KAPTEYN ASTRONOMICAL INSTITUTE 2004

KAPTEYN ASTRONOMICAL INSTITUTE

University of Groningen

ANNUAL REPORT

2004

Groningen, May 2005

Cover: Portrait of prof. A. Blaauw painted by Janneke Viegers in 2003 for the collection of emiriti professors in the Faculty Room of Mathematics and Natural Sciences of the University of Groningen.

CONTENTS 1. FOREWORD............................................................................................ 1 2. EDUCATION............................................................................................ 7 3. RESEARCH ............................................................................................10

3.1 History of astronomy .........................................................................10 3.2 Solar System.....................................................................................11 3.3 Stars..................................................................................................11 3.4 Circumstellar Matter, Interstellar Medium and Star Formation ..........12 3.5 Structure and Dynamics of Galaxies .................................................17 3.6 Quasars and Active Galaxies ............................................................32 3.7 Clusters, High-Redshift Galaxies and Large Scale Structure............36 3.8 Computing at the Kapteyn Astronomical Institute..............................46 3.9 Instrumentation .................................................................................48

APPENDIX I : PUBLICATIONS 2004 ...............................................................57 I.1 Papers in scientific journals, books..........................................................57 I.2 Conference papers ..................................................................................65 I.3 Dissertations............................................................................................74 I.4 Popular articles........................................................................................75

APPENDIX II : Participation in scientific meetings............................................77 APPENDIX III : Visits to institutes abroad.........................................................87

III.1 Work visits .............................................................................................87 III.2 Observing trips.......................................................................................90

APPENDIX IV : Colloquia, popular lectures......................................................93 IV.1 Colloquia given outside Groningen........................................................93 IV.2 Popular lectures ....................................................................................95

APPENDIX V : Colloquia in Groningen.............................................................97 APPENDIX VI : Visiting scientists in Groningen .............................................103 APPENDIX VII : Memberships, etc.................................................................105 APPENDIX VIII : Personnel (Dec. 31, 2004) ..................................................111 APPENDIX IX : Organisation of the Kapteyn Astronomical Institute...............113 APPENDIX X : Telephone numbers and electronic mail addresses ...............115 APPENDIX XI : Address .................................................................................119

1

1. FOREWORD

This annual report follows the usual format. The staff of the Kapteyn Astro-nomical Institute is responsible for the educational program in astronomy at Groningen University and for the astronomical research, including development of instrumentation. 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. General

Joe Silk was appointed the Blaauw visiting professor for 2004. He visited the Institute for a month and will visit again in the course of 2005. Joe did give the Blaauw lecture on "Formation of the Galaxies" on November 16, 2004. Amina Helmi won the Christiaan Huygens Science Prize 2004 for her disser-tation "The formation of the Galactic Halo" (University of Leiden – cum laude dissertation). The prize was presented by the Minister of Education, Culture and Science on October 28, 2004, from 14.30 in the "Oude Kerk" in Voorburg. The Christiaan Huygens Prize exists since 1998. The winner gets an amount of 10.000 euro, a deed and a bronze statue of Christiaan Huygens. The jury is put together by the Royal Academy of Sciences (KNAW). The annual prize is meant for a researcher who defended a dissertation which gives a highly origi-nal and important contribution to a certain discipline. On April 12, Prof. Adriaan Blaauw celebrated his 90th birthday. This was com-memorated with a reception on Saturday April 17 at Castle Nienoord in Leek, hosted jointly with Leiden Observatory, where Adriaan has spend also a major part of his career. The gathering was attended by a very large group of indi-viduals from the Netherlands and abroad that have played major parts in Adriaan's career and astronomical life. Most appropriately, Adriaan wrote the introductory chapter "My cruise through the world of astronomy" in the 2004 issue of the Annual Review of Astronomy and Astrophysics. Georg Comello received a royal distinction and was knighted “Ridder in de Orde van Oranje Nassau” for his work as an amateur variable star observer. At the meeting of the American Association of Variable Star Observers in July in Berkeley, Georg was honoured with the highest “Observing Achievement Award” for providing more than 100,000 visual observations; in fact he reported 105,865 observations over the period 1966 to 2003. On June 6 the permanent staff of the Institute held a retreat at the Piloersema-borg in Den Ham, discussing for a full day aspects of the future of the Institute. The Kapteyn Astronomical Institute has adapted its by-laws to adapt to the changing organizational structure of universities in the Netherlands. This involved the formal institutioning of the adjunct-director (and Thijs van der Hulst was appointed as such), the Management Team and the Advisory Council

(Raad van Advies). The latter body has representations from all parts of the Institute and meets regularly with the directorate and Management Team. With all initiatives that the Institute is involved in (NOVA instrumentation initia-tives for the VLT, VST and ALMA, OmegaCen, AstroWise, CHAMP+, LOFAR, etc.) the number of persons working in the Zernike Building is steadily increas-ing. Already the Institute and SRON-Groningen have been assigned more office and laboratory space in the building and during 2004 this was even further increased at the top floor. More space was secured on a temporary basis. During 2005 the major part of this floor (and the full two other floors) will be occupied by astronomy and space research activities. The Kapteyn Astronomical Institute was this year responsible for the organi-zation of the Netherlands Astronomers Conference. This is a meeting spread over three days where all staff and students in astronomy in the Netherlands and in Flanders gather to discuss scientific issues. The meeting was held at the Frisian island of Vlieland on 26, 27 and 28 May and was very successful. The organization was very ably coordinated by Rien van de Weijgaert. Education

The new bachelor/master system entered its third year. While this system has slowly stabilized, discussion has started about the introduction of a major/minor system. Under this regime a student would get a bachelor in Natural Science and Technology and major in astronomy. Other majors within this bachelor are mathematics, physics and chemistry. The planning is to start with the bachelor in Natural Science and Technology in 2006. A committee consisting of several astronomy staff members and students has defined the content of the astro-nomy major program. Further development of the new program will take considerable effort, but has the advantage that we will be able to offer students a flexible program so they can tailor the bachelor to their own interest and career perspective. The new curriculum for Instrumentation and Informatics in Physics, Astronomy and Space Research has started. There were a few students who took the first courses. The curriculum is supported by the Kapteyn Institute, the Kernfysisch Versneller Instituut (KVI), Technical Physics, ASTRON and SRON. The hope is that it will attract many students in the future. The program will be advertised internationally. The total number of students at the end of 2004 was 37. 3 students received a masters degree. The staff of the Kapteyn Institute taught 19 courses. NOVA

The Netherlands Research School for Astronomy (NOVA) consists of the astro-nomical research institutes of the Universities of Amsterdam, Groningen, Leiden and Utrecht and the astronomy department at the Radboud University of Nijmegen. It has been awarded extra funding in the "bonus-incentives scheme" (in Dutch "dieptestrategie") for top research schools in the Netherlands in 1998. In 2004 this program was evaluated and the Minister decided to continue all the six research schools that are receiving such funding. 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 in the advice to her by the NWO Board, the Minister did not provide additional funds over and above what was

3

foreseen at the start of the scheme. In 2004 the final plans for Phase 2 been defined and adapted to the funding provided. In the meantime astronomers in the Netherlands have started to think and discuss how to proceed with the NOVA program after its termination at the end of 2008. The fist step that was started and will be completed during 2005 is the writing of a Strategic Plan for Astronomy in the Netherlands for the period up to about 2015. 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 91 published papers in refereed journals, 81 contributions to printed conference proceedings and 5 Ph.D. theses. In this year staff members gave 34 invited reviews and contributions at international meetings and 44colloquia at other institutes. The number of foreign researchers visiting Groningen was 74. 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 2004 in the following table. Again there is a wide range in both categories. Area Papers Facility Papers General 14 Radio 14 Solar System 1 (Sub)millimeter 4 Star Formation/ISM/CSM 29 Optical/near IR 25 Galaxies 29 Space 13 Active Galactic Nuclei 6 Theory/interpretation 32 Large Scale Structure/ Cosmology

7 Instrumentation 3

Surveys 6 Laboratory 1 NOVA supports so-called NOVA colloquium speakers. These are senior scien-tists from abroad who are invited to visit the Netherlands and give colloquia at some or all of the NOVA participating institutes. In 2004 these were Sandra Faber (Univ. California, Santa Cruz), Alex Szalay (Johns Hopkins), Zoltan Haiman (Columbia), Paul Schechter (MIT), Donald Goldsmith (Berkeley), Norm Murray (CIYA), Jim Houck (Cornell), Eva Grebel (Basel), Luis Ho (Pasadena), Massimo Stiavelli (Baltimore)

Staff

Three new staff members arrived during 2004, namely Leon Koopmans, Saleem Zaroubi and Marc Verheijen. 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./annexuk.pdf). Such appointments 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 since 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 successful 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 2004 staff already present could opt for being evaluated and channeled into the system if appropriate. Reynier Peletier participated successfully in that exercise. Early 2005 he was appointed adjunct professor in extragalactic obser-vational and instrumentational astronomy. 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 on July 1, 2004. Jacqueline van Gorkom was formally appointed on a special visiting professor-ship in extragalactic radio astronomy on behalf of the Leonardo da Vinci Foundation. In an appointment shared between the University of Groningen and ASTRON, Wim Brouw started work related to LOFAR at the end of the year. A special professorship in radio synthesis techniques and signal processing was requested also from the Leonardo da Vinci Foundation to be made effective early in 2005. Georg Comello has worked at the Kapteyn Institute for more than 40 years and ended his position as institute librarian. However, he continues to work in various supporting capacities at the Institute on a part-time basis. Hilda Koster took over the responsibility for the library. The zero-appointment of Paul Wesselius was extended for another two years. In the area of postdocs, 4 left in 2004 (Nissim Kanekar, J.-P. Macquart, Ole Möller, Neil Nagar), while also 2 new appointments were made (Emanuele Ripamonti, Martin Smith). Five persons defended their theses and obtained their Ph.D. in 2004: Stéphanie Cazaux, Hans-Rainer Klöckner, Emilio Romano Díaz, Leslie Hunt and Kambiz Fathi. Electronic versions (in pdf format) of these theses are avail-able via the Web-site of the Institute. During 2005 10 new Ph.D. students started in Groningen: Alicia Berciano Alba, Wilfred Frieswijk, Jonathan Heiner, Willem Jellema, Peter Kamphuis, Yang Shyang Li, Chris Ormel, Teffie Schneider, Paola Serra, Alvaro Villalobos. The total number of Ph.D. students at the end of 2004 was 27. They are funded through various channels: 4 on the regular Institute budget, 14 on other University appointments, 4 Ubbo Emmius grants, 1 NOVA, 3 NWO and 1 on external funds (including the European Union). As I reported last year, 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

5

Kapteyn and Adriaan Blaauw. The Van Rhijn family was received in the Kapteyn Room and shown the location of the drawing during a visit to the Institute on Dec. 1, 2004. Many staff members have contributed to this Annual Report, but I am particu-larly grateful to Gineke Alberts and Jackie Zwegers-Morris for their work on its preparation. Groningen, July 2005 Pieter C. van der Kruit Director

7

2. EDUCATION

Astronomy Students

Per 31 December 2004, 23 older-year students were registered with Astronomy as their principal subject. There were 7 older-year ‘Physics and Astronomy’ students registered with Astronomy as their principal subject; The table below lists the number of students in the past 12 years:

Table 1 - Number of students in the last 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 2004 37

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 7 women among the 30 older-year students. The analysis of students in year and achievement (as of 31–12–2004) is as follows:

next exam: number of students: per year: propedeuse 17 of which 7 1st year’s 5 2nd 1 3rd 1 4th 0 5th 2 6th + more bachelor 2 of which 1 2nd year’s 1 3rd doctoraal 19 of which 2 4th 4 5th 13 6th + more

The table below (in 2 parts) gives some statistics (as of 31-12-2004) concerning the progress of students since 1985:

Year 85 86 87 88 89 90 91 92 93 94 No 1st year (31 Dec) 14 6 5 13 7 10 13 9 9 10 Influx after the propedeuse 12 1 0 1 3 4 2 2 0 4 No. of females 4 0 0 0 0 3 1 1 1 5 Gained propedeuse 8 5 3 10 6 8 11 7 6 8 Propedeuse in 12 months 5 0 0 5 0 1 3 3 1 3 Doctorandus degree 6 3 3 8 3 5 6 5 5 5 Ph.D. Study 3 1 1 5 2 3 4 5 1 5 Stopped/switched 9 5 3 5 4 8 11 6 6 5

Year 95 96 97 98 99 00 01 02 03 04 No 1st year (31 Dec) 18 14 14 10 22 15 16 11 8 7 Influx after the propedeuse 4 0 1 1 0 1 0 0 0 0 No. of females 1 2 1 1 6 3 3 2 3 2 Gained propedeuse 15 7 8 8 13 8 3 - 1 - Propedeuse in 12 months 8 4 4 4 8 1 3 1 1 - Doctorandus degree 8 4 7 2 1 - - - - - Ph.D. Study 5 4 5 2 1 - - - - - Stopped/switched 13 10 8 6 12 12 13 9 2 0

• Based on a period of 18 years (from 1985 through 2002), 54% of the

students gain their propedeuse, and 26% 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.

9

• 61% of the total number of students during the years from 1985 to 2002 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 fairly high percentage of the doctorandi (54% during the years '85–'99) continue with a Ph.D.-study.

Examinations

The following examinations were taken in 2004: Propedeuse: T.P.R. van der Laan, D.D. Land, B. Scholten Finals: J.S. Heiner, C.W. Ormel, L. Vermaas

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.C. Spaans (student counsellor) and Ms. 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 organizing 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 communication with the coordinator can be established. Individual discussions between students and the coordinator take place regularly. Meetings of the Education Committee were held twice per term during 2004. Lectures

In 2004 the following lectures were given: 1st semester (2nd quarter) and 2nd semester courses 2003/2004: The Evolving Universe P.D. Barthel, B. Holwerda Introductory Astronomy 1B J.M. van der Hulst Astrophysics A S. Zaroubi, J.R. Macquart Astrophysics B M.C. Spaans Galaxies A. Helmi High Energy Astrophysics R.H. Sanders Recent research E. Tolstoy Cosmology M.A.M. van de Weygaert Observing Techniques in Astronomy II A.G. de Bruyn, J.W. Pel

Stellar Evolution S.C. Trager Computer course M.G.R. Vogelaar 1st semester courses 2004/2005: Introductory Astronomy 1A P.D. Barthel Statistical methods R.F. Shipman Dynamics of Galaxies R.H. Sanders Astrophysics B M.C. Spaans Introductory Astronomy 1B J.M. van der Hulst Signal Processing in Astronomy R.F. Peletier Observing Techniques in Astronomy I N. Douglas, R.F. Peletier Large Scale Structure of the Universe M.A.M. van de Weygaert In Utrecht interacademical lectures were given on the theme “History of Astronomy” during the first months of 2004. Outreach

Staff members of the Kapteyn Institute are spending an increasing amount of time on education and outreach. Several projects for schools and the general public were carried out. Barthel taught the first course for the Groningen Children's University, for 1200 elementary school kids. He is also is involved in the set-up of the Groningen University Academy for high school students, and became member of a (national) committee to revise the Dutch high school physics curriculum.

3. RESEARCH

3.1 History of astronomy

Adriaan Blaauw wrote a concise biography of A. van Maanen for the Biographic Encyclopedia of Astronomers (editor Th. Hockey, to be published by Kluwer Academic Publishers). He also wrote the article Early Encounters with Viktor Amazaspovich Ambartsumian for a memorial volume edited by Elma Parsamyan, to be published by the Armenian Academy of Sciences.

History of Radio Astronomy At the 2003 General Assembly in Sydney, the International Astronomical Union (IAU) formed a Working Group on Historic Radio Astronomy. As a member of this Working Group, and in collaboration with Strom (ASTRON, Dwingeloo), Van Woerden is bringing together documentation on early radio telescopes in The Netherlands. The project is essentially complete for the Kootwijk 7.5-meter Würzburg, used for the early 21-cm line surveys of Galactic neutral hydrogen,

11

and for several other Würzburg dishes; it is well advanced for the Dwingeloo 25-meter dish. Documentation for the Westerbork Synthesis Radio Telescope will also be assembled.

3.2 Solar System

Cometary X-ray emission Strong X-ray and far-ultraviolet emission from comets is the direct result of charge exchange reactions of solar wind ions with the neutral coma of comets. Together with Bodewits and Hoekstra (KVI, Groningen), Tielens has continued his analysis of the X-ray emission from comets. The KVI is a world leader in experimental studies of state-selective cross sections of electron capture and these have been used to predict cometary line emission. Specifically, these have been used to model the He line emission. The results show that helium line ratios are a direct diagnostic of the solar wind velocity, while their absolute intensities are linked to the local density of the solar wind. In addition, spectral lines due to other species with energies greater than 650 eV contain a wealth of information on the original composition of the wind, while lines at lower ener-gies are used best to study the interaction processes themselves.

3.3 Stars

Late phases of stellar evolution Infrared spectroscopy is a powerful tool to probe the inventory of solid state and molecular species in circumstellar ejecta. Together with Justtanont (Stockholm Observatory), and others, Tielens has analyzed the infrared spectrum of the Asymptotic Giant Branch star W Hya, obtained by the Short and Long Wave-length Spectrometers on board of the Infrared Satellite Observatory. These spectra show evidence for the presence of amorphous silicates, aluminum oxide, and magnesium-iron oxide grains, as well as molecular absorption bands due to H2O, OH, CO, CO2, SiO, and SO2. This source is the only one for which high-resolution Fabry-Perot spectra of the three CO2 bands in the 15 �m region could be obtained. In these data, the bands are resolved into individual Q-lines in emission, which allows the direct determination of the excitation temperature and column density of the emitting gas. This reveals the presence of a warm (~450 K) extended layer of CO2 between the photosphere and the dust forma-tion zone.

Physics and chemistry of gas in planetary nebulae Pottasch in collaboration with Beintema (SRON, Groningen), Feibelman (NASA), Surendiranath (Bangalore), Hyung (Korea) and Garcia-Lario (Vilspa), has derived accurate chemical abundances and physical condi-tions of several planetary nebulae (PNe) using ISO data. Together wit Bernard-Salas (Cornell Univ.) and others, abundances have been derived in a Magellanic Cloud plane-

12

tary nebula SMP 83 using data obtained in the Spitzer satellite observatory. These data have been interpreted in order to better understand the nucleosyn-thesis history of the progenitor star. Most of the nebulae studied are fainter nebulae which have undergone only the first and third dredge-up stages during the AGB phase and are therefore carbon rich. 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.

Ca triplet metallicity index Cole, with Tolstoy, Gallagher (Wisconsin), Smecker-Hane and Bosler (Irvine) published a new calibration of the calcium triplet metallicity index based on a sample of open clusters added to the traditional globular cluster sample. Contrary to some expectations, the linear relation between Ca triplet line strength and metallicity was preserved up to solar metallicity and for clusters as young as 2 Gyr. Further work on this subject is urgently needed, as more groups attempt to measure the abundance distributions in giant galaxies like M31 and M33. Cole and Tolstoy obtained calcium triplet spectra using the AF2/WYFFOS spectrograph at the William Herschel Telescope, measuring tens of giants in a sample of twelve Galactic open clusters spanning the metallicity range from -0.7 < [Fe/H] < +0.3 and ages from 0.9–9 Gyr. This will provide the broadest calibration yet of the Ca triplet metallicity index for individual red giants.

3.4 Circumstellar Matter, Interstellar Medium and Star Formation

PAHs as carriers of diffuse interstellar bands Spaans, Ruiterkamp (Leiden), Cox (Amsterdam), Kaper (Amsterdam), Foing (ESTEC) and Ehrenfreund (Leiden/Amsterdam) have investigated the proper-ties 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, the translucent cloud HD 147889 has been modeled 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 wavelength and strength of electronic transitions in a large set of PAH molecules, the computation of electronic spectra, that can be compared to observations, was possible. Good agreement was found for the line of sight toward HD 147889 and it was concluded that

13

small PAHs, with less than NC = 50 carbon atoms, provide a good fit to the observations of HD 147889 given the dependence of PAH ionization potentials and electronic band strengths on NC.

The profile of the interstellar 10 micron silicate feature Together with F. Kemper (UCLA), Vriend and Tielens have studied the dust along the line of sight toward the Galactic center using Short Wavelength Spectrometer data obtained with the Infrared Space Observatory. In this way, this group has derived a very accurate profile for the silicate band. This inter-stellar absorption band is exceedingly smooth and featureless and is well re-produced using a mixture of 15% amorphous pyroxene and 85% of amorphous olivine by mass. Moreover, in contrast to silicates around Asymptotic Giant Branch stars, there is no evidence for substructure due to crystalline silicates. This implies that crystalline silicates injected by these stellar objects are rapidly amorphized in the interstellar medium.

H2 formation in the interstellar medium The most abundant interstellar molecule, H2, is generally thought to form by recombination of H atoms on grain surfaces. Cazaux, in collaboration with Tielens, has developed a model for molecular hydrogen formation on surfaces of astrophysical relevance. This model solves the time-dependent kinetic rate equation for atomic and molecular hydrogen and their isotopes, taking the presence of physisorbed and chemisorbed sites, as well as quantum mechani-cal diffusion and thermal hopping, into account. The results show that the time evolution of this system is mainly governed by the binding energies and barriers against migration of the adsorbed species. The results of this model are bench-marked against laboratory experiments on the formation of HD on silicate and carbonaceous surfaces under irradiation by atomic H and D beams at low and at high temperatures. Implications for the formation of H2 in the interstellar medium are assessed and it is demonstrated that H2 formation can be efficient even at elevated dust temperatures.

The IR emission features and the star formation rate Together with Peeters (NASA Ames) and Spoon (Cornell), Tielens has studied the interrelationship of the well-known IR emission features at 3.3, 6.2, 7.7, and 11.2 micron and the star formation activity of galaxies. These features trace the FUV stellar flux and are thus a measure of star formation. Based upon an ex-tensive data set of 2.5–40 micron SWS spectra obtained with the ISO satellite, this group has examined the IR spectral characteristics of Galactic massive star-forming regions and of normal and starburst galaxies, as well as active galactic nuclei (AGNs) and ultraluminous infrared galaxies (ULIRGs). This has lead to the development of a new mid-infrared (MIR)/far-infrared (FIR) diagnos-tic diagram based on our Galactic sample, which has been compared to previ-ous diagnostic tools. It is concluded that, under well defined restrictions, the strength of the IR emission features can be related to the star formation rate.

14

The Excitation of Water in the S140 PDR Spaans and Poelman have considered the excitation of water in the photon-dominated region (PDR) S140. With the use of a two- and three-dimensional escape probability method the level populations of ortho- and para-water up to 350 K (i.e., the first 8 levels), as well as line intensities for various transitions, were computed. Density, temperature and abundance distributions inside the cloud were computed with the use of a self-consistent physi-chemical PDR model in order to reproduce the observed line intensities with SWAS. Predic-tions have been made for the HIFI instrument on Herschel.

The Polytropic Equation of State of Primordial Gas Clouds Spaans and Silk (Oxford) have computed the polytropic equation of state (EOS) of primordial gas clouds with modest enrichment, motivated by the recent observations of very Fe-deficient stars, [Fe/H] ~ 10-3.5–10-5, such as HE 0107–5240 and CS 29498-043. These stars are overabundant, relative to Fe, in C and O. It is assumed that the observed abundances of species like C, O, Si and Fe are representative of the gas from which the currently observed metal-defi-cient stars formed. Under this assumption, it is found that this primordial metal abundance pattern has profound consequences for the thermal balance and chemical composition of the gas, and hence for the EOS of the parental cloud. The polytopic EOS is soft for low, [O/H] < 10-3, oxygen abundances, but stiffens to a polytropic index � large than unity for [O/H] > 10-2 due to the large opacity in the CO and H2O cooling lines. It is further found that a regulating role is played by the presence and temperature of the dust, even when the overall carbon abundance is only [C/H] ~ 10-2 . When the dust is warmer than the gas, a region with � ~ 1.2 results around a density of ~104 cm-3. When the dust is colder than the gas, a region with � ~ 0.8 is found for a density of ~106 cm-3.

Models for interpreting waterline observations Poelman has continued his PhD project under supervision of Tielens, Spaans, and Helmich (SRON). It involves creating a state-of-the-art computer model (3D Monte Carlo radiative transfer code) to reanalyze and interpret existing obser-vations of H2O in different environments, and to make predictions for the line intensities of submillimeter lines to be observed with the HIFI instrument on board of the Hershel telescope. This model will be used to study water in differ-ent astrophysical environments, e.g., molecular clouds and disks around young stellar objects. A detailed model has been constructed to investigate the excitation of water in the S140 Photon Dominated Region (PDR). The S140 molecular cloud lies at a distance of ~900 pc (Crampton & Fisher 1974) and is illuminated from the south-western side by the B0V star HD 211880. The molecular cloud consists of two distinct regions. An extended molecular cloud, and the interface region at the south-west edge of the cloud (PDR). The computed temperature, density and water abundance distribution resulting from the self-consistent physi-chemical model of Spaans (1996) is used as input in the waterline transfer code of Poelman. We are able to reproduce the observed value of the 557 GHz

15

110 � 101 ground state transition of ortho-H216O, and make predictions for other

transitions of ortho- and para-H2O.

Formation of primordial stars Ripamonti and Abel (Pennsylvania State, now at Stanford) investigated the final phases of the collapse of a primordial gas cloud into a primordial star, in order to learn about the IMF of the very first stars in the universe, and in particular whether they are really very massive as hinted by several authors. This was done with both analytical and numerical methods. With the first, they investi-gated the physics of the collapse and whether fragmentation instabilities (trig-gered by previously unaccounted mechanisms, such as Collisional Induced Emission) are present. The result is that such instabilities are present, but their growth is slower than the protostellar collapse, so that actual fragmentation is unlikely. As a side they also found approximate prescriptions for modifying the H2 cooling rate in 3D simulations in order to account for the cloud optical depth. The numerical effort instead dealt with obtaining the first self-consistent 1-D simulation of the formation of a primordial star, including the poorly understood (but critical) accretion phase. This work is still in progress.

Formation of planets around T-Tauri stars Ormel started his thesis research under the supervision of Tielens and Spaans. This project concerns the question of how dust in protoplanetary disks of clas-sical T-Tauri stars coagulates to form the (interiors of gas-) planets. Although this question has been outstanding for several decades, it is still not well under-stood by which mechanism dust grows in the intermediate size (cm � km) regime. After studying some of the recently proposed candidates like radially drift induced gravitational instability and other particle concentration mecha-nisms (e.g. vortices, convective flows), Ormel focused his attention on coagu-lation processes within a turbulent environment. Shear turbulence, in particular, is of importance, since it is poised to happen as soon as the dust density in the midplane has exceeded that of the gas. It is therefore considered a crucial evolutionary stage. These aspects were all being investigated with the aim of incorporating these into detailed coagulation models.

Chemistry in regions of star formation In collaboration with Ceccarelli (Observatoire de Grenoble), Caux and Parise (CESR, Toulouse), Castet (Observatoire de Bordeaux), Tielens has continued his studies of the chemistry in regions of star formation. This study has focused on the composition of chemical composition of regions of warm gas around low mass protostars. Specifically, he has continued the unbiased spectral survey in the 350 GHz band using the JCMT of the prototypical low mass protostar, IRAS 16293–2422 (see Figure 1). This survey is complemented by surveys of the 85–281GHz bands using the IRAM 30 m telescope. The first results of this survey have revealed a dazzling array of emission lines due to complex molecules. This study demonstrates that the warm gas around low mass proto-stars harbor a wide organic inventory, including abundant amounts of formic

16

acid, acetaldehyde, methyl formate, dimethyl ether, acetic acid, methyl cyanide, ethyl cyanide, and propyne. This is supported by high resolution studies of the emission by some complex molecules in this region using the Plateau de Bure interferometer. In addition, submillimeter studies of the low mass protostar, NGC 1333 IRAS 4A, using the IRAM 30 m telescope, have revealed that the warm gas around this low mass protostar is also rich in complex organic molecules. Finally, in a separate study, triply deuterated methanol (CD3OH) was detected for the first time in space. This study revealed that this species has an abundance which is 0.01 that of isotopomer, CH3OH, despite he low interstellar elemental abundance of deuterium (0.00001)!

Infrared Dark Clouds in the Outer Galaxy Besides the study on Inner Galaxy IRDCs (Infrared Dark Clouds) Frieswijk started the search for IRDCs in the Outer Galaxy. A region which is significantly different in environment and so far neglected due to the lack of sufficient back-ground emission at 8 micron. Using the 2 Micron All Sky Survey (2MASS) Point Source Catalog (PSC) high density regions similar to IRDCs can be identified through near-IR star counts and reddening of background stars. The method has been tested on well-known Inner Galaxy IRDCs. The first candidate IRDCs in the Outer Galaxy have now been identified in a pilot region and follow-up observations with the JCMT confirm the presence of high density material. Additional observations on this pilot sample with the Effelsberg 100m tele-scope, the IRAM telescope at Pico Veleta and the JCMT are scheduled for 2005. The extraction of candidate IRDCs in the complete Outer Galactic Plane is expected to be finished late next year.

17

Figure 1: The incredibly rich line spectrum of the prototypical class 0 protostar, IRAS 16293–2422. This represents about half of the frequency window observed with the JCMT. The spectral resolution is 1.25 km/s and thetypical rms is 10–15 mK. Most of the spectral structure apparent in this figure is due to molecular rotational transitions.

3.5 Structure and Dynamics of Galaxies

Structure in the Milky Way halo Battaglia completed her work with Helmi and the Spaghetti Team on the radial velocity dispersion profile of the Milky Way halo. The aim of the project was to derive the mass and the density profile of the MW dark matter halo. The sample they used, consisting of globular clusters, satellite galaxies, field horizontal branch stars (FHB) and red giant branch stars from the Spaghetti survey, extends out to about 120 kpc and allows a reliable determination of the radial velocity dispersion profile out to very large distances. The radial velocity disper-sion shows and almost constant value of 120 km/s out to 30 kpc and then con-tinuously declines down to 50 km/s at 120 kpc. In the hypothesis of a constant velocity anisotropy, the observed declines rules out an isothermal sphere as model for the Galactic DM halo. The observed radial velocity dispersion profile is consistent with both a DM halo of mass 1.2+1.8

-0.5 × 1012 Msun following a steep density profile (Truncated Flat model) and with a halo of mass 0.8+1.2

-0.2 × 1012 Msun following a NFW mass model.

Population in dwarf spheroidals Battaglia started a preliminary analysis of the VLT/FLAMES data for the Sculp-tor, Fornax and Sextans dwarf spheroidal galaxies. For the first time spectra of stars out to the tidal radius were obtained for each of the 3 dSphs, making an analysis of their overall kinematical and metallicity properties possible. The analysis shows the presence of two stellar populations: a metal poor compo-nent more spatially extended and a "metal rich" component more centrally con-centrated. These stellar components show signs of different kinematical behaviour.

Substructures in the Galaxy: probing its formation and its dark matter halo Helmi has shown that the spatial distribution of the debris from the Sagittarius dwarf galaxy could not be used to determine the shape of the Galactic halo, due to its young dynamical age. However, more recently, radial velocities were for a large sample of M giants from the 2MASS catalog, selected to be part of the Sgr dwarf leading and trailing streams. Comparison of models of the Sgr dwarf debris orbiting Galactic potentials, with halo components of varying degrees of flattening and elongation, shows that the leading stream contains sufficiently old debris that its kinematics provide for the first time direct evidence

18

that the dark-matter halo of the Galaxy has a prolate shape with an average density axis ratio within the orbit of Sgr close to 5/3 (Figure 2).

The formation of thick disk in galaxies The formation and evolution of galaxies is one of the great outstanding problems of astrophysics. The current paradigm for the formation of structure in the Universe postulates that galaxies grow in a hierarchical fashion, through the mergers of smaller subunits. Even within this broad context, we have only a crude picture of how galaxies like our own came into existence. The aim of the PhD project of Villalobos is to develop a physical model for the formation of what seems to be one of the most ubiquitous components of late-type galaxies: the thick disk. On the one hand, the goal is to provide a detailed physical picture of how the thick disk of our Galaxy came about and in what ways it is associated to the primordial galactic building blocks. On the other hand, and using the basic assumptions of the hierarchical paradigm, he wishes to address statistical aspects of the galaxy population, such as the expected frequency of thick disks and their stellar population characteristics. The major part of the research carried out so far has consisted in: first, to learn the usage of the simulation code adopted in this project; and second, to find suitable values for the parameters in this code in order to get a good compro-mise between physical realism and efficiency. The additional codes developed thus far have to do with the generation of initial conditions, for both disk galax-ies and spherical satellites, aimed to get stable structures in time. The current stage of the project is the analysis of outcomes of several mergers simulations setted up for many relevant orbits, inclination, densities and sizes for the satel-lites.

19

Figure 2: Comparison of the velocities of stars in the Sagittarius dwarf streams (Law et al. 2004) to those predicted in numerical simulations of the evolution of Sgr in a Galactic potential with different dark halo flat-tenings: oblate, spherical and prolate (left, middle and right panel respec-tively). The best match corresponds to the prolate halo case.

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 microlensing halo will induce a clear signal in the spatial distribution of the microlensing events. The MEGA (Microlensing Exploration of the Galaxy and Andromeda) collabo-ration, consisting of de Jong, Kuijken (Leiden), Crotts, Uglesich, Alves, Czjernes (Columbia University), Sackett (Mt. Stromlo), Sutherland (Cambridge), Baltz (Stanford), Gyuk (Chicago), Widrow (Queens) is performing a survey of two large fields in M31, using special techniques to detect microlensing of un-resolved stars. Several telescopes are being used for several years, among which the Isaac Newton Telescope (INT) on La Palma. The first results, based on a two-year data set obtained at with the INT, were published. The sample of

20

14 candidate microlensing events is suggestive of the presence of a micro-lensing halo, but for a more significant signal the full dataset is needed. In 2004 de Jong continued to work on the analysis of the full four-year INT data set.

Nearby dwarf irregular galaxies Cole continued his work on the star formation and chemical evolution histories of isolated Local Group dwarf irregular galaxies. Learning the detailed distri-butions of age and metallicity in these systems will be an important test for theories of galaxy formation and evolution, constraining the roles of supernova and photoionization feedback on star formation. Spectra at the calcium II near-infrared triplet were obtained through the latter half of 2003 and early 2004 for 30–100 red giants in each of the galaxies Phoenix, NGC 6822, IC 1613, and WLM. These data are being used to investigate the temporal evolution of the dwarf galaxy mass-metallicity relation, and to elucidate the differences between dwarf spheroidals and dwarf irregulars during in the early universe. This project involves Tolstoy, Irwin (Cambridge), and Venn (Macalester). In collaboration with Gallagher and Wilcots (Wisconsin), and Taylor (Sacramento), Cole obtained deep optical images with the Hubble Space Tele-scope Advanced Camera for Surveys of the nearest starburst galaxy, IC 10. This poorly studied system lies behind the galactic plane at latitude b = –3 and is the only Local Group galaxy for which no previous color magnitude diagram reaching the horizontal branch has been obtained.

Star clusters in the Magellanic Clouds Cole continued his work on the metallicity distribution function of red giants in the Large Magellanic Cloud, measuring abundances for large samples of stars using the calcium II near infrared triplet. He found that the center of the LMC has a G dwarf problem similar to that of the Solar neighborhood. Because the LMC bar is primarily younger than 4 Gyr and contains no bulge, pre-enrichment cannot be a solution to the G dwarf problem in this galaxy. In collaboration with Tolstoy, Gallagher (Wisconsin), and Smecker-Hane (Irvine), Cole began to quantify the shallow radial abundance gradient in the LMC. In collaboration with Geisler (Concepcion), Sarajedini (Florida), and Smith (NOAO/Gemini), Cole began a major program to securely measure the abun-dances of a large sample of star clusters in the LMC. The existing catalog of metallicities is incomplete and inhomogeneous and for many clusters large uncertainties remain. Using the FORS2 spectrograph at the VLT, abundances for 38 clusters, based on 3–10 red giants per clusters, have been obtained, and the data are being analyzed to trace the age-metallicity relation and spatial patterns in chemistry of the cluster population of the LMC.

High-Velocity Clouds Together with Wakker (Wisconsin), Schwarz (Groningen and Nijmegen) and de Boer (Bonn), Van Woerden has edited a book on "High-Velocity Clouds". In 17 chapters, contributed by 23 authors, the book covers essentially all aspects of HVC research. The book has been published by Kluwer Academic Publishers.

21

For this book, Van Woerden and Wakker have reviewed available information about the distances and metallicities of high-velocity clouds. So far, a firm distance bracket based on absorption-line spectra is available for only one HVC: Complex A (5 < z < 7 kpc above the Galactic plane). Upper limits are known for Complex M and Complex WE; lower distance limits are known for Complex C, Complex H and several other HVCs. Metallicity values have been determined by several research teams, mostly using HST and, especially, the FUSE satellite. Results are summarized for Complexes A, C, M, the Magellanic Stream, and several smaller HVCs. Most metallicity values found lie between about 0.05 and 0.3 times solar, suggesting origins in intergalactic space or in Galactic satellites; for Complex M, a Galactic-Fountain origin is probable.

The Fornax dwarf galaxy In 2004, Letarte analyzed VLT/UVES spectra of 9 individual stars in 3 Globular Clusters belonging to the Fornax Dwarf Spheroidal Galaxy. The three clusters are found to be some what more metal poor than previous work using different techniques. They also found the most metal poor globular cluster known to date, Fornax Cluster 1, at [Fe/H] = –2.6. This work was done in collaboration with Jablonka and Hill (Observatoire de Paris-Meudon) and Tolstoy. The first results were presented at the ESO/Arcetri Meeting: Chemical Abundances and Mixing in Stars in the Milky Way and its Satellites, during September 2004 in Italy. In 2004 Letarte also began the reduction and analysis of a large and complex VLT/FLAMES data set of high resolution observations of 107 field stars in the centre of the Fornax dwarf. For each star, they have around 120 spectral lines, with about 60 of them being Fe I lines and some 15 other elements, including Ca, Ti, Mg, O, and Eu. The metallicity in the centre of Fornax is expected to vary from around –0.5 to –2.5 dex, which makes our sample quite challenging. Letarte spent 3 months at the Observatoire de Paris-Meudon working with Vanessa Hill to gain the required experience.

Nearby dwarf spheroidal galaxies Tolstoy has continued her work on galaxy formation and evolution with particu-lar interest in the resolved stellar populations of nearby dwarf galaxies. 2004 has been dedicated to contuining the acquisition and analysis of data for her ESO Large Programme “Dwarf galaxies: remnants of galaxy formation and corner stones for understanding galaxy evolution" with VLT/FLAMES multi-fibre spectrograph and the ESO-MP/2.2m Wide Field Imager. This programme is to study the detailed properties of many hundreds of individual stars in three nearby dwarf spheroidal galaxies. This project involves Helmi and two graduate Kapteyn students (Letarte and Battaglia) and a post-doc (Cole) and a group of international collaborators: Hill, Jablonka and Francois (Paris-Meudon); Primas, Kaufer and Szeifert (ESO); Irwin (Cambridge), Venn (Macalester), Shetrone (Texas), Abel (Penn State) Arimoto (NOAJ) and Sadakane (Osaka). They have called themselves the Dwarf Abundances and Radial velocities Team, or DART. In 2004 they published the first paper from the Large Programme as an ApJ Letter (Tolstoy et al. 2004). They reported the discovery of evidence for

22

two distinct ancient stellar components in the Sculptor dwarf spheroidal galaxy. Both components are >10Gyr old They used the ESO Wide Field Imager in conjunction with the Very Large Telescope/FLAMES spectrograph to study the properties of the resolved stellar population of Sculptor out to and beyond the tidal radius. They found that the two components are discernible in the spatial distribution of horizontal branch stars in our imaging and in the [Fe/H] and vhel

distributions for our large sample of spectroscopic measurements. They can be generally described as a “metal-poor” component ([Fe/H] � –1.7) and a “metal-rich” component ([Fe/H] � –1.7). The metal-poor stars are more spatially ex-tended than the metal-rich stars, and they also appear to be kinematically distinct. These results provide insight into the formation processes of small sys-tems in the early universe and the conditions found there. Even this simplest of galaxies appears to have had a surprisingly complex early evolution (Figure 3).

Figure 3: Here is vhel as a function of elliptical radius for all stars that were observed with VLT/FLAMES in the Sculptor dwarf spheroidal satisfying S/N > 10. The 308 stars that are potential members are plotted as asterisks ([Fe/H] > –1.7) and open circles ([Fe/H] < –1.7), while the 93 crosses are assumed to be non-members. The systemic velocity of Sculptor, at 110 km/s, is plotted as a dashed line. The dashed lines are the 3� velocity limits for membership of stars in Sculptor dwarf spheroidal. The position of the tidal radius is also marked.

Tolstoy also worked with Venn (Macalester), Shetrone (Texas), Irwin and Tout (Cambridge) and Hill (Paris-Meudon) to reanalyze a large sample of Galactic stellar abundances from the literature assigning the stars to standard Galactic components. The abundance patterns of these different Galactic components were then compared to the chemistries of stars in the Milky Way dwarf spher-oidal (dSph) satellite galaxies, from UVES based work. This allows them to

23

make a detailed comparison of the abundance properties of stars in small and large galaxies and test the role of the smaller dwarf they see around them today in a hierarchical galaxy formation scenario. There is marginal overlap in the high [�/Fe] ratios between dSph stars and Galactic halo stars on extreme retrograde orbits (V < –420 km/s), but this is not supported by other element ratios. Other element ratios compared in this paper include r- and s-process abundances, where they find a significant offset in the [Y/Fe] ratios, which results in a large overabundance in [Ba/Y] in most dSph stars compared with Galactic stars. Thus, the chemical signatures of most of the dSph stars are distinct from the stars in each of the kinematic components of the Galaxy. This result rules out continuous merging of low-mass galaxies similar to these dSph satellites during the formation of the Galaxy. However, they do not rule out very early merging of low-mass dwarf galaxies, since up to one-half of the most metal-poor stars ([Fe/H] –1.8) have chemistries that are in fair agreement with Galactic halo stars. They also do not rule out merging with higher mass galax-ies, although we note that the LMC and the remnants of the Sgr dwarf galaxy are also chemically distinct from the majority of the Galactic halo stars. Forma-tion of the Galaxy's thick disk by heating of an old thin disk during a merger is also not ruled out; however, the Galaxy's thick disk itself cannot be comprised of the remnants from a low-mass (dSph) dwarf galaxy, nor of a high-mass dwarf galaxy like the LMC or Sgr, because of differences in chemistry.

Simulation of dwarf galaxies and their chemical evolution In the framework of the results being obtained by the DART collaboration about kinematics and metallicities of stars in Local Group Dwarf Galaxies, a numerical code (based on the widely known N-body code GADGET) is being developed by Ripamonti Tolstoy, Helmi, Abel (at Pennsylvania State, now Stanford). This code is aimed at obtaining numerical simulations of dwarf galaxies, including star formation and detailed feedback effects from Supernovae and stellar winds, with particular attention to chemical properties. This code will be employed for studying the chemical evolution of dwarf galaxies (although morphological and kinematical aspects can be studied, too).

Stellar kinematics Peletier continued his involvement in the SAURON project. In 2004 a data-paper containing the stellar kinematics of 48 ellipticals and spirals in the SAURON survey was published. This is the first survey presenting 2-dimen-sional spectroscopy of nearby galaxies. With this survey one can study devia-tions from axisymmetry in galaxies. One gets a much better view on kinemati-cally decoupled cores, and their statistics. From the survey several galaxies with peculiar kinematics have been found. Work is going on to analyze the stellar kinematics in detail. Also in 2004 a significant amount of work has been put into determining the gas kinematics and the absorption line strength maps, which will lead to 2 more large data papers in 2004. Fathi presented his PhD thesis in December 2004. A large part of his thesis consists of the analysis of the gas velocity fields of the 24 spiral galaxies in the SAURON survey. Allard, a PhD student of Knapen (Hertfordshire), came to Groningen for 2 visits to analyze with Peletier a SAURON mosaic of M 100. She will study the relation

24

between the bar, the kinematics of gas and stars, and the stellar populations in the galaxy. From January to August Sanchez-Blazquez (Universidad Complutense Madrid) visited the Kapteyn Institute on a EU Marie Curie visitor grant for PhD students. In this period she finished several chapters of her thesis about central stellar populations and gradients in ellipticals. With Peletier, Vazdekis (IAC), Selam (Ankara), Gorgas (UCM), Falcon-Barroso (Leiden) and Jimenez (Granada) she finished the data paper of the MILES stellar library, a new stellar library con-taining spectra between 350 and 750 nm of 1000 stars, to be used for stellar population synthesis. In August she presented her PhD thesis in Madrid. In November Kutdemir (Ankara) came for a period of 6 months to exploit the MILES library. In 2004, Peletier, together with Cardiel (Calar Alto), Mouhcine (Nottingham), Ivanov (ESO), Falcon-Barroso (Leiden) and Ganda started a project to obtain a stellar library with a resolution of about 2000 for population synthesis in the near-infrared H and K band. Observations have been obtained at Calar Alto and further observations are scheduled at UKIRT.

Late-type spiral galaxies Ganda has been working with Peletier on a PhD project to study kinematics and stellar populations of late-type spiral galaxies (type Sb-Sd). These objects have been studied very little, since they are difficult to observe due to their low surface brightness, and complicated to analyze, since they contain large amounts of dust, and a mix of young and old stars that won't allow us to use the standard methods developed for the analysis of populations in ellipticals (single-stellar-populations models). In a collaboration with the SAURON team (mainly de Zeeuw, Falcon-Barroso, Cappellari and McDermid from Leiden) they obtained SAURON integral-field spectroscopy for a sample of 18 late-type spirals. The galaxies were selected in order to be nearby spirals of types Sb to Sd, not too faint and not known to be peculiar objects. The data will allow them to study the internal kinematics of gas and stars for our objects, as well as their stellar populations, following the methods already developed/under develop-ment within the SAURON team. This sample will be complemented with long-slit spectroscopy both in the optical (with the double-beam spectrograph ISIS at the WHT, La Palma) and near infrared (with SOFI, NTT, La Silla). These additional data will give more information to understand the star formation his-tory in late-type spirals. The work carried out so far has mainly addressed the data reduction and measurement of kinematics in the SAURON spectra, and the next goal will be the study of gas kinematics from the two-dimensional SAURON maps.

High velocity HI in external galaxies Boomsma has continued his thesis project (with van der Hulst, Sancisi, Oosterloo and Fraternali (Dwingeloo)) on the vertical structure and kinematics of HI gas in spiral galaxies. Two galaxies are studied in detail, NGC 6946 and NGC 253.

25

Last year he has concentrated on writing a paper on HI in the halo of the southern spiral galaxy NGC 253. This starburst galaxy turns out to have an HI halo similar to NGC 891 and NGC 2403, but also plumes of gas extending to 8 kpc from the disk. A starburst in the center of NGC 253 is ejecting a superwind. This superwind has probably brought up the HI from the halo layer, producing the plumes. From the data it is also clear that the HI disk of NGC 253 is much smaller than the stellar disk. The paper has been accepted for publication in Astron. & Astrophys. Boomsma has also been concentrating on sensitive HI observations of the nearby face-on spiral galaxy NGC 6946. In the direction of the inner disk of NGC 6946, large complexes of kinematically anomalous HI have been detected as well as many HI holes. Both are believed to be produced by the massive star formation in the disk. He and his collaborators also found signs for a present accretion event on the edge of NGC 6946.

Figure 4: An image of the HI distribution in NGC 6946. The contours show where HI is found with velocities anomalous to normal galactic rotation.

The study of gaseous halos Kamphuis has started a PhD study of gaseous halos around edge-on spiral galaxies. The improved sensitivity of the WSRT for local HI studies imply that we are now able to detect much fainter gas above the plane than before. Fraternali et al. (2004) nicely show this for NGC 891. For this study a diameter limited sample of 16 edge-on spiral galaxies has been constructed. His sample covers a wide range in masses, star formation rates and morphological types to be able to study correlations between galaxy properties and their halos. For 6 galaxies archival data exists and for 2 galaxies new WSRT 21 cm observations have been obtained. To obtain rotation curves at different scale heights above

26

the plane Kamphuis has written a fully automatic IDL code. The IDL code retrieves the rotation curves through the method of envelope tracing. During a visit to Australia Kamphuis and Freeman tried to find the optical cutoff radius of the galaxy NGC 2915 in the R-band. Averaging profiles along the minor axis no cutoff radius was found. This implies an upper limit of the radial cutoff �R =25.

Modified dynamics and cosmic dark matter Sanders has developed a tensor-vector-scalar theory which reconciles the gal-axy-scale success of modified Newtonian dynamics (MOND) with the cosmo-logical scale evidence for CDM. The theory contains an evolving effective potential, and scalar field oscillations in this potential comprise the cold dark matter; the de Broglie wavelength of these soft bosons, however, is sufficiently large that they cannot accumulate in galaxies. The theory predicts, inevitably, a constant anomalous acceleration in the outer solar system which, depending upon the choice of parameters, can be consistent with that detected by the Pioneer spacecrafts. Milgrom (Weizman Inst.) and Sanders have examined two corollaries of MOND pertaining to properties of the equivalent dark-matter halo. MOND predicts for pure exponential disks a tight relation involving the halo and disk scale lengths and the mean acceleration in the disk– a relation which was found to test favorably against the Verheijen sample of Ursa Major galaxies. A correlation between halo and disk length scales is also apparent when the "maximum disk" contribution is assumed, but it is demonstrated that this follows from the more general MOND prediction. The second MOND prediction involves the existence of a maximum halo acceleration which also tests favorably against the Ursa Major sample.

The mass distribution in early type disk galaxies Noordermeer continued his PhD work on the mass distribution in early-type disk galaxies, under the supervision of Van der Hulst and in collaboration with Sancisi, Van Albada and Swaters (Maryland). A major part of their study in-volves the imaging, with the WSRT, of the neutral hydrogen component in 68 galaxies of type S0 to Sab. The reduction of these observations, which are part of the WHISP survey, was finished in 2004; the results will be published in the next few months. Rotation curves were derived from the HI velocity fields, com-plemented by long-slit optical spectra for the inner regions. The rotation veloci-ties are found to rise extremely fast in the central regions, and reach maximum values of up to 400 km/s. At intermediate radii, they often decline, but they usually flatten out again in the outer parts. To study the dark matter properties of these galaxies, work continued on a careful modeling of the stellar mass distribution. Deep optical images are decomposed into bulge and disk components, and the 3D density distribution in each component is carefully measured. The bright bulges are found to domi-nate the gravitational potential in the inner regions of these galaxies and are responsible for the steep rise and subsequential decline in the rotation curves; their mass-to-light ratios are tightly constrained by the observed rotation curves. The stellar disks can explain the rotation velocities at intermediate radii, but the

27

shape of the rotation curve in the outer parts can only be understood if a sub-stantial amount of dark matter is present in these galaxies. The neutral gas is found to have little 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 seem less dark matter dominated than most late-type and dwarf galaxies.

Square Kilometer Array (SKA) preparation In preparation for the Square Kilometre Array (SKA) science case van der Hulst worked on a chapter on aspects of HI research with the SKA. These mostly concern the possibility of studying the HI content of galaxies in deep surveys (one to several months of observing time) in different environments between redshifts of z = 0 and z = 4. SKA is the prime instrument to literally determine where and when gas is turned into stars, since considerable evolution takes place over this range of redshift. The chapter addresses in addition the use of deep continuum surveys for probing star formation activity as a function of red-shift as at the nanoJy sensitivity levels that can be reached the sky is domi-nated by star forming galaxies. There is the prospect of even detecting the first black holes and the first star forming objects. This chapter was written in colla-boration with Sadler (Sydney), Jackson (ATNF), Hunt (Firenze), Verheijen and van Gorkom (Columbia University).

The Disk Mass project Verheijen continues his research project with Bershady and Westfall (Madison), Swaters (College Park), Andersen (Victoria), and Kelz (Potsdam), aiming at measuring the vertical stellar velocity dispersion of stars in the disks of 40 nearly face-on spiral galaxies. From this kinematic information, the mass sur-face density of the stellar disks can be derived and the disk-halo degeneracy in the decomposition of galaxy rotation curves can be broken. For this purpose, two custom-built wide-field Integral Field Units (IFUs) have been developed and commissioned, and are currently employed at the 3.5m telescope on Calar Alto and the WIYN facility on Kitt Peak. During eight observing runs in 2004, H-alpha velocity fields and stellar kinematics in the MgI- and the CaII-regions of the spectrum were measured using these IFUs. For the parent sample of 100 spiral galaxies, optical and near-infrared images were obtained with the 2.1m telescope on Kitt Peak. Data reduction and the development of analysis soft-ware is in progress.

28

Figure 5: Left: The P-Pak Integral Field Unit, custom-built for the Disk Mass project. The 331 object fibers span 64x74 arcsec on the sky and are surrounded by 36 sky-fibers. Together with the PMAS spectrograph at CAHA it provides a spectral resolution of R=8000. Upper left panel: A typical face-on galaxy studied by the Disk Mass project. Upper right panel: The regular H-alpha velocity field of the galaxy shown on the left. Bottom panel: Stellar absorption line spectra, azimuthally averaged in 5 radial bins. The lower spectrum originates in the outer disk at a surface brightness level of 23.9 (B-mag/arcsec2). Absorption lines from MgI and Fe are clearly visible at all radii.

Kinematics of the Low Surface Brightness galaxy DDO 39 In collaboration with Swaters (College Park) and Bershady (Madison), Verheijen has collected deep HI kinematic data on DDO 39 using the VLA in its B-configuration. The aim is to obtain an unambiguous high-precision HI rotation curve of this regular, exponential LSB disk. The data will be used to study the mass distribution in the inner region and the overall shape of the rotation curve of this dark matter dominated galaxy, and to confirm or falsify the predictions from numerical simulations of galaxy formation. In particular the central cusp and the concentration index of the dark matter density profile will be addressed.

Opacity of spiral disks from numbers of distant galaxies The PhD project of Holwerda concerns opacity measurements from the number of distant galaxies seen through a foreground disk of a spiral galaxy. These numbers were calibrated using the “Synthetic Field Method” of Gonzalez et al. (1998). The synthetic field method calibrates the number of distant galaxies

29

found for the crowding and confusion of the foreground disk, with a series of synthetic fields. These are the original science field with a dimmed deep field added. From these, the relation between the dimming of the deep field and the number of added galaxies retrieved from the synthetic field is found. This rela-tion and the actual number of distant galaxies in the science field gives an average opacity of a science field or a section thereof. In 2004, a paper des-cribing the automated method and subsequent analysis was accepted by the Astronomical Journal for publication in 2005. A companion paper detailing the radial opacity of spiral disks was also accepted. The relations between opacity and Hubble type, spiral arms and surface brightness were explored as well. The brighter regions of spiral disks and spiral arms are more opaque then the rest of the disk. Evidence of the patchy nature of dust in disk was found from the average color of the distant galaxies and the invariance of the profiles with foreground disk inclinations. A research note on the limitations of the synthetic field method was submitted to A&A. The above results were presented at the 2004 AAS summer meeting in Denver. Work was started on two more papers; one comparing the HI surface density profiles with the opacity values and one exploring the relation between surface brightness and opacity.

A search for the lowest mass galaxies Kova� continued her PhD research started in November 2002 under super-vision of Oosterloo (Dwingeloo) and van der Hulst. They study the faint end of the HI mass function (HIMF) in order to test the predictions of the CDM theory on the number density of objects with small (dark) masses. The neutral hydro-gen is a much better tracer of the underlying mass distribution compared to the luminous matter and can be used to test the existence of a population of small galaxies in which the star formation has been partially or completely sup-pressed during cosmic evolution. Due to technical limitations, the existing HI surveys are not very sensitive on masses below 108 HI M�� For this study a blind HI survey, sensitive for objects with small HI masses, has been designed. In spring 2004 they completed the observational part of the survey. In total, they observed 60 × 12 hr using the Westerbork Synthesis Radio Telescope in mosaic mode. The observed area covers �86 deg2 of sky in the region of Canis Venatici groups of galaxies. Only data with observed veloci-ties in the range –350 < cz < 1400 km s-1 were used in further data reduction and analysis process. The data reduction has been completed, and the sample has been partially analyzed. They detected 69 objects, 22 of them for the first time in HI. All new HI detections fall in the lower part of the mass-histogram, confirming our ability to detect galaxies with small HI masses. The fitted HIMF of Schechter form to the data has a flat slope (� ~ 1), different from the steep rise predicted by CDM models.

Truncation of stellar disks in galaxies at z~1 Perez Martin has presented the first evidence for stellar disk truncation at high redshift, based on surface photometry of a sample of 16 high redshift (0.6 < z < 1.0) disk galaxies from the GOODS HST/ACS data. The radial profiles are best fit by a double exponential profile. This result agrees with the profile of disks in

30

Figure 6: Left: A schematic of the method to find the relation between dust dimming and the number of distant galaxies: the Synthetic Field Method. The starting point is an image of a face-on spiral galaxy made with the Hubble Space Telescope. Many such images are now in the Hubble Archive. Right: Since a single image does not have many distant galaxies in it, 32 HST/WFPC2 images were combined. Here the average color of distant galaxies, their number and the derived extinction using the method explained to the left are shown as a function of radius from the center of the foreground galaxy. Top: The average color of the distant galaxies seen through the foreground galaxies. Note that this average color barely changes. Middle: the number of distant galaxies found through the foreground galaxies as well as the number of simulated galaxies without any dimming. Bottom: the derived extinction from the numbers of real distant galaxies, compared to the simulations. The radius is scaled with the deVaucouleur's R25. local galaxies. The cosmological surface brightness dimming at this redshift range only allows us to detect galaxies with spatially “early” truncation, Rbr/hin � 3.5. Six galaxies show the radial double exponential structure, with an average value of Rbr/hin ~ 1.8. Such “early” truncated galaxies are missing in local samples so far. This result opens the ground for observing directly disk evolu-tion through the study of the truncation radius as a function of redshift.

Gas flow and dark matter in the inner parts of early-type barred galaxies Perez Martin in collaboration with Fux (Geneva) and Freeman (Mt. Stromlo) have been working on dynamical simulations run in the potential derived from

31

the light distribution of early-type barred spiral galaxies. The aim is to determine whether the mass distribution together with the hydrodynamical simulations can reproduce the observed line-of-sight velocity curves and the gas morphology in the inner regions of these barred galaxies. The SPH models using the stellar mass models obtained directly from the H-band light distributions give a good representation of the gas distribution and dynamics of the modeled galaxies, supporting the maximum disk assumption. This result indicates that the gravita-tional field in the inner region is mostly provided by the stellar luminous compo-nent. This result has large implications for the galaxy evolution picture; either we are in the presence of the dramatic consequences of secular evolution and we need to explain the mechanism to redistribute the dark matter halo mass, or we are in the presence of a break down of the galaxy formation paradigm.

The influence of the environment on the evolution of galaxies Sikkema, in collaboration with Peletier and Valentijn analyzed the HST_ACS shell galaxy data set in V and I. Shell galaxies are elliptical galaxies and are thought to be remnants of a recent minor or major mergers. The V-I colors of the globular cluster (GC) systems and the shells might tell us whether and how many new stars were formed during the merger. Preliminary findings: globular cluster properties of two galaxies (NGC2865 and NGC7626) might contain evidence for recent GC formation: the NGC2865 GCs have somewhat bluer colors. NGC7626 shows much brighter GCs than the other galaxies. NGC2865 is know to be an intermediate age (few Gyr old) merger remnant, it contains a rotating HI disk and a KDC. For the shells it was found that the V-I colors have the same or redder colors than the underlying galaxy light. This is probably best explained if dust is swept up by the shells. V-I color maps of the galaxy light of NGC474 and NGC3923 show large-scale red rings (0.05 mag higher in V-I than their surroundings). Their origin is unknown and no similar examples exist in the literature. The best shell candidate for follow-up spectroscopy to determine its dynamics, is located in NGC2865. This shell also coincides with a bright HI patch. Currently work is focused on finishing two papers describing the results on the globular cluster results and the shells. In October, observations were made with the WFI@2.2m at La Silla in V, R, I of about four square degrees which covers several clusters and empty regions near z = 0.1. Reductions have started with the Astrowise pipeline which is still in development. The goal will be to study galaxy evolution in different environ-ment, using optical, morphological data. The results and analysis will be part of the thesis.

The stellar populations of gas-selected early-type galaxies Serra has started his PhD project under the supervision of Trager, van der Hulst, Oosterloo (ASTRON) and Morganti (ASTRON). Neutral hydrogen gas and stellar properties of a sample of early-type galaxies are being studied. The main goal is to establish whether the presence of HI gas traces young stellar populations and (if this is the case) whether HI and stellar properties give the same indications of the formation of these galaxies.

32

The data obtained in 2004 have been partially reduced and analyzed, with par-ticular focus on the galaxy IC 4200. Three galaxies (IC 4200, ESO 92–21, ESO 381–47) were observed at 21 cm wavelengths. They show extended (tens of kpc in radius) and massive (over 109 M�) HI disks. IC 4200 HI disk shows hints of an interaction with a companion. They were able to reproduce the kinematics of the observed disks with quite simple models: if these galaxies were formed via a major merger, the epoch of formation derived from the HI disks properties is at least 2 Gyr ago. Stellar indexes are being measured from their optical spectra; the results in terms of stellar populations will be compared to what found from their radio data. IC 4200 spectrum shows emission lines likely to be produced both by nuclear activity and on-going star formation; these lines will also enable them to connect the ionized gas kinematics in the stellar body to the larger scale rotation of the neutral hydrogen gas disk.

PN Spectrograph project The project, to determine galaxy dynamics by the very efficient determination of Planetary Nebula velocities, has been described in previous annual reports. This was a year of consolidation in which Douglas, Napolitano and Kuijken developed improved data-reduction techniques and again had a generous allo-cation of observing time at the La Palma Observatory run by the international ING consortium. This year (2004) an NWO grant was awarded against severe competition. The grant includes a post-doctoral position and 48k in equipment, which will be used in part to help complete the new camera. This will operate in "piggy-back" with the main spectrograph and provide deep H-alpha images.

Intracluster light Napolitano has continued his collaboration with an international team aimed at the study of the dynamical properties of the intracluster light, using Planetary Nebulae as tracers. In particular this team has reported a first catalogue of 40 PN radial velocities in different intracluster regions of Virgo Cluster (Arnaboldi et al., 2004, ApJL, 614, 33). The measured velocity distributions confirm the nonuniform dynamical structure and ongoing assembly of the Virgo Cluster similar to the one predicted in N-body simulation (Napolitano et al., 2003, ApJ, 594, 172).

3.6 Quasars and Active Galaxies

Radio properties of LINER galaxies Barthel is collaborating with Ho (Carnegie) and Filho (Porto) 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. A paper describing the radio luminosity func-tion of galaxies down to very low radio flux densities is nearing completion. The

33

radio data are being supplemented with X-ray as well as optical data. A collabo-rative effort with Groningen staff member Peletier and the SAURON group led by De Zeeuw (Leiden) finds an intriguing trend between accretion and circum-nuclear gas properties: this trend is being pursued further, focusing on the possibility of mass loss from star clusters.

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 star formation. Radio and optical imaging is being combined with molecular gas spectroscopy: more JCMT data have been acquired supporting the AGN-star formation symbiosis. An extensive census of molecular gas in nearby QSO Hosts with the 30m IRAM telescope is being planned.

Extremely high redshift QSO’s The search for extremely high redshift QSOs, being conducted in a collabo-rative effort of Barthel with Neeser (Munich) and Maza (Santiago), is continuing. Analysis of VLT spectroscopy of two dozen candidate faint ultra-distant QSOs is underway.

Orientation of quasars and radio galaxies Barthel and co-workers are continuing their study of the far-IR properties of AGN. 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. ASTRO-F will be launched in early 2006. Some data using the new VISIR infrared instru-ment on the VLT have and are being obtained (collaboration with Pel); this work will continue, and will eventually culminate with guaranteed time Herschel studies (see below). 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).

Stars, gas and dust in the host galaxies of compact extragalactic radio sources Following up on a previous Groningen-Baltimore project, the present project of Labiano deals with the precise nature of Compact Steep Spectrum (CSS) quasars and radio galaxies, and will investigate the higher order astrophysical mechanisms contributing to the observed position of these objects in ratio source evolution and unification scenario's. In particular, the PhD research focuses on ionization mechanisms including radio jet – interstellar medium interaction and host galaxy interstellar medium as well as stellar composition. As part of that the thesis project, in 2004 the research of Labiano has focused on: HST-STIS long-slit spectroscopy of the emission line nebulae in the CSS

34

sources 3C67, 3C277.1, and 3C303.1. He has derived BPT diagnostic emis-sion line ratios for the nebulae consistent with a mix of shock excitation and photo-ionization in the extended gas. In addition, line ratios indicative of lower ionization gas were found to be associated with higher gas velocities. The results are consistent with a picture in which these galaxy scale radio sources interact with dense clouds in the interstellar medium of the host galaxies, shocking the clouds thereby ionizing and accelerating them. Labiano has also worked on European VLBI Network spectral line of the 21 cm (HI) line in two sized CSS radio galaxies. They have detected HI absorption towards the western radio lobe of 3C49 and the northern lobe of 3C268.3. The radio lobes with HI absorption (1) are brighter and closer to the core than the opposite lobes; (2) are depolarized; and (3) are preferentially associated with optical emission line gas. The association between the HI absorption and the emission line gas, supports the hypothesis that the HI absorption is produced in the atomic cores of the emission line clouds. They suggest that the asym-metries in the radio and optical emission are due to interaction of the radio source with an asymmetric distribution of dense clouds in their environment. The results are consistent with a picture in which compact steep spectrum sources interact with clouds of dense gas as they propagate through their host galaxy. The research has been carried out in collaboration with O'Dea, Baum, Axon (Rochester), Gelderman (Western Kentucky) de Vries (Lawrence Livermore), Barthel, Capetti (Torino), Fanti (Instituto di Radioastronomia), Koekemoer (Baltimore), Gallimore (Bucknell), Morganti, Vermeulen and Braun (Dwingeloo), Tadhunter (Sheffield).

A galactic rotation measure anomaly Brentjens and de Bruyn have performed a small 21 cm polarization survey of 15 sources in a 6 x 6 degree area around the Perseus cluster. With this mini-survey they mapped out the galactic rotation measure structure on scales of the order of approximately two degrees. They have discovered a smooth gradient of approximately 16 radians per square meter per degree running from West (-20 to -30) to East (+80). The foreground RM expected from the large scale galactic magnetic field is negative and close to zero. On top of this anomaly, there is an excess of +50 radians per square meter caused by the Perseus cluster. It is highly unlikely that this excess is located in our own galaxy. Their work on large scale structure formation continued. They have observed Abell 2256, the Coma cluster (in collaboration with Feretti, Bologna), and a wide area around the Perseus cluster (in collaboration with Vogt, Dwingeloo). These observations will be reduced and analyzed next year. They have written two papers: “Faraday Rotation Measure Synthesis" (Brentjens and de Bruyn 2005) and "Polarized emission associated with the Perseus cluster" (de Bruyn and Brentjens, 2005), which will appear in Astronomy and Astrophysics.

Origin and evolution of nearby radio galaxies Emonts continued his PhD work on the origin and evolution of nearby powerful radio galaxies observed with HI observations and optical spectroscopy under supervision of Morganti (Dwingeloo) and van der Hulst. In collaboration with

35

Tadhunter (Sheffield), Oosterloo (Dwingeloo) and Holt (Sheffield) they con-cluded a detailed study of the ionized gas in radio galaxy 3C 293. The disturbed kinematics and ionization-state of the gas show clear indications of outflows in the central region of this nearby powerful radio galaxy. In particular a fast out-flow of ionized gas (up to 1000 km/s) is observed to be due to an interaction between the radio jet and the ISM. This outflow resembles a similar outflow found in HI (Morganti et al. 2003, ApJ, 593, L69). Detailed analysis of this out-flow shows that, despite the high energies involved in the jet-ISM interaction, most of the outflowing gas is in its neutral state.

Interaction in nearby radio galaxies Emonts, Morganti and van der Hulst, in collaboration with Tadhunter, Oosterloo, Wills (Sheffield), van Moorsel (Socorro) and Sadler (Sydney), also continued their work on the origin of radio galaxies by tracing merger/interaction events in these systems. They nearly completed HI observations of a complete sample of nearby radio galaxies in order to trace and date long-lived merger structures. At least 20–25% of the sample sources show HI in emission around the host galaxy. In most of these cases the HI is fairly settled in large disks, up to 180 kpc in size. These HI disks indicate that a major merger event occurred in these systems more than 1 Gyr ago. Given the relatively young ages of the radio sources, the AGN activity has started very late in the lifetime of this merger. It is striking that the most massive HI disks (over 1010 solar masses) are only found around compact radio sources, while the more extended radio sources (of type FR-I) do not show these large amounts of HI. For one of the HI rich compact radio sources optical spectra have been reduced and show that the light of the galaxy is dominated by an intermediate age stellar population, likely also formed by a major merger event.

XDRs in Active Galactic Nuclei X-ray dominated regions (XDRs) are regions in the ISM where the hard radia-tion field of an accreting black hole completely determines the temperature and chemical composition of interstellar gas. As such, XDRs are direct manifes-tations of the energy balance of interstellar gas and their study allows one to determine how the ISM survives the accretion of gas by a central black hole. X-ray photons from nearby sources heat through photo-ionization and dissociate the gas by UV emission from collisions of H and H2 with secondary electrons. Fine-structure lines of [OI] and [CII] as well as molecular emission of, e.g., CO and H2 provide cooling. Detailed models have been constructed of XDRs by Spaans and Meijerink (Leiden) that allow for complex geometries. These models are relevant to the luminous centers of galaxies like NGC 1068, and are necessary to interpret existing ground-based data as well as future data from Herschel, SOFIA and ALMA.

36

3.7 Clusters, High-Redshift Galaxies and Large Scale Structure

Weak gravitational lensing Christen continues his PhD research on the shapelets method applied to weak gravitational lensing under the supervision of Kuijken. The KSB technique and the Shapelets method are implemented. They both produced the ellipticities of objects corrected from the point spread function to measure the cosmic shear and are in agreement. They were validated using simulated images and 50 VLT FORS I reduced data. The Shapelets technique can be used to measure the objects’ ellipticity. They now focus on distortion field measurement with both techniques and on galaxy-galaxy lensing.

Strong gravitational lensing Koopmans has continued his work on determining the internal mass structure of early-type galaxies to z = 1, using joint constraints from strong gravitational lensing and stellar dynamics. He developed a non-parametric algorithm to model the lens-galaxy mass distribution and the structure of highly magnified sources, with only limited prior assumptions. Observationally, he continues to work with Treu (UCSB) and Fassnacht (UC Davis) on the analysis and acquisition of HST and ground-based spectroscopic data, as part of the Lenses Structure and Dynamics (LSD) Survey. In collabo-ration with Treu, Bolton (MIT/CfA), Burles (MIT) and Moustakas (STScI/ JPL), he has initiated a highly-successful snapshot survey with HST – the Sloan Lens ACS (SLACS) Survey – to image all spectroscopically selected lens candidates from the SDSS. The observations results and analyzes are currently being written up. Koopmans is a founding member of the "Astrophysics Network for Galaxy Lensing Studies" (ANGLES) and member of its steering committee. The ANGLES network is set up to study galaxies through strong and micro-lensing and train PhD students and Postdocs, with a strong emphasis on mobility and collaborations between network nodes. During 2004 he also became part of the LOFAR Epoch-of-Reionization (EoR) key-project and the Astronomy Research Committee (ARC) of LOFAR.

The Epoch of Reionisation of the Universe The Epoch of Reionisation (EoR) is a term used to describe the period during which the gas in the Universe went from being almost completely neutral to a state in which it became almost completely ionized. This watershed event – which has occurred when the Universe was a few hundred million years old (about a twentieth of its current age) and the first radiating objects formed – is intimately linked to many fundamental questions in cosmology and structure formation and evolution. Without a clear understanding of the EoR, we will not fully apprehend how the Universe evolved from its primordial condition to form the astrophysical object we routinely observe today.

37

Despite its pivotal role, the EoR is one of the least understood epochs in the Universe's evolution. A large amount of theoretical effort, guided by very limited observational evidence, is currently dedicated to understanding the physical processes that trigger this epoch, govern its evolution, and what ramifications it had on subsequent structure formation. In the near future, the LOFAR tele-scope, which has the EoR as one of its key projects, is set to measure the neutral gas fraction in the Universe as a function of redshift and angular posi-tion through the hydrogen hyperfine spin-flip 21 cm line. The 21 cm line is, probably, the only observable tracers of the gas during the EoR. It allows detailed mapping the EoR as it progresses in time and space. Currently, Zaroubi's (together with de Bruyn and Koopmans) main objective is to develop the necessary data-analysis and theoretical tools to, initially, prepare the ground and, subsequently, fully exploit the LOFAR-EoR data set, expected to be available within 3–4 years. The synergy between three independent areas of expertise: theory, observation and data analysis, will facilitate addressing the fundamental EoR related questions. Zaroubi and Silk (Oxford) have proposed use of the thickness of the ionization front as a discriminant between alternative modes of reionisation in the early universe, by stars or by miniquasars. Zaroubi, Sugiyama (NAOJ, Tokyo) and Silk have shown that introducing and additional component of a non-scale-free isocurvature power spectrum together to the normal scale-free adiabatic power spectrum can account for the early reionisation detected by the WMAP polarization data.

Matter power spectrum at small scales: Estimation from the Lyman-alpha forest Zaroubi, Nusser (Haifa), Viel, Haehnelt and Kim (Cambridge) have measured the matter power spectrum on small scales from 33 Lyman-alpha spectra spanning the redshift range of 1.5–3.5. The optical depth for Lyman-alpha absorption of the intergalactic medium, obtained from the flux using the inver-sion method of Nusser & Haehnelt, is converted to density by using a simple power law relation. The authors find that a CDM power spectrum amplitude is 0.6 < 8 < 0.8 (with 3 confidence level) consistent with previous measure-ments. This result is somewhat low relative to the concordance model. The authors also argue that the data support a non-adiabatic temperature evolution at certain stages, consistent with full helium reionisation at about z = 3.

On the density and velocity correlation functions Zaroubi and Branchini (Roma) have introduced a simple linear equation relating the line-of-sight peculiar-velocity and density contrast correlation functions. Estimation of the cosmological density parameter with this equation from the Point Source Catalogue Redshift (PSC) survey and the SEcat catalogue of peculiar velocities is consistent with = 0.3. The applicability of the method to future data set is discussed.

38

The 2dF Galaxy Redshift Survey: Wiener reconstruction of the cosmic web Zaroubi, Erdogdu (Cambridge), Lahav (UC London) and the 2dF collaboration, have reconstructed the underlying density field of the Two-degree Field Galaxy Redshift Survey (2dFGRS) for the redshift range 0.035 < z < 0.200 using the Wiener filtering method. They identify all major superclusters and voids in the survey. In particular, they find two large superclusters and two large local voids.

Formation and evolution of galaxy clusters The PhD project of Araya Melo focuses on the formation and evolution of clusters within the context of the surrounding large scale structure. Clusters are forming at the intersections of filamentary features in the large scale matter distribution. Matter is transported towards the clusters via these filamentary extensions. The PhD project seeks to analyze the dynamical evolution of the dark matter and gas content of clusters and their immediate surroundings. The study is based upon numerous numerical N-body and cosmological hydro-simulations. The simulations are run using GADGET, a massively parallel tree N-body/SPH code (Springel et al. 2001). They manipulate the settings of the simulations by means of constrained initial (Gaussian) conditions. Properties like mass of the cluster, shape, tidal shear and power spectrum shape set the large scale envi-ronment. To this end they use the Constrained Random Field code (van de Weijgaert and Bertschinger 1996). The code was extended by Araya Melo and Aragon Calvo in order to be able to achieve a much higher dynamical range by enabling hundreds of constraints. Of crucial importance is the unbiased resolution of hierarchy of substructures and the anisotropic geometry of the surrounding matter distribution. To this end Araya Melo is applying and extending the DTFE method introduced by Schaap and van de Weijgaert (2000). The aspects that they are studying are the dynamics, flow patterns and ther-modynamics of the infall regions, the precise morphology of filamentary struc-tures and the virialization of the dark matter as well as the gas inside the cluster itself. For a systematic assessment of the influence of the cosmological scenario, they are comparing similar initial conditions in a range of power-law power spectra simulations. This year Aragon Calvo continued the observations of A262 and AWM3 fila-ments of galaxies using the INT (optical) and WSRT (radio) telescopes. He also started the data reduction from the last WSRT run. On the theoretical part he applied a filtering method for galaxy classification based the local geometry of the density field. This method has been used in computer vision and medical imaging. Currently he is writing a paper presenting the method and its appli-cation to a galaxy catalog (SDSS) and N-body simulations. Besides this, he continued with N-body tools and simulations and investigated possible use of highly parallel machines.

39

Large-scale structure Scientific work of van de Weijgaert concentrated on the • study of the evolving hierarchy of voids in gravitational instability scenarios (with Sheth (Philadelphia) and Platen). • the development of the Delaunay Tessellation Field Estimator (DTFE) technique (with Schaap, Romano-Diaz, Araya, Platen and Jones) and the related higher order Natural Neighbour Field Estimator (with Vegter, Kruithof, Eldering, Platen). • the application of DTFE to pattern recognition in the 2dF galaxy distri-bution (with Schaap). • the application of DTFE for the analysis of cosmic density and velocity fields in reconstructions of the Local Cosmic Neighbourhood, sampled by the PSCz catalogue (with Romano-Diaz and Schaap). • the application of DTFE to the analysis of density and velocity fields in large (GIF) N-body simulations, in order to find the characteristics of the cosmic web (with Schaap, Araya, Platen). • an investigation of the pattern recognition abilities of Delaunay and Voronoi tessellations and DTFE/NNFE (with Jones) and their relation to wavelet and other multiscale geometric methods (with Martinez, Donoho, Starck). • the development of a new void detection algorithm, the based on the so-called watershed formalism from the field of computer visualization. The input fields are DTFE fields (with Platen). • development of filament detection algorithm using the second order deriva-tive of density field at a hierarchy of embedded scales, using the DTFE density field (with Aragon). • a radio study of galaxy spin alignments in and near the Perseus and Coma Supercluster (with Aragon and van der Hulst). • a study of galaxy alignments in the cosmic web traced by SDSS (with Aragon, Szalay and van der Hulst) • the formulation and development of a large wide-angle photometric survey of the Hercules and Horologium supercluster complexes (collaboration with Valentijn, P.I., and a sizeable international consortium). Around the Omegacam photometric survey additional tracks have been set up, consisting of a) spectro-scopic, b) X-ray, c) radio and d) theoretical study. I function as coordinator of the theory group. • using Voronoi kinematic models as testbeds for a MCMC reconstruction technique of the cosmic web (with Moeller, Martinez, Vedel-Jensen, Skare). • using evolutionary Voronoi kinematic models, followed by more elaborate constrained primordial density and velocity field realizations, to set the scene for the cosmic reionization radiative transfer calculations with the triangulation radiative transfer code (with Ritzerveld, Icke, Mellema).

Evolving hierarchy of voids The void hierarchy project involves the description of the cosmic foam as the results of a hierarchically evolving network of voids. It is based upon an analyti-cal study in collaboration with Sheth (Philadelphia). The evolving void hierarchy

40

is described by means of an 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 pro-genitors. The second process 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 distinct contrast to the distri-bution of virialized halo masses which does not have a small-scale cut-off. In the conventional description for the hierarchical evolution of halos, the excur-sion 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 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. The void size distribution is therefore 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, evolving 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 computer models of structure formation. In addition, the natural tendency of voids to peak around a characteristic size and expan-sion velocity provides an explanation 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 demonstrated to reproduce a multitude of clustering characteristics. Numerical investigation and testing of the excursion set void hierarchy model by means of N-body simulations is the topic of a current study with Platen. First stage of this program involved the development of a new void detection algo-rithm allowing the finding of void substructure. Starting from density maps of large (GIF) N-body simulations generated by means of the DTFE algorithm, the watershed algorithm allowed the detection of a rich void structure and the iden-tification of collapsing and contracting subvoids within the cosmic foam. The first results shows that void merging is particularly evident in and around the central regions of the large voids. Void collapse, on the other hand, is mainly concentrated near the edges of the large voids where they get squeezed while being “pushed” against the surrounding overdense structures. These prelimi-nary results are systematically investigated, for a choice of cosmologies and environmental circumstances, while the finding that the collapse of small voids is mainly a manifestation of shearing will be translated into a modified excursion set formalism for the evolving void hierarchy.

The Delaunay Tessellation Field Estimator The Delaunay Tessellation Field Estimator technique initiated by the work of Schaap and Weijgaert has become a major project involving some 8 collabo-

41

rators from astrophysics and mathematics/computer science. In the meantime it has found recognition in various contributions by other groups. 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 simultane-ously a wealthy internal substructure 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. Schaap has been investigating many syste-matic effects and has proven that DTFE manages to reproduce the hierarchical density field of fractal-like point distributions to high accuracy. In a related study he investigated and compared the performance of DTFE with respect to TSC and SPH interpolation methods and has demonstrated its superior rendering of fine filamentary and wall-like structures. At the moment by means of DTFE the density distribution and weblike structure of the cosmic web in the 2dF galaxy redshift survey is systematically investigated. It has lead to accurated 3-D renderings of iso-density surfaces. This will be the starting point with Shandarin and collaborators to apply the DTFE formalism within the SURFGEN formalism to characterize galaxy and matter distributions by Minkowski functionals at dif-ferent density excursion levels. Romano-Diaz has been applying DTFE to the velocity flows in N-body simulations of cosmic structure formation, and has established its proper reproducing of the density-velocity field relations expected for the mildly nonlinear regime. In a meticulous analysis of the PSCz sample velocity field and density field, the cosmography of the local Universe was analyzed in detail. Well-known features of the local cosmic density distri-bution as well as the corresponding velocity flows were readily visible. Most telling was the success in reproducing the outflow out of large scale voids.

Cosmic structure in de local universe In a collaboration with Vegter, Kruithof and Eeldering, we have started a project to extend our analysis on the basis of the linear interpolation DTFE procedure to the higher order natural neighbour interpolation formalism, also based upon the Delaunay tessellation of a point distribution. Via our collaboration we have been able to use the cgal computational geometry routines and get access to the not yet public 3-D Natural Neighbour routines. The results are rather similar to the DTFE results, but do not have the triangular artifacts found for the latter. Expanding upon these results we have also embarked upon a study of the topology/geometry of the cosmic web by so-called alpha-shapes and betti numbers. In another branch of our focus on the DTFE method, we are looking into the connection to wavelet-based characterizations of the cosmic matter distribution. It forms the basis of a project with Martinez, Starck and Donoho.

42

Figure 7: DTFE density and velocity fields projected along the z-super-galactic plane in a thin slice. The color bar indicates the plotted density scale. Velocities have been normalized to the maximum plotted velocity.

A search for OH megamasers in ultra-luminous infra-red galaxies Kanekar used the WSRT and the ATCA to carry out a search for 1667 MHz OH megamasers (OHMs) in nine ultra-luminous infra-red galaxies (ULIRGs) in the redshift range 0.23 < z < 0.35, to test whether the probability of OHM emission continues to increase with far-infra-red luminosity at the high end of the OHM luminosity function. All the galaxies had extremely high FIR luminosities (LFIR � 12.5) and were part of a larger sample of 32 systems at 0.23 < z < 0.45 selected from the IRAS PSCz catalogue on the basis of their 60 µm flux density. The observations resulted in the detection of two z ~ 0.25 OHMs, IRAS00397–1312 and IRAS16300+1558. The former is one of the most powerful known HMs, with a line luminosity LOH = 3.84, just below the giga-maser level. It also has the second highest redshift of any known OHM, z ~ 0.262. Surprisingly, despite their high FIR luminosity, only three of the ten ULIRGs were found to show OHM emission. If this trend persists, it will not be

43

possible to use 1667 MHz megamasers as a tool to study the merger history of galaxies. The rest of the sample is currently being observed.

A search for HI 21cm absorption in high redshift damped Lyman-� sys-tems Kanekar and Chengalur (NCRA-TIFR) used the GMRT to search for HI 21cm absorption in a sample of high redshift damped Lyman-� systems (DLAs), resulting in several strong upper limits on the 21cm optical depth and the detection of 21cm absorption at z ~ 3.39 towards PKS0201+113. This is the highest redshift at which 21cm absorption has been found in a DLA. Besides this, Kanekar, Chengalur (NCRA-TIFR), Lane (NRL) and Ellison (ESO) used the GBT to search for HI 21cm absorption in another DLA sample, with two detections at z ~ 2.4. The observations suggest the majority of high redshift DLAs have high spin temperatures, with small fractions of gas in the cold phase. These high Ts values are consistent with the absorbers being small, low metallicity objects, rather than dwarf galaxies. The results also hint at evolution in the relative fraction of the cold and warm phases from high redshifts to today.

An anti-correlation between spin temperature and metallicity in DLAs Kanekar, Smette (ESO), Briggs (ATNF, ANU) and Chengalur (NCRA-TIFR) used VLT-UVES observations to measure the metallicity [Zn/H] of a sample of high redshift damped absorbers with measured spin temperatures Ts. These resulted in the detection of an anti-correlation between Ts and [Zn/H] in a sample of 15 DLAs, clearly implicating gas metallicity in determining the tempe-rature of the neutral ISM. It is plausible that the high spin temperatures of DLAs arise because the ISM in small galaxies is inefficiently cooled due to the lack of metals, resulting in a lack of radiation pathways.

The strange case of a sub-DLA with very little HI Kanekar and Chengalur (NCRA-TIFR) carried out a deep GMRT search for HI 21cm emission from a z = 0.00632 sub-damped absorber toward PG1216+069. No emission was detected; the 5 upper limit on the mass of any associated galaxy is MHI � 107 M��, nearly three orders of magnitude less than MHI*. The z ~ 0.006 absorber is thus the most extreme known deviation from the standard paradigm in which high column density quasar absorption lines arise in the disks of gas-rich galaxies.

Tiny HI clouds in the local ISM Kanekar and Braun (ASTRON) used high spectral resolution WSRT HI 21cm observations of four high latitude compact radio sources to detect a new popu-lation of tiny, discrete clouds in the diffuse ISM, with peak optical depths � ~ 0.1–2% and HI column densities of 0.4–8 × 1018 cm-2. Imaging detections con-firm these low column densities and imply linear dimensions of a few thousand AU, assuming a distance of 100 pc. The physical origin of these tiny HI struc-

44

tures and their distribution in the ISM is at present unknown. The results sug-gest significant injection of small-scale power into the ISM.

Galaxies in the early universe Obri� has finished the project in the collaboration with Ivezi� (Washington) and the SDSS group. They studied panchromatic properties of SDSS galaxies also detected by eight other sky surveys, covering the wavelength range from X-ray to radio. Some of the findings are: strong correlations between the detection fraction at other wavelengths and optical properties of galaxies (flux, colors, emission line strengths); the SDSS u and r band data, supplemented with red-shift, can be used to predict K band magnitudes measured by 2MASS with an rms scatter of 0.2 mag; the interstellar dust content inferred from optical spectra is indeed higher for galaxies detected by IRAS, and it can be used to predict IRAS 60 �m flux within a factor of 2, based on SDSS data alone; the position of a galaxy in the emission-line based Baldwin-Phillips-Terlevich diagram is cor-related with the light concentration index and u-r color; the BPT diagram changes the morphology when requiring detections at other wavelengths; SDSS galaxies detected by GALEX include a non-negligible fraction (10–30%) of AGNs, and hence do not represent a clean sample of starburst galaxies. This project is the observational basis for the continuation of her PhD project with Spaans in which she will study the modeling of the emission line galaxies and their properties. Obri� has finished reducing the data, completed the surface brightness photo-metry of galaxies and obtained Kormendy relations for four clusters, as a part of the project with Trager in which they study impact of stellar populations on the Fundamental Plane tilt in multiple bands.

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 con-tinued. Trager, Bell and Rix (MPIA-Heidelberg), Tran (ETH-Zurich), and Franx (Leiden) began an observing campaign using the VIMOS spectrograph at ESO's VLT to determine the masses, star formation rates, ages, and compo-sitions of the most massive galaxies at a time when the Universe was half of its current age. First data were acquired in November 2004 and data collection continued through January 2005. In a related study, Trager's spectral line ana-lysis of early-type galaxies provided a significant part of a paper by Dressler et al. on the stellar populations of cluster galaxies at intermediate redshifts. Obri� and Trager have completed the majority of data reduction in 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; first results were presented at the 2004 NAC. Trager, Serra, and van der Hulst, Oosterloo and Morganti (ASTRON), Sadler (Sydney) and van Gorkom (Columbia/Kapteyn) continued their study of 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). Data on the Southern sample from

45

successful observing runs at ATCA and NTT at ESO's La Silla are mostly reduced and are begin analyzed presently; data from a mostly-unsuccessful observing run at the WHT on La Palma may not be very useful for the Northern sample. Trager, Polko and Somerville (STScI) continued to examine the stellar popu-lation parameters inferred from semi-analytic models of galaxy formation. They have made an important discovery: at least some of the "overabundance" of magnesium in the spectra of early-type galaxies actually arises from the fact that these objects are composed of multiple stellar populations and is not entirely due to true chemical evolution effects. Trager and Worthey (Washington State) continued their development of 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) in order to improve the accuracy and preci-sion of stellar population age-dating techniques.

ISO survey and source counts Héraudeau et al. (2004) have presented their results derived from the analysis of a survey performed with the Infrared Space Observatory (ISO) in the far infrared. Number counts in the European Large-Area Iso survey 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. Observations from the Wide-Field Imager archive at ESO have been selected to be analyzed with the Astro-Wise pipeline. These data (representing about 1Tb of disk space) will be used as a test sample for the data reduction and data mining of the large amount of data produced by OmegaCAM.

Hercules cluster Schneider started her PhD project "Getting on the outskirts of Hercules" on the first of April with Valentijn and van de Weijgaert. The project contains a multi-wavelength study of the relatively compact and nearby 12 square degree Hercules supercluster. The optical part will be observed with the new Omega-CAM camera on ESO's VLT Survey telescope in Chili in spring 2006. In collaboration with other members of VESUVIO, this data will be combined with radio and X-ray observations. The PhD project started with the preparation of 8 nights of observation with the 8K wide field camera on the MDM 2.4 m telescope at the Kitt-peak site in Arizona USA. Not the whole planned 12 square degrees could be covered here, since the 8K camera has a much smaller field of view than OmegaCAM, but a selection was made covering the main parts of the Hercules supercluster, including the very interesting and until now hardly studied intercluster regions within the supercluster. The data is being reduced with the Astro-Wise system at OmegaCEN, which is currently being adjusted to also serve other instru-ments. Concerning the 8K this data has provided a large contribution toward this goal. Also, this data serves to make a preliminary assessment of the field and the whole data reduction plus analysis trajectory.

46

Furthermore the project will consider the connection between the cluster distri-bution and the overall matter distribution in the cosmic foam through the appli-cation of constrained random field codes. A collaboration has been set up with van Kampen (Innsbrück) to do these simulations.

3.8 Computing at the Kapteyn Astronomical Institute

Hardware In 2004 the computer group started to implement a new strategy for building a reliable system consisting of independent servers and workstations both pro-tected by a firewall. For essential services they purchased new hardware. After a new mail server they installed a ‘login’ server to establish connections from the outside world to machines in the so called safe- or desktop zone. Also, al-most all of the workstations have been migrated to the new safe environment in preparation of the use of a new file server early 2005. They installed a wireless network with a number of access points. It is used intensively by a growing number of laptop users. The system proved to be mobile and flexible during a number of workshops and meetings in November and December.

Software In 2004 they started to use the network installation of Windows XP provided by the faculty FWN for secretariat-, guest- and some public Windows machines. The installation was not a trivial matter because first, they were unfamiliar with a the necessary Novell network environment and second, they strictly require that the XP machines are protected by our own central firewall. In cooperation with the specialists of the faculty they figured out how to connect the systems. After that they configured them for the use of local printers and local home directories. So finally the secretariat is equipped with standard XP machines which offer complete compatibility with other FWM secretariat machines. In total, fifteen computers are running the new XP software for a couple of months and the number of reported problems is lower than expected. After a period of experiments to improve the quality of maintenance of oper-ating system and system software, they decided to enter into a contract with RedHat, a company that sells a supported Linux distribution for companies. They use their installation- and maintenance services for the Linux Enterprise 3 distribution. Every night new software updates and security patches are installed automatically on all our connected Linux machines. This system works satisfactory. It certainly saves a lot of time. The ‘howto’ database, maintained by the computer group, is used intensively and is still growing in size. It contains more than 130 howto’s. Some of them have been visited more than a thousand times. Other sources of information are the (rpm based) software database and the computing news pages. They observe that users know the way to get the appropriate computer information

47

and we almost never get any helpdesk questions for which an answer can be found in the howto’s. A new database, accessible only at our intranet, has a focus on education. It is implemented and used for maintaining course infor-mation, see: (https://www.astro.rug.nl/KAPTEYN_DB/cursus_db.php). It is also the base of our local electronic learning environment (http://www.astro.rug.nl/intranet/onderwijs/dlo/dlo.php) which is an experiment to create a uniform course environment on the web. In contrast to Nestor, this environment does not manage content but it manages menu structures and links. GIPSY A student from the HanzeHogeschool Groningen explored the new GIPSY Python environment and was challenged to build a complex task with a graphi-cal user interface. The last GIPSY application that needed to be ported to 24 bits display was BLOT. In a short time, the student managed to learn object oriented programming in Python and migrated and extended the task BLOT. The migrated task is called PYBLOT.

Organization In December they were confronted with a proposal to reorganize the local IT-organizations of the university with respect to the installation and maintenance of Linux. The proposal is to extract manpower from local support to form a central group with the mission to provide and maintain a Linux distribution. It is difficult to draw conclusions from this ill defined proposal but in a staff meeting it was emphasized that at the moment it is not clear how they possibly could benefit from the proposed centralization and that the proposal seems to be written with an office environment in mind and not for scientific support.

Security The investment in a more secure computer environment finally paid off. No valuable time was lost in repairing machines visited by hackers.

Meetings In September they organized a meeting with the project manager of EMAP (the project for implementing central email facilities). The discussion focused on the (in)flexibility of the new system with respect to the user administration. They concluded that central mail and local mail do not exclude each other because both are based on the IMAP protocol which is handled very well by modern mail clients. The official launch date for EMAP at our department is May 2005. In November they attended a meeting about the authentication and encryption of mail. They learned that digitally signed mail has legal the status of a letter.

Linux 110 MS-Windows 16 Distribution of platforms in 2004

48

3.9 Instrumentation

VISIR, the mid-infrared imager and spectrometer for the ESO-VLT For VISIR 2004 was a crucial and very successful year. After completion of the laboratory tests related to the “Preliminary Acceptance Europe” process at Saclay in January, VISIR with all its auxiliary instrumentation was air-lifted to Chile in March. An additional 1500 km of very careful, slow transport by road brought the 10 tons of equipment safely to the VLT on Cerro Paranal. Post-transport tests and mounting on the telescope went very smoothly and on April 28 the instrument was fully cooled and operational at the cassegrain focus of VLT telescope No. 3 “Melipal”, ready to start the on-sky commissioning program. The magic “first light” moment followed the next night, with the first beautiful images and spectra of southern infrared sources. A selection of these early results and a taste of the scientific potential of VISIR were presented to the community in ESO Press Release Nr. 13/04 of 12 May 2004 and in articles in the ESO Messenger (Nr. 117, Sept. 2004 and Nr. 119, March 2005). The commissioning program was executed in three periods over the months April-September. Two staff members from the Kapteyn institute participated: Pel (PI for the spectrometer) and Peletier, who has taken an active part in the Dutch VISIR team immediately after his move to Groningen in 2003. Although the weather did not always cooperate – a large part of the second commis-sioning run was lost due to bad weather- the commissioning was very suc-cessful. From the very first night on the telescope, VISIR has worked without any technical failure and has demonstrated that all instrument modes work as predicted. At the moment of writing the commissioning process has not yet been fully closed. Not all observing modes have been released to the users community yet, but the first “guaranteed time” observing runs with VISIR started in Novem-ber 2004, followed by the first “open time” observing in April 2005. After nearly a decade of designing, building and testing, the scientific harvesting has now started (http://www.astron.nl/visir/). In December 2004 the European consortium that develops the mid-infrared instrument MIRI for the JWST successfully passed the Preliminary Design Review. After this PDR milestone the optical design of the combined imager and integral field spectrometer is now implemented in a compact, modular design that puts all optical elements in place within the strict required toler-ances. Prototypes of important subsystems have already undergone vibration tests and the project has now entered the detailed design phase.

49

VISIR at the cassegrain focus of “Melipal’, the 3rd VLT telescope.

MIRI, the mid-infrared instrument for the James Webb Space Telescope The Dutch MIRI contribution, which is part of the NOVA instrumentation effort, consists of the main spectrometer optomechanical subsystem. This is being developed by the NOVA-ASTRON MIRI team at ASTRON, Dwingeloo, led by Dutch MIRI co-PI van Dishoeck (RUL) and by Jager (SRON, NL MIRI project manager). The Kapteyn Institute is involved via Tielens, Barthel and De Graauw (members of the NL MIRI science team) and Pel, who supports the MIRI team at ASTRON as scientific-technical advisor. For more details on the MIRI project see previous Annual Reports and the MIRI pages on the ASTRON website (http:/www.astron.nl/miri-ngst).

50

Preparing Wide field Surveys with OmegaCAM Staff of the Institute (Héraudeau, Trager, Valentijn, van de Weijgaert) designed an extensive observing program of nearby superclusters for the future OmegaCAM optical camera at the VLT Survey Telescope on Paranal. The program will start with a deep 10 square degree survey of the Hercules super-cluster and extending this later with a large 100 square degree survey of the Horologium supercluster. For this multispectral study also X-ray XMM obser-vations (Böhringer, Kaastra) and HI observations (Verheyen, van Gorkom) are planned. Within the framework of the EU RTN network SISCO (Spectroscopic and Imaging Surveys for Cosmology), in which OmegaCEN is participating, the supercluster collaboration with Italian colleagues (Busarello, Merluzzi) at the Observatorio di Capodimonte was set up and named VESUVIO, PI’s are Capaccioli and Valentijn. Joined meetings were held at Napoli (June) and Groningen (September). Schneider started her PhD project on the Hercules Supercluster (supervisors van de Weijgaert and Valentijn) and made broad band wide fields images at the MDM telescope of a long strip in the supercluster, as a preparation for the large survey.

51

Sikkema (supervisors Peletier and Valentijn) used the Wide field imager at ESO's 2.2m telescope to obtain broad band image data for a large area in the 2dF South regions, which also contains supercluster filamentary structure. The data will be used to study galaxy evolution and structural properties over very large areas. Both the MDM and the WFI data sets were reduced using the new OmegaCEN/AstroWise system.

OmegaCEN The Institute hosts OmegaCEN, an Astronomical Data centre supporting WIDE-FIELD astronomical imaging. The centre is building and supporting an advanced survey system: the VIRTUAL SURVEY TELESCOPE. OmegaCEN is an initiative of NOVA, supporting NOVA's instrumentation programme, in par-ticular OmegaCAM. In 2004 the centre has further developed and qualified the AstroWise information system and performed first "stress-tests" by ingesting about 15.000 WFI@2.2m telescope sky images into the system. In total 225.000 2k*4k CCD readouts were ingested into the system, of which about half of the data serve calibration purposes. OmegaCEN is leading the European Research and Technical Development programme Astro-Wise. In the third year the project plan as outlined in the con-tract has been continued. Following the plan for Phase II of the project, the prototype of the AstroWise system has been evaluated and prepared for mass production. Following the recommendations set at the AstroWise workshop at the end of the previous year (November 2003) the prototype has been further developed and made ready for mass production. To test this, 10 Terabyte of data of a smaller imaging camera (WFI@2.2m) has been ingested into the system. This in itself, was a first test of ingestion of large amounts of raw data. With these test data the system has been further qualified and optimized. In November an AstroWise workshop was held at the Institute at which the work plan for the remaining part of the work was defined. The consortium had to face the late delivery of one of the most important infrastructure facilities the project is supporting: ESO’s VLT-Survey Telescope and OmegaCAM. Details of the work packages have been specified for the remaining development work of the project: i) the introduction of context/privileges, ii) the design for distributed processing, iii) distributed archiving and iv) Quality control. On 3 December an AstroWise PI meeting was organized at the Institute, chaired by Valentijn. Hardware, 10 Terabyte disk storage and computers have been upgraded. The central database systems have been upgraded, migrated to Oracle 10g and the fileserver has been updated. A new way to handle catalogues of astronomical data (Source lists) and methods to associate catalogues (Associate) have been implemented (Begeman). Boxhoorn further developed the AstroWise database system while Tempelaar build and improved a web based advanced viewer to the database. In the context of the partnership with the Lofar/Bsik consortium OmegaCEN started with preparations for proto-type GRID services for end users of the LOFAR radio telescope. Vriend started to work on this project on 1 November. OmegaCEN organized several brainstorms: one on 6/7 May with represen-tatives of the German GAVO, European AVO (now called Euro-VO), UK Astro-Grid and Astron/Lofar and one on large databases with CWI and Astron/Lofar on 10 September. In December a workshop/course was organized at the Insti-

52

tute on "running Projects and Surveys". In September the EU-RTN network SISCO met at the Institute. OmegaCEN is involved in a proposal to ESO for a very large 1700 Square degree survey of the 2dF regions, called KIDS (PI Kuijken, co-I Valentijn). A KIDS consortium meeting was held at the Institute on 2 December. Valentijn visited several Euro-VO related meetings: the Science Working Group meeting in Strassbourg and the Euro-VO Datacenter alliance board (Paris, December) a new consortium in which OmegaCEN participates and which has the goal to coordinate the connection of the Virtual Observatory infrastructure to National institutions.

OmegaCAM The OmegaCAM team delivered the pipeline software to ESO for integration in ESO's data flow system. Preliminary acceptance Europe was successfully com-pleted. Valentijn and Vermeij produced a first version of the u,g,r,i,z, secondary standard star catalogues for 8 one square degree fields (Landolt), based on three observing runs at the INT wide field camera. New methods for auto-matically deriving the 'illumination correction" of the flat field, one of the domi-nant photometric calibration problems of some wide field cameras, have been developed and applied to WFI@2.2m and INT data. Begeman and Deul (Leiden) started developing a new global astrometric solu-tion method which can improve the astrometric accuracy of wide-field images by factors 2-3 when using the overlap of dithered exposures.

Atacama Large Millimeter Array The ALMA project is a collaboration between Europe, North America, and Japan to build an aperture synthesis telescope consisting of 64 12-m antennas located at 5000 m altitude in Chile. In its full configuration, ALMA will observe in 10 frequency bands between 30 and 950 GHz, with a maximum baseline of up to 18 km, which will provide astronomers with unprecedented spatial reso-lutions and sensitivities at millimeter and sub-millimetre wavelengths. Within the Netherlands, a collaboration of NOVA, RuG, SRON, and TU Delft are developing 600-720 GHz receivers for Band 9 of the ALMA project. As the highest frequency band in the baseline ALMA project, Band 9 will provide the observatory’s highest spatial resolutions, in addition to probing higher tempe-rature scales that will complement observations in the lower-frequency bands in the baseline project (84–116, 211–275, and 275–370 GHz). The SIS mixers that are being used in the ALMA Band 9 cartridge were developed within the framework of a NOVA Phase 1 instrumentation project. In 2004, the individuals in the ALMA Band 9 collaboration were: Baryshev, Hesper, Gerlofsma, Adema, Koops, Barkhof, and Mena at the Institute; Jackson and Schaeffer at SRON; and Zijlstra, Kroug, Lodewijk, and Klapwijk at TU Delft. Additional staff will be added in 2005 in preparation for production of the ALMA cartridges. Work on the ALMA project is funded by a contract between NOVA and the European Southern Observatory to produce 8 pre-production receivers by mid-2006. Discussions with ESO over a contract for the production of the receivers needed to populate the bulk of the ALMA antennas have started. Other work in the group is funded by NWO (for the CHAMP+

53

mixer arrays) and NOVA and the EU’s FP6 Framework (for the development of side-band separating 650 GHz mixers).

ALMA Band 9 Progress in 2004 The detailed design of the first Band 9 cartridge (see Figure 8) was completed in 2004, in collaboration with Mecon, a commercial mechanical design com-pany. The design passed a Preliminary Design Review organized by ESO and ALMA in March of 2004. Fine mechanical work for the manufacturing of the first cartridge was primarily outsourced to 3 local companies, while the FWN work-shop contributed significantly to prototyping and test equipment development. In total, approximately 80 companies in Europe, Russia, and the USA are sup-plying components and equipment to the Band 9 effort. With respect to the verification of the cartridge design, a key step was taken in 2004 with the verification of the design and manufacturing (by precision CNC machining) of the cartridge’s compact optics assembly (see Figure 8). This verification was done in collaboration with a scientist from the University of Ireland in Maynooth, using a room-temperature beam-pattern measurement system that was built in 2004 for testing the ALMA optics during series pro-duction. A key to the development of the cartridge’s 4-12 GHz IF system con-tinues to be the development of 4–12 GHz isolators by Pamtech, an American company. The ongoing development of SIS junctions for ALMA are discussed below in the context of the CHAMP project. In parallel with the evaluation of critical components of the cartridge, assembly of the first full cartridge proceeded in 2004, resulting in feedback to the car-tridge design to ease the manufacturing and assembly of later units. Progress was also made in the development of equipment for testing the Band 9 car-tridges prior to delivery to the project. Agreements between SRON, the Kapteyn Institute, and the University were also reached regarding additional space for several purposes, including the assembly of the band 9 cartridges.

The CHAMP+ Project The ALMA group is also involved in the CHAMP+ project, a pathfinder project for ALMA that requires two focal plane arrays of 7 mixers each (see Figure 9) for the frequency ranges 600–720 and 780–950 GHz (the so-called low-colour *and high-colour arrays). The CHAMP+ receiver will be installed on the APEX telescope, a copy of one of the prototype 12-m ALMA antennas, which is located at the ALMA site at 5000-m altitude in Chile. The CHAMP mixer design is similar to that of the ALMA prototype and the mixers have been manufactured primarily by local industry. All of the compo-nents of the low-colour array are ready, except for the electronics board. This includes a set of 7 state-of-the-art 600–720 GHz SIS mixers – the product of a continuing collaboration with TU Delft to improve the performance of the SIS junctions at the heart of both the CHAMP+ arrays and the Band 9 cartridge. For the high-colour array, an improvement of the junction quality is still desirable. The CHAMP+ project is a collaboration with MPIfR in Bonn.

54

Figure 8: (left) The cryogenic portion of the ALMA Band 9 cartridge, with and without the fiberglass rings that separate the cartridge’s four tem-perature levels. (right) The 4K optics assembly. The surface and relative alignment accuracies of the 5 mirror surfaces are typically several microns, or better. This allows the system to be assembled without a need for mechanical alignment.

55

Figure 9: The CHAMP+ mixer block containing a focal plane array of 7 600–720 GHz SIS mixers (seen in the left-hand view), together with asso-ciated bias circuitry (not seen).

57

APPENDIX I : PUBLICATIONS 2004

I.1 Papers in scientific journals, books

Abbas, M.M., Craven, P.D., Spann, J.F., Tankosic, D., LeClair, A., Gallagher,

D.L., West, E.A., Weingartner, J.C., Witherow, W.K., Tielens, A.G.G.M., Laboratory Experiments on Rotation and Alignment of the Analogs of Interstellar Dust Grains by Radiation, Astrophys. J. 614, 781–795, 2004.

Alcalá, J.M., et al. (including Napolitano, N.), The Capodimonte Deep Field.

Presentation of the survey and first follow-up studies, Astron. Astrophys. 428, 339–352, 2004.

Arnaboldi, M., Gerhard, O., Aguerri, J.A.L., Freeman, K.C., Napolitano, N.R.,

Okamura, S., Yasuda, N., The Line-of-Sight Velocity Distributions of Intracluster Planetary Nebulae in the Virgo Cluster Core, Astrophys. J. 614, L33–L36, 2004.

Bernard-Salas, J., Houck, J.R., Morris, P.W., Sloan, G.C., Pottasch, S.R.,

Barry, D.J., Spitzer Infrared Spectrograph (IRS) Observations of Large Magellanic Cloud Planetary Nebula SMP 83, Astrophys. J. Suppl. 154, 271–274, 2004.

Blaauw, Adriaan, My Cruise Through the World of Astronomy, Annual Review

of Astron. & Astrophys. 42, 1–37, 2004. Bodewits, D., Juhász, Z., Hoekstra, R., Tielens, A.G.G.M., Catching Some

Sun: Probing the Solar Wind with Cometary X-Ray and Far-Ultraviolet Emission, Astrophys. J. 606, L81–L84, 2004.

Boekel, R.van, Waters, L.B.F.M., Dominik, C., Dullemond, C.P.,Tielens,

A.G.G.M., de Koter, A., Spatially and spectrally resolved 10 �m emission in Herbig Ae/Be stars, Astron. Astrophys. 418, 177–184, 2004.

Bottinelli, S., Ceccarelli, C., Lefloch, B., Williams, J.P., Castets, A., Caux, E.,

Cazaux, S., Maret, S., Parise, B., Tielens, A.G.G.M., Complex Molecules in the Hot Core of the Low-Mass Protostar NGC 1333 IRAS 4A, Astrophys. J. 615, 354–358, 2004.

Bottinelli, S., Ceccarelli, C., Neri, R., Williams, J.P., Caux, E., Cazaux, S.,

Lefloch, B., Maret, S., Tielens, A.G.G.M., Near-Arcsecond Resolution Observations of the Hot Corino of the Solar-Type Protostar IRAS 16293–2422, Astrophys. J. 617, L69–L72, 2004.

58

Bradac, M., Schneider, P., Lombardi, M., Steinmetz, M., Koopmans, L.V.E.,

Navarro, J.F., The signature of substructure on gravitational lensing in the LambdaCDM cosmological model, Astron. Astrophys. 423, 797–809, 2004.

Brown, R.L., Wild, W., Cunningham, Ch., ALMA – the Atacama large millimeter

array, Advances in Space Research 34, 555–559, 2004. Cazaux, S., Spaans, M., Molecular Hydrogen Formation on Dust Grains in the

High-Redshift Universe, Astrophys. J. 611, 40–51, 2004. Cazaux, S., Tielens, A.G.G.M., H2 Formation on Grain Surfaces, Astrophys. J.

604, 222–237, 2004. Cole, A.A., Smecker-Hane, T.A., Tolstoy, E., Bosler, T.L., Gallagher, J.S., The

effects of age on red giant metallicities derived from the near-infrared CaII triplet, Mon. Not. Roy. Astron. Soc. 347, p. 367–379, 2004.

Curran, S.J., Kanekar, N., Darling, J.K., Measuring changes in the fundamental

constants with redshifted radio absorption lines, New Astronomy Reviews 48, 1095–1105, 2004.

Demers, S., Battinelli, P., Letarte, B., A Carbon star approach to IC 10:

Distance and correct size, Astron. Astrophys. 424, 125–132, 2004. Diedenhoven, B. van, Peeters, E., Van Kerckhoven, C., Hony, S., Hudgins,

D.M., Allamandola, L.J., Tielens, A.G.G.M., The Profiles of the 3–12 Micron Polycyclic Aromatic Hydrocarbon Features, Astrophys. J. 611, 928–939, 2004.

Dressler, A., Oemler, A. Jr., Poggianti, B.M., Smail, I., Trager, S., Shectman,

S.A., Couch, W.J., Ellis, R.S., Studying the Star Formation Histories of Galaxies in Clusters from Composite Spectra, Astrophys. J. 617, 867–878, 2004.

Emsellem, E., Cappellari, M., Peletier, R.F., McDermid, R.M., Bacon, R.,

Bureau, M., Copin, Y., Davies, R. L., Krajnovic, D., Kuntschner, H., Miller, B.W., de Zeeuw, P.T., The SAURON project – III. Integral-field absorption-line kinematics of 48 elliptical and lenticular galaxies, Mon. Not. Roy. Astron. Soc. 352, 721–743, 2004.

Erdogdu, P., et al. (including Zaroubi, S.), The 2dF Galaxy Redshift Survey:

Wiener reconstruction of the cosmic web, Mon. Not. Roy. Astron. Soc. 352, 939–960, 2004.

Falcke, H., Körding, E., Nagar, N.M., Compact radio cores: from the first black

holes to the last, New Astronomy Reviews Vol. 48 , 1157–1171, 2004.

59

Fender, Rob, De Bruyn, Ger, Pooley, Guy, Stappers, Ben, The radio counterpart of IGR J00291+5934, The Astronomer's Telegram, #361, 2004.

Filho, M.E., Fraternali, F., Markoff, S., Nagar, N.M., Barthel, P.D., Ho, L.C.,

Yuan, F. Further clues to the nature of composite LINER/H II galaxies, Astron. Astrophys. 418, 429–443, 2004.

Fraternali, F., Oosterloo, T., Sancisi, R., Kinematics of the ionised gas in the

spiral galaxy NGC 2403, Astron. Astrophys. 424, 485–495, 2004. Gibb, E.L., Whittet, D.C.B., Boogert, A.C.A., Tielens, A.G.G.M., Interstellar Ice:

The Infrared Space Observatory Legacy, Astrophys. J. Suppl. Series 151, 35–73, 2004.

Hagiwara, Y., Klöckner, H.-R., Baan, W., VLBI imaging of OH absorption: the

puzzle of the nuclear region of NGC3079, Mon. Not. Roy. Astron. Soc. 353, 1055–1063, 2004.

Haverkorn, M., Katgert, P., de Bruyn, A.G., Properties of the warm magnetized

ISM, as inferred from WSRT polarimetricimaging, Astron. Astrophys. 427, 169–177, 2004.

Haverkorn, M., Katgert, P., de Bruyn, A.G., Structure in the polarized Galactic

synchrotron emission, in particular "depolarization canals'', Astron. Astrophys. 427, 549–559, 2004.

Helmi, A., Velocity Trends in the Debris of Sagittarius and the Shape of the

Dark Matter Halo of Our Galaxy, Astrophys. J. 610, L97–L100, 2004. Helmi, A., Is the dark halo of our Galaxy spherical?, Mon. Not. Roy. Astron.

Soc. 351, 643–648, 2004. Héraudeau, Ph., et al., The European Large Area ISO Survey – VIII. 90-µm

final analysis and source counts, Mon. Not. Roy. Astron. Soc. 354, 924–934, 2004.

Hulst, J.M. van der, Sadler, E.M., Jackson, C.A., Hunt, L.K., Verheijen, M.,

van Gorkom, J.H., From gas to galaxies, New Astronomy Reviews 48, 1221–1237, 2004.

Hyung, S., Pottasch, S.R., Feibelman, W.A., Photoionization model analysis of

the planetary nebula Hu1-2, Astron. Astrophys. 425, 143–149, 2004. Jaffe, W. et al. (including Pel, J.-W.), The central dusty torus in the active

nucleus of NGC 1068, Nature 429, 47–49, 2004. Jong, J.T.A. de, Kuijken, K., Crotts, A.P.S., Sackett, P.D., Sutherland, W.J.,

Uglesich, R.R., Baltz, E.A., Cseresnjes, P., Gyuk, G., Widrow, L.M., First

60

microlensing candidates from the MEGA survey of M 31, Astron. Astrophys. 417, 461–477, 2004.

Justtanont, K., de Jong, T., Tielens, A.G.G.M., Feuchtgruber, H., Waters,

L.B.F.M., W Hya: Molecular inventory by ISO-SWS, Astron. Astrophys. 417, 625–635, 2004.

Kanekar, N., Briggs, F.H., 21-cm absorption studies with the Square Kilometer

Array, New Astronomy Reviews 48, 1259–1270, 2004. Kanekar, N., Chengalur, J.N., The use of OH m̀ain' lines to constrain the

variation of fundamental constants, Mon. Not. Roy. Astron. Soc. 350, L17–L20, 2004.

Kanekar, N., Chengalur, J.N., Ghosh, T., Conjugate 18cm OH Satellite Lines at

a Cosmological Distance, Physical Review Letters, vol. 93, Issue 5, id. 051302, 2004.

Katz, D. et al. (including Helmi, A.), Spectroscopic survey of the Galaxy with

Gaia– I. Design and performance of the Radial Velocity Spectrometer, Mon. Not. Roy. Astron. Soc. 354, 1223–1238, 2004.

Kaufer, A., Venn, K.A., Tolstoy, E., Pinte, Ch., Kudritzki, R.-P., First Stellar

Abundances in the Dwarf Irregular Galaxy Sextans A, Astron. J. 127, 2723–2737, 2004.

Kemper, F., Vriend, W.J., Tielens, A.G.G.M., The Absence of Crystalline

Silicates in the Diffuse Interstellar Medium, Astrophys. J. 609, 826–837, 2004.

Klöckner, H.-R., Baan, W.A., An embedded circumnuclear disk in Mrk 273,

Astron. Astrophys. 419, 887–896, 2004. Koopmans, L.V.E., Blandford, R.D., Gravitational lenses, Physics Today, 45–

51, 2004. Koopmans, L.V.E., Browne, I.W.A., Jackson, N.J., Strong gravitational lensing

with SKA, New Astronomy Reviews 48, 1085–1094, 2004. Kregel, M., Kruit, P.C. van der, Radial truncations in stellar discs in galaxies,

Mon. Not. Roy. Astron. Soc. 355, p. 143–146, 2004. Kregel, M., Kruit, P.C. van der, Structure and kinematics of edge-on galaxy

discs – III. The rotation curves in the gas, Mon. Not. Roy. Astron. Soc. 352, 787–803, 2004.

Kregel, M., Kruit, P.C. van der, Blok, W.J.G. de, Structure and kinematics of

edge-on galaxy discs – II. Observations of the neutral hydrogen, Mon. Not. Roy. Astron. Soc. 352, 768–786, 2004.

61

Kregel, M., Kruit, P.C. van der, Freeman, K.C., Structure and kinematics of edge-on galaxy discs – I. Observations of the stellar kinematics, Mon. Not. Roy. Astron. Soc. 351, 1247–1265, 2004.

La Franca, F. et al. (including Héraudeau, P.), The Nature of the Mid-Infrared

Population from Optical Identifications of the ELAIS-S1 Sample, Astron. J. 127, 3075–3088, 2004.

Lagage, P.O., et al. (including Pel, J.W., Peletier, R.), Successful

commissioning of VISIR: the mid-infrared VLT instrument’, ESO Messenger 117, 12, 2004.

Lazio, T. Joseph W., Cordes, J.M., de Bruyn, A.G., Macquart, J.-P., The

microarcsecond sky and cosmic turbulence, New Astronomy Reviews Vol. 48, Issue 11–12, 1439–1457, 2004.

Leinert, Ch. et al. (including Pel, J.-W.), Mid-infrared sizes of circumstellar disks

around Herbig Ae/Be stars measured with MIDI on the VLTI, Astron. Astrophys. 423, 537–548, 2004.

Lipkin, Y.M., Ofek, E.O., Gal-Yam, A., Leibowitz, E.M., Poznanski, D., Kaspi,

S., Polishook, D., Kulkarni, S.R., Fox, D.W., Berger, E., Mirabal, N., Halpern, J., Bureau, M., Fathi, K., Price, P.A., Peterson, B.A., Frebel, A., The Detailed Optical Light Curve of GRB 030329, Astrophys. J. 606, L381, 2004.

Macquart, J.-P., Scattering of gravitational radiation. Second order moments of

the wave amplitude, Astron. Astrophys. 422, 761–775, 2004. Macquart, J.-P., Fender, R.P., Circular Polarisation from Relativistic Jet

Sources, Circular Polarisation from Relativistic Jet Sources. Edited by J.-P. Macquart, and R.P. Fender. Reprinted from Astrophys. and Space Science, Vol. 288, Nos. 1–2, 2003, 2004.

Maret, S., Ceccarelli, C., Caux, E., Tielens, A.G.G.M., Jörgensen, J.K., van

Dishoeck, E., Bacmann, A., Castets, A., Lefloch, B., Loinard, L., Parise, B., Schöier, F.L., The H2CO abundance in the inner warm regions of low mass protostellar envelope, Astron. Astrophys. 416, 577–594, 2004.

McDermid, R., Bacon, R., Adam, G., Benn, C., Emsellem, E., Cappellari, M.,

Kuntschner, H.. Bureau, M., Copin, Y., Davies, R.L., Falcon-Barroso, J., Ferruit, P., Krajnovic, D., Peletier, R.F., Shapiro, K., de Zeeuw, P.T., Under the Microscope: Galaxy Centres with OASIS, The Newsletter of the Isaac Newton Group of Telescopes (ING Newsl.), issue no. 8, p. 3, 2004.

McKean, J.P., Koopmans, L.V.E., Browne, I.W.A., Fassnacht, C.D., Blandford,

R.D., Lubin, L.M., Readhead, A.C.S., Keck spectroscopy of Cosmic Lens All-Sky Survey gravitational lenses, Mon. Not. Roy. Astron. Soc. 350, 167–174, 2004.

62

Merín, B. et al. (including Wesselius, P.R.), Study of the properties and spectral energy distributions of the Herbig AeBe stars HD 34282 and HD 141569, Astron. Astrophys. 419, 301–318, 2004.

Middelberg, E., Roy, A.L., Nagar, N.M., Krichbaum, T.P., Norris, R.P., Wilson,

A.S., Falcke, H., Colbert, E.J.M., Witzel, A., Fricke, K.J., Motion and properties of nuclear radio components in Seyfert galaxies seen with VLBI, Astron. Astrophys. 417, 925–944, 2004.

Mokiem, M.R., Martín-Hernández, N.L., Lenorzer, A., de Koter, A., Tielens,

A.G.G.M., Metallicity and the spectral energy distribution and spectral types of dwarf O-stars, Astron. Astrophys. 419, 319–334, 2004.

Mora, A., et al. (including Wesselius, P.R.), Dynamics of the circumstellar gas

in the Herbig Ae stars BF Orionis, SV Cephei, WW Vulpeculae and XY Persei, Astron. Astrophys. 419, 225–240, 2004.

Napolitano, N.R., Romanowsky, A.J., Douglas, N.G., Capaccioli, M.,

Arnaboldi, M., Kuijken, K., Merrifield, M.R., Freeman, K.C., Gerhard, O. Galaxy dynamics with the Planetary Nebula Spectrograph, Memorie della Societa Astronomica Italiana Supplement, Vol. 5, p. 255, 2004.

Navarro, Julio F., Helmi, Amina, Freeman, Kenneth C., The Extragalactic

Origin of the Arcturus Group, Astrophys. J. 601, L43–L46, 2004. Orchiston, W., Davies, R., Denisse, J.-F., Kellermann, K., Morimoto, M., Slysh,

S., Swarup, G., van Woerden, H., The IAU Historic Radio Astronomy Working Group. I: progress report, Journal of Astronomical History and Heritage 7, 53–56, 2004.

Parise, B., Castets, A., Herbst, E., Caux, E., Ceccarelli, C., Mukhopadhyay, I.,

Tielens, A.G.G.M., First detection of triply-deuterated methanol, Astron. Astrophys. 416, 159–163, 2004.

Peeters, E., Allamandola, L.J., Bauschlicher, C.W., Jr., Hudgins, D.M.,

Sandford, S.A., Tielens, A.G.G.M., Deuterated Interstellar Polycyclic Aromatic Hydrocarbons, Astrophys. J. 604, 252–257, 2004.

Peeters, E., Spoon, H.W.W., Tielens, A.G.G.M., Polycyclic Aromatic Hydro-

carbons as a Tracer of Star Formation?, Astrophys. J. 613, 986–1003, 2004.

Peng, B., de Bruyn, A.G., Evidence for Microarcsecond Structure in the BL

Lacertae Object AO 0235+164, Astrophys. J. 610, 151–155, 2004. Pérez, I., Truncation of stellar disks in galaxies at z ~ 1, Astron. Astrophys. 427,

L17–L20, 2004.

63

Pérez, I., Fux, R., Freeman, K., Gas flow and dark matter in the inner parts of early-type barred galaxies. I. SPH simulations and comparison with the observed kinematics, Astron. Astrophys. 424, 799–815, 2004.

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

Abundances of Planetary Nebulae IC 418, IC 2165 and NGC 5882, Astron. Astrophys. 423, 593–605, 2004.

Rawlings, S., Abdalla, F.B., Bridle, S.L., Blake, C.A., Baugh, C.M., Greenhill,

L.J., Hulst, J.M. van der, Galaxy evolution, cosmology and dark energy with the Square Kilometer Array, New Astronomy Reviews 48, 1013–1027, 2004.

Rowan-Robinson, M., et al. (including Héraudeau, Ph.), The European Large-

Area ISO Survey (ELAIS): the final band-merged catalogue, Mon. Not. Roy. Astron. Soc. 351, 1290–1306, 2004.

Sánchez-Pena, J.M., Urruchi, V., Pérez, I., Vázquez, C., Characterization

protocol to evaluate chiral smectic liquid crystals for high-end display applications, Optics Express 12, p.1205, 2004.

Serjeant, S., et el. (including Héraudeau, Ph.), The European Large Area ISO

Survey – IX. The 90-µm luminosity function from the Final Analysis sample, Mon. Not. Roy. Astron. Soc. 355, 813–818, 2004.

Sheth, R.K., Weygaert, R. van de, A hierarchy of voids: much ado about

nothing, Mon. Not. Roy. Astron. Soc. 350, 517–538, 2004. Slavin, J.D., Jones, A.P., Tielens, A.G.G.M., Shock Processing of Large Grains

in the Interstellar Medium, Astrophys. J. 614, 796–806, 2004. Spaans, M., The Synthesis of the Elements and the Formation of Stars, in:

Astrobiology: Future Perspectives (Ehrenfreund et al. ed.), p. 1–16, Kluwer Academic Publishers, Dordrecht, 2004.

Spoon, H.W.W., Armus, L., Cami, J., Tielens, A.G.G.M., Chiar, J.E., Peeters,

E., Keane, J.V., Charmandaris, V., Appleton, P.N., Teplitz, H.I., Burgdorf, M.J., Fire and Ice: Spitzer Infrared Spectrograph (IRS) Mid-Infrared Spectroscopy of IRAS F00183–7111, Astrophys. J. Suppl. Series 154, 184–187, 2004.

Spoon, H.W.W., Moorwood, A.F.M., Lutz, D., Tielens, A.G.G.M.,

Siebenmorgen, R., Keane, J.V., Mid-infrared spectral evidence for a luminous dust enshrouded source in Arp 220, Astron. Astrophys. 414, 873–883, 2004.

Stern, D., van Dokkum, P.G., Nugent, P., Sand, D.J., Ellis, R.S., Sullivan, M.,

Bloom, J.S., Frail, D.A., Kneib, J.-P., Koopmans, L.V.E., Treu, T., Discovery of a Transient U-Band Dropout in a Lyman Break Survey: A Tidally Disrupted Star at z=3.3?, Astrophys. J. 612, 690–697, 2004.

64

Stickel, M., van der Hulst, J.M., van Gorkom, J.H., Schiminovich, D., Carilli,

C.L., First detection of cold dust in the northern shell of NGC 5128 (Centaurus A), Astron. Astrophys. 415, 95–102, 2004.

Sugiyama, N., Zaroubi, S., Silk, J., Isocurvature fluctuations induce early star

formation, Mon. Not. Roy. Astron. Soc. 354, 543–548, 2004. Surendiranath, R., Pottasch, S.R., García-Lario, P., Abundances in planetary

nebulae: Me 2–1, Astron. Astrophys. 421, 1051–1061, 2004. Tolstoy, E., Irwin, M., Cole, A., Fraternali, F., Szeifert, T., Marconi, G., Stellar

Spectroscopy of Individual Stars in Local Group Galaxies with the VLT, The Messenger (ISSN0722–6691) No.115 (March, 2004), 32–34, 2004.

Tolstoy, Eline, Irwin, M.J., Helmi, A., Battaglia, G., Jablonka, P., Hill, V., Venn,

K.A., Shetrone, M.D., Letarte, B., Cole, A.A., Primas, F., Francois, P., Arimoto, N., Sadakane, K., Kaufer, A., Szeifert, T., Abel, T. , Two Distinct Ancient Components in the Sculptor Dwarf Spheroidal Galaxy: First Results from the Dwarf Abundances and Radial Velocities Team, Astrophys. J. 617, L119–L122, 2004.

Treu, T., Koopmans, L.V.E., Massive Dark Matter Halos and Evolution of

Early-Type Galaxies to z ~ 1, Astrophys. J. 611, 739–760, 2004. Uemura, M., et al. (including Macquart, J.-P.), Outburst and Post-Outburst

Active Phase of the Black Hole X-Ray Binary V4641 Sagittarii in 2002, Publications of the Astronomical Society of Japan, Vol. 56, No. SP1, S61–S75, 2004.

Uglesich, R.R., Crotts, A.P.S., Baltz, E.A., de Jong, J., Boyle, R.P., Corbally,

C.J., Evidence of Halo Microlensing in M31, Astrophys. J. 612, 877–893, 2004.

Van Malderen, R., Decin, L., Kester, D., Vandenbussche, B., Waelkens, C.,

Cami, J., Shipman, R.F., On the analysis of band 3 of the ISO-SWS calibration sources, Astron. Astrophys. 414, 677–697, 2004.

Venn, K.A., Irwin, M., Shetrone, M.D., Tout, C.A., Hill, V., Tolstoy, E., Stellar

Chemical Signatures and Hierarchical Galaxy Formation, Astron. J. 128, 1177–1195, 2004.

Wakker, B.P., de Boer, K.S., Woerden, H. van, History of HVC Research – an

overview, in: in High-Velocity Clouds (eds. H. van Woerden, B.P. Wakker, U.J. Schwarz, and K.S. de Boer), Astrophysics and Space Science Library, Vol. 312, p. 1–24, Kluwer Academic Publishers, Dordrecht, 2004.

Woerden, H. van, and Wakker, B.P., Distances and Metallicities of HVCs, in: in

High-Velocity Clouds (eds. H. van Woerden, B.P. Wakker, U.J. Schwarz,

65

and K.S. de Boer), Astrophysics and Space Science Library, Vol. 312, 195–226, Kluwer Academic Publishers, Dordrecht, 2004.

Woerden, H. van, Wakker, B.P. Schwarz, U.J., de Boer, K.S. (eds.), High

Velocity Clouds, Astrophysics and Space Science Library Vol. 312, 400 pgs., Kluwer Academic Publishers, Dordrecht, 2004.

I.2 Conference papers

Agüeros, M.A., Walkowicz, L.M., Ivezic, Z., Obric, M., The UV and Optical Properties of GALEX-SDSS sources, Bull. American Astron. Soc. (204th Meeting of the American Astronomical Society), #91.04, 2004.

Allen, R.J., Holwerda, B.W., Gonzalez, R.A., van der Kruit, P.C., Arm and

inter-arm opacities from counts of background galaxies, Bull. American Astron. Soc. (204th Meeting of the American Astronomical Society), #40.22, 2004.

Baryshev, A., Carter, M., Jellema, W., Hesper, R., Design and evaluation of

ALMA band 9 quasioptical system In: Proc of the 5th International Conf. on Space Optics (ICSO 2004) (ed.: B. Warmbein), 30 March–- 2 April 2004, Toulouse, France, ESA SP–554, 365–371, ESA Publications Division, Noordwijk, Netherlands, 2004.

Battaglia, G., Tolstoy, E., Helmi, A., Irwin, M., Kinematics and metallicity

relations for dwarf galaxies in the Local Group, in: Baryons in Dark Matter Halos (eds. R. Dettmar, U. Klein, P. Salucci), Conf. Proc. (Novigrad, Croatia, 5–9 Oct 2004) published by SISSA, Proceedings of Science, http://pos.sissa.it, p. 54.1, 2004.

Battaglia, Giuseppina, Kinematics and metallicity relations for dwarf galaxies

in the Local Group, in: Baryons in Dark Matter Halos (eds. R. Dettmar, U. Klein, P. Salucci), Conf. Proc. (Novigrad, Croatia, 5–9 Oct 2004) published by SISSA, Proceedings of Science, http://pos.sissa.it, p. 54, 2004.

Boomsma, R., Oosterloo, T., van der Hulst, T., Sancisi, R., Holes and High

Velocity HI in NGC 6946, in: Recycling Intergalactic and Interstellar Matter (eds. Pierre-Alain Duc, Jonathan Braine and Elias Brinks), IAU Symp. 217 (Sydney, Australia, July 2033), p.142, San Francisco: Astronomical Society of the Pacific, 2004.

Bosler, T.L., Smecker-Hane, T.A., Cole, A., Stetson, P.B., Stellar Populations

of the Leo I and Leo II dSph Galaxies: Chemical Abundances and Ages, in: Origin and Evolution of the Elements, from the Carnegie Observatories Centennial Symposia. Carnegie Observatories Astrophysics Series (eds. A. McWilliam and M. Rauch),

66

http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html, Pasadena: Carnegie Observatories, 2004.

Brentjens, M.A., Bruyn, A.G. de, Polarized Emission Throughout the Perseus

Cluster, in: The Riddle of Cooling Flows in Galaxies and Clusters of Galaxies (eds. T. Reiprich, J. Kempner, and N. Soker), Conf. Proc (Charlottesville, USA, May 31 – June 4, 2003), published at www.astro.virginia.edu/coolflow/, 2004.

Bringa, E.M., Bajt, S., Baragiola, R.A., Bradley, J., Dai, Z., Dukes, C., Felter, T.,

Graham, G., Kucheyev, S., Loeffler, M.J., Tielens, A., Torres, D., Vanbreugel, W. Can cosmic rays amorphize silicate dust particles? American Geophysical Union, Fall Meeting 2004, abstract #SH51D–0297, 2004.

Candotti, M., Cahill, G.A., Finn, T.J., Jellema, W., Lavelle, J., Murphy, J.A.,

O'Sullivan, C., Trappe, N.A., Quasi-optical verification of the focal plane optics of the heterodyne instrument for the far-infrared (HIFI), in: Optimizing Scientific Return for Astronomy through Information Technologies (eds. Quinn, P.J., Bridger, A.), Proc. of the SPIE Vol. 5497, p. 565–576, The International Society for Optical Engineering, 2004.

Carter, M.C., Baryshev, A., Harman, M., Lazareff, B., Lamb, J., Navarro, S.,

John, D., Fontana, A.-L., Ediss, G., Tham, Ch.Y., Withington, S., Tercero, F., Nesti, R., Tan, Gie-Han, Sekimoto, Yu., Matsunaga, M., Ogawa, H., Claude, S., ALMA front-end optics, Proc. of the SPIE Vol. 5489, 1074–1084, The International Society for Optical Engineering, 2004.

Chiar, J.E., Tielens, A.G.G.M., Peeters, E., Circumstellar Carbonaceous

Material Associated with Late-Type Dusty WC Wolf-Rayet Stars, in: Bioastronomy 2002: Life Among the Stars (eds. R. Norris, and F. Stootman), IAU Symp. 213, p. 193, San Francisco: Astronomical Society of the Pacific, 2004.

Christen, F., Cavadore, C.m Baade, D.m Iwert, O., Kuijken, K., Gaillard, B.,

Darbon, S., Characterizing the CCDs of the OmegaCAM Wide-Angle Camera, in: Scientific Detectors for Astronomy, The Beginning of a New Era (eds. Amico, P., Beletic, J.W., Beletic, J.E.), Conf. Proc., p. 485–488, Kluwer Academic Publ., Dordrecht, 2004.

Cole, A.A., Smecker-Hane, T.A., Tolstoy, E., Gallagher, J.S., Abundance

Patterns of the Large Magellanic Cloud Disk and Bar, in: Origin and Evolution of the Elements, from the Carnegie Observatories Centennial Symposia. Carnegie Observatories Astrophysics Series (eds. A. McWilliam and M. Rauch), http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html, Pasadena: Carnegie Observatories, 2004.

67

Cole, A.A., Tolstoy, E., Irwin, M.; Szeifert, T., Venn, K., Paleochemistry of Local Group Dwarf Irregular Galaxies, Bull. American Astron. Soc. (205th Meeting of the American Astronomical Society), #93.11, 2004.

Covone, G., Napolitano, N.R., A detailed view on the kinematics of candidate

intermediate luminosity early-type galaxies with a lack of dark matter, Astronomische Nachrichten, 104–107, 2004.

Crotts, A.P.S., Uglesich, R.R., Baltz, E.A., de Jong, J., Boyle, R.P., Corbally,

C.J., Evidence for Halo Microlensing from a Survey of M31, in: Dark Matter in Galaxies (eds. S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July, 2003, Sydney, Australia), p. 121, San Francisco: Astronomical Society of the Pacific, 2004.

Dietrich, J. P., Clowe, D., Schneider, P. Kerp, J., Romano-Díaz, E., Weak

lensing evidence for a filament between A222/A223, in: Outskirts of Galaxy Clusters: Intense Life in the Suburbs (ed. Antonaldo Diaferio), IAU Coll. #195, 34–38, Cambridge Univ. Press, 2004.

Douglas, N.G., Romanowsky, AJ.., Kuijken, K., Merrifield, M.R., Napolitano,

N.R., Arnaboldi, M., Freeman, K., Capaccioli, M., Gerhard, O. , Early-Type Galaxy Halo Dynamics Inferred Using the PN Spectrograph, in: Dark Matter in Galaxies (eds. S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July 2003, Sydney, Australia), p. 171, San Francisco: Astronomical Society of the Pacific, 2004.

Falcón-Barroso, J., Bacon, R., Bureau, M., Cappellari, M., Davies, R.L.,

Emsellem, E., Krajnovic, D., Kuntschner, H., McDermid, R., Peletier, R.F., de Zeeuw, P.T., A SAURON look at galaxy bulges, Astronomische Nachrichten, 92–95, 2004.

Filho, M.E., Fraternali, F., Markoff, S., Nagar, N.M., Barthel, P.D., Ho, L.C.,.

Yuan, F. Emission mechanisms in composite galaxies, in: The Interplay among Black Holes, Stars and ISM in Galactic Nuclei (eds. T. Storchi-Bergmann, L.C. Ho & H.R. Schmitt), IAU Symp. 222 (March 2004, Gramado, RS, Brazil), 91–92, Cambridge Univ. Press, 2004.

Fiorentin, P. Re, Helmi, A., Lattanzi, M. G., Spagna, A., More evidence of

substructure in the motions of nearby halo stars, in: Outskirts of Galaxy Clusters: Intense Life in the Suburbs ((ed. A. Diaferio), Proc. IAU Coll. 195, 508–510, Cambridge Univ. Press, 2004.

Fraternali, F., Oosterloo, T., Sancisi, R., The HI halo of spiral galaxies,

Astrophysics and Space Science, p. 377–380, 2004. Fraternali, F., Oosterloo, T., Boomsma, R., Swaters, R., Sancisi, R., High

Velocity Gas in the Halos of Spiral Galaxies, in: Recycling Intergalactic and Interstellar Matter (eds. Pierre-Alain Duc, Jonathan Braine and Elias Brinks), IAU Symp. 217 (Sydney, Australia, July 2033), p. 136, San Francisco: Astronomical Society of the Pacific, 2004.

68

Graauw, T. de, Heterodyne Instrument for the Far Infrared (HIFI)for the

Herschel Space Observatory, Bull. American Astron. Soc. (205th Meeting of the American Astronomical Society), #93.04, 2004.

Haverkorn, M., Katgert, P., de Bruyn, A G., Heitsch, F., Unraveling the

Structure in the ISM Through Radio Polarimetry, in: The Magnetized Interstellar Medium (eds. B. Uyaniker, W. Reich, and R. Wielebinski), Conf. Proc. (Antalya, Turkey, Sept. 2003), p. 81–86, Copernicus GmbH, Katlenburg-Lindau, 2004.

Helmi, A., Navarro, J.F., Meza, A., Steinmetz, M., Eke, V.R., On the nature of

the ring-like structure in the outer Galactic disk, in: Satellites and tidal streams (eds. F. Prada & D. Martinez-Delgado), ASP Conf. Series Vol. 327, p. 87, San Francisco: Astron. Soc. of the Pacific, 2004.

Holwerda, B.W., Gonzalez, R.A., Allen, R.J., van der Kruit, P.C., The opacity

of spiral disks from counts of distant galaxies, Bull. American Astron. Soc. (205th Meeting of the American Astronomical Society), #122.051, 2004.

Holwerda, B.W., Gonzalez, R.A., Allen, R.J., van der Kruit, P.C., The Opacity

of Spiral Galaxies from Counts of Distant Background Galaxies iin: Dark Matter in Galaxies (S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July, 2003, Sydney, Australia), p. 323, San Francisco: Astron. Soc. of the Pacific, 2004.

Holwerda, B.W., Gonzalez, R.A., Allen, R.J., van der Kruit, P.C., Radial

Extinction in Spiral Disk from the numbers of background galaxies, Bull. American Astron. Soc. (204th Meeting of the American Astronomical Society), #15.06, 2004.

Hulst, J.M. van der, Sancisi, R., Evidence for Gas Accretion in Galactic Disks,

in: Recycling Intergalactic and Interstellar Matter (eds. Pierre-Alain Duc, Jonathan Braine and Elias Brinks), IAU Symp. 217 (Sydney, Australia, July 2033), p. 122, San Francisco: Astronomical Society of the Pacific, 2004.

Jellema, W., Huisman, R., Candotti, M., Finn, T., Trappe, N., Murphy, J.A.,

Withington, S., Wild, W., Comparison of near-field measurements and electromagnetic simulations of the focal plane unit of the Heterodyne Instrument for the Far-Infrared, In: Proc of the 5th International Conf. on Space Optics (ICSO 2004) (ed.: B. Warmbein), 30 March – 2 April 2004, Toulouse, France, ESA SP–554, p. 303–322, ESA Publications Division, Noordwijk, Netherlands 2004.

Jellema, W., Wijnholds, S.J., Wesselius, P.R., Withington, S., Yassin, G.,

Murphy, J.A., O S̀ullivan, C., Trappe, N., Peacocke, T., Leone, B., Performance Chararacterisation and Measurement Resluts of a submillimeter-Wave Near-Field Facility for the heterodyne Instrument for the Far-Infrared, in: Proc of 3rd ESA Workshop on Millimeter Wave

69

Technology and Application (Millilab, Expoo, Finland, May 21–23, 2003), 2004.

Jong, J. de, Probing MACHOs in M31, in: Baryons in Dark Matter Halos (eds.

R. Dettmar, U. Klein, P. Salucci), Conf. Proc. (Novigrad, Croatia, 5–9 Oct 2004), Published by SISSA, Proceedings of Science, http://pos.sissa.it, p. 93, 2004.

Kelz, A., Verheijen, M., Roth, M.M., Laux, U., Bauer, S.-M., Development of

the wide-field IFU Ppak, in: Ground-based Instrumentation for Astronomy (eds. Alan F. M. Moorwood and Iye Masanori), Proc. of the SPIE Vol. 5492, 719–730, The International Society for Optical Engineering, 2004.

Koopmans, L.V.E., Treu, T., The Lenses Structure and Dynamics Survey, in:

Multiwavelength Cosmology (ed. Manolis Plionis), Conf. Proc. (Mykonos Island, Greece, 17–20 June 2003), Astrophysics and Space Science Vol. 301, p. 23, Kluwer Academic Publ., Dordrecht, 2004.

Koopmans, Leon, Dark-Matter and Baryons in Early-type Lens Galaxies, in:

Proc of Baryons in Dark Matter Halos (eds. R. Dettmar, U. Klein, P. Salucci) Published by SISSA, Proceedings of Science, http://pos.sissa.it (Novigrad, Croatia, 5–9 Oct 2004), p. 66, 2004.

Kraemer, K.E., Price, S.D., Shipman, R.F., Mizuno, D.R., Kuchar, T., Carey,

S.J., Large-Scale Observations of Galactic Star Forming Regions with the Midcourse Space Experiment, in: Milky Way Surveys: The Structure and Evolution of our Galaxy (eds. D. Clemens, R. Shah, and T. Brainerd), Proc. ASP Conference #317, 5th Boston University Astrophysics Conf. (June 2003, Boston), p. 145, San Francisco: Astronomical Society of the Pacific, 2004.

Kress, M.E., McKay, C., Tielens, A.G., Frenklach, M., Chemical Kinetics of

Polycyclic Aromatic Hydrocarbons in Comet Impacts, American Geophysical Union, Fall Meeting 2004, #P31A-0973, 2004.

Kress, M.E., Tielens, A.G.G.M., Frenklach, M.E., Chemical Kinetics of the

Growth and Destruction of PAHs in Circumstellar Environments, Bull. American Astron. Soc. (205th Meeting of the American Astronomical Society), #58.05, 2004.

Kruizinga, B., Visser, H., Pel, J.W., Moddemeijer, K., Smorenburg, C., MIRI

spectrometer optical design, In: Proc of the 5th International Conf. on Space Optics (ICSO 2004) (ed.: B. Warmbein), 30 March – 2 April 2004, Toulouse, France, ESA SP–554, 263–271, ESA Publications Division, Noordwijk, Netherlands, 2004.

Kuijken, Konrad, et al. (including, Valentijn, Ed, Begeman, K.G., Boxhoorn,

D., Christen, F.), OmegaCAM: wide-field imaging with fine spatial resolution, in: UV and Gamma-Ray Space Telescope Systems (eds.:

70

Hasinger, Günther; Turner, Martin J.L.), Proc. of the SPIE Vol. 5492, p. 484–493, The International Society for Optical Engineering, 2004.

McDermid, R., Emsellem, E., Cappellari, M., Kuntschner, H., Bacon, R.,

Bureau, M., Copin, Y., Davies, R.L., Falcón-Barroso, J., Ferruit, P., Krajnovic, D., Peletier, R.F., Shapiro, K., Wernli, F., de Zeeuw, P.T., OASIS high-resolution integral field spectroscopy of the SAURON ellipticals and lenticulars, Astronomische Nachrichten, 100–103, 2004.

Meijerink, R., Spaans, M., Israel, F.P., Diagnostics of dense irradiated gas

around galaxy nuclei, in: The Interplay among Black Holes, Stars and ISM in Galactic Nuclei (eds. T. Storchi-Bergmann, L.C. Ho & H.R. Schmitt), IAU Symp. 222 (March 2004, Gramado, RS, Brazil), 343–344, Cambridge University Press, 2004.

Mirabal, N., Halpern, J.P., Bureau, M., Fathi, K., A Search for Short Time-Scale

Optical Variability in the GRB 030329 Afterglow, in: Gamma-Ray Bursts: 30 Years of Discovery (eds. E.E. Fenimore and M. Galassi), AIP Conf. Proc. Vol. 727 (September 2003, Santa Fe, New Mexico), 337–338, Melville, NY: American Institute of Physics, 2004.

Morganti, R., Oosterloo, T., Emonts, B.H.C., Tadhunter, C.N., Holt, J. Gas

Outflows in Radio Galaxies, in: Recycling Intergalactic and Interstellar Matter (eds. P.-A. Duc, J. Braine, and E. Brinks), IAU Symp. 217 (July, 2003, Sydney, Australia), p. 332, San Francisco: Astronomical Society of the Pacific, 2004.

Nagar, N.M., Falcke, H., Wilson, A.S., Radio Luminosity Function, Importance

of Jet Power, and Radio Properties of Nearby Low-Luminosity Active Galactic Nuclei, in: Proc. 7th Symp. of the European VLBI Network on New Developments in VLBI Science and Technology (eds. R. Bachiller, F. Colomer, J.-F. Desmurs, and P. de Vicente) (Oct. 2004, Toledo, Spain), p. 51–54, Observatorio Astronomico Nacional of Spain, 2004.

Nagar, N.M., Falcke, H., Wilson, A.S., AGNs in LLAGNs: High resolution radio

observations of the Palomar sample, in: The Interplay among Black Holes, Stars and ISM in Galactic Nuclei (eds. T. Storchi-Bergmann, L.C. Ho & H.R. Schmitt), IAU Symp. 222 (March 2004, Gramado, RS, Brazil), p. 461–462, Cambridge Univ. Press, 2004.

Napolitano, N., Dark-to-luminous properties of early type galaxies, in: Proc of

"Baryons in Dark Matter Halos" (eds. R. Dettmar, U. Klein, P. Salucci), Novigrad, Croatia, Oct 2004. Published by SISSA, Proceedings of Science, http://pos.sissa.it, p. 67, 2004.

Napolitano, N.R., Capaccioli, M., Arnaboldi, M., Merrifield, M.R., Douglas,

N.G., Kuijken, K., Romanowsky, A.J., Freeman, K.C. Is there a dichotomy in the Dark Matter as well as in the Baryonic Matter properties of ellipticals?, in: Dark Matter in Galaxies (eds: S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July 2003, Sydney,

71

Australia), p. 173, San Francisco: Astronomical Society of the Pacific, 2004.

Noordermeer, E., van der Hulst, T., Sancisi, R., Swaters, R., The Mass

Distribution in Early Type Disk Galaxies, in: Dark Matter in Galaxies (eds: S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July 2003, Sydney, Australia), p. 287, San Francisco: Astronomical Society of the Pacific, 2004.

Noordermeer, E., van der Hulst, T., Swaters, R., Rotation curves and dark

matter in early type disk galaxies, in: Proc of "Baryons in Dark Matter Halos" (eds. R. Dettmar, U. Klein, P. Salucci), Novigrad, Croatia, Oct 2004. Published by SISSA, Proceedings of Science, http://pos.sissa.it, p. 68.1, 2004.

Obric, M., Ivezic, Z., Lupton, R.H., Kauffmann, G., Knapp, G.R., Gunn, J.E.,

Schlegel, D., Strauss, M.A., Anderson, S., Multiwavelength view of SDSS galaxies, in: The Interplay among Black Holes, Stars and ISM in Galactic Nuclei (eds. T. Storchi-Bergmann, L.C. Ho & H.R. Schmitt), IAU Symp. 222 (March 2004, Gramado, RS, Brazil), p. 533–534, Cambridge Univ. Press, 2004.

Oosterloo T.A., Morganti, R., Emonts, B.H.C., Tadhunter, C.N., Fast outflows

of neutral hydrogen in radio galaxies, in: The Interplay among Black Holes, Stars and ISM in Galactic Nuclei (eds. T. Storchi-Bergmann, L.C. Ho & H.R. Schmitt), IAU Symp. 222 (March 2004, Gramado, RS, Brazil), p.353–354, Cambridge Univ. Press, 2004.

Oosterloo, T., Morganti, R., Sadler, E.M., Ferguson, A., van der Hulst, T.,

Jerjen, H., Tidal Remnants and Intergalactic HII Regions, in: Recycling Intergalactic and Interstellar Matter (eds. Pierre-Alain Duc, Jonathan Braine and Elias Brinks), IAU Symp. 217 (Sydney, Australia, July 2033), p. 486, San Francisco: Astronomical Society of the Pacific, 2004.

O'Sullivan, C., Murphy, J.A., Cahill, G., Gradziel, M.L., Trappe, N., White, D.,

Yurchenko, V., Withington, S., Jellema, W., Developments in quasi-optical design for THz, in: Astronomical Structures and Mechanisms Technology (eds. Antebi, J., Lemke, D.), Proc. of the SPIE Vol. 5498, p. 320–331, The International Society for Optical Engineering, 2004.

Peletier, R., Balcells, M., Falcón-Barroso, J., Graham, A., The formation of

galactic bulges, in: Baryons in Dark Matter Halos (eds. R. Dettmar, U. Klein, P. Salucci), Conf. Proc. (Novigrad, Croatia, 5–9 Oct 2004) published by SISSA, Proceedings of Science, http://pos.sissa.it, p. 60.1, 2004.

Perez Martin, I., Dark matter in the inner parts of barred galaxies, in: Baryons

in Dark Matter Halos (eds. R. Dettmar, U. Klein, P. Salucci), Conf. Proc. (Novigrad, Croatia, 5-9 Oct 2004) published by SISSA, Proceedings of Science, http://pos.sissa.it, p. 47.1, 2004.

72

Pérez, I., Truncation of stellar disks at high redshift, in: Penetrating Bars

through Masks of Cosmic Dust (eds. D. Block, I. Puerari, K.C. Freeman, R. Groess, E.K. Block), Astrophysics and Space Science Library Vol. 319, 2004.

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

Napolitano, N.R., Merrett, H., Capaccioli, M., Freeman, K.C., Gerhard, O., R., Freeman, Kenneth C. Elliptical Galaxies: Darkly Cloaked or Scantily Clad? in: Dark Matter in Galaxies (eds: S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July 2003, Sydney, Australia), p. 165, San Francisco: Astronomical Society of the Pacific, 2004.

Romanowsky, A.J., Napolitano, N.R., Capaccioli, M., Douglas, N.G.,

Merrifield, M.R., Kuijken, K., Gerhard, O., Arnaboldi, M., Freeman, K.C. Halo masses of early-type galaxies: theory vs observation, Bull. American Astron. Soc. (205th Meeting of the American Astronomical Society), #31.07, 2004.

Sakai, S., Kennicutt, R.C., van der Hulst, J.M., The Deep, Wide-field Halpha

Survey of Nearby Clusters of Galaxies, in: Origin and Evolution of the Elements, from the Carnegie Observatories Centennial Symposia. Carnegie Observatories Astrophysics Series (eds. A. McWilliam and M. Rauch), www.ociw.edu/ociw/symposia/series/symposium3/proceedings3.html, 2004.

Salter, D.M., Paardekooper, J.-P., Röttgering, H.J.A., Bähren, L., Brentjens,

M., Falcke, H., Wijnholds, S., LOFAR - The New Eye for the Low-Frequency Universe, Bull. American Astron. Soc. (205th Meeting of the American Astronomical Society), #105.06, 2004.

Sancisi, R., The Visible Matter - Dark Matter Coupling, in: Dark Matter in

Galaxies (eds: S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July 2003, Sydney, Australia), p. 233, San Francisco: Astronomical Society of the Pacific, 2004.

Sanders, R.H., Are there alternatives to dark matter? in: Where Cosmology

and Fundamental Physics meet (eds. V. Le Brun, S. Basa, A. Mazure), Conf. Proc., 108–117, Frontier Group, 2004.

Swaters, R.A., Verheijen, M.A.W., Bershady, M.A., Andersen, D.R., The

Kinematics in the Cores of Low Surface Brightness Galaxies, in: Dark Matter in Galaxies (eds. S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July, 2003, Sydney, Australia), p. 77, San Francisco: Astronomical Society of the Pacific, 2004.

Tielens, A.G.G.M., Peeters, E., Spectroscopy of Interstellar PAHs, in: The

Dense Interstellar Medium in Galaxies (eds. S.Pfalzner, C. Kramer, C.

73

Staubmeier, and A. Heithausen), Proc. 4th Cologne-Bonn-Zermatt Symp. (Zermatt, Switzerland, 22-26 Sept. 2003), Springer proceedings in physics Vol. 91, p. 497, Berlin, Heidelberg: Springer, 2004.

Tielens, A.G.G.M., Peeters, E., Bakes, E.L.O., Spoon, H.W W., Hony, S.,

PAHs and Star Formation, in: Star Formation in the Interstellar Medium: In Honor of David Hollenbach, Chris McKee and Frank Shu (eds. D. Johnstone, F.C. Adams, D.N.C. Lin, D.A. Neufeld, and E.C. Ostriker), ASP Conf. Proc. Vol. 32., p. 135, San Francisco: Astronomical Society of the Pacific, 2004.

Tielens, X., Waters, R., Bernatowicz, T., The Composition, Origin and

Evolution of Dust in Circumstellar and Interstellar Environments, Workshop on Chondrites and the Protoplanetary Disk, Nov. 8–11, 2004, Kauai, Hawaii, abstract no. 9118, 2004.

Trager, S.C., Abundances from the Integrated Light of Globular Clusters and

Galaxies, in: Origin and Evolution of the Elements, from the Carnegie Observatories Centennial Symposia. Carnegie Observatories Astrophysics Series (eds. A. McWilliam and M. Rauch), http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html, p. 391, Pasadena: Carnegie Observatories, 2004.

Trappe, N.A., Lanigan, B., Finn, T.J., Jellema, W., Murphy, J.A., Withington, S.,

Gaussian beam mode analysis of standing waves in submillimeter telescope and receiver systems, in: Optimizing Scientific Return for Astronomy through Information Technologies (eds. Quinn, P.J., Bridger, A.), Proc. of the SPIE Vol. 5497, 531–541, The International Society for Optical Engineering, 2004.

Treu, T., Koopmans, L.V.E., Sand, D.J., Smith, G.P., Ellis, R.S., The dark

matter halos of spheroidal galaxies and clusters of galaxies, in: Dark Matter in Galaxies (eds: S.D. Ryder, D.J. Pisano, M.A. Walker, and K.C. Freeman), IAU Symp. 220 (July 2003, Sydney, Australia), p. 159, San Francisco: Astronomical Society of the Pacific, 2004.

Valentijn, E.A., Kuijken, K., ASTRO-WISE: An Astronomical Wide-Field

Imaging System for Europe, in: Toward an International Virtual Observatory (eds. P.J. Quinn, and K.M. Gorski), Proc. ESO/ESA/NASA/NSF Conf. (Garching, Germany, 10-14 June 2002), ESO Astrophysics Symposia, p. 19, Berlin: Springer, 2004.

Venn, K.A., Tolstoy, E., Kaufer, A., Kudritzki, R.P., Stellar Abundances in

Dwarf Irregular Galaxies, in: Origin and Evolution of the Elements, from the Carnegie Observatories Centennial Symposia. Carnegie Observatories Astrophysics Series (eds. A. McWilliam and M. Rauch), http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html, Pasadena: Carnegie Observatories, 2004.

74

Verheijen, M.A.W., Galaxy evolution in dense environments: a concise HI perspective, in: Outskirts of Galaxy Clusters: Intense Life in the Suburbs (ed. Antonaldo Diaferio), IAU Colloquium 195, 394–400, Cambridge Univ. Press, 2004.

Villalobos, A., Formation of thick disks in galaxies, in: Baryons in Dark Matter

Halos (eds. R. Dettmar, U. Klein, P. Salucci), Conf. Proc. (Novigrad, Croatia, 5-9 Oct 2004) published by SISSA, Proceedings of Science, http://pos.sissa.it, P. 90.1, 2004.

Wesselius, P.R., Astronomy at IR/submm and the microwave background

Space-based astronomy COSPAR E1.5 and IAF Q1 Symposium, Advances in Space Research, 475–476, 2004.

Weygaert, R. van de, Sheth, R., Void Hierarchy, in: Multiwavelength

Cosmology (ed. Manolis Plionis), Conf. Proc. (Mykonos Island, Greece, 17–20 June 2003), Astrophysics and Space Science Vol. 301, p. 223, Kluwer Academic Publ., Dordrecht,, 2004.

Weygaert, R. van de, Sheth, R., Platen, E., A hierarchy of voids, in: Outskirts

of Galaxy Clusters: Intense Life in the Suburbs (ed. Antonaldo Diaferio), IAU Colloquium 195, p. 58–63, Cambridge Univ. Press, 2004.

Wong, T., Blitz, L., van der Hulst, J.M., Comparing the CO and HI Distributions

in Nearby Spiral Galaxies at High Resolution, Astrophysics and Space Science Vol. 289, p. 211–214, 2004.

I.3 Dissertations

Cazaux, Stephanie, Grain Surface Chemistry in Astrophysical objects: From H2 to Complex Molecules, Promotor: Prof. er. A.G.G.M. Tielens, co-promotor: Dr. M.C. Spaans, Dissertation Faculty Mathematic and Natural Sciences, University of Groningen (06-02-2004), 144 pgs., 2004.

Fathi, Kambiz, Morphology and Dynamics in the Inner Regions of Spiral

Galaxies, Promotor: Prof. dr. P.C. van der Kruit, co-promotor: Dr. R.F. Peletier, beoordelingscommissie: Prof. dr. P.D. Barthel, Prof. dr. J.H. Knapen, Prof. dr. R. Sancisi, Dissertation Faculty Mathematic and Natural Sciences, University of Groningen (17-12-2004), 188 pgs., 2004.

Hunt, Leslie Kipp, Building Galaxies: From Low-Metallicity Compact Dwarfs

to Active Galactic Nuclei, Promotor: Prof. dr. P.C. van der Kruit; beoordelingscommissie: Prof. dr. P.D. Barthel, Prof. dr. A.G. de Bruyn, Prof. dr. J.M. van der Hulst, Dissertation Faculty Mathematic and Natural Sciences, University of Groningen (15-10-2004), 299 pgs., 2004

75

Klöckner, H.-R., Extragalactic Hydroxyl, Promotor: Prof. dr. J.M. van der Hulst, co-promotor: Dr. W.A. Baan, Dissertation Faculty Mathematic and Natural Sciences, University of Groningen (19-03-2004), 160 pgs., 2004.

Romano-Diaz, Emilio, Probing Cosmic Velocity Flows in the Local

Universe, Promotoren: Prof. dr. M.A.M. van de Weijgaert, Prof. dr. R.H. Sanders; beoordelingscommissie: Prof. dr. T.S. van Albada, Prof. dr. J.M. van der Hulst, Prof. dr. M. Plionis, Dissertation Faculty Mathematic and Natural Sciences, University of Groningen (08-10-2004), 312 pgs., 2004

I.4 Popular articles

Barthel, P. , Beta-columns Universiteitskrant (Sept, Oct, Nov, Dec), 2004. Bruyn, G. de, LOFAR, Kijk, 20, 2004. Comello, Georg, Rho Cassiopeiae in: Sterrengids 2004 (Matt Drummen en

Jan Meeus), Stichting "De Koepel", in opdracht van de Koninklijke Nederlandse Vereniging voor Weer- en Sterrenkunde, p. 144–145, 2004.

Echternach, E., Barthel, P., RuG Kinderuniversiteit, Zenit, Nov., 2004. Peeters, E., Tielens, X., Cami, J., Teer en roet tussen de sterren, Zenit, Jan.,

p. 25-30, 2004. Schilling, G., Barthel, P., Het Heelal is van ons allemaal, Intermediair 15, April,

2004. Shipman, R., Roelfsema, P., de Graauw, Th., De erfenis van de Short Wave-

length Spectrometer, Zenit, Jan., 4-10, 2004. Woerden, Hugo van, Professor Blaauw negentig jaar, Zenit 31, nr. 4, 194-195,

2004.

77

APPENDIX II : Participation in scientific meetings

203rd Meeting of the American Astronomical Society (Atlanta, USA; 4–8 Jan. ’04): A.A. Cole (short comm.: “Chemical evolution and star formation history of the Large Magellanic Cloud” – Cole, A.A., Smecker-Hane, T.A., Gallagher, J.S., Tolstoy, E.,), K. Fathi (“Exploring non-circular gaseous motions in early-type spirals” – K. Fathi, J. Falcón-Barroso ,̀ R.F. Peletier, Emsellem, E.), B.W.Holwerda. (“Radial Extinction in Spiral Disks” – Holwerda, B.W., Gonzalez, R.A., Allen, R.J., van der Kruit, P.C.). Dutch Astronomer’s Club Spring Meeting (Nijmegen, 23 Jan. ‘04): J.M. van der Hulst, R. van de Weijgaert, H. van Woerden. RAS Meeting “The Role of AGN in the Universe” (London, UK; 16–19 Feb. ’04): J.-P. Macquart. Dwingeloo Workshop (Zwolle; 17–20 Feb. ’04): M.C. Spaans (review: “Irradiated dense molecular gas: from YSO’s to AGN”). HIFI Core Science Meeting and CHAMP+ Meeting (Leiden, 27 Feb. ’04): M.C. Spaans. IAU Symposium 222 “The Interplay among Black Holes, Stars and ISM in Galactic Nuclei” (Gramado, Brazil; 1–5 March ’04): N. Nagar (“AGNs in LLAGNs: High resolution radio observations of the Palomar sample” – Neil M. Nagar, Heino Falcke, Andrew S.), M. Obri� (poster: “Multiwavelength view of SDSS galaxies” – M. Obri�, Z. Ivezi�, G. Kauffmann G.R. Knapp, J.E. Gunn, D. Schlegel, M.A. Strauss and S. Anderson). IAU Colloquium 195 “Outskirts of Galaxy Clusters: intense life in the suburbs” (Torino, Italy; 12–16 March ’04): M.A. Aragón Calvo, P.A. Araya Melo, M.A. Brentjens (“Mpc scale polarized radio emission in the Perseus cluster” – Brentjens, M.A. and de Bruyn, A.G.), G. Sikkema (poster: “HST ACS observations of six shell galaxies”), E.A. Valentijn,

78

M. Verheijen (inv. review: “Galaxy evolution in dense environments”), R. van de Weijgaert (SOC) (“A hierarchy of voids”). IRQA Meeting “Western Australia low frequency array” (Hawaii, USA; 19–22 March ’04): A.G. de Bruyn (“NL-LOFAR plans, and some ITS/LFFE results”). 5th International Conference on Space Optics (Toulouse, France; 1 April ’04): W. Jellema (“Comparison of near-field measurements and electro-magnetic simulations of the focal plane unit of the HIFI”). XXIVth Moriond Astrophysics Meeting “The young local Universe” (La Thuile, Aosta Valley, Italy: 21–28 March ’04): W. Frieswijk (poster: “Infrared dark clouds in a galactic context”). Workshop “Radiative Transfer Modeling of Water” (Leiden, the Nether-lands; 22–24 March ’04): F.P. Helmich ( “HIFI: the Heterodyne Instrument for the Far-Infrared”), D. Poelman, M.C. Spaans. Dutch Astrophysics Days (Nijmegen, he Netherlands; 1–2 April ’04): D. Poelman, M.C. Spaans. 1st ANGLES Network Workshop (Bonn, Germany; 5–6 April ’04): L.V.E. Koopmans (inv. contr.: “Probing High-z galaxies through lensing and dynamics”). IDW-ISS Workshop (Dwingeloo, the Netherlands; 5–7 April ’04): A.G. de Bruyn (“J1819+3845: modulations, evolution, polarization and other properties”). Workshop “Benchmarking of Photon Dominated Region (PDR) Models” (Leiden, the Netherlands; 5–8 April ’04): D. Poelman, M.C. Spaans (inv. contr.: “Photon processes in inhomogeneous PDR’s”). Workshop (Schloss Ringberg, Germany; 13–17 April ’04): X. Tielens (inv. contr.: “The physics of circumstellar disks”). Congresso della Società Astronomica Italiana “I colori dell’Universo” (Milan, Italy; 19–23 April ’04): N.R. Napolitano. Oort/Sunyaev Workshop (Leiden, the Netherlands; 26–28 April ’04): A.G. de Bruyn (“LOFAR and the EoR: strategies and observables”), K. Kovaç.

79

Astronomical Data Analysis III (San’Agata sui due Golfi, Italy; 21 April – 1 May ’04): R. van de Weijgaert (“Analysing the Cosmic Foam: the Delaunay Tessellation Field estimator”). Workshop “The Large Scale Structure of Gas and Mass” (Technion, Haifa, Israel; May ’04): S. Zaroubi (inv. contr.: “The thermal history of the IGM” and “Morphological reshifts for Sunyaev-Zeldovich clusters”). 15th International Symposium “Space Terahertz Technology” (Northhampton, USA; 26–30 April ’04): W. Jellema (“Herschel-Heterodyne Instument for the Far Infrared: overview, development status and test results”; poster: “Modal analysis and experimental study of high-order mode contribution to standing waves in quasi-optical systems” – W. Jellema, S. Withington, N. Trappe, J.A. Murphy and W. Wild). Astronomical Data Analysis III (Sant’ Agata, Sui due Golfi, Italy; 28 April – 1 May ‘04): R. van de Weijgaert (“Analyzing the Cosmic Foam: the Delaunay tessellation field estimation”). Workshop on Secular Evolution of Galaxies (Ringberg, Germany; 17–21 May ’04): R.F. Peletier (inv. contr.: “Secular Evolution from Galaxy Colours”). ESO Workshop “Planetary Nebulae along the Milky Way” (Garching, Germany; 19–21 May ’04): N.G. Douglas (“Galaxy dynamics and the PNe population”), N.R. Napolitano (short comm.: ”Planetary nebulae as dynamical tracers: dark-to-luminous properties of early-type galaxies” – N.R. Napolitano, A.J. Romanowsky, N.G. Douglas, M. Capaccioli, M. Arnaboldi, K. Kuiken, M.R. Merrifield, K.C. Freeman, O. Gerhard). Workshop “The Nature and Composition of Active Galactic Nuclei” (Florence, Italy; 24 May – 3 June ’04): N. Nagar (inv. contr.: “The [FeII]/[PII] ratio as a tracer of shocks in AGN”). 59th Nederlandse Astronomen Conferentie “Spring in the Universe: the Birth of the Stars”, including a special program in honour of the 90th birthday of Prof. A. Blaauw (Vlieland; 26–28 May ’04): A. Blaauw, R. Boomsma (“High velocity HI in nearby spiral galaxies”), B. Emonts (poster: “Outflow of netural and ionized gas from Radio Galaxy 3C 293” – B.H.C. Emonts, R. Morganti, T.A. Oosterloo, J. Holt, C.N. Tadhunter and J.M. van der Hulst ), K. Fathi (“Non-circular gas in early-type spirals” – K. Fathi and SAURON Team), W. Frieswijk (poster: “Infrared dark clouds in a galactic context: the first IRDC candidate in the outer galaxy”),

80

Th. de Graauw (poster.: “The heterodyne instrument for the far-infrared” – M.W.M. de Graauw, F.P. Helmich and N. Whyborn), F.P. Helmich (posters: “Star formation studies” and “Exploratory Submm sPace Radio Interferometric Telescope (ESPRIT)”), K. Kovaç (“A search for the lowest mass galaxies: first results” – K. Kovaç, T.A. Oosterloo and J.M. van der Hulst), M. Obri� (poster: “Impact of stellar populations on the Fundamental Plane tilt in multiple bands” – M. Obri� and S.C. Trager), C.W. Ormel (poster: “Exposing the infrared dark clouds” – R.F. Shipman, C.W. Ormel, W. Frieswijk et al.), R.F. Peletier (poster: “First results of VISIR” – J.W. Pel, R.F. Peletier, T. Schoenmaker, P.-O. Lagage, E. Pantin, A. Claret, U. Käufl, R. Siebenmorgen), M. Spaans (inv. contr.: “Early Star Formation: the Equation of State”), S.C. Trager (SOC, LOC), R. van de Weijgaert (SOC, LOC), H. van Woerden (invited talk: "A profile of Adriaan Blaauw"). 204th Meeting of the American Astronomical Society (Denver, USA; 30 May – 3 June ’04): M. de Graauw (“Heterodyne Instrument for the Far Infrared (HIFI) for the Herschel Space Obsrvatory”), B.W. Holwerda (“Arm and inter-arm opacities from counts of background galaxies” – R.J. Allen, B.W. Holwerda, R.A. Gonzalez and P.C. van der Kruit; “Radial extinction in spiral disk from the numbers of background galaxies” – B.W. Holwerda, R.A. Gonzalez, R.J. Allen and P.C. van der Kruit). Conference on “Extra-planar Gas” (Dwingeloo; the Netherlands; 7–11 June ’04): R. Boomsma (“High velocity HI in NGC 6946 and extra-planar gas in NGC 253” – R. Boomsma, F. Fraternali, T. Oosterloo, et al.), B. Emonts (“Fast outflow of neutral and ionized gas from the Radio Galaxy 3C 293” – Emonts, B.H.C., Morganti, R, Van der Hulst, J.M. et al.), J.M. van der Hulst (“Evidence for gas eccretion in galactic disks” – J.M. van der Hulst and R. Sancisi), P. Kamphuis, N. Kanekar, R.F. Peletier, R. Sancisi (inv. contr.: “The extraplanar neutral gas in the edge-on spiral galaxy NGC 253” – F. Fraternali, T. Oosterloo, R. Sancisi and R. Waters; “Stationary fluid models for the extraplanar gas in spiral galaxies” – M. Barnabè, L. Ciotti, F. Fraternali and R. Sancisi), E. Tolstoy, M. Verheijen, H. van Woerden. Conference “Penetrating Bars through Masks of Cosmic Dust: the Hubble tuning fork strikes a new note” (Pilansberg National Park, South Africa; 7–12 June ’04): I. Peréz Martin (poster: “Truncation of stellar disks at high redshift”).

81

SAURON Workshop (Aussois, France; 13–19 June ’04): K. Fathi, K. Ganda, N. Nagar ( “SAURON observations of a Seyfert+Control sample”), R.F. Peletier (“Gas in ellipticals and spirals”). Workshop “Adaptive Mesh Refinements Simulations in Cosmology” (Durham, U.K.; 14–18 June ’04): P.A. Araya Melo (“The Delaunay Tessellation Field estimator”). VESUVIO Meeting (Naples, Italy; 21–22 June ’04): P. Heraudeau, E.A. Valentijn (”Observing superclusters”), R. van de Weijgaert. SRON Science Days (Dalfsen, the Netherlands; 14–15 June ’04): W. Frieswijk, C.W. Ormel (“Cores in infrared dark clouds”), M. Spaans (inv. contr.: “Cooling of the neutral ISM”), W. Wild (Inv. contr.: “ALMA – the Atacama Large Millimter Array – Science and Technology”). DART Modeling Workshop (Oxford, U.K.; 23–25 June ’04): G. Battaglia, E. Ripamonte (talk: “Numerical simulations of local dwarf and comparison to DART observations”), E. Tolstoy. “50 Jaar LKBF” (Leiden, the Netherlands; 2 July ’04): A. Blaauw (inv. contr.: “Over het ontstaan van de Stichting LKBF”). Workshop “Magnetic Fields in Galaxies” (Leiden, the Netherlands; 5–8 July ’04): M.A. Brentjens (inv. contr.: “Application of RM-synthesis to the Perseus Cluster” – M.A. Brentjens and A.G. de Bruyn; “RM–synthesis: background” – M.A. Brentjens and A.G. de Bruyn), A.G. de Bruyn (“LOFAR and the magnetic Universe”). Conference “The Quest for a Concordance Cosmology and Beyond” (Oxford, U.K.; 5–9 July ’04): L.V.E. Koopmans (talk: “Dark-matter halos and evolution of early-type galaxies to z=1”). MIT-EoR Workshop “Epoch of Reionization” (Cambridge, USA; 12–13 July ’04): A.G. de Bruyn (“EoR analysis and foreground removal”), S. Zaroubi (inv. contr.: “Data analysis issues with LOFAR”).

82

Conference “Cores, Disks, Jets and Outflows inLlow and High Mass Star Forming Environments: observations, theory and simulations” (Banff, Canada; 12–16 July ’04): D. Poelman (poster: “Excitation mechanisms of H2O in molecular clouds”), R.F. Shipman (poster: “The nature of an infrared dark cloud complex”). SKA 2004 Conference (Penicton, Canada; 18–24 July ’04): J.M. van der Hulst. IAU Symposium 225: “Impact of Gravitational Lensing on Cosmology” (Lausanne, Switzerland; 19–23 July ’04): F. Christen, L.V.E. Koopmans (talk: “Dark-matter halos and evolution of early-type galaxies to z=1”). Lorentz Center Workshop “The Nuclei of Galaxies” (Leiden; 26–30 July ’04): K. Fathi, K. Ganda, R.F. Peletier. Conference “The Environments of Galaxies: from Kiloparsecs to Mega-parsecs” (Chania, Crete; 9–13 August ’04): R. Boomsma (poster: “High velocity HI in NGC 6946 and NGC 253” – R. Boomsma, T. Oosterloo, F. Fraternali et al.), J.T.A. de Jong (poster: “Probing MACHO’s in M31” – J.T.A. de Jong, K.H. Kuijken, A.P.S. Crotts et al.), K. Kovaç (poster: “A search for the lowest mass galaxies: first results” – K. Kovaç, T.A. Oosterloo and J.M. van der Hulst), R. Sancisi. YERAC Conference (Cork, Eire; 28 August – 2 Sept. ’04): B. Emonts (“Origin and evolution of radio galaxies investigated with HI observations” – B.H.C. Emonts, R. Morganti, J.M. van der Hulst, et al.), K. Kovaç (talk: “A search for the lowest mass galaxies: the HI view” – K. Kovaç, T.A. Oosterloo and J.M. van der Hulst). Summer School “Data Analysis in Cosmology” (Valencia, Spain; 6–10 Sept. ’04): E. Platen, S.R. Schneider, R. van de Weijgaert (“Stochastic geometry and voids in LSS”). Conference “Identification of Dark-Matter” (Edinburgh, U.K.; 6–9 Sept. ’04): A. Helmi (short comm.:”The prolate shape of the galactic dark matter halo”). ASTRO-F Mission Planning Meeting #5 (Nagoya, Japan; 9–16 Sept. ’04): P.D. Barthel (“AGN Far-IR spectral energy distributions”).

83

Conference “Voronoi Diagrams in Science and Engineering” (Tokio, Japan: 13–15 Sept. ’04): R. van de Weijgaert (inv. contr: “Voronoi tessellations and the cosmic foam: spatial patterns and clustering across the Universe”). Conference “Chemical Abundances and Mixing in Stars in the Milky Way and its Satellites” (Castiglione della Pescaia, Italy; 13–17 Sept. ’04): G. Battaglia (poster: Kinematics and metallicity relations for dwarf spheroidals in the Local Group” – G. Battaglia, E. Tolstoy, M. Irwin, A. Helmi and DART team), B. Letarte (poster: “High resolution spectroscopy in a hundred RGB stars in Fornax”), E. Tolstoy (inv. contr.: “Abundances as tracers of the formation and evolution of galaxies”). COSMO-04 International Conference on Particle Physics and Cosmology (Toronto, Canada; 17–21 Sept. ’04): R. van de Weijgaert (“Much Ado about Nothing: a hierarchy of voids”). Vesuvio and SISCO Meetings (Groningen; 21–24 Sept. ’04): P. Heraudeau, R.F. Peletier, S.R. Schneider (“Getting on the outskirts of Hercules”), S.C. Trager, E.A. Valentijn (Chair), M.A.W. Verheijen. European IGM-Net Meeting (Leiden, the Netherlands; Sept. ’04): S. Zaroubi (inv. contr.: “Small Scale Matter power spectrum from the Lyman-alpha forest). Conference “The Spectral Energy Distribution of Gas-rich Galaxies: confronting Models with Data” (Heidelberg, Germany; 4–8 Oct. ’04): A. Villalobos (“Constraining age and metallicity of bulges embedded in low sur-face brightness galaxies” – G. Galaz, L. Infante, A. Villalobos and J. Dalcanton). Conference “Baryons in Dark Matter Halos” (Novigrad, Croatia; 5–9 Oct. ’04): G. Battaglia (“Kinematics and metallicity relations for dwarf spheroidals in the Local Group” – G. Battaglia, E. Tolstoy, M. Irwin, A. Helmi and DART team), J.T.A. de Jong (“Probing MACHO’s in M31” – J.T.A. de Jong, K.H. Kuijken, A.P.S. Crotts et al.), L.V.E. Koopmans (“Massive dark matter halos around early-type galaxies at z~1”) N.R. Napolitano (talk: “Galaxy dynamics with the PN.s”), E. Noordermeer (talk: “Rotation curves and dark matter in early-type disk galaxies” – E. Noordermeer, J.M. van der Hulst, R. Sancisi, and R. Swaters.), R.F. Peletier (“The formation of galactic bulges” – R.F. Peletier, M. Balcells, J. Falcon-Barroso and A. Graham),

84

I. Perez Martin (“Gas flow and dark matter in the inner parts of barred galaxies”), E. Ripamonte, M.A.W. Verheijen (“The disk mass project” – M. Verheijen, M. Bershady, D.R. Andersen R.A. Swaters, K. Westfall, A. Kelz, M.M. Roth, E. Popow). Symposium “The Three Dimensional Universe with GAIA” (Paris, France; 4–7 Oct. ’04): A. Blaauw. NOVA Fall School (Dwingeloo, 4–8 Oct. ’04): P.D. Barthel, W. Frieswijk, P. Kamphuis, B. Letarte, M. Obric, C. Ormel, S.R. Schneider, P. Serra, S.C. Trager. ELT Meeting (Florence, Italy; 7–10 Oct. ’04): E. Tolstoy (inv. contr.: “Resolved stellar populations”) 15th Annual October Astrophysics Conference (College Park, USA; 11–13 Oct. ’04): A.A. Cole (“Star formation histories from resolved stellar populations”). 7th EVN Symposium on new developments in VLBI Science and Techno-logy (Toledo, Spain; 12–15 Oct. ’04): N. Nagar. Conference “The Dusty and Molecular Universe: a prelude to HERSCHEL and ALMA” (Paris, France; 27–-29 Oct. ’04): P.D. Barthel (inv. contr.: “Herschel and galaxies/AGN”). Workshop on Chondrites and the Protoplanetary disk (Kauai, Hawaii, USA; 8–11 Nov. ’04): A.G.G.M. Tielens (inv. contr.: “The origin and evolution of interstellar dust”). MGA Workshop IV “Multiscale Geometric Methods in Astronomical Data Analysis” (Los Angeles, USA; 8–12 Nov. ’04): R. van de Weijgaert (inv. contr.: “DTFE: analysis of geometric and structured patterns”). Conference “The Spitzer Space Telescope: New views of the Cosmos” (Pasadena, USA; 9–12 Nov. ’04): F.P. Helmich on behalf of the ESPRIT consortium (poster: “Exposing the Infrared dark clouds”).

85

KIPAC Strong Lensing Workshop (Stanford, USA; 15–16 Nov. ’04): L.V.E. Koopmans (inv. contr.: “The Sloan Lens ACS Survey”). Workshop “Structure and Evolution of the Milky Way and its surroundings” (Schloss Ringberg, Germany; 5–9 Dec. ’04): G. Battaglia (poster: “Radial velocity dispersion of the Milky Way halo” – G. Battaglia, A. Helmi and SPAGHETTI team), A.A. Cole (inv. contr.: “Age-metallicity relation of the Large Magellanic Cloud”), A. Helmi (inv. contr.: “The shape of the galactic dark halo”), M.C. Smith, A. Villalobos (poster: “Formation of thick disks” – A. Villalobos and A. Helmi). 2nd Advanced Chilean School “First Large Scale Structures in the Universe and their Evolution” (Santiago, Chile; 6–10 Dec. ’04): P. Araya Melo (“The Delaunay Tessellation field estimator”), M.A. Brentjens (“Mpc scale polarized radio emission in the Perseus cluster”). ANGLES School (Santander, Spain; 10–14 Dec. ’04): L.V.E. Koopmans (“Hubble’s Constant from everything but lensing” ; “Optical constraints in gravitational lensing”). Conference “25 years after the discovery: some current topics on Lensed QSOs” (Santander, Spain; 15–17 Dec. ’04): L.V.E. Koopmans (“Non-intrinsic variability and chromaticity of lensed radio sources”). KIDS and AstroWISE Workshop “Preparing for Running Surveys” (Groningen; 29 Nov. – 2 Dec. ’04): K. Begeman (“Distributed processing”), D. Boxhoorn (“Astro-wise Context – Concepts”), E. Helmich, Ph. Héraudeau (“Quality control”), M.J. Tempelaar, R. Vermeij, W.-J. Vriend, E.A. Valentijn (Chair). BlueGene/LOFAR Workshop (Groningen; 7–8 Dec. ’04): L.V.E. Koopmans, E. Ripamonte.

87

APPENDIX III : Visits to institutes abroad

III.1 Work visits

M.A. Aragón Calvo Space Telescope Science Telescope Inst. (Baltimore, USA); 17 June – 9 July P. Araya Melo Pontificia Universidad Catolica (Santiago, Chile); 13–24 Dec. P.D. Barthel Space Telescope Science Telescope Inst. (Baltimore, USA); 22–24 Jan. CalTech/IPAC/JPL (Pasaden, USA); 25–31 Jan. Imperial College (London, UK); 17–18 Feb. G. Battaglia Observatoire de Paris (France); 30 Jan. – 4 Feb. K. Fathi CRAL (Obs. De Lyon, France); June Uppsala Astronomical Obs. (Sweden); August ASIAA (Taipei, Taiwan); Oct. Rochester Inst. Of Technology (Rochester, USA); Nov. W. Frieswijk Astronomy Department (Boston, USA); 2–6 Dec. K. Ganda IAC (La Laguna, Spain); 26–31 Jan. ETH (Zürich, Switzerland); 16–20 March A. Helmi Institute of Astronomy (Cambridge, UK); 28–29 July P. Heraudeau MPI für Astronomie (Heidelberg, Germany); 7–10 March, 26–30 April B.W. Holwerda Space Telescope Science Inst. (Baltimore, USA); Jan, March, June, Sept. J.M. van der Hulst Istituto di Astronomia (Bologna, Italy); 1–7 May European Southern Observatory (Garching, Germany); 22–23 Sept.

88

J.T.A. de Jong Columbia University (New York, USA); 27 June – 4 July P. Kamphuis Mt. Stromlo and Siding Springs Obs. (Australia); 6 June – 17 Sept. Anglo Australian Obs. (Sydney, Australia); 21 Sept. N. Kanekar Mt. Stromlo and Siding Springs Obs. (Australia); 19–20 Feb. ATNF (Sydney, Narrabri, Australia); 1 Feb. – 1 March L.V.E. Koopmans IAEF (Bonn, Germany); 8–18 April, 1–5 Nov. KIPAC (Stanford, USA); 6 Nov. – 4 Dec. K. Kovaç Space Telescope Science Inst. (Baltimore, USA); 5 July – 5 Aug. P.C. van der Kruit ESO Council, Garching (Germany); 8–9 Feb., 6–8 June, 27–28 Sept., 18–20 Oct., 6–8 Dec. ALMA team meeting, Tokyo (Japan); 23–27 Feb. Space Telescope Science Telescope Inst. Baltimore, VLA, Socorro (USA); 20 March – 9 April ESO, München (Germany); 21–23 June Madrid (Spain); 15–16 July Rome (Italy); 29 Sept. – 4 Oct. ESO-VLT (Paranal, Chile); 31 Oct. – 6 Nov. A. Labiano Ortega Space Telescope Science Inst. (Baltimore, USA); Jan. – Sept. B. Letarte Observatoire de Paris-Meudon (France); 23 Jan. – 4 Feb., 16–23 July, 12 Oct. – 15 Dec. Institute of Astronomy (Cambridge, UK); 28–30 July N.M. Nagar IAC, La Palma (Spain); 27 March – 3 April E. Noordermeer University of Sheffield (UK); Feb.–April J.W. Pel Service d’Astrophysique (Saclay, France); 13–16 Jan., 9–10 March, 12–13 July, Royal Observatory (Edinburgh, UK); 18–20 Feb. ESO-VLT (Paranal, Chile); 16 April–13 May, 25 June–10 July, 27 Aug.–7 Sept. Zeiss (Oberkochen, Germany); 30 Nov.–1 Dec.

89

MIRI consortium meeting (Dublin, Ireland); 6–9 Dec. R.F. Peletier Service d’Astrophysique (Saclay, France); 13–15 Jan. IAC (Tenerife, Spain); 17–19 Jan. University of Nottingham (UK); several visits ETH (Zürich, Switzerland); 16–20 March ESO (Garching, Germany); 21–27 Nov. Sternwarte (Munich, Germany); 7–11 Dec. I. Pérez Martín Universidad Complutense (Madrid, Spain); 29 March – 4 April IAA (Granada, Spain); 3–6 Aug. E. Ripamonte Pennsylvania State University (USA); 17 April – 4 June M.C. Smith Institute of Astronomy (Cambridge, UK); 12–17 Dec. M. Spaans Osservatorio di Firenze (Italy); 4–8 Oct. A.G.G.M. Tielens Observatoire de Grenoble (Saint-Martin d’Hères, France); 15 March – 11 June, 1 Oct. – 12 Dec. Cornell University (New York) and NASA Ames (USA); 27 June – 1 Sept. Toulouse and Bordeaux (France); 19–23 Sept. E. Tolstoy Observatoire de Paris (Meudon, France); 1–4 Feb. Institute of Astronomy (Cambridge, UK); March Dept. of Astronomy (Oxford, UK); 1–31 July, 15 Nov. – 15 Dec. S.C. Trager Observatory Capodimonte (Naples, Italy); 22–23 Jan. Carnegie Observatories (Pasadena, USA); 2–13 Aug. Washington State University (Pullman, USA); 16–20 Aug. Univ. of Washington (Seattle, USA); 23 Aug. MPI für Astronomie (Heidelberg, Germany); 27–29 Oct. E.A. Valentijn Observatory Capodimonte (Naples, Italy); 14–16 Jan., 13–18 June ESO (Munich, Germany); 2–3 April, Strasbourg (France); 10–11 June, Sternwärte (Bonn, Germany); 10 Nov. IAP, Paris (France); 5–7 Dec. M.A.W. Verheijen Centro Astronomico Hispano Aleman (Calar Alto, Spain); 20–27 Oct.

90

M.A.M. van de Weijgaert Astronomisches Institut (Basel, Switzerland); 26–28 Jan. CITA (Toronto, Canada); 22–25 Sept. University of Pennsylvania (Philadelphia, USA); 3–8 Nov. S. Zaroubi Technion (Haifa, Israel); May III.2 Observing trips

M.A. Aragón Calvo Isaac Newton Telescope (La Palma, Spain); 6–20 April, 6–12 Nov. G. Battaglia Anglo-Australian Telescope; 7–12 April A.A. Cole William Herschel 4.2 mtr. Telescope (La Palma, Spain); 27–28 June N.G. Douglas NTT, ESO (Chile); 8–12 April PN Spectrograph (La Palma, Spain); 12–14 April B. Emonts William Herschel Telescope (La Palma, Spain); 12–13 Jan. W. Frieswijk JCMT (Hawaii, USA); 9–21 Feb., 8–28 Sept. K. Ganda William Herschel Telescope (La Palma, Spain); 19–26 Jan. A. Helmi Isaac Newton Telescope (La Palma, Spain); 1–9 Feb., 4–14 Sept. J.M. van der Hulst ATCA (Narrabri, Australia); 1–17 March N. Kanekar ATCA (Narrabri, Australia); 3–14 Feb. Green Bank Telescope (West Virginia, USA); 15–21 April. F. Lugt William Herschel Telescope (La Palma, Spain); 30 Jan. – 11 Feb.

91

N.M. Nagar William Herschel Telescope (La Palma, Spain); 20 March – 26 April 1–16 Dec. R.F. Peletier William Herschel Telescope (La Palma, Spain); Jan. VLT (Paranal, Chile); April, June, Sept. S.R. Schneider MDM 2.4 mtr. Hiltner Telescope (Kitt Peak, USA); 6–13 May P. Serra ATCA (Narrabri, Australia); March NTT, La Silla Observatory (Chile); July William Herschel Telescope (La Palma, Spain); Sept. G. Sikkema MPG/ESO (La Silla, Chile); 1–14 Oct. E. Tolstoy Subaru Telescope (Hawaii, USA); Feb. S.C. Trager NTT (La Silla, Chile); 11–14 July William Herschel Telescope (La Palma, Spain); 18–21 Sept. M.A.W. Verheijen 3.5 mtr. Telescope (Calar Alto, Spain); 24–28 March, 7–22 Nov.

93

APPENDIX IV : Colloquia, popular lectures

IV.1 Colloquia given outside Groningen

P.D. Barthel – “To be or not to be active”: Space Telescope Science Institute, Baltimore, USA (23 Jan.), IPAC, Pasadena, USA (28 Jan.), Leiden Observatory, the Netherlands (1 April), University of Amsterdam, the Netherlands (7 May), ASTRON, Dwingeloo, the Netherlands (14 May). G. Battaglia – “Radial velocity dispersion of the Milky Way Halo”: Swinburne University, Australia (22 April). A.A. Cole – “Chemical evolution of the Large Magellanic Cloud” : ASTRON, Dwingeloo, the Netherlands (March), ESO, Garching, Germany (June). “Chemical evolution and kinematics of the LMC Bar”: Rutgers University, New Brunswick, USA (Sept.). N.G. Douglas – “Galaxy dynamics with the PN Spectrograph”: John Moore University, Liverpool, UK (27 Oct.). K. Fathi – “2D kinematics and dynamics in spirals”: Academia Sinica Inst. of Astronomy, Taipei, Taiwan (28 Oct.), National Tsing Hua University, Hsinchu, Taiwan (2 Nov.) “Exploring non-circular gaseous motions in early-type spirals”: Columbia University, New York, USA (10 Feb.), UC Berkeley, USA (14 Jan)., CalTech, Pasadena, USA (20 Jan.), University of Kentucky, Lexington, USA (21 Jan.), Space Telescope Science Institute, Baltimore,USA (27 Jan.), University of Maryland, USA (29 Jan.). A. Helmi – “Using streams to test hierarchical galaxy formation models for the Milky Way” : University of Nijmegen, the Netherlands (18 May). B.W. Holwerda – “Extinction in spiral disks”: UNAM, Morelia, Mexico (Jan.). P. Kamphuis – “The formation of population III stars in the presence of a radiation field” : Mt. Stromlo Observatory, Australia (17 Sept.). N. Kanekar – “Using OH lines to measure changes in fundamental constants” : ATNF, Epping, Australia (17 Feb.), University of New South Wales, Sydney, Australia (18 Feb.). “Do the fundamental constants change with time?” : ATNF, Epping, Australia (17 Feb.), ASTRON, Dwingeloo, the Netherlands (17 March)

94

L.V.E. Koopmans – “Massive halos and the evolution of E/SO galaxies to z=1”: STScI, Baltimore, USA (13 Jan.). “The Hubble Constant with the gravitational lens B1608+656”: IAEF, Bonn, Germany (13 April). “Dark Matter in the most massive galaxies in the Universe”: KIPAC/Stanford, USA (18 Nov.). E. Noordermeer – “Rotation curves and Dark Matter in early-type disk galaxies”: Sheffield University, UK (28 April), Nottingham University, UK (29 April). R.F. Peletier – Why are galaxies active?”: ETH Zürich, Switzerland (18 March). “Gas in elliptical galaxies and bulges”: ESA/ESTEC, Noordwijk, the Netherlands (2 April). “The formation of galactic bulges”: Leiden Observatory, the Netherlands (24 June), Sterrenkundig Instituut, Amsterdam, the Netherlands (25 June), Sternwarte, München, Germany (8 Dec.). I. Perez Martín – Gas flow and Dark Matter in the inner parts of barred galaxies”: Universidad Complutense, Madrid, Spain (April). E. Ripamonti – “Numerical modeling of primordial protostellar collapse”: ASTRON-JIVE, Dwingeloo, the Netherlands (10 Dec.). R. Sancisi – “Luminous and Dark Matter in spiral galaixes”: Osservatorio Astromomico di Arcetri, Italy (19 Feb.). “Extraplanar gas in spiral galaxies”: ESO-MPI Joint colloquium, Garching, Germany (4 Nov.). R.H. Sanders – “Modified Newtonian dynamics as an alternative to cosmic dark matter”: University of Vienna, Austria (3 May). “More on modified dynamics”: Laboratoire d”Astrophysique, Marseille, France (25 June). M.A.W. Verheijen – “Galaxy evolution in clusters: an HI perspective”: ASTRON, Dwingeloo, the Netherlands (24 Sept.). R. van de Weijgaert – “Analyzing the Cosmic Foam: the Delaunay Tessellation Field estimator” : University of Basel, Switzerland (27 Jan.), MPI für Radioastronomie, Bonn, Germany (4 June). S. Zaroubi – “Cosmology from the Lyman Forest”: ASTRON, Dwingeloo, the Netherlands (Dec.), University of Utrecht, the Netherlands (Nov.).

95

IV.2 Popular lectures

P.D. Barthel – “Herschel Science”: NVR, Utrecht (9 March), TV Noord “Adams-appel” (13 and 14 March) “Extragalactic Astronomy” HOVO Utrecht (15 and 22 March). “Tijd in het Heelal” GSP, Groningen (18 May). “Venus: schone verschijning of schone schijn” Groningen (8 June). “Het ongelofelijke Heelal” Inaugural lecture, Groningen (8 June). “Op reis door het Heelal” Kinderuniversiteit, Groningen (29 June), KRO radio show (5 July) “Radio astronomy” EAAE Summer School, Dwingeloo (24 July). “Het ongelofelijke Heelal” HOVO, Groningen (11 Oct.). “Iets boven Groningen” RuG (20 Dec.). K. Begeman – “Sterrenkunde”: Chr. Basisschool de Hoeksteen, Hoogezand (8 April). A. Blaauw – “Astronomical background of the LOFAR project” Probus Society, Haren (27 Oct.) R. Boomsma – “Extragalactische Sterrenkunde”: KNVWS Leeuwarden (27 Nov.) “Melkwegstelsels” : VWS Thales, Zwolle (12 Feb.), WS Noord-Drenthe, Assen (9 April). M.A. Brentjens – Dag van de Radio Amateur”: Aurora, Apeldoorn (9 Oct.). A.G. de Bruyn – “ASTRON, WSRT and LOFAR” : Visitors to ASTRON and Westerbork (several occasions) B.H.C. Emonts – “De hemel om ons heen” College Caroussel Rug (16 April) “Exoplaneten” Open Dag, Kapteyn Institute (24 Oct.) “Zoektocht naar exoplaneten” en “Wat is sterrenkunde?”: Raayland College, Venray (23 Nov.). J.T.A. de Jong – “Gravitatielenzen en hun belang voor de sterrenkunde”: KNVWS Triangulum, Eefde (18 March), Artis Planetarium, Amsterdam (3 Aug.), KNVWS Thales, Zwolle (30 Sept.). E. Noordermeer – “Eilanden in het heelal: Sterrenstelsels gezien vanaf La Palma” : KNVWS Zuid Drenthe, Hoogeveen (26 Nov.). C.W. Ormel – “Stervorming” : KNVWS, Noord Drenthe, Assen . G. Sikkema – “Bolhopen” : KNVWS, Groningen (23 Sept.) “Gallileo”, “AGNs” : KNVWS, Heerlen (30 Oct.)

96

M.C. Spaans – “Een week uit het leven van een astronoom” : OSG Piter Jelles, Leeuwarden (28 Oct.). R. van de Weijgaert – “Van primordiale ruis tot kosmisch schuim: structuur-vorming in het Heelal” : Koninklijk Natuurkundig Genootschap, Groningen (17 Feb.). P.R. Wesselius – “Exoplanets” : KNVWS, Zaandam (26 Feb.). H. van Woerden – "Eet de Melkweg? Of ademt hij?": KNVWS-Symposium, Leiden (25 Sept.) "De Levensloop van Sterren": Senioren Academie RU Groningen (11 Oct.). S. Zaroubi – “The evolution of the Universe” : The Intellectual Club, Nazareth, Israel (Dec.).

97

APPENDIX V : Colloquia in Groningen

January 19 Neil Nagar (Kapteyn Institute, Groningen): The Not-So-Silent Majority: Accretion in Nearby 'Normal' Galaxies January 26 Ole Möller (Kapteyn Institute, Groningen): Not all that glitters is gold:the search for the "Golden Lens" and why it failed February 2 Magda Arnaboldi (INAF, Osservatorio Astronomio, Torino, Italia): The Polar Ring February 9 (NOVA Colloquium) Sandra Faber (University of California, Santa Cruz, USA): Recent Results from the DEEP February 12 (RUG Physics Seminar) John Heise (SRON, Utrecht): Ashes to ashes: a new type of nuclear explosions on neutron stars February 16 George Hau (ESO, Garching, Germany): The kinematics and stellar populations of the giant haloes of brightest cluster galaxies February 23 (NOVA colloquium) Alex Szalay (Dept. Physics, Johns Hopkins Univ., Baltimore, USA): The Sloan Digital Sky Survey: Mapping the Cosmic Large Scale Galaxy Distribution March 1 Hans-Rainer Klöckner (Kapteyn Institute, Groningen): Extragalactic Hydroxyl March 8 Melanie Johnston-Hollitt (Sterrewacht Leiden): Properties of Mpc-Scale Diffuse Radio Emission and the Galaxy Clusters that Harbour it March 15 (NOVA colloquium) Zoltan Haiman (Dept. Astronomy, Columbia University, New York, USA): Reionization History of the Universe March 22 (NOVA colloquium) Paul Schechter (MIT, Cambridge, Massachusetts, USA): Flux ratio anomalies in lensed quasars: micro-lensing or milli-?

98

March 25 Sukyoung Yi (Dept. Astronomy, Univ. Oxford, UK): On the star formation history of early-type galaxies derived from GALEX observations March 29 Peter Barthel (Kapteyn Institute, Groningen): To be or not to be active April 6 Jacco Vink (SRON, Utrecht): X-ray studies of Cassiopeia A: Exposing Core Collapse to the Core April 15 Marijn Franx (Sterrewacht Leiden, the Netherlands): Evolved Galaxies at High Redshift April 19 Harm Habing (Sterrewacht Leiden, the Netherlands): Maser stars and the inner Milky Way Galaxy (MWG) April 21 Montse Villar-Martin (Instituto de Astrofica de Andalucia, Granada, Espana): Giant Nebulae around Distant Radio Galaxies April 27 (Kapteyn Seminar Special) Wolfhard Schlosser (Astronomisches Institut, Ruhr-Universität Bochum, Germany): The Sky Disc of Nebra April 28 Art Wolfe (Center Astrophys. Space Sciences, Univ. California, San Diego, USA): CII* Absorption in Damped Lyman Alpha Systems: A new Window on the Star Formation History of the Universe May 10 Peter Hoyng (SRON Utrecht, the Netherlands): The magnetic field of the Earth, Sun and planets May 17 Ana Achucarro (Lorentz Institute, Leiden): The virtues of defects May 24 Siebren van der Werf (KVI, University of Groningen, the Netherlands): The Novaya Zemlya effect May 25 Charles Lada (Center for Astrophysics, Harvard, Cambridge, USA): A History of Star Formation Research: From Aristotle to Ambartsumian June 1 (NOVA colloquium) Donald Goldsmith (Berkeley, California, USA): Popularization of Astronomy in the US

99

June 7 Hayley Bignall (JIVE, Dwingeloo): Interstellar Telescope: a probe of microarcsecond-scale structure in quasars June 15 (NOVA colloquium) Norm Murray (CITA, Toronto, Canada): Extrasolar Planets June 21 Joeri van Leeuwen (Astronomical Institute, Utrecht, the Netherlands): Drifting subpulses and why pulsars shine June 28 (NOVA colloquium) Jim Houck (Dept. Astronomy, Cornell Univ., Ithaca, USA): ) Star Formation at Low Metallicity a window on the early Universe ? July 5 Matt Fleenor (Dept. of Physics & Astronomy, Univ. North Carolina, Chapel Hill, USA): The Horologium-Reticulum Supercluster: Large-Scale Structure and Dynamics July 26 Martin Smith (Jodrell Bank Observatory, Univ. Manchester, UK): Gravitational microlensing within the local group August 30 Russ Shipman (SRON, Groningen): The Rosette Nebula: Those Dirty Details September 6 Clovis Hopman (Fac. Physics, Weizman Institute of Science, Rehovot, Israel): The Swansong of Stars orbiting Massive Black Holes September 7 Igor Karachentsev (Special Astroph. Observatory, Karachaevo-Cherkesia, Russia): The Local Universe: population, structure, velocity field September 9 Antonella Maselli (Osservatorio Astrofisico di Arcetri, Firenze, Italia): Proximity Effect Around High-redshift Galaxies September 13 Ad van den Berg (KVI, University of Groningen, the Netherlands): From Nuclear to Particle Astrophysics September 21 Arlette de Waard (Leiden Institute of Physics, Leiden): miniGRAIL, the first spherical gravitational wave detector

100

September 27 Helen Fraser (Sterrewacht Leiden) CO'ded' messages ? What can we learn about Star Forming Regions from Surface Chemistry September 28 (Oort Professor Colloquium) Rashid Sunyaev (Max Planck Institut für Astrophysik, Garching, Germany/ Space Research Institute, Russian Academy of Sciences, Moscow, Russia): Cosmic Microwave Background: Clusters of Galaxies and Cosmology September 29 Emilio Romano-Diaz (Kapteyn Institute, Groningen, the Netherlands): Probing cosmic velocity flows in the Local Universe October 4 (NOVA colloquium) Eva Grebel (Astron. Institut, Univ. Basel, Switzerland): The Violent Local Group: A History of Accretion and Survival October 5 Victor Flambaum (Dept. Theor. Physics, Univ. New South Wales, Sydney, Australia): Effects of variation of fundamental constants from Big Bang to atomic clocks October 11 Peter Woitke (Sterrewacht Leiden, the Netherlands): Multi-dimensional models for dust-driven AGB star winds October 12 (NOVA colloquium) Luis Ho (Carnegie Observatories, Pasadena, USA): Nuclear Activity in the Local Universe October 18 (NOVA colloquium) Massimo Stiavelli (STScI, Baltimore, USA): The Hubble Ultra Deep Field October 25 (Blaauw Professor Colloquium) Ken Freeman (Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, Australia): Galactic Disks November 1 (Blaauw Professor Colloquium) Joe Silk (Dept. Astron., Univ. Oxford, UK): Some Current Issues in Star and Galaxy Formation Theory November 4 Julio Navarro (Dept. Physics & Astron., Univ. Victoria, British Columbia, Canada/Max-Planck Institut für Astrophysik, Garching): Cold Dark Matter, Galaxy formation and the Formation of the Galaxy November 8 David Teyssier (ESA/SRON Groningen, the Netherlands): Carbon chemistry in Photo-Dominated regions

101

November 12 Joe Silk (Dept. Astron., Univ. Oxford, UK): Blackboard Colloquium: The First Stars November 15 Bram Achterberg (Sterrenkundig Inst., Univ. Utrecht, the Netherlands): Origin of Highest Energy Astroparticles November 22 (Kapteyn Seminar Special) Freek Beekman (University Medical Center, Utrecht): Single Photon Emission Tomography in Men and Mice November 29 Vincent Icke (Sterrewacht, Leiden, the Netherlands): Oscillating Giant Stars December 7 Huib Henrichs (Sterrenkundig Instituut, UvA/VU, Amsterdam): Magnetic fields in Massive Stars December 9 Floris van der Tak (Max Planck Institut für Radioastronomie, Bonn, Germany): The earliest stages of High-mass Star Formation December 13 Bernhard Brandl (Sterrewacht, Leiden, the Netherlands): Starburst Studies with the Spitzer Space Telescope December 15 Kambiz Fathi (Rochester Institute of Technology, Rochester, NY, USA): Morphology and Dynamics in the Inner Regions of Spiral Galaxies December 16 Johan Knapen (Astronomy Research Group, Univ. Hertfordshire, UK): Fuelling starbursts and AGN

103

APPENDIX VI : Visiting scientists in Groningen

E. Allard University of Hertfordshire, UK M. Arnaboldi INAF, Turin, Italy A. Berciano Alba Instituto de Astrofísica de Canarias, Spain E. Branchini Degli Studi di Roma Tre, Rome, Italy C. del Burgo European Space Agency, Noordwijk M. Cappaccioli Osservatorio Astronomico Capodimonti, Italy N. Cardiel Calar Alto Observatory, Almeria, Spain A. Chung Columbia University, New York, USA O.-M. Cordes Universität Bonn, Germany M. Dijkstra Columbia University, New York, USA S.M. Faber UCO/Lick Observatory, Santa Cruz, USA J. Falcón-Barroso Leiden Observatory I. Ferreras Imperial College, London, UK I. Fejes, U of Budapest/Satellite Geodetical Obs., Penc, Hungary V. Flambeau University of New South Wales, Sydney, Australia M. Fleenor University of North Carolina, USA K. Freeman Australian National University O. Gerhard University of Basel, Switzerland F. Getman Osservatorio Astronomico Capodimonti, Italy D. Goldsmith University of Berkeley, California, USA E.K. Grebel University of Basel, Switzerland Z. Haiman Columbia University, New York, USA G.K.T. Hau ESO, Garching, Germany L. Ho Carnegie Observatories, USA J. Holt University of Sheffield, UK J. Houck Cornell University, USA J. Chris Howk Univ. of California, San Diego, USA L. Hunt CAISMI-CNR, Firenze, Italy R. Jansen Arizona State University, USA V. Jelic University of Zagreb, Croatia R. Jesseit Universitäts-Sternwarte München, Germany R. de Jong Space Telescope Science Institute, Baltimore, USA E. van Kampen Institute for Astrophysics, Innsbrück, Austria E. Kutdemir University of Ankara, Turkey C. Lada Center for Astrophysics, Harvard, USA J. van Leeuwen University of British Columbia, Vancouver, Canada O. López Cruz INAOE, Tonantzintla, Mexico M. Mapelli SISSA, Trieste, Italy A. Maselli Arecetri Observatory, Firenze, Italy J. McCallum University of Tasmania Y. Mellier Institut d’Astrophysique, Paris, France

104

N. Murray Canadian Institute for Theoretical Astrophysics, Toronto J. Navarro University of Victoria, Canada M. Neeser Universitäts-Sternwarte München, Germany M. Plionis Observatory of Athens, Greece M. Pohlen Instituto de Astrofísica de Canarias, Spain M.-Y. Rhee Yonsei University Observatory, Korea E. Ripamonte Pennsylvania State University, USA A.J. Romanowsky University of Nottingham, UK R. Saglia Universitäts-Sternwarte München, Germany P. Sanchez Blasquez University Complutense, Madrid, Spain P. Schechter MIT, Cambridge, USA W. Schlösser Ruhr-University of Bochum, Germany N. Scoville Caltech, Pasadena, USA F. Shu National Tsing Hua University, Hsinchu, Taiwan J. Silk Oxford University, UK R. Silvotti Osservatorio Astronomico Capodimonti, Italy A. Smette ESO and University of Liège, Belgium M.C. Smith Jodrell Bank Observatory, UK J. Snigula Universitäts-Sternwarte München, Germany M. Stiavelli Space Telescope Science Institute, Baltimore, USA R. Sunyaev MPI for Astrophysics, Garching, Germany R.A. Swaters University of Maryland, College Park, USA A. Szalay Johns Hopkins University, Baltimore, USA F. van der Tak MPI für Radioastronomie, Bonn, Germany A. Villalobos Pontificia Universidad Catolica, Chile M.M. Villar Martin Inst. de Astrofísica de Andalucia, Granada, Spain J. Vink SRON Utrecht, the Netherlands A. Volpicelli Osservatorio Astronomico Capodimonti, Italy W.H. de Vries University of California, Davis & UNL, USA B. Warren Mt. Stromlo Observatory, Australia A.M. Weijmans Leiden Observatory, the Netherlands M. Williams ANU, Canberra, Australia A. Wolfe UC San Diego, USA S.K. Yi Oxford University, UK M.A. Zwaan European Southern Observatory, Garching, Germany

105

APPENDIX VII : Memberships, etc.

T.S. van Albada: Lid, Koninklijke Ned. Akademie van Wetenschappen Voorzitter, Kapteyn Fonds (until summer 2004) Voorzitter, Stichting Pastoor Schmeits voor

Sterrenkunde (until summer 2004) P.D. Barthel: Member, ESA FIRST/Herschel Science Team

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

Extragalactic Background) Chairman, National and NOVA Astronomy Education

Committee Chairman, NAC High School Astronomy Education

Working Group Chairman, Lorentz International Center Astronomy

Board (Leiden) Member, Minnaert Committee for Public Outreach in

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

Mission) Member LOFAR Survey Consortium Member Organizing Committee EAAE Teacher Astro-

summer school (July 2004) 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

106

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. (tot

Sept. 04) Ere-lid Koninklijke Nederlandse Vereniging voor

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

Techniques) Member, Scientific Organizing Committee ESO Work-

shop “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 A. Helmi Member, RAVE, Executive Working Group Member, Gaia, Radial Velocity Working Group Member, NWO, Beoordelingscomissie Astronomie

(BCA) Member, NWO, Veni comcittee F.P. Helmich: Member, ASTRON-PC Ph. Héraudeau: Member, Societé Francaise d’Astronomie et

d’Astrophysique J.M. van der Hulst: Member, IAU 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, Nederlands Platform voor de Natuurkunde Coordinator Network-1 of NOVA L.V.E. Koopmans Member, Astronomy Research Committee (ARC) of

LOFAR

107

Member, Steering committee of the EU-RTN Network "Astrophysics Network for Galaxy LEnsing Studies" (ANGLES)

P.C. van der Kruit: Voorzitter, Bestuur Nederlandse Onderzoekschool

voor Astronomie (NOVA) Voorzitter, Nederlands Comité Astronomie (NCA) Chairman of the Board, Atacama Large Millimeter

Array (ALMA) President of Council, European Southern

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 Member, Hubble Space Telescope Time Assigning

Committee for cycle 13 and chairman of the panel “Extragalactic II''

Chairman, ESO Negotiating Team for the accession of Spain

Chairman, ESO Contact Commissie (KNAW) Treasurer (until June 2004) and chairman of the

Board (from July 2004), Stichting Groninger Universiteits Fonds (GUF; Foundation Groningen University Fund)

Chairman, Koninklijk Natuurkundig Genootschap (Royal Physical Sciences Society), Groningen

Member and chairman (from November 2004), Board of Directors, Leids Sterrewacht Fonds

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

Bosscha Fonds Chairman, Jacobus C. Kapteyn Fund (from summer

2004) Chairman, Foundation Pastoor Schmeits Prijs (from

summer 2004) Member, IAU Commission 28 (Galaxies), 33

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

C. Ormel: Member, Faculty Council RUG (until August 2004) J.W. Pel: Principal Investigator “VISIR” spectrometer (Mid-IR

Imager/Spectrometer for ESO Very Large Tele-scope)

108

Lid ESO Contact Commissie Kon. Nederlandse Akademie van Wetenschappen

Member IAU Commission 25 (Stellar Photometry and Polarimetry)

R.F. Peletier: Member ESO OPC panel Member, NWO-VENI grant committee 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 A.G.G.M. Tielens: Project scientist, HIFI project E. Tolstoy: Member, ESO Telescope Time Allocation committee Member, NOVA Instrument Steering Committee Member, Directors Advisory Committee, Isaac

Newton Group Subaru Time Allocation Commitee Referee S.C. Trager Member, NFRA Program Committee Lecturer, NOVA Fall School 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 Member, Data Center Alliance Board (DCA) Co-PI, KIDS project (A 1700 Sq Deg OmegaCAM

Survey) Co-PI, Vesuvio project (OmegaCAM survey of nearby

superclusters) Co-Investigator, VST-16 project (photo-z with

OmegaCAM)

109

P.R. Wesselius: 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: Board member, 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 H. van Woerden: Ere-Voorzitter Koninklijke Nederlandse Vereniging

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

111

APPENDIX VIII : Personnel (Dec. 31, 2004)

(d) = personnel employed by a third party contract (n) = personnel employed by NWO (u) = personnel employed by University of Groningen Full Professors (Hoogleraren) P.D. Barthel (u) J.W. Pel (u) 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)(u) Adjunct Professors M.A.M. van de Weijgaert (u) Tenure Track A. Helmi (NOVA) E. Tolstoy (u) (KNAW) L.V.E. Koopmans (u) (from 02/04) S.C. Trager (u) R.F. Peletier (NOVA) M.A.W. Verheijen (u) (from 04/04) M.C. Spaans (u) S. Zaroubi (u) (from 02/04) Research Staff J. Adema (NOVA) R. Hesper (NOVA) A. Baryshev (NOVA) P. Mena Mena (NOVA) (from 07/04) K. Begeman (u) E.A. Valentijn (u) (NOVA) N.G. Douglas (u) Blaauw professor J. Silk 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.) Emeriti T.S. van Albada S.R. Pottasch A. Blaauw H. van Woerden

112

Research Associates (postdocs) A.A. Cole (u) N.M. Nagar (u) Ph. Heraudeau (u) N.R. Napolitano (d) N. Kanekar (u) (until 09/04) I. Pérez-Martín (u) J.-P. Macquart (u) (until 07/04) E. Ripamonti (u) (from 04/04) O. Möller (d) (until 08/04) M.C Smith (u) (from 11/04) Guest staff members R. Bottema P. Sanchez (until 7/04) G. Mellema W.E. Schaap M. Mendez A.A. Schoenmaker (until 06/04) R. Morganti M. Walker (from 12/04) T.A. Oosterloo Ph.D. students M. Angel Aragon Calvo (u) P. Kamphuis (u) (from 01/04) P. Araya Mayo (d) H.-R. Klöckner (d) (until 04/04) G. Battaglia (u) K. Kovacs (u) A. Berciano Alba (n) (from 11/04) A. Labiano-Ortega (u) R. Boomsma (u) B. Letarte (u) M. Brentjens (n) Y.S. Li (u) (from 11/04) S. Cazaux (u) (until 03/04) N. Mohammed (d) F. Christen (u) E. Noordermeer (u) B. Emonts (u) M. Obric (n) K. Fathi (u) (until 01/05) C. Ormel (u) (from 09/04) W Frieswijk (u) (from 01/04) E. Romano-Diaz (d) (until 11/04) K. Ganda (u) S.R. Schneider (NOVA) (from 04/04) J. Heiner (d) (from 07/04) P. Serra (u) (from 01/04) B.W. Holwerda (d) G. Sikkema (u) W. Jellema (u) (from 04/04) F. Simatupang (d) (until 09/04) J.T.A. de Jong (u) A. Villalobos (u) (from 05/04) General Co-ordinator G. de Vries (u) Computing staff E.M. Helmich (d) (ASTRO-Wise) R. Vermeij (d) (ASTRO-Wise) J.P. Terlouw (u) W.J. Vriend (d) (ASTRO-Wise) E. Tiesinga (u) M.G.R. Vogelaar (u) M. Tempelaar (d) W. Zwitser (u) Technical personnel Library J. Barkhof (u) (NOVA) G. Comello (u) (0.8) (until 10/04) D.R. Boxhoorn (u) (NOVA) H. Koster (u) (0.5) (from 10/04) G. Comello (u) (0.2) G.J. Gerlofsma (u) (NOVA) Secretariat M.G. Alberts (u) (0.7) H. Zondervan-Kimsma (u) (0.6) G. Comello (0.8) (from 10/04) J. Zwegers-Morris (u) (0.7)

113

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) R. Boomsma (until 12/04) E. Starkenburg (student) (from 03/04) W. Frieswijk (from 12/04) M.G.R. Vogelaar J.M. van der Hulst G. de Vries P.C. van der Kruit (chair) P.R. Wesselius (SRON) (until 06/04) F.F.H. Lugt (student) (until 03/04) W. Wild (SRON) (from 06/04) R.F. Peletier H. Zondervan-Kimsma R.H. Sanders Education Committee student members M.G. Alberts (secretary) J.S. van Bethlehem R. Boomsma (advisor) (until 11/04) T. P.R. van der Laan (until 11/04) W. Frieswijk (advisor) (from 11/04) W. Oosterheert (from 11/04) J.M. van der Hulst (advisor) S. P.C. Peters L.V.E. Koopmans (from 09/04) B. Scholten (from 03/04) M.C. Spaans E. Starkenburg (ASO) (from 03/04) R.H. Sanders (until 09/04) F.F.H. Lugt (ASO) (until 03/04) A.G.G.M. Tielens (chair ) E. Tolstoy (from 09/04) M.G.R. Vogelaar (advisor) G. de Vries (advisor) M.A.M. van de Weijgaert (until 09/04) Education Committee (Raad van Advies) M.G. Alberts (secretary) E. Starkenburg (student) (from 03/04) J.M. van der Hulst (chair) A.G.G.M. Tielens F. Lugt (student) (until 03/04) G. de Vries M.C. Spaans Groningen members of the National Astronomy Education Committee P.D. Barthel (chair) E. Starkenburg

114

Study advisor Study co-ordinator M.C. Spaans G. de Vries Library Committee W. Jellema H. Koster (from 10/04) P.D. Barthel J.W. Pel G. Comello (until 10/04) R. van de Weijgaert N.G. Douglas PhD-supervisor committee J.-W. Pel S.C. Trager 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 (until 08/04) C. Ormel (until 08/04) T.P.R. van der Laan (from 09/04) T.P.R. van der Laan (from 09/04) Library Committee Comittee Education and Research H. Koster T.P.R. van der Laan 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) M. Franx R.T.A. Witmer (financial control) J. Kuipers K. Groen (secretary) N. Langer K. Wakker (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)

115

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 4083 Aragon Calvo, Drs. M.A. M.A.Aragon 4060 Araya Melo, Drs. P. P.Araya 4064 Barthel, Prof. dr. P.D. P.D.Barthel 3476 Barmabe, M.Sc. M. M.Barnabe 4081 Battaglia, Mevr. Drs. G. G.Battaglia 4091 Bethlehem, J.S. van J.S.van.Bethlehem 2454 Begeman, Dr. K. K.Begeman 3505 Berciano Alba, Mevr. M.Sc A A.Berciano 4084 Blaauw, Prof. dr. A. A.Blaauw 4087 Boersma, Drs. C. C.Boersma 4081 Boomsma, R. Drs. R.Boomsma 4091 Bos, N. N.Bos 4087 Bottema, Dr. R. R.Bottema 2454 Boxhoorn, Drs. D.R. D.R.Boxhoorn 8326 Brentjens, Drs. M.A. M.A.Brentjens 4067 Brouw, Prof. dr. W.N. W.N. Brouw 4057 Bruyn, Prof. Dr. A.G. de A.G.de.Bruyn 8689 Buddelmeijer, H. H.Buddelmeijer 3505 Chi, M.Sc S. S.Chi 4098 Christen, Drs. F. F.Christen 3487 Coccato, Dr. L. L.Coccato 4059 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 4045 Helmi, Mevr. Dr. A. A.Helmi 4061 Helmich, E.M. E.M.Helmich 4036 Heraudeau, Dr. Ph. P.Heraudeau 4061 Hocuk, S. S. Hocuk 4054 Hulst, Prof. Dr. J.M. van der J.M.van.der.Hulst 4083 Jones, Dr. B. B.Jones 4081 Jong, Drs. J.T.A. de J.de.Jong 8322 Kamphuis, P. P.Kamphuis 6519 Koopmans. Dr. L. L.Koopmans 4050 Koster, Mevr. H.J. H.J.Koster 4085 Kovac, Drs. K. K.Kovac 4062 Kruit, Prof. Dr. P.C. van der P.C.van.der.Kruit

116

Tel. Name user@astro.rug.nl 4070 Kuijken, Dr. K.H. K.H.Kuijken 4060 Labiano Ortega, Drs. A. A.Labiano 4061 Land, D.D. D.D.Land 4083 Letarte, Drs. B. B.Letarte 4053 Li, Mevr. M.Sc. Y.S. ysleigh 4078 Loenen, Drs. A.F. A.F.Loenen 8326 McFarland, Dr. J. J.McFarland 4080 Mellema, Dr. G. G.Mellema 4060 Mohamed, N.M.A. N.M.Mohamed 4080 Morganti, Mevr. Dr. R. R.Morganti 4098 Noordermeer, Drs. E. E.Noordermeer 4063 Obric, Mevr. Drs. M. M.Obric 4080 Oosterloo, Dr. T.A. T.A.Oosterloo 4085 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, Mevr. Dr. I. I.PerezMartin 4083 Pizzo, M.Sc. R. R. Pizzo 4087 Platen, E. E.Platen 4063 Poelman, Drs. D. D.Poelman 4095 Pohlen, Dr. M. M.Pohlen 8689 Polko, Drs. P. P.Polko 4078 Popping, Drs. P. A.Popping 4097 Pottasch, Prof. Dr. S.R. S.R.Pottasch 4053 Ripamonti, Dr. E. E.Ripamonti 4057 Sancisi, Prof. Dr. R. R.Sancisi 4065 Sanders, Prof. Dr. R.H. R.H.Sanders 3505 Sansa, Mevr. Drs. J. J.Sansa 4085 Schaap, Drs. W.E. W.Schaap 4098 Schneider, Mevr. Drs. T. T.Schneider 4061 Seekles, D. D.Seekles 7753 Serra, Drs. P. P.Serra 8689 Siegers, A. A.Siegers 3476 Sikkema, Drs. G. G.Sikkema 4093 Smith, Dr. M.C. M.C.Smith 4094 Spaans, Dr. M. M.Spaans 4091 Starkenburg, Mevr. E. E. Starkenburg 2535 Tempelaar, Dr. M.J. M.J.Tempelaar 4068 Terlouw, J.P. J.P.Terlouw 3476 Thomas, Drs. R.M. R.M.Thomas 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 2535 Vermeij, Dr. R. R.Vermeij 4053 Villalobos, Drs. A. A. Villalobos 4096 Vogelaar, Drs. M.G.R. M.G.R.Vogelaar

117

Tel. Name user@astro.rug.nl 2535 Vriend, Drs. W.-J. W.J.Vriend 4076 Vries, Mevr. Drs. G. G.de.Vries 4089 Walker, Dr. M. M.Walker 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 3487 Yatawatta, Dr. S. S.Yatawatta 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

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.P. 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

119

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