, D. Boxhoorn (“ASTRO-WISE federation overview and status”), Ph. Héraudeau, R. Vermeij (“The ASTRO-WISE photometric pipeline: software implementation”), E.A. Valentijn. Workshop “High resolution infrared spectroscopy in astronomy” (ESO, Garching, Germany; 18–24 Nov. ‘03): A.G.G.M. Tielens (inv. review: “Regions of massive star formation”). IDISIEEP Conference “The Olympic spirit and human progress” (Thessaloniki, Greece; 5–7 Dec. ’03): R. van de Weijgaert (inv. talk: “Climbing Mount Olympus: geometry as pathway to the Universe”). Conference “Multiwavelength AGN Surveys” (Cozumel, Mexico; 8–12 Dec. ’03): N.M. Nagar (inv. contr. “Radio properties of local AGN”). ICM Meeting (Leiden, 11 Dec. ‘03): M.C. Spaans.

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Workshop “Light on Planetary Atmospheres: from the solar system to exoplanets” retirement of Prof. J.W. Hovenier (Amsterdam, 15 Dec. ’03): P.D. Barthel, H. van Woerden.

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APPENDIX III : Visits to institutes abroad

III.1 Work visits

P.D. Barthel Universum (Bremen, Germany); 14–15 April Institute for Astronomy (Honolulu, Hawaii, USA); 30 May – 28 June Univ. of Kent (Canterbury, UK); 17–19 Sept. CSIC (Madrid, Spain); 12–15 Oct. Jodrell Bank (Macclesfield, UK); 7–10 Dec. Imperial College (London, UK); 11 Dec. M.A. Brentjens NRAO (Charlottesville, USA); 4–6 June A.A. Cole Observatoire de Paris-Meudon (France); 19–21 Jan. Univ. of Basel (Switzerland); 2–6 Sept. Univ. of Minnesota, Macallester College (Minnesota, USA); 27–29 Oct. N.G. Douglas Univ. of New South Wales (Sydney, Australia); 28 July – 1 Aug. Anglo-Australian Observatory (Australia); 29 July B.H.C. Emonts Dept. of Physics & Astronomy (Sheffield, UK); 11 March–18 May K. Fathi CRAL (Obs. De Lyon, France); 7–14 July Uppsala Astronomical Obs. (Sweden); 18 Dec. J.M. van der Hulst La Palma (Spain); 7–10 Oct. N. Kanekar National Centre for Radio Astrophysics (Pune, India); 21 Feb. – 9 March, 23 Oct. – 3 Nov., 17–29 Nov. Max Planck Institut für Radioastronomie (Bonn, Germany); 3–6 Sept. Univ. of California (San Diego, USA); 18–22 Dec. P.C. van der Kruit Washington (USA); 27–29 Jan, 23–26 Feb., 24–26 Sept., 3–5 Dec. Garching (Germany); 19–20 Feb., 11–12 May, 25–27 May, 9–11 June, 29 Oct., 8–10 Dec.

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Antofagasta and Paranal (Chile); 10–16 March Helsinki (Finland); 27–28 April, 26–27 Nov. Paris (France); 6–7 Oct. Santiago and Chajnantor (Chile); 30 Oct.–12 Nov. B. Letarte Observatoire de Paris-Meudon (France); 7–8 April, 12–16 May, 9–13 June, 4–8 Aug. J.-P. Macquart University of Sydney (Australia); 2–9 July, 28 July–1 Aug. Mt. Stromlo & Siding Springs Obs. (Australia); 5–8 Aug. Univ. of California (San Diego, USA); 1–30 Oct. JPL (Pasadena, USA); 9 Oct. O. Möller Caltech (Pasadena, USA); 1–15 Dec. N.M. Nagar INAOE (Tonanzintla, Mexico); 23 June – 12 July Arcetri Observatory (Firenze, Italy); 18–23 August. N.R. Napolitano Observatory Capodimonte (Naples, Italy); 27 June – 5 July E. Noordermeer Department of Astronomy, Univ. of Wisconsin (Madison, USA); 8 Oct. M. Obri� Princeton University (New Jersey, USA); 20 Oct.–8 Nov. Columbia University (New York, USA); 8 –12 Nov. J.W. Pel Service d’Astrophysique (Saclay, France); 3–5 Jan., 11–16 May, 17–19 Sept., 6–9 Oct., 3–7 Nov., 12–15 Nov., 2–5 Dec., 10–11 Dec. Royal Observatory (Edinburgh, UK); 19–22 May, 9–11 July, 30 Sept. – 2 Oct. ESO (Garching, Germany); 16–17 Sept. Astrium Space Laboratories (Stevenage, UK); 25–26 Feb. I. Pérez Martín Geneva Observatory (Switzerland); 17–24 Nov. M. Spaans Johns Hopkins University and Space Telescope Science Institute (Baltimore, USA): 4–11 Oct. H.W.W. Spoon Cornell University (Ithace, USA); 3–7 March

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A.G.G.M. Tielens University of California (Berkeley, USA); 1 Oct. 2002 – 1 March 2003 Space Science Telescope Institue (Baltimore, USA); 24–26 March Lawence Livermore National Laboratories (California, USA); 2–9 June, 27 June – 29 Aug. University College (London, UK); 28 Oct. University of Leuven (Belgium); 4 Nov. E. Tolstoy Observatoire de Paris (Meudon, France); 3–5 March, 3–12 April, 10–27 June Institute of Astronomy (Bologna, Italy); 17–23 May European Southern Observatory (Garching, Germany); 5 June Institute of Astronomy (Cambridge, UK); 30 July – 5 Aug., 17–25 Sept. Dept. of Astronomy (Oxford, UK): 26 Sept. E.A. Valentijn Observatory Capodimonte (Naples, Italy); 19–23 Jan. Astronomisches Institut (Bonn, Germany); 8–9 May ESO (Munich, Germany); 1–2 Oct. M.A.M. van de Weijgaert Queen Mary & Westfield College, Univ. London (London, UK); 16–20 May Institute of Astronomy (Cambridge, UK); 26 May – 4 June III.2 Observing trips

A.A. Cole VLT/UT4 8.2m Telescope (Paranal, Chile); 17–25 Aug. 4m. Telescope (Kitt Peak, USA); 23 Oct. N.G. Douglas William Herschel Telescope (PN.s) (La Palma, Spain); 26 Feb.– 4 March E.M. Helmich Isaac Newton Telescope (La Palma, Spain); 10–17 Feb. N. Kanekar Giant Metre-wavelength Radio Telescope (Pune, India); 29 Jan. –20 Feb., 12–22 Oct. Green Bank Telescope (West Virginia, USA); 18 Dec. – 10 Jan. ‘04 B. Letarte WFI 2.2m Telescope (La Silla, Chile); 18–19 Sept. VLT (Paranal, Chile); 28 Sept. – 1 Oct. N.M. Nagar JCMT (Hawaii, USA); 16–21 Dec.

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N.R. Napolitano William Herschel Telescope (PN.s) (La Palma, Spain); 28 Feb. – 8 March, 29 Sept. – 6 Oct. M. Obri� Jacobus Kapteyn Telescope (La Palma, Spain); 28 May – 5 June C. Ormel Telescopio Infrarosso del Gornergrat (TIRGO) (Zermatt, Switzerland); 1–16 Dec. P. Roelfsema JCMT (Mauna Kea, Hawaii, USA); 18–27 May S.C. Trager VLT (Paranal, Chile); Nov–Dec. L. Vermaas Jacobus Kapteyn Telescope (La Palma, Spain); 26 June – 9 July R. Vermeij Isaac Newton Telescope (La Palma, Spain); 11–15 Feb.

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APPENDIX IV : Colloquia, popular lectures

IV.1 Colloquia given outside Groningen

M.A. Aragón Calvo – “The Sunyaev-Zeldovich Effect” ASTRON, Dwingeloo, the Netherlands (18 Nov.) P.D. Barthel – “Low luminosity in active galaxies” Institute for Astronomy, Honolulu, Hawaii, USA (4 June) J. Bernard Salas – “Physics and chemistry of gas in Planetary Nebulae” Cornell University, Ithaca, USA (10 April) A.G. de Bruyn – “J1819+3845: microarcsec resolution through the interstellar telescope” : Leiden Observatory, the Netherlands (25 Feb. ) A.A. Cole – “Chemical evolution of the Bar of the LMC” Observatoire de Paris-Meudon, France (20 Jan. ) “The Epoch of Bar formation in the LMC” University of Basel, Switzerland (4 Sept. ) “Star-formation history of the LMC” University of Minnesota, USA (28 Oct.) “Red Giant metallicities across the Local Group” University of Notre Dame, USA (30 Oct.) “Chemical evolution of the Large Magellanic Cloud” University of Notre Dame, USA (31 Oct.) N.G. Douglas – “Counter-dispersed imaging: problems with CDM?” ASTRON, Dwingeloo, the Netherlands (9 May) “A dearth of dark matter: first results with the PN.Spectrograph” University of New South Wales, Australia (30 July) B.H.C. Emonts – “Radio galaxies: the ISM-AGN connection” Sheffield University, UK (15 May) Ph. Heraudeau – “SISCO framework” Osservatorio di Capodimonte, Naples, Italy (2 Sept.) N. Kanekar – “21cm absorption studies of damped Lyman � systems” ASTRON, Dwingeloo, the Netherlands (14 March) “HI 21cm absorption studies of damped Lyman � systems”

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Max-Planck-Institut für Radioastronomie, Bonn, Germany (5 Sept.) “Molecules at low frequencies” Max-Planck-Institut für Radioastronomie, Bonn, Germany (4 Sept.) NCRA-TIFR, Pune, India (21 Nov.) M. Kregel – “Edge-on galaxies: stellar dynamics and new implications for dark matter” : ASTRON, Dwingeloo, the Netherlands (12 Dec. ) J.-P. Macquart – “Intra-day variability and the structures of high brightness temperature” Max-Planck-Institut für Kernphysika, Heidelberg, Germany (28 Jan.) “Viewing high brightness temperature AGN through the Interstellar Telescope” University of Amsterdam, the Netherlands (12 June) “Imaging Intra-day variable quasars with the Interstellar Telescope” University of Sydney, Australia (Aug.) “Imaging an Intra-day variable quasar with the Interstellar Telescope” Mt. Stromlo and Siding Springs Observatories, Australia (Aug.) “Probing structure through inhomogeneous media” University of Melbourne, Australia (Aug.) “J1819+3845: the Rosetta Stones of Intra-day variable radio sources” University of California, Berkeley, USA (Oct.) “Recent advances in (understanding) Intra-day variable radio sources” Caltech, USA (Oct.) O. Möller – “Complications in lensing: discs, doubles and groups” ASTRON, Dwingeloo, the Netherlands (Sept.) M. Obri� – “Multiwavelength properties of galaxies observed by ROSAT, SDSS, 2MASS, IRAS,GB6, FIRST, NVSS and WENSS surveys” Columbia University, New York, USA (11 Nov.) I. Pérez Martín – “Gas glows and dark matter in the inner parts of barred galaxies” : Geneva Observatory, Switzerland (Nov. ) R.H. Sanders – “Astronomical constraints on the accelerating Universe and modifications of Newtonian gravity” Leiden Observatory, the Netherlands (27 March) “Modified Newtonian dynamics as an alternative to dark matter” Physics Department, Univ. of Groningen, the Netherlands (15 May) R. Shipman – “Infrared dark clouds toward W51” Physikalisches Institut, Köln, Germany (26 Nov.) M.C. Spaans – “Star formation in the early Universe” Leiden Observatory, the Netherlands (23 Jan. ) “The Green’s Function in radiative transfer problems” SRON/EOS Utrecht, the Netherlands (27 June) E. Tolstoy – “Dwarf galaxies: important clues to galaxy formation” Paris-Meudon Observatory, France (10 April)

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Osservatorio Astronomico, Bologna, Italy (19 May) S.C. Trager – “The timescale of galaxy formation: clues from stellar populations” SRON/Astronomy Institute Joint Colloquium, Utrecht, the Netherlands (12 March) “Directly detecting galaxy evolution from starlight” Leiden Observatory, the Netherlands (6 Nov. ) Astronomical Institute, Univ. of Amsterdam, the Netherlands (21 Nov.) Theoretical Astrophysics Group, Oxford University, UK (25 Nov.) E.A. Valentijn – “OmegaCAM and AstroWise” University of Liège, Belgium (1 April) W. Wild – “ALMA: the Atacama Large Millimeter Array” ESTEC, Noordwijk, the Netherlands (10 Oct. ) IV.2 Popular lectures

P.D. Barthel – “Nieuwe ontwikkelingen in de kosmologie” : Enschede (6 Jan.) “ESO’s Very Large Telescope” : Hoogeveen (17 Jan.); Assen (12 Sept.) “Astronomy in High School” : KNW Teachers Meeting, Groningen (14 Feb.); Groningen (6 Nov.) “Astronomical Outreach” : Beta+ Symposium, Groningen (2 April) R. Boomsma – “Neutraal waterstof in nabije melkwegstelsels” KGVWS, Groningen (17 Jan.) “Melkwegstelsels” : Triangulum, Apeldoorn (18 Sept.) “Wiskunde in de Sterrenkunde” : Wiskundedocentendag, Wolters-Noordhoff, Zwolle (21 Nov.) A.G. de Bruyn – “ASTRON, WSRT and LOFAR” Visitors to ASTRON and Westerbork (several occasions) G. Comello – “Lichthinder” : TV Noord “Adamsappel” (10 March) N.G. Douglas – “Zonnerotatie meting” : Scholieren Meppel (17 Feb.) B.H.C. Emonts – “Zoektocht naar Exoplaneten” KNVWS Noord-Drenthe, Beilen (10 Oct. ) KNVWS Zuid-Drenthe, Hoogeveen (14 Nov. ) F. Helmich – “Stervorming” 22 April – KNVWS Eemsmond, Appingedam J.T.A. de Jong – “Gravitatielenzen en hun belang voor de sterrenkunde” KNVWS Zaanstreek, Oostzaan (27 March) KNVWS Eemsmond, Appingedam (7 Oct.)

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J.P. Macquart – “Probing quasar black holes with the interstellar telescope” Sutherland Astronomical Society, Sydney, Australia (21 Aug.) E. Noordermeer – “Eilanden in het heelal: Sterrenstelsels gezien vanaf La Palma” : KNVWS Arnhem (19 March); KNVWS Groningen (19 Sept.) Weer- en Sterrenkundige Kring Zaanstreek, Oostzaan (27 Nov.) KNVWS Noord Drenthe, Assen (12 Dec.) R.F. Peletier – Het kosmisch ecosystem” Open day, University of Groningen (19 Oct.) M. Spaans – Snaartheorie” Rotary Club, Sassenheim (23 Sept.) M.A.M. van de Weijgaert – “Van primordiale ruis tot kosmisch schuim” Astroweekend KNVWS, Tilburg (1 Nov.) P.R. Wesselius – “Exoplanten” KNVWS Eemsmond, Appingedam (4 March) H. van Woerden – “Eet de Melkweg? Of ademt hij?” KNVWS, ‘s Hertogenbosch (15 Jan..); NVWS, Arnhem (24 Sept.) “Zestig jaar Sterrenkunde” KNVWS, Zwolle (10 Oct.); KNVWS, Dordrecht (7 Nov.) “Sterrenstelsels – de bouwstenen van het Heelal” KNVWS, Amersfoorrt (9 April)

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APPENDIX V : Colloquia in Groningen

January 20 Marco Beijersbergen (Kapteyn Institute, Groningen): The galaxy population in the Coma Cluster January 27 Ralph Wijers (Sterrenkundig Instituut “Anton Pannekoek”, Amsterdam): Black holes shining brightly February 3 Andrew Cole (Kapteyn Institute, Groningen): Natural History of a Triple Nebula: the 2MASS view through the inner Milky Way February 11 (NOVA Colloquium) George Helou (IPAC, Caltech, Pasadena, USA): Infrared Surveys: planned serendipity February 17 Sacha Hony (Sterrenkundig Instituut, Amsterdam/ESTEC, Noordwijk): The composition of dust surrounding carbon-rich stars February 24 Onno Pols (Sterrenkundig Instituut, Utrecht) : Evolution and nucleosynthesis of AGB stars in binaries March 3 Jelle Kaastra (SRON, Utrecht): XMM-Newton discovery of the warm and hot intergalactic medium March 10 Bartjan van Tent (Spinoza Institute, Utrecht): Cosmological inflation with multiple fields and the theory of density fluctuations March 13 (RuG Physics Seminar) Alex Ollongren (Mathematical Institute, Leiden): Communication with Extra Terrestrial Intelligence (CETI) March 17 Andreas Quirrenbach (Sterrewacht Leiden): Taking the measure of the Universe March 18 Michiel Hogerheijde (Steward Observatory, Tucson, USA): Infall and rotation around young stars: formation and evolution of protoplanetary disks

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March 20 Thijs van der Hulst (Kapteyn Institute, Groningen) : Galaxies on collision course March 24 (NOVA colloquium) Tom Abel (Penn State University, USA): The first stars in the Universe March 25 Joop Schaye (Institute for Advanced Study, Princeton, USA): The chemical enrichment of the intergalactic medium March 31 Garrelt Mellema (Sterrewacht Leiden): The hydrodynamics of radiative feedback: from clouds to mini-haloes April 1 Henk Hoekstra (CITA, Toronto, Canada): The hunt for the equation of state of the Universe April 2 Marc Verheijen (Astrophysikalisches Institut Potsdam, Germany): The evolution of galaxies in clusters April 3 Léon Koopmans (Space Telescope Science Institute, Baltimore, USA): Gravitational lensing: a tool for cosmology and astrophysics April 4 (Oort Professor Colloquium) Alexander Dalgarno (Center for Astrophysics, Cambridge, Massachusetts, USA): X-rays in the Solar System April 7 Klaus Meisenheimer (Max-Planck-Institut für Astronomie, Heidelberg, Germany): The evolution of the galaxy populations in the last 10 Gyrs April 14 (NOVA colloquium) John Lattanzio (Monash University, Victoria, Australia): AGB stars and the chemical evolution of the galaxy April 16 Kim Venn (Dept. Astronomy, Univ. Minnesota, Minneapolis, USA): Stellar abundances in local group dwarf galaxies April 23 Stacy McGaugh (Dept. Astronomy, Univ. Maryland, College Park, USA): Cosmology and dark matter halos April 24 Evan Skillman (Dept. Astronomy, Univ. Minnesota, Minneapolis, USA): New clues to dwarf galaxy evolution

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April 28 (NOVA colloquium) Craig Sarazin (Dept. Astronomy, Univ. Virginia, USA): CHANDRA observations of low mass X-ray binaries, globular clusters and hot gas in elliptical galaxies May 8 Kinwah Wu (Mullard Space Science Lab., University College London, UK): Radiative transfer in curved spacetime May 12 (Kapteyn Seminar Special) Paul Wignall (School of Earth Sciences, Leeds, UK): Giant volcanic provinces and mass extinctions May 15 (RuG Physics Seminar) Bob Sanders (Kapteyn Institute, Groningen): Modified Newtonian Dynamics as an alternative to dark matter May 19 Cesar Gonzalez-García (Kapteyn Institute, Groningen): Elliptical galaxies: merger simulations and the fundamental plane May 26 Jim Rose (University of North Carolina, Chapel Hill, USA): Elliptical galaxies: the ages and chemical compositions of early-type galaxies June 2 (NOVA colloquium) Ortwin Gerhard (Observatory of Basel, Switzerland): Large-scale structure of the Milky Way June 11 Jacqueline van Gorkom (Dept. Astronomy, Columbia University, New York, USA): The evolution of galaxies in clusters: an HI perspective June 16 (NOVA colloquium) Giuseppe Bono (Osservatorio Astronomico di Roma, Italy): Cepheids and RR Lyrae: observations, theory and distance scales June 23 Michael Dopita (ANU, Mount Stromlo and Siding Spring Observatory, Australia): Star formation rates in galaxies: H-Alpha, what is it good for? June 30 Rogier Windhorst (Dept. of Physics and Astronomy, Arizona State Univ., Tempe, USA): An HST mid-UV survey of nearby galaxies: quantitative tools to understand high-redshift galaxy structure July 1 Michael Eracleous (Dept. Astronomy, Penn State University, USA): Observing the structure and dynamics of accretion flows onto supermassive black holes in active galaxies

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September 1 Valerie de Lapparent (IAP, Paris, France): Galaxy luminosity functions: present status and perspective raised by the ESO-Sculptor Survey September 8 Robert Braun (ASTRON, Dwingeloo): Tidal streams and low mass companions of Messier 31 September 15 Isabel Perez Martin (Kapteyn Institute, Groningen): Dark matter in the inner part of barred galaxies September 17 Jaron Kurk (Osservatorio Astrofisico di Arcetri, Firenze, Italy): The cluster environment and gaseous halo of PKS 1138–262 September 22 Daphne Stam (Sterrenkundig Instituut “Anton Pannekoek”, Amsterdam): Towards the direct detection of extrasolar planets September 29 Piotr Popowski (Max-Planck-Institut für Astrophysik, Garching, Germany): Non-microlensing applications of microlensing surveys: galactic extinction October 6 Michele Capellari (Sterrewacht, Leiden): The orbital distribution in nearby galaxies as seen from the SAURON survey October 13 Jeronimo Bernard Salas (Kapteyn Institute/SRON, Groningen): Physics and chemistry of gas in planetary nebulae October 21 (NOVA colloquium) Dave Sanders (Institute of Astronomy, Univ. Hawaii, Honolulu, USA): The Infrared Universe: the cosmic evolution of superstarbursts and massive black holes October 24 Henrik Spoon (Kapteyn Institute, Groningen): An icy view of ULIRGs October 27 (NOVA colloquium) David Spergel (Princeton University Observatory, USA): First year results from WMAP: implications for cosmology and inflation November 3 Natascha Foerster Schreiber (Sterrewcht, Leiden): New views of the high-redshift Universe from the deep near-infrared FIRES survey

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November 7 Heino Falcke (Sterrenkundig Instituut, Nijmegen/ASTRON): The galactic center and its supermassive black hole November 10 Anthony Brown (Sterrewacht, Leiden): GAIA – Taking the galactic census: current status and activities November 14 Michiel Kregel (Kapteyn Institute, Groningen): Edge-on galaxy disks: stellar dynamics and new implications for dark matter November 18 Peter Suetterlin (Sterrekundig Instituut, Utrecht): DOT Speckles: the observation and data reconstruction system of the Dutch Open Telescope November 20 Sarah Bridle (Institute of Astronomy, Univ. Cambridge, UK): Post-WMAP cosmology November 24 Tracy Webb (Sterrewacht, Leiden): The submillimeter properties of extremely red objects December 1 (NOVA colloquium) Andy Fabian (Institute of Astronomy, Univ. Cambridge, UK): Heating and cooling in the cores of clusters of galaxies December 11 Nicola Napolitano (Kapteyn Institute, Groningen): Intracluster planetary nebulae December 15 Stephanie Cazaux (Kapteyn Institute, Groningen): Grain surface chemistry in astrophysical objects: H2 in Space December 18 (Kapteyn Seminar Special, co-organization with Physics seminar) Sidney Bludman (DESY, Hamburg, Germany/Univ. Pennsylvania, USA): The Star of Bethlehem December 19 Sidney Bludman (DESY, Hamburg, Germany/Univ. Pennsylvania, USA): Critique of tracking quintessence

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APPENDIX VI : Visiting scientists in Groningen

R. Allen Space Science Telescope Institute, Baltimore, USA M. Baes Sterrenkundig Obs. University of Gent, Belgium G. Bono Rome Observatory, Italy H. Bignall JIVE, Dwingeloo E. de Blok University of Cardiff, UK S. Bludman DESY, Hamburg, Germany/Univ. Pennsylvania, USA I. Bond Royal Observatory, Edinburgh, UK S. Bridle Institute of Astronomy, Cambridge, UK A. Chung Columbia University, New York, USA K. Daisuke National Astronomical Obs. of Japan M. Dijkstra Columbia University, New York, USA E. Deul Sterrewacht, Leiden A. Fabian Institute of Astronomy, Cambridge, UK J. Falcon-Barroso Sterrewacht, Leiden K. Fathi University of Nottingham, UK P. François Paris-Meudon Observatory, France K. Freeman Australian National University O. Gerhard University of Basel, Switzerland F. Getman Osservatorio di Capodimonte, Naples, Italy J. van Gorkom Columbia University, New York, USA C. Gössl Universitäts-Sternwarte München, Germany N. Hambly Royal Observatory, Edinburgh, UK A. Helmi M.P.I. für Astrophysik, Garching, Germany G. Helou CalTech, Pasadena, USA V. Hill Paris-Meudon Observatory, France L. Ho OCIW, Pasadena, USA H. Hoekstra Canadian Institute for Theoretical Astrophysics, Toronto M. Hogerheijde Steward Observatory, Tucson, USA J. Holt University of Sheffield, UK L. Hunt CAISMI-CNR, Firenze, Italy M. Irwin Institute of Astronomy, Cambridge, UK D. Jauncey ATNF, Australia K. Ji Hoon University of Maryland, College Park, USA B.J.T. Jones London, UK and Copenhagen Observatory, Denmark V. de Lapparent Institut d’Astrophysique, Paris, France J. Lattanzio CSPA, Monash Univ., Melbourne, Australia J.V. Keane NASA, Ames Research Center, USA L.V.E. Koopmans Space Science Telescope Inst., Baltimore, USA F. Magnard Institut d’Astrophysique, Paris, France H.J. McCracken Institut d’Astrophysique, Paris, France S. McGaugh University of Maryland, College Park, USA

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R. Meijerink Sterrewacht, Leiden K. Meisenheimer MPI für Astronomie, Heidelberg, Germany Y. Mellier Institut d’Astrophysique, Paris, France N. Nagar Arcetri Observatory, Italy M. Neeser Universitäts-Sternwarte München, Germany M. Novicki Cavendish Astrophysics, Cambridge, UK A. Omar Raman Research Institute, Bangalore, India B. Parise CESR, Toulouse, France M. Pavlov Osservatorio di Capodimonte, Naples, Italy R. Peletier University of Nottingham, UK C. Power University of Durham, UK E. Puddu Osservatorio di Capodimonte, Naples, Italy R. Rengelink Sterrewacht, Leiden A. Romanowsky University of Nottingham, UK J. Rose University of North Carolina, USA D. Sanders Institute for Astronomy, Honolulu, Hawaii, USA C. Sarazin University of Virginia, USA J. Schaye Institute for Advanced Study, Princeton, USA U.J. Schwarz Arnhem, the Netherlands R. Silvotti Osservatorio di Capodimonte, Naples, Italy E. Skillman University of Minnesota, Minneapolis, USA J. Snigula Universitäts-Sternwarte München, Germany E. Sutorius Royal Observatory, Edinburgh, UK R. Swaters Johns Hopkins University, Baltimore, USA P. Teuben University of Maryland, College Park, USA M. Trenti Scuola Normale Superiore, Pisa, Italy K. Venn University of Minnesota, Minneapolis, USA M.A.W. Verheijen AIP, Potsdam, Germany A. Volpicelli Osservatorio di Capodimonte, Naples, Italy K. Wu University College London, UK S. Zaroubi M.P.I. für Astrophysik, Garching, Germany

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APPENDIX VII Memberships, etc.

T.S. van Albada: Lid, Koninklijke Ned. Akademie van Wetenschappen Lid, Bestuur ASTRON Voorzitter, Kapteyn Fonds Voorzitter, Stichting Pastoor Schmeits voor

Sterrenkunde Lid, Advies Commissie Astronomie GBE, NWO P.D. Barthel: Member, ESA FIRST/Herschel Science Team

(Mission Scientist) Member, EC Network POE (Probing Origin of

Extragalactic Background) Member SOC/LOC NVWS symposium 2002

(Groningen, 5 October) Chairman, National and NOVA Astronomy Education

Committee Chairman, NAC High School Astronomy Education

Working Group Member, Minnaert Committee for Public Outreach in

Dutch Astronomy Member/co-founder IKSG Consortium (ASTRO-F

Mission) Member Bachelor Committee Groningen University

Faculty of Mathemtics and Pysical Sciences Member Organising Committee EAAE Teacher Astro-

summerschool (July 2004) Member Astronomy Board, Lorentz International

Center (Leiden) A. Blaauw: Lid, Koninklijke Ned. Akademie van Wetenschappen Foreign Honorary Member, American Academy of

Arts and Sciences Member, Royal Society of Sciences, Uppsala Foreign member, Koninklijke Academie voor

Wetenschappen, Letteren en Schone Kunsten van België

Foreign member, Royal Danish Academy of Sciences and Letters

Associate, Royal Astronomical Society Complimentary Member, Astronomical Society of the

Pacific Honorary Member, American Astronomical Society Lid, Hollandsche Maatschappij der Wetenschappen Member, Academia Europaea

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A.G. de Bruyn: Lid, Bestuur Leids Kerkhoven-Bosscha Fonds Lid, Bestuur Jan Hendrik Oort fonds Lid, Bestuur Leids Sterrewacht Fonds Member, MERLIN Steering Committee Member, NoEMI study group, ASTRON/NWO-STW G. Comello: Lid, Facultaire Bibliotheekcommissie R.U.G. Ere-lid Koninklijke Nederlandse Vereniging voor

Weer- en Sterrenkunde N.G. Douglas: Member, IAU Commission 9 (Instrumentation &

Techniques) Member, Scientific Organizing Committee ESO

Workshop “Planetary Nebulae beyond the Milky Way” PI, Planetary Nebula Spectrograph Th. de Graauw: PI, HIFI Project Member, coordinating group for submm. research Member, IAU Commission 44 Editor, Journal of Experimental Astronomy Member, NOVA Instrument Steering Committee F.P. Helmich: Member, ASTRON-PC Member, Scientific Organizing Committee “New

perspectives for post-Herschel Infrared Astronomy from Space (Madrid, Spain)

Ph. Héraudeau: Member, Societé Francaise d’Astronomie et

d’Astrophysique J.M. van der Hulst: Member, IAUnion Commission 28 (Galaxies), 34

(Interstellar Matter) and 40 (Radio Astronomy) Chair, Kamer Sterrenkunde van de VSNU Member, ASTRON Board Member NWO/EW Advies Commissie Astronomie Member, ING Board Member, Nederlandse Astronomen Club Member, Nederlands Platform voor de Natuurkunde Member, VSNU DNT Coordinator Network-1 of NOVA P.C. van der Kruit: Voorzitter, Bestuur Nederlandse Onderzoekschool

voor Astronomie (NOVA) Voorzitter, Nederlands Comité Astronomie (NCA) Lid, Gebiedsbestuur Exacte Wetenschappen Neder-

landse Organisatie voor Wetenschappelijk Onderzoek (NWO) (till 08/03)

Chairman, Atacama Large Millimeter Array (ALMA) President of Council, European Southern

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Observatory (ESO) Co-chair, Search committee for the Key Personnel in

the Joint ALMA Office Member, European ALMA Board Co-chair of the ALMA Japan Negotiating Team Chairman, ESO Contact Commissie (KNAW) Member and treasurer, Stichting Groninger

Universiteits Fonds (GUF) Chairman, Koninklijk Natuurkundig Genootschap,

Groningen Member, Board of Directors, Leids Sterrewacht

Fonds Member, Board of Directors, Jan Hendrik Oort Fonds Member, Board of Directors, Leids Kerkhoven-

Bosscha Fonds Member, IAU Commission 28 (Galaxies), 33

(Structure and Dynamics of the Galactic System) and 40 (Radio Astronomy)

J.W. Pel: Member, NOVA Instrument Steering Committee (till

Sept. 2003) Lid, Begeleidingscommissie “Dutch Open Telescope”

(DOT) Principal Investigator “VISIR” spectrometer (Mid-IR

Imager/Spectrometer for ESO Very Large Telescope) Lid ESO Contact Commissie Kon. Nederlandse

Akademie van Wetenschappen Member IAU Commission 25 (Stellar Photometry and

Polarimetry) Instrument Scientist in study team for “MIRI”

spectroometer (Mid-IR Instrument for James Webb Telescope)

R.F. Peletier: Member ESO OPC panel Member, PATT UKIRT Time Allocation Committee Member, HST Time Allocation Panel S.R. Pottasch: Member, Academia Europae P.R. Roelfsema: Member, IAU Commission 34 (Interstellar Matter) and

40 (Radio Astronomy) Member, ESA FIRST Ground segment Advisory

Group Member, ESA FIRST Ground Segment Engineering

Group Member, Herschel Ground Segment review board R. Sancisi: Member, Time Allocation Committee, Italian National

Telescope Galileo

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M.C. Spaans: Visiting scientist SRON/EOS, Utrecht (May – Sept. 2003)

A.G.G.M. Tielens: Project scientist, HIFI project Visiting Miller Research Professor, University of

California, Berkeley (10/2002–02/2003) E. Tolstoy: Member, NWO Open Competition selection

committee Member, NWO Telescope Time Alllocation committee Member, NWO VENI selection committee Member, ESO Telescope Time Allocation committee Lid, Adviescommissie Astronomie, GBE, NOW Member, NOVA Instrument Steering Committee Member, Directors Advisory Committee, Isaac

Newton Group Subaru Open Use observing time proposal selection

committee S.C. Trager Member, NWO VIDI selection committee E.A. Valentijn: Member, IAU Working Group on Sky Surveys Member, IAU commission 28 on Galaxies Co-Investigator, OmegaCAM project Coordinator, ASTRO-WISE consortium Co-Investigator, Lofar Bsik Consortium OmegaCEN P.R. Wesselius: MSO COSPAR 2004 Symp E1.7 Editor Proceedings COSPAR 2002 Symp E1.5 Member, NOVA-ALMA Steering group Member, IAU Division VI, Commission 44 Coordinator Integrated Receiver INTAS proposal Member, Organizing Committee SPIE 2004, Glasgow Lid, Stuurgroep North Stars R. van de Weijgaert: Bestuurslid, Assessor, Nederlandse Astronomen

Club Member, Computational Science curriculum

committee Member, Physics Colloquium Committee Member Netherlands Science Steering Group

LOFAR Member, CWI project “Markov sequential point

processes for image analysis and statistical physics” Member, Nationale Contact Raad, ASTRON W. Wild: FP-6 RadioNet Board NOVA-ALMA Technical Steering and Advisory

Committee SRON Strategisch beraad

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Nederlands URSI-comite (NUC) H. van Woerden: Ere-Voorzitter Koninklijke Nederlandse Vereniging

voor Weer- en Sterrenkunde Erelid, Werkgroep Meteoren KNVWS Lid, Commissie Dr. J. Van der Bilt-prijs NVWS 2002,

2003 Lid, Redactie Maandblad Zenit Lid, Commissie van Aanbeveling, Volkssterrenwacht

Mercurius, Dordrecht Lid, Commissie van Aanbeveling, Volkssterrenwacht

Halley, Heesch Member, IAU, Commissions 28, 33, 34, 40 and 41 Member, Organizing committee, working group on

Historical Radio Telescopes, IAU Commissions 41 and 40

H. Zondervan: Uitvoerend secretaris, Kapteyn Fonds Uitvoerend secretaris, Stichting Pastoor Schmeits

voor Sterrenkunde

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APPENDIX VIII : Personnel (Dec. 31, 2003)

(d) = personnel employed by a third party contract (n) = personnel employed by NWO (u) = personnel employed by University of Groningen Full Professors (Hoogleraren) A.G. de Bruyn (0.3) (u) R. Sancisi (0.3) (u) J.M. van der Hulst (u) R.H. Sanders (u) P.C. van der Kruit (u) A.G.G.M. Tielens (0.42)(u) Associate and Assistant Professors P.D. Barthel (u) M.A.M. van de Weijgaert (u) J.W. Pel (u) Tenure Track A. Helmi (from 9/03) (NOVA) E. Tolstoy (u) (KNAW) R.F. Peletier (from 9/03) (u) S.C. Trager (u) M. Spaans (u) Research Staff A. Baryshev (NOVA) R. Hesper (NOVA) K. Begeman (u) E.A. Valentijn (u) (NOVA) N.G. Douglas (u) Zero Appointments H.R. Butcher (ASTRON, full prof.) K.H. Kuijken (Leiden, full prof.) J.H. van Gorkom (Columbia Univ., full prof.)

P.R. Roelfsema (SRON, assist. prof.)

M.W.M. de Graauw (SRON, assoc. prof.) R. Shipman (SRON, assist. prof.) F.P. Helmich (SRON, assist. prof.) P.R. Wesselius (SRON, assoc. prof.) B. Jones (serior scientist) W. Wild (SRON, assoc. prof.) Research Associates (postdocs) A. Cole (u) O. Möller (d) A.M.N. Ferguson (u) (NOVA) (until 2/03) N. Nagar (u) (from 3/03) Ph. Heraudeau (u) N.R. Napolitano (d) N. Kanekar (u) I. Pérez-Martín (u) (from 6/03) J.-P. Macquart (u) Emeriti T.S. van Albada S.R. Pottasch A. Blaauw H. van Woerden

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Blaauw professor K.C. Freeman Guest staff members R. Bottema R. Morganti E. Brogt T.A. Oosterloo L. Costa-Ferrer (until 5/03) P. Sanchez (until 7/03) F. Fraternali (until 11/03) W.E. Schaap W. Frieswijk (from 9/03) A.A. Schoenmaker P. Kamphuis (from 10/03) D. Setia Gunawan (until 8/03) M. Kregel (from 12/03) Ph.D. students M. Angel Aragon Calvo (u) J.T.A. de Jong (u) P. Araya Mayo (d) H.-R. Klöckner (d) G. Battaglia (u) (from 6/03) K. Kovacs (u) M. Beijersbergen (u) (until 2/03) M. Kregel (u) (until 12/03) J. Bernard-Salas (u) (until 10/03) A. Labiano-Ortega (u) R. Boomsma (u) B. Letarte (u) M. Brentjens (n) N. Mohammed (d) S. Cazaux (u) E. Noordermeer (u) F. Christen (u) M. Obric (n) B. Emonts (u) D. Poelman (u) (from 9/03) K. Fathi (u) (from 9/03) E. Romano-Diaz (d) M.E. Filho (d) (until 5/03) G. Sikkema (u) (from 9/03) K. Ganda (u) (from 9/03) F. Simatupang (d) C. Gonzalez-Garcia (d) (until 5/03) H. Spoon (u) (until 12/03) B.W. Holwerda (d) General Co-ordinator G. de Vries (u) Computing staff J.P. Terlouw (u) R Vermeij (d) (ASTRO-Wise) E. Tiesinga (u) M.G.R. Vogelaar (u) M. Tempelaar (d) W. Zwitser (u) Technical personnel Library D.R. Boxhoorn (u) (NOVA) G. Comello (u) (0.8) G. Comello (u) (0.2) G.J. Gerlofsma (u) (NOVA) Secretariat M.G. Alberts (u) (0.7) J. Zwegers-Morris (u) (0.7) H. Zondervan-Kimsma (u) (0.6)

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APPENDIX IX : Organisation of the Kapteyn Astronomical Institute

Director of Research Director of Education P.C. van der Kruit J.M. van der Hulst General co-ordinator G. de Vries Management Team P.C. van der Kruit (chair) G. de Vries J.M. van der Hulst H. Zondervan-Kimsma Raad van Advies (Advisory council) C. Boersma (student) (until 3/03) R.F. Peletier (from 10/03) R. Boomsma (from 4/03) B. Sanders J.T.A. de Jong (until 4/03) M.G.R. Vogelaar J.M. van der Hulst G. de Vries P.C. van der Kruit (chair) P.R. Wesselius (SRON) F. Lugt (student) (from 3/03) H. Zondervan-Kimsma Education Committee student members M.G. Alberts (secretary) W. Aaldering (until 9/03) R. Boomsma (advisor) from 3/03) J. van Bethlehem J.M. van der Hulst (advisor) F. Oostenbrug (until 3/03) J.T.A. de Jong (advisor) untio (3/03) T. van der Laan (from 9/03) K.H. Kuijken (until 6/02) S. Peters (from 9/03) M. Spaans (from 9/02) E. Platen (until 9/03) R.H. Sanders (from 9/02) E. Starkenburg (from 3/03) A.G.G.M. Tielens (chair from 9/03) F. Lugt (ASO) M. Vogelaar (advisor) G. de Vries (advisor) R. van de Weijgaert (chair until 9/03) Education Committee (Raad van Advies)

M.G. Alberts (secretary) A.G.G.M. Tielens J.M. van der Hulst (chair) G. de Vries F. Lugt R. van de Weijgaert Groningen members of the National Astronomy Education Committee P.D. Barthel (chair) L. Vermaas

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Study advisor Study co-ordinator M.C. Spaans (from 10/03) G. de Vries R. van de Weijgaert (until 10/03) Library Committee W. Jellema N.G. Douglas P.D. Barthel J.W. Pel G. Comello R. van de Weijgaert PhD-supervisorcommittee P.D. Barthel R. van de Weijgaert R.H. Sanders G. de Vries M.C. Spaans Members of committees of the Faculty of Mathematics and Natural Sciences Faculty Council Finance Committee C. Ormel C. Ormel Library Committee Comittee Education and Research G. Comello C. Ormel P.D Barthel Dutch Graduate School for Astronomy (NOVA) NOVA is a federation of research institutes from the universities of Leiden (Sterrewacht, Leiden), Amsterdam and Utrecht (together forming the Center for High Energy Astrophysics CHEAF), Groningen (Kapteyn Astronomical Institute) and the Department of Astronomy and Nuclear Physics of the Vrije Universiteit Amsterdam. Board P.C. van der Kruit (chair) P.T. de Zeeuw (director) E.P.J. van den Heuvel (vice-chair) W. Boland (deputy director) G.K. Miley R.T.A. Witmer (financial control) J. Kuipers M. Zaal (secretary) A. Achterberg J.A.M. Bleeker (observer) H.R. Butcher (observer) NOVA International Advisory Board J. Bahcall (Princeton, chair) M. Rees (Cambridge, UK) R. Ekers (Australia Telescope) F. Shu (Tsing Hua and Berkeley) K. Freeman (Mt. Stromlo, Australia) R. Sunyaev (Max Planck, Munich)

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APPENDIX X : Telephone numbers and electronic mail addresses

Tel. Name user@astro.rug.nl 050–3634089 Albada, Prof. Dr. T.S. van T.S.van.Albada

4073 Alberts, Mevr. M.G. M.G.Alberts 6647 Aragon Calvo, Drs. M.A. M.A.Aragon 4060 Araya Melo, Drs. P. P.Araya 4064 Barthel, Dr. P.D. P.D.Barthel 4081 Battaglia, Mevr. Drs. G. G.Battaglia 4059 Begeman, Dr. K. K.Begeman 4084 Blaauw, Prof. Dr. A. A.Blaauw 4091 Boersma, C. C.Boersma 4078 Boomsma, R. Drs. R.Boomsma 4091 Bos, N. N.Bos 4087 Bottema, Dr. R. R.Bottema 4056 Boxhoorn, Drs. D.R. D.R.Boxhoorn 8326 Brentjens, Drs. M.A. M.A.Brentjens 4057 Bruyn, Prof. Dr. A.G. de A.G.de.Bruyn 8689 Buddelmeijer, H. H.Buddelmeijer 4098 Christen, Drs. F. F.Christen 8321 Cole, Dr. A. A.Cole 4050 Comello, G. G.Comello 4088 Douglas, Dr. N.G. N.G.Douglas 4053 Emonts, Drs. B.H.C. B.H.C.Emonts 4083 Frieswijk, Drs. W.F. W.F.Frieswyk 8322 Ganda, Mevr. Drs. K. K.Ganda 4061 Helmich, E.M. E.M.Helmich 4036 Heraudeau, Dr. Ph. P.Heraudeau 4095 Holwerda, Drs. B.W. B.W.Holwerda 4054 Hulst, Prof. Dr. J.M. van der J.M.van.der.Hulst 4095 Jones, Dr. B. B.Jones 4091 Jong, Drs. J.T.A. de J.de.Jong 8322 Kamphuis, P. P.Kamphuis 6519 Koopmans. Dr. L. L.Koopmans 4078 Kemper, P. P.Kemper 4085 Kovac, Drs. K. K.Kovac 4098 Kregel, Drs. M. M.Kregel 4062 Kruit, Prof. Dr. P.C. van der P.C.van.der.Kruit 4089 Kuijken, Dr. K.H. K.H.Kuijken 4083 Letarte, Drs. B. B.Letarte 4078 Loenen, A.F. A.F.Loenen 4060 Mohamed, N.M.A. N.M.Mohamed 4080 Morganti, Mevr. Dr. R. R.Morganti

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Tel. Name user@astro.rug.nl 4095 Nagar, Dr. N.M. N.M.Nagar 4087 Napolitano, Dr. N. N.R.Napolitano 4098 Noordermeer, Drs. E. E.Noordermeer 4063 Obric, Mevr. Drs. M. M.Obric 4080 Oosterloo, Dr. T.A. T.A.Oosterloo 4091 Ormel, Drs. C.W. C.W.Ormel 4082 Pel, Dr. J.W. J.W.Pel 6647 Peletier, Dr. R.F. R.F.Peletier 4036 Pérez Martin, Dr. I. I.PerezMartin 4078 Platen, E. E.Platen 4063 Poelman, Drs. D. D.Poelman 8689 Polko, P. P.Polko 4097 Pottasch, Prof. Dr. S.R. S.R.Pottasch 4053 Ripamonti, Dr. E. E.Ripamonti 4085 Romano-Díaz, Drs. E. E.Romano-Diaz 4057 Sancisi, Prof. Dr. R. R.Sancisi 4065 Sanders, Prof. Dr. R.H. R.H.Sanders 4085 Schaap, Drs. W.E. W.Schaap 4098 Schneider, Drs. T. T.Schneider 4061 Seekles, D. D.Seekles 4063 Serra, Drs. P. P.Serra 4087 Sikkema, Drs. G. G.Sikkema 4094 Spaans, Dr. M. M.Spaans 8326 Tempelaar, Dr. M.J. M.J.Tempelaar 4068 Terlouw, J.P. J.P.Terlouw 4092 Tielens, Prof. Dr. A.G.G.M. X.Tielens 4017 Tiesinga, E. E.Tiesinga 8323 Tolstoy, Dr. E. E.Tolstoy 6625 Trager, Dr. S.C. S.Trager 4011 Valentijn, Dr. E.A. E.A.Valentijn 4077 Verheijen, Dr. M.A.W. M.A.W.Verheijen 8326 Vermeij, Drs. R. R.Vermeij 4053 Villalobos, Drs. A. A. Villalobos 4096 Vogelaar, Drs. M.G.R. M.G.R.Vogelaar 4076 Vries, Mevr. Drs. G. G.de.Vries 4086 Weijgaert, Dr. M.A.M. van de R.van.de.Weygaert 4066 Woerden, Prof. Dr. H. van H.van.Woerden 8689 Wolk, G. van der G.van.der.Wolk 4055 Zaroubi, Dr. S. S.Zaroubi 4075 Zondervan, Mevr. H. H.Zondervan 4073 Zwegers-Morris, Mevr. J.I. J.I.Zwegers-Morris 4071 Zwitser, W. W.Zwitser

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Laboratorium voor Ruimteonderzoek (SRON) Tel. Name user@sron.rug.nl 050–3638936 Adema, Ir. J. J.Adema

4026 Barkhof, J. J.Barkhof 8287 Baryshev, A.M. A.M.Baryshev 4053 Gerlofsma, G.J. G.J.Gerlofsma 4031 Graauw, Dr. M.W.M. de Th.de.Graauw 4799 Helmich, Drs. F. F.Helmich 8287 Hesper, Dr. R. R.Hesper 4058 Jellema, Drs. W. W.Jellema 4035 Drs. P. Mena Mena P.Mena.Mena 4043 Dr. P.R. Roelfsema P.R.Roelfsema 7753 Shipman, Dr. R. R.Shipman 4038 Wesselius, Dr. P.R. P.R. Wesselius 6243 Wild, Dr. W. W.Wild

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APPENDIX XI : Address

KAPTEYN ASTRONOMICAL INSTITUTE Address: (mail) Postbus 800, 9700 AV Groningen, visit: Landleven 12, 9747 AD Groningen. Telephone: 31 – (0)50 – 3634073 Telefax: 31 – (0)50 – 3636100 Electronic mail: secr@astro.rug.nl World Wide Web: http://www.rug.nl/sterrenkunde Redactie: P.C. van der Kruit Opmaak: M.G. Alberts Bijlagen: M.G. Alberts en J.I. Zwegers-Morris Druk: Regenboog, Groningen ISSN: 0925-5826