ADS BibCode:
2003Msngr.114....1.
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2003Msngr.114....2.
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
A momentous event took place on 6 November, at the site of the ALMA “Operations Support Facility” (OSF), near Chajnantor where the array will be built. About 170 scientists and dignitaries from Europe, North America, Japan and Chile attended the groundbreaking ceremony for this global project. The pictures shown here and two of the speeches that were given (those by the ESO Director General and President of Council) tell the story.

ADS BibCode:
2003Msngr.114....3.
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
We are children of the universe. Actually, we are children of the universe in a very strict sense. Look at our bodies. By weight we are made up for about a quarter or so of hydrogen. The rest is in other chemical elements, of which carbon, nitrogen and oxygen are the major contributors. In contrast, the Universe, when it was about three minutes old and sufficiently cool that atomic nuclei could exist, consisted for three-quarters of hydrogen and one quarter of helium. There was no carbon, no nitrogen, no oxygen or any other chemical element except traces of lithium and boron. We now know that the chemical elements that make up most of our bodies were formed by nuclear reactions in heavy stars that live for a very short while and blow themselves up as supernovae and release the heavy elements into the interstellar gas so that new planets and possibly life can be formed. We are stardust.

ADS BibCode:
2003Msngr.114....4.
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
This is a great day for Astronomy. This is indeed a great day for Chile, for the II Region and for San Pedro de Atacama. And this is indeed a great day for all of us, a moment to which we have all been looking forward with great anticipations. This is the real beginning of a joint adventure. We will be reaching towards the stars, searching for the earliest, remotest objects in the Universe, peering beyond current horizons into the deep unknown.

ADS BibCode:
2003Msngr.114....5M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Moorwood, A.
AA(European Southern Observatory)
Abstract:
The CRyogenic InfraRed Echelle Spectrograph being developed by ESO will provide a totally new capability for high resolution (R ˜ 105) infrared spectroscopy between 1 and 5 μm and open up entirely new fields of research with the VLT starting in 2005.

ADS BibCode:
2003Msngr.114....9W
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Wilson, R.N.
AA(ESO)
Abstract:
Following my article, l received a most interesting e-mail from my ex-colleague of ESO and good friend, Daniel Enard. He was concerned about the precise chronology of the development of the ESO Shack-Hartmann image analyser − see the second section of my article. Enard pointed out that he and l first visited Roland Shack together in February 1976, before the 3.6 m telescope was set up some months later. Already before then I knew of the Shack proposal as I had been receiving the “Optical Sciences Center Newsletter”, in which it was first published in 1971 (see Ref. W99 in my article). This was why we visited Shack to learn more about it. Shack complained bitterly of lack of interest in the American community and was encouraged by our deep and practical interest.

ADS BibCode:
2003Msngr.114...10B
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Bagnulo, S.; Jehin, E.; Ledoux, C.; Cabanac, R.; Melo, C.; Gilmozzi, R.; The ESO Paranal Science Operations Team
AA(European Southern Observatory), AB(European Southern Observatory), AC(European Southern Observatory), AD(European Southern Observatory), AE(European Southern Observatory), AF(European Southern Observatory), AG(European Southern Observatory)
Abstract:
We present the UVES Paranal Observatory Project, consisting of acquisition, reduction, and public release of high-resolution, large wavelength coverage, and high signal-to-noise ratio stellar spectra obtained with the UVES instrument of the ESO Very Large Telescope. Data for about 400 stars across the Hertzsprung-Russell diagram have been taken and reduced by members of the Paranal Science Operations Team and made publicly available through a WEB interface at www.eso.org/uvespop.
References:
Ballester, P., Modigliani, A., Boitquin, O., Cristiani,
S., Hanuschik, R., Kaufer, A., & Wolf,
S., 2000, The UVES Data Reduction
Pipeline,The ESO Messenger, 101, 31
Buscombe,W., 1999, 14th General Catalogue of
MK Spectral Classification,VizieR On-line
Data Catalog: III/222. Originally published
in: Northwestern Univ., Evanston, Illinois
ISBN 0-939160-12-9 (1999)
Dekker, H., D’Odorico, S., Kaufer, A., Delabre,
B., Kotzlowski, H., 2000, Design, construction
and performance of UVES, the echelle
spectrograph for the UT2 Kueyen telescope
at the ESO Paranal Observatory, SPIE
Munich [4008-534]
ESA, 1997, The Hipparcos Catalogue, ESA SP-
1200
Hanuschik, R.W., 2003,A&A, 407, 1157
Kaufer, A., D’Odorico, S., & Kaper, L., 2003,
UVES User manual, Doc. No. VLT-MANESO-
13200-1825
Kupka, F., Piskunov, N. E., Ryabchikova, T. A.,
Stempels, H. C., & Weiss, W. W., 1999,
A&AS, 138, 119
Renson, P., Gerbaldi. M., & Catalano, F. A.,
1991,A&AS, 89, 429
WEB LINKS CITED IN THIS PAPER:
[1] The VALD database:
http://www.astro.univie.ac.at/~vald/
[2] The WEBDA database:
http://obswww.unige.ch/webda/
[3] The UVES web pages:
http://www.eso.org/instruments/uves/
[4] The UVES pipeline:
http://www.eso.org/observing/dfo/quality/UVES/
pipeline/
[5] Problems with the pipeline reduced spectra:
http://www.eso.org/observing/dfo/quality/UVES/
pipeline/pipe_reduc.html#problems
[6] How to flux calibrate UVES data:
http://www.eso.org/observing/dfo/quality/UVES/qc/
response.html
[7] The UVES master response Curves:
http://www.eso.org/observing/dfo/quality/UVES/qc/
std_qc1.html#response
[8] The ESO UVES archive:
http://archive.eso.org/wdb/wdb/eso/uves/form

ADS BibCode:
2003Msngr.114...15B
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Bonaccini, D.; Hackenberg, W.; Taylor, L.
AA(EUROPEAN SOUTHERN OBSERVATORY, GARCHING, GERMANY) AB(EUROPEAN SOUTHERN OBSERVATORY, GARCHING, GERMANY) AC(EUROPEAN SOUTHERN OBSERVATORY, GARCHING, GERMANY & UNIVERSITY OF CALIFORNIA, LAWRENCE LIVERMORE NATIONAL LABORATORY, USA)
Abstract:
In the context of developments toward mature Adaptive Optics systems for large telescopes, we describe the present activities at ESO in the area of fibre lasers.
References:
Beuzit, J-L., Demailly, L., Gendron, E. et al.,
1997, in Experimental Astronomy, 7, 285
Beckers, J.M., 1998, in Proc. “ESO Conference
on Very Large Telescopes and Their Instrumentation”,
ed M-H Ulrich, p. 693
Dawson J.W., Drobshoff A., Liao Z.M. et al.,
2003, in ”Advances in Fibre Lasers” ed.
L.N. Durvasula, SPIE Proc. 4974, p. 75
Ellerbroek B., Rigaut F., Bauman B. Et al.,
2003, in ”Adaptive Optical System Technologies”,
eds P.Wizinowich and D. Bonaccini,
SPIE Proc. vol 4839, p. 55
Gavel D., Gates E., Max C. et al., 2003, in
”Adaptive Optical System Technologies”,
op. cit., p. 354
Hackenberg W., Bonaccini D. and Werner D.,
2003, in ”Adaptive Optical System Technologies”,
op. cit., p. 421
Takami H.,Takato N., Hayano Y. et al., 2003, in
”Adaptive Optical System Technologies”,
op. cit. p. 21
Wizinowich P.L., Le Mignant D., Stomski P.J.Jr.
et al., 2003, in ”Adaptive Optical System
Technologies”, op. cit., p. 9

ADS BibCode:
2003Msngr.114...20M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Mayor, M.; Pepe, F.; Queloz, D.; Bouchy, F.; Rupprecht, G.; Lo Curto, G.; Avila, G.; Benz, W.; Bertaux, J.-L.; Bonfils, X.; dall, Th.; Dekker, H.; Delabre, B.; Eckert, W.; Fleury, M.; Gilliotte, A.; Gojak, D.; Guzman, J. C.; Kohler, D.; Lizon, J.-L.; Longinotti, A.; Lovis, C.; Megevand, D.; Pasquini, L.; Reyes, J.; Sivan, J.-P.; Sosnowska, D.; Soto, R.; Udry, S.; van Kesteren, A.; Weber, L.; Weilenmann, U.
AA(OBSERVATOIRE DE GENÈVE, SWITZERLAND) AB(OBSERVATOIRE DE GENÈVE, SWITZERLAND) AC(OBSERVATOIRE DE GENÈVE, SWITZERLAND) AD(LABORATOIRE D'ASTROPHYSIQUE DE MARSEILLE, FRANCE) AE(ESO GARCHING) AF(ESO LA SILLA) AG(ESO GARCHING) AH(PHYSIKALISCHES INSTITUT DER UNIVERSITÄT BERN, SWITZERLAND) AI(SERVICE D'AÉRONOMIE, VERRIÈRES LE BUISSON, FRANCE) AJ(OBSERVATOIRE DE GENÈVE, SWITZERLAND) AK(ESO LA SILLA) AL(ESO GARCHING) AM(ESO GARCHING) AN(ESO LA SILLA) AO(OBSERVATOIRE DE GENÈVE, SWITZERLAND) AP(ESO LA SILLA) AQ(ESO GARCHING) AR(ESO LA SILLA) AS(OBSERVATOIRE DE HAUTEPROVENCE, FRANCE) AT(ESO GARCHING) AU(ESO GARCHING) AV(OBSERVATOIRE DE GENÈVE, SWITZERLAND) AW(OBSERVATOIRE DE GENÈVE, SWITZERLAND) AX(ESO GARCHING) AY(ESO GARCHING) AZ(OBSERVATOIRE DE HAUTEPROVENCE, FRANCE) BA(OBSERVATOIRE DE GENÈVE, SWITZERLAND) BB(ESO LA SILLA) BC(OBSERVATOIRE DE GENÈVE, SWITZERLAND) BD(ESO GARCHING) BE(OBSERVATOIRE DE GENÈVE, SWITZERLAND) BF(ESO LA SILLA)
Abstract:
By October 1st, 2003, ESO's new and unique planet-hunting machine HARPS (High-Accuracy Radial velocity Planetary Searcher) has become operational. The measurements made during the commissioning phase and the first weeks of operation are of outstanding quality. In this article we report among other examples on the first extra-solar planet discovered with HARPS and on the detection of tiny stellar oscillations. The results presented demonstrate that HARPS is currently the most precise Doppler- measurements machine in the world. With this acquisition ESO places itself at the head of a scientific domain, whose interest has continued to grow during the past years.
References:
Bouchy F. & Carrier F., 2001, ESO Messenger,
106, 32
Bouchy F. & Carrier F., 2002, A&A, 390, 205
Konacki M. et al., 2003, Nature, 421, 507
Pepe F. et al., 2002, ESO Messenger, 110, 9
Queloz D. & Mayor M., 2001, ESO Messenger,
105, 1
Santos N. et al., 2001, A&A, 373, 1019

ADS BibCode:
2003Msngr.114...25G
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Germany, L.
AA(SciOps)
Abstract:
Documentation; SOFI; FEROS; SEST; MARS

ADS BibCode:
2003Msngr.114...26R
Section:
Reports from Observers
Author(s)/Affiliation(s):
Richichi, A.; Paresce, F.
AA(ESO) AB(ESO)
Abstract:
The ESO Very Large Telescope Interferometer (VLTI) has been included for the first time in the official call for proposals requesting ESO telescopes for the period starting in April 2004. This marks the official start of public interferometric observations open to the community. It is the start of a new approach to interferometry as a standard astronomical technique, and a point of pride and satisfaction for all the people who have been working with this challenging goal for many years. But it should not be forgotten that the VLTI has already logged over two years of intensive commissioning, as well as some initial science demonstration runs. Over 16,000 observations of hundreds of objects have been collected and are available publicly over the ESO archive on the WEB. In 2003, the first scientific results of this remarkable effort have appeared. Already more than a dozen papers based on VLTI data have been submitted or accepted by refereed journals, with a similar volume of contributions to workshops and conferences of a scientific nature. We provide here an overview of this early scientific production of the VLTI, ranging from the determination of fundamental parameters of many classes of stars to the first interferometric measurement of the inner regions of the nucleus of the Seyfert galaxy NGC 1068.
References:
First radius measurements of very low
mass stars with the VLTI, Sègransan
et al., 2003,A&A, 397, L5
The diameters of a Centauri A and B: a
comparison of the asteroseismic and
VLTI views, Kervella et al., 2003,
A&A, 404, 1087
Interferometry and asteroseismology:
The radius of t Cet, Pijpers et al.,
2003,A&A, 406, L15
The spinning-top Be star Achernar from
VLTI-VINCI, Domiciano de Souza et
al., 2003,A&A, 407, L47
The interferometric diameter and internal
structure of Sirius A, Kervella et
al., 2003,A&A, 408, 681
First VLTI observations of Mira stars,
Richichi and Wittkowski, 2003,
Ap&SS, 286, 219
The VLTI Calibrators Program: Getting
ready for high accuracy measurements,
Percheron, Richichi, and
Wittkowski, 2003,Ap&SS, 286, 105
Direct measurement of the size of the star
h Carinae, Van Boekel et al., 2003,
A&A, in press (astro-ph/0310399)
Tests of stellar model atmospheres by
optical interferometry: VLTI/VINCI
limb-darkening measurements of the
M4 giant y Phe, Wittkowski et al.,
2003,A&A, in press
The diameter and evolutionary state of
Procyon A, Kervella et al., 2003,
A&A, in press (astro-ph/0309148)
J-K DENIS photometry of a VLTI-selected
sample of bright southern stars,
Kimeswenger et al., 2003, A&A, in
press
Introduction to VINCI/VLTI interferometric
data analysis, Kervella et al.,
2003,A&A, submitted
Calibration observations of Fomalhaut
with the VLTI, Davis et al., 2003,
A&A, submitted
Dust in the nucleus of the active galaxy
NGC1068: structure and composition
on parsec scales, Jaffe et al., 2003,
Nature, submitted.
Baraffe, Chabrier, Allard, Hauschildt, 1998,
A&A 337, 403
Baraffe, Chabrier, Barman, Allard, Hauschildt,
2003, A&A 402, 701
Dwarkadas, Owocki, 2002, ApJ 581, 1337
Monnier, J.D. 2003, Reports on Progress in
Physics,Volume 66, Issue 5, p. 789
Richichi A., Percheron I. 2002,A&A, 386, 492
Wittkowski, Schoeller, Hubrig, Posselt, von der
Luehe, 2002, AN 323, 241

ADS BibCode:
2003Msngr.114...35A
Section:
Reports from Observers
Author(s)/Affiliation(s):
Alves, J.; Homeier, N.
AA(EUROPEAN SOUTHERN OBSERVATORY, GARCHING, GERMANY) AB(JOHN HOPKINS UNIVERSITY, BALTIMORE, USA)
Abstract:
In this article we present the first results from a near-infrared campaign to characterize our Galaxy's own starburst event, W49A, a prodigious factory of massive stars at a distance of about 12 kpc and concealed from observations at visible wavelengths by more than 25 magnitudes of intervening dust extinction. Our results so far reveal the presence of previously unknown massive stellar clusters containing more than 100 OB stars, some as massive as 120 Mȯ, most still embedded in their parental molecular cloud and with ages as young as 104-5 yr. We argue that this ongoing starburst appears to have been multi-seeded instead of resulting from a coherent trigger.
References:
Alves, J., & Homeier, N. 2003, ApJ, 589, 45
De Pree, C.G., Mehringer, D.M., Goss, W. M.
1997, ApJ, 482, 307
Elmegreen, B. G., & Lada, C. J. 1977, ApJ, 214,
725
Gwinn, C. R., Moran, J. M., & Reid, M. J. 1992,
ApJ, 393, 149
Homeier, N., & Alves, J. 2004, A&A in prep.
Lejeune,T., & Schaerer,D. 2001,A&A, 366, 538
Mezger, P. G., Schraml, J., & Terzian, Y. 1967,
ApJ, 150, 807
Shaver, P.A., & Goss,W.M. 1970,AuJPA, 14, 133
Simon, R., Jackson, J.M., Clemens, D.P., Bania,
T. M., & Heyer, M. H. 2001, ApJ, 551, 747
Welch,W. J., Dreher, J.W., Jackson, J. M., Terebey,
S., & Vogel, S. N. 1987, Science, 238,
1550
Wilner, D. J., De Pree, C. G., Welch, W. J., &
Goss,W. M. 2001, ApJLet, 550, L81

ADS BibCode:
2003Msngr.114...39T
Section:
Reports from Observers
Author(s)/Affiliation(s):
Tuellmann, R.; Rosa, M. R.; Elwert, T.; Bomans, D. J.; Ferguson, A. M. N.; Dettmar, R.-J.
AA(Astronomisches Institut, Ruhr-Universität Bochum, Germany) AB(Space Telescope-European Coordinating Facility, Garching, Germany) AC(Astronomisches Institut, Ruhr-Universität Bochum, Germany) AD(Astronomisches Institut, Ruhr-Universität Bochum, Germany) AE(Max-Planck-Institut für Astrophysik, Garching, Germany) AF(Astronomisches Institut, Ruhr-Universität Bochum, Germany)
Abstract:
We present the first VLT spectra of two compact Hα- emitting objects, located in the halo of the edge-on spiral galaxy NGC 55. The detection of stellar continuum and the observed emission-line characteristics indicate that these objects are extraplanar HII-regions. CLOUDY model simulations establish photoionisation by single OB-type stars as ionisation mechanism and finally confirm the HII-region character. Hydrodynamical considerations unambiguously restrict the origin of these regions to the halo. Their creation was most likely triggered by star formation activity in the disc below. In this picture the gas clouds, out of which the OB stars formed, could cool and collapse only between two successive bursts of star formation.
References:
Christensen-Dalsgaard, J., 1998, Space Sci.Rev.
85, 19
Dettmar, R.-J., 1992, Fundamentals of Cosmic
Physics, 15, 143
Ferguson,A. M.N.,Wyse, R. F.G., & Gallagher,
J. S., 1996, AJ 112, 2567
Ferguson, A. M. N., 2002, BAAS 200, 3306
Graham, J. A., & Lawrie, D. G., 1982, ApJ 253,
L73
Grevesse, N., & Sauval, A. J., 1998, Space Sci.
Rev. 85, 161
Keenan, F. P., 1992, QJRAS 33, 325
Tüllmann, R., Rosa, M. R., Elwert,T., Bomans,
D. J., Ferguson, A. M. N., & Dettmar, R.-J.,
2003,A&A, 412, 69

ADS BibCode:
2003Msngr.114...43.
Section:
Reports from Observers
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
In recent dramatic observations using NAOS-CONICA on the VLT, near-infrared flares from the direction of the the black hole at the Galactic centre have been detected.The signals, rapidly flickering on a scale of minutes, must come from hot gas falling into the black hole, just before it disappears below the "event horizon" of the monster. The new observations strongly suggest that the Galactic Centre black hole rotates rapidly. Never before have scientists been able to study phenomena in the immediate neighbourhood of a black hole in such a detail. These results were published recently by Reinhard Genzel and colleagues* in the journal Nature**, and were presented in ESO Press release PR 26/03.

ADS BibCode:
2003Msngr.114...44.
Section:
Reports from Observers
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
N44 in the Large Magellanic Cloud is a spectacular example of a giant HII region. Having observed it in 1999 (see ESO PR Photos 26ad/ 99), a team composed of Fernando Comerón and Nausicaa Delmotte from ESO, and Annie Laval from the Observatoire de Marseille (France), again used the Wide-Field-Imager (WFI) at the MPG/ESO 2.2-m telescope of the La Silla Observatory, pointing this 67-million pixel digital camera to the same sky region in order to provide another striking - and scientifically extremely rich - image of this complex of nebulae. With a size of roughly 1,000 light-years, the peculiar shape of N44 clearly outlines a ring that includes a bright stellar association of about 40 very luminous and bluish stars.

ADS BibCode:
2003Msngr.114...46L
Section:
Reports from Observers
Author(s)/Affiliation(s):
Leibundgut, B.; Grothkopf, U.; Treumann, A.
AA(European Southern Observatory), AB(European Southern Observatory), AC(European Southern Observatory)
Abstract:
Based on publication statistics, we provide a first assessment of ESO's scientific impact after four years of VLT operation. A brief discussion of the complexity of measuring scientific success and its inherent problems is given. We present publication and citation statistics drawn from the ESO publication database and provide some preliminary interpretation.

ADS BibCode:
2003Msngr.114...50S
Section:
Other Astronomical News
Author(s)/Affiliation(s):
Shaver, P.
AA(ESO)
Abstract:
Astronomers of ESA and ESO share their views on future cooperation between space and ground-based astronomy.

ADS BibCode:
2003Msngr.114...50H
Section:
Other Astronomical News
Author(s)/Affiliation(s):
Hau, G.; Alloin, D.
AA(ESO) AB(ESO)
Abstract:
Advances in ground- and space-based observational capabilities, as well as modelling tools, have enabled the study of resolved stellar populations with unprecedented details. This topical meeting, held at ESO Vitacura on June 27, 2003, was aimed at bringing astronomers together to examine the progress that has been made in this field.

ADS BibCode:
2003Msngr.114...51B
Section:
Other Astronomical News
Author(s)/Affiliation(s):
Brandner, W.; Kasper, M.
AA(MPIA Heidelberg, Germany) AB(ESO Garching)
Abstract:
From September 16 to 19, 2003, the ESO Workshop on “Science with Adaptive Optics” took place at ESO Headquarters in Garching. Its scope was to bring together users of adaptive optics (AO) from all fields of astronomy in order to discuss the latest scientific results obtained with AO systems, and to exchange ideas on how to reduce and analyse such observations.

ADS BibCode:
2003Msngr.114...52K
Section:
Other Astronomical News
Author(s)/Affiliation(s):
Käufl, H.U.; Moorwood, A.
AA(ESO) AB(ESO)
Abstract:
Infrared Spectroscopy at a resolution of a few km/s allows to study rotational-vibrational transitions of many abundant molecules as well as important atomic lines in a multitude of interesting astrophysical environments. The ESO VLT will shortly be equipped with two unique infrared spectrometers which combine spectral resolution with spatial resolutions of = 0.2 arcsec:

ADS BibCode:
2003Msngr.114...53R
Section:
Other Astronomical News
Author(s)/Affiliation(s):
Renzini, A.
AA(ESO, Garching)
Abstract:
Co-organized with the Universitäts-Sternwarte-München and the Max-Planck-Institut für Extraterrestrische Physik, this workshop was held in Venice, Italy, from October 13 through 16, 2003.The venue, on the premises of the Venice International University on the island of S. Servolo, proved ideal for hosting the 173 participants for the four full days of the meeting.

ADS BibCode:
2003Msngr.114...55.
Section:
Other Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
On June 8, 2004, Venus passes in front of the Sun as seen from the Earth. This very rare event (the last one was in 1882 and no living person has ever seen one!) lasts about 6 hours and will be visible from most of Europe, Africa and Asia. It will most certainly generate unprecedented attention from the media and the public, not just in these areas, but all over the world.

ADS BibCode:
2003Msngr.114...56M
Section:
Other Astronomical News
Author(s)/Affiliation(s):
Mackowiak, B.; West, R.
AA(ESO) AB(ESO)
Abstract:
The teaching of Physics in Europe’s schools is changing. In a growing number of places, thanks to well-informed and dedicated teachers, it is becoming an increasingly fascinating subject, appreciated by the students. More and more educators are beginning to realize that physics lessons may be a stage for demonstrations of how our daily life is influenced by numerous physical phenomena and processes. Moreover, as new frontiers of research open, new opportunities arise for interesting and effective teaching means and methods.

ADS BibCode:
2003Msngr.114...57.
Section:
Other Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
GEORGE HAU; NURIA HUELAMO; ELENA MASON

ADS BibCode:
2003Msngr.114...58.
Section:
Announcements
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
Planetary nebulae (PN) can be detected out to quite large distances from their strong emission lines, principally of [O III]. Photometry of the [O III]5007Å emission line allows distance determination through the Planetary Nebula Luminosity Function. Spectrophotometry of the emission lines can provide nebular abundances, enabling the use of PN as chemical probes of galaxies. The emission lines are also narrow, making PN ideal kinematic probes of a galaxy's gravitational potential. Thus the properties of dark-matter haloes can be studied by modelling the PN kinematics. Recently PN have been detected in intra-cluster regions of nearby galaxy clusters. These PN can bring a unique handle on the stars in regions that may harbour a substantial amount of mass.

ADS BibCode:
2003Msngr.114...58N
Section:
Announcements
Author(s)/Affiliation(s):
Nielbock, M.
AA(ESO)
Abstract:
MY first contact with ESO was a visit at the SEST on La Silla in 2000 in order to help with the installation and testing of the computer facilities for the planned bolometer array SIMBA. This matched my scientific background of early stages of star formation for which I mostly investigate in the millimetre and sub-millimetre, but also in the infrared regime of the electromagnetic spectrum. It was the team leader Lars-Ake Nyman who encouraged me to apply for the ESO Fellowship programme. At that time, I was in the middle of working on my PhD in Bochum (Germany) under the supervision of Rolf Chini, and I really had not thought about post-doc positions yet, but the prospect sounded very tempting. So, I applied and got the job. But this also meant, I had to speed up and finish the PhD within 2,5 years, since the installation of SIMBA required me to assume this new position on June 1st, 2001.

ADS BibCode:
2003Msngr.114Q..59.
Section:
Announcements
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2003Msngr.114R..59.
Section:
Announcements
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
Assignment: The Instrumentation Division consists of about 30 astronomers, physicists and engineers, who work closely with other Divisions at ESO plus many national and international Institutes to define, design, build, commission and use cutting-edge optical and infrared instrumentation on ESO’s telescopes at its Paranal (VLT) and La Silla observatories in Chile.

ADS BibCode:
2003Msngr.114Q..60.
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2003Msngr.114R..60.
Section:
Announcements
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
ESO Workshop Proceedings Still Available