ADS BibCode:
2008Msngr.133....2S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Spyromilio, J.; Comerón, F.; D’Odorico, S.; Kissler-Patig, M.; Gilmozzi, R.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO)
Abstract:
In December 2006 the ESO Council gave the go-ahead for the European Extremely Large Telescope (E-ELT) three-year Phase B study. The Baseline Reference Design (BRD) was presented to the ESO committees in 2006 and to the community at the Marseille meeting in December 2006. Phase B has been running for one and a half years and a progress report is presented covering science activities, telescope design, instrumentation, site selection and operations. The designs are maturing, in close synergy with industrial contracts, and the proposal for E-ELT construction is expected to be presented to the ESO Council in June 2010.
References:
Cuby, J.-G. 2007, The Messenger, 127, 25; Gilmozzi, R. & Spyromilio, J. 2007, The Messenger, 127, 11; Gilmozzi, R., Monnet, G. & Robinson, M. 2008, The Messenger, 132, 48; Hook, I. 2007, The Messenger, 127, 20; Monnet, G. 2007, The Messenger, 127, 24

ADS BibCode:
2008Msngr.133...10L
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Liske, J.; Grazian, A.; Vanzella, E.; Dessauges, M.; Viel, M.; Pasquini, L.; Haehnelt, M.; Cristiani, S.; Pepe, F.; Bonifacio, P.; Bouchy, F.; D’Odorico, S.; D’Odorico, V.; Levshakov, S.; Lovis, C.; Mayor, M.; Molaro, P.; Moscardini, L.; Murphy, M.; Queloz, D.; Udry, S.; Wiklind, T.; Zucker, S.
AA(ESO) AB(INAF – Osservatorio Astronomico di Roma, Italy) AC(INAF – Osservatorio Astronomico di Trieste, Italy) AD(Observatoire de Genève, Switzerland) AE(INAF – Osservatorio Astronomico di Trieste, Italy; Institute of Astronomy, University of Cambridge, United Kingdom) AF(ESO) AG(Institute of Astronomy, University of Cambridge, United Kingdom) AH(INAF – Osservatorio Astronomico di Trieste, Italy) AI(Observatoire de Genève, Switzerland) AJ(Cosmological Impact of the First STars (CIFIST) Marie Curie Excellence Team, GEPI, Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS), France; INAF – Osservatorio Astronomico di Trieste, Italy) AK(Laboratoire d’Astrophysique de Marseille, France; Observatoire de Haute-Provence, France) AL(ESO) AM(INAF – Osservatorio Astronomico di Trieste, Italy) AN(Ioffe Physico-Technical Institute, St. Petersburg, Russian Federation) AO(Observatoire de Genève, Switzerland) AP(Observatoire de Genève, Switzerland) AQ(INAF – Osservatorio Astronomico di Trieste, Italy) AR(Università di Bologna, Italy; INFN – National Institute for Nuclear Physics, Sezione di Bologna, Italy) AS(Swinburne University of Technology, Melbourne, Australia) AT(Observatoire de Genève, Switzerland) AU(Observatoire de Genève, Switzerland) AV(Space Telescope Science Institute, Baltimore, USA; Affiliated with the Space Sciences Department of the European Space Agency) AW(Tel Aviv University, Israel)
Abstract:
The redshifts of all cosmologically distant sources are expected to experience a small, systematic drift as a function of time due to the evolution of the Universe’s expansion rate. Here, we briefly review the motivation for measuring this effect and summarise our reasons for believing that the E-ELT will be the first telescope to detect it.
References:
Heavens, A. 2003, MNRAS, 343, 1327; Liske, J., et al. 2008, MNRAS, 386, 1192; Loeb, A. 1998, ApJ, 499, L111; Perlmutter, S., et al. 1999, ApJ, 517, 565; Riess, A. G., et al. 1998, AJ, 116, 1009; Sandage, A. 1962, ApJ, 136, 319; Seo, H.-J., Eisenstein, D. J. 2003, ApJ, 598, 720

ADS BibCode:
2008Msngr.133...14A
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Aldenius, M.; Kerber, F.; Bristow, P.; Nave, G.; Ralchenko, Y.; Sansonetti, C.J.
AA(ESO) AB(ESO) AC(ESO) AD(National Institute of Standards and Technology, Gaithersburg, Maryland, USA) AE(National Institute of Standards and Technology, Gaithersburg, Maryland, USA) AF(National Institute of Standards and Technology, Gaithersburg, Maryland, USA)
Abstract:
Extremely Large Telescopes (ELTs) and most of their instrumentation will be optimised for operation in the Near-InfraRed (NIR) because of the wavelength dependent performance of adaptive optics. Few established sources for wavelength calibration exist in this wavelength domain. A project is described which aims to provide the basic data to select the best calibration sources for NIR instruments at the European ELT (E-ELT) as a function of wavelength range and spectral resolution. This work directly supports the Phase A studies of E‑ELT instruments; in addition its results will be highly valuable for future use in analysis of NIR science observations.
References:
Aldenius, M., et al. 2008, SPIE 7014-209, in press Araujo-Hauck, C., et al. 2007, The Messenger, 129, 24; Cowan, R. D. 1981, The Theory of Atomic Structure and Spectra (Berkley: University of California Press), ftp://aphysics.lanl.gov/pub/cowan Kerber, F., Saitta, F. & Bristow, P. 2007, The Messenger, 129, 21; Kerber, F., et al. 2006, Proc. SPIE 6269, 626942; Kerber, F., Nave, G. & Sansonetti, C. J. 2008, ApJS, in press Outred, M. 1978, J. of Phys. Chem. Ref. Data, 7, 1; Ralchenko, Y., et al. 2008, NIST Atomic Spectra Database version 3.1.5 (National Institute of Standards and Technology, Gaithersburg, Maryland), http://physics.nist.gov/asd3

ADS BibCode:
2008Msngr.133...17M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Melo, C.; Pasquini, L.; Downing, M.; Deiries, S.; Naef, D.; Hanuschik, R.; Palsa, R.; Castillo, R.; Peña, E.; Bendek, E.; Gieles, M.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO) AJ(ESO) AK(ESO)
Abstract:
In May 2008, a new CCD, called Carreras, was installed in the GIRAFFE spectrograph to replace Bruce, the old detector. Carreras is more sensitive to wavelengths redward of 700 nm. The main characteristics and results obtained in the commissioning of Carreras are reported.
References:
Pasquini, L., et al. 2002, The Messenger, 110, 1; Battaglia, G., et al. 2008, MNRAS, 383, 183; Blecha, A., et al. 2000, Proc. SPIE, 4008, 467; Royer, F., et al. 2002, Proc. SPIE, 4847, 184; Armandroff, T. E. & Da Costa, G. S. 1991, AJ, 101, 1329; Cole, A. A., et al. 2004, MNRAS, 347, 367

ADS BibCode:
2008Msngr.133...21M
Section:
Astronomical Science
Author(s)/Affiliation(s):
Minniti, D.; Melo, C.; Naef, D.; Udalski, A.; Pont, F.; Moutou, C.; Santos, N.; Queloz, D.; Mazeh, T.; Gillon, M.; Mayor, M.; Udry, S.; Diaz, R.; Hoyer, S.; Ramirez, S.; Pietrzynski, G.; Gieren, W.; Ruiz, M.T.; Zoccali, M.; Tamuz, O.; Shporer, A.; Kubiak, M.; Soszynski, I.; Szewczyk, O.; Szymanski, M.; Ulaczyk, K.; Wyrzykowski, L.
AA(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile; Specola Vaticana, Città del Vaticano, Italy) AB(ESO) AC(ESO) AD(Warsaw University Observatory, Poland; The OGLE Team) AE(Observatoire de Genève, Sauverny, Switzerland) AF(Laboratoire d’Astrophysique de Marseille, France) AG(Centro de Astrofísica, Universidade do Porto, Portugal) AH(Observatoire de Genève, Sauverny, Switzerland) AI(School of Physics and Astronomy, R. and B. Sackler Faculty of Exact Sciences, Tel Aviv University, Israel) AJ(Observatoire de Genève, Sauverny, Switzerland) AK(Observatoire de Genève, Sauverny, Switzerland) AL(Observatoire de Genève, Sauverny, Switzerland) AM(Instituto de Astronomía y Física del Espacio, Buenos Aires, Argentina) AN(Departmento de Astronomía, Universidad de Chile, Santiago, Chile) AO(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AP(Warsaw University Observatory, Poland; Departamento de Astronomía, Universidad de Concepción, Chile) AQ(Departamento de Astronomía, Universidad de Concepción, Chile) AR(Departmento de Astronomía, Universidad de Chile, Santiago, Chile) AS(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile) AT(School of Physics and Astronomy, R. and B. Sackler Faculty of Exact Sciences, Tel Aviv University, Israel) AU(School of Physics and Astronomy, R. and B. Sackler Faculty of Exact Sciences, Tel Aviv University, Israel) AV(Warsaw University Observatory, Poland; The OGLE Team) AW(Warsaw University Observatory, Poland; The OGLE Team) AX(Warsaw University Observatory, Poland; The OGLE Team) AY(Warsaw University Observatory, Poland; The OGLE Team) AZ(Warsaw University Observatory, Poland; The OGLE Team) BA(The OGLE Team; Institute of Astronomy, University of Cambridge, United Kingdom)
Abstract:
This is the story of the Large Programme 666, dedicated to discover sub-stellar objects (extrasolar planets and brown dwarfs), and to measure their masses, radii, and mean densities. We hunt selected OGLE transit candidates using spectroscopy and photometry in the ‘twilight zone’, stretching the limits of what is nowadays possible with the VLT.
References:
Bouchy, F., et al. 2005, A&A, 431, 1105; Guillot, T., et al. 2006, A&A, 453, L21; Pont, F. 2006, MNRAS, 373, 231; Pont, F., et al. 2005, A&A, 438, 1123; Pont, F., et al. 2008, A&A, in press Torres, G., et al. 2008, ApJ, 677, 1324; Udalski, A., et al. 2008, A&A, 482, 299

ADS BibCode:
2008Msngr.133...26E
Section:
Astronomical Science
Author(s)/Affiliation(s):
Eckart, A.; Schödel, R.; García-Marín, M.; Witzel, G.; Weiss, A.; Baganoff, F.; Morris, M.R.; Bertram, T.; Dovcˇiak, M.; Downes, D.; Duschl, W.; Karas, V.; König, S.; Krichbaum, T.; Krips, M.; Kunneriath, D.; Lu, R.; Markoff, S.; Mauerhan, J.; Meyer, L.; Moultaka, J.; Muži´c, K.; Najarro, F.; Pott, J.; Schuster, K.; Sjouwerman, L.; Straubmeier, C.; Thum, C.; Vogel, S.; Wiesemeyer, H.; Zamaninasab, M.; Zensus, A.
AA(University of Cologne, Cologne, Germany; Max-Planck-Institut für Radioastronomie, Bonn, Germany) AB(Instituto de Astrofísica de Andalucía, Granada, Spain) AC(University of Cologne, Cologne, Germany) AD(University of Cologne, Cologne, Germany) AE(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AF(Centre for Space Research, Massachusetts Institute of Technology, Cambridge, USA) AG(Department of Physics and Astronomy, University of California, Los Angeles, USA) AH(University of Cologne, Cologne, Germany) AI(Astronomical Institute, Academy of Sciences, Prague, Czech Republic) AJ(Institut de Radio Astronomie Millimétrique, St. Martin d’Heres, France) AK(Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität, Kiel, Germany; Steward Observatory, The University of Arizona, Tucson, USA) AL(Astronomical Institute, Academy of Sciences, Prague, Czech Republic) AM(University of Cologne, Cologne, Germany) AN(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AO(Harvard-Smithsonian Centre for Astrophysics, Cambridge, USA) AP(University of Cologne, Cologne, Germany; Max-Planck-Institut für Radioastronomie, Bonn, Germany) AQ(Max-Planck-Institut für Radioastronomie, Bonn, Germany; University of Cologne, Cologne, Germany) AR(Astronomical Institute “Anton Pannekoek”, University of Amsterdam, the Netherlands) AS(Department of Physics and Astronomy, University of California, Los Angeles, USA) AT(Department of Physics and Astronomy, University of California, Los Angeles, USA) AU(LATT, Université de Toulouse, CNRS, Toulouse, France) AV(University of Cologne, Cologne, Germany) AW(DAMIR, Instituto de Estructura de la Materia, Consejo Superior de Investigaciones Científicas, Madrid, Spain) AX(Department of Physics and Astronomy, University of California, Los Angeles, USA; W. M. Keck Observatory, CARA, Kamuela, USA) AY(Institut de Radio Astronomie Millimétrique, St. Martin d’Heres, France) AZ(National Radio Astronomy Observatory, Socorro, USA) BA(University of Cologne, Cologne, Germany) BB(Institut de Radio Astronomie Millimétrique, St. Martin d’Heres, France) BC(Department of Astronomy, University of Maryland, College Park, USA) BD(IRAM, Granada, Spain) BE(University of Cologne, Cologne, Germany; Max-Planck-Institut für Radioastronomie, Bonn, Germany) BF(Max-Planck-Institut für Radioastronomie, Bonn, Germany)
Abstract:
On 3 June 2008 an international team of researchers observed one of the brightest near-infrared flares close to SgrA*, the black hole at the centre of the Milky Way. For the very first time the flare emission was detected in infrared light, with one of the VLT telescopes, and time delayed in sub-millimetre radiation with the APEX telescope. Recent simultaneous X-ray and infrared flares from SgrA* have been detected and can be explained by spots on relativistic orbits around the central, accreting supermassive black hole. The observations of flares now also show some evidence for time evolution of the spot properties. The investigation of dusty stars and filaments in the central stellar cluster also indicates the presence of a wind from the central region – possibly with a contribution from SgrA* itself.
References:
Baganoff, F. K., et al. 2001, Nature, 413, 45; Do, T., et al. 2008, JPhCS, accepted and ApJ, submitted Eckart, A., et al. 2008, A&A, 479, 625; Eckart, A., et al. 2006, A&A, 450, 535; Eckart, A., et al. 2002, MNRAS, 331, 917; Eisenhauer, F., 2003, ApJ, 597, L121; Genzel, R., et al. 2003, Nature, 425, 934; Ghez, A. M., et al. 2004, ApJ, 601, 159; Ghez, A. M., et al. 2005, ApJ, 620, 744; Karas, V., et al. 2007, Proceedings of the Workshop on Black Holes and Neutron Stars, eds. S. Hledik & Z. Stuchlik, 99 (astro-ph0709.3836) Kunneriath, D., et al. 2008, JPhCS, accepted Hornstein, S. D., et al. 2007, ApJ, 667, 900; Lu, R.-S., et al. 2008, JPhCS, accepted Marrone, D. P., et al. 2008, ApJ, in press (arXiv0712.2877M) Mauerhan, J. C., et al. 2005, ApJ, 623, L25; Meyer, L., et al. 2007, A&A, 473, 707; Meyer, L., et al. 2008, ApJ, submitted Muži´c, K., et al. 2008, A&A, 482, 173; Muži´c, K., et al. 2007, A&A, 469, 993; Pott, J.-U., et al. 2008a, A&A, 480, 115; Pott, J.-U., et al. 2008b, A&A, in press (arXiv:0805.4408) Schödel, R., et al. 2002, Nature, 419, 694; Schödel, R., et al. 2007, A&A, 469, 125; Siringo, G., et al. 2007, The Messenger, 129, 2; Yusef-Zadeh, F., et al. 2008, ApJ, accepted (arXiv0712.2882Y)

ADS BibCode:
2008Msngr.133...31M
Section:
Astronomical Science
Author(s)/Affiliation(s):
Morelli, L.; Pompei, E.; Pizzella, A.; Méndez-Abreu, J.; Corsini, E.M.; Coccato, L.; Saglia, R.; Sarzi, M.; Bertola, F.
AA(Dipartimento di Astronomia, Università di Padova, Italy; Department of Astronomy, Pontificia Universidad Católica de Chile, Santiago, Chile) AB(ESO) AC(Dipartimento di Astronomia, Università di Padova, Italy) AD(Dipartimento di Astronomia, Università di Padova, Italy; INAF-Osservatorio Astronomico di Padova, Italy) AE(Dipartimento di Astronomia, Università di Padova, Italy) AF(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AG(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AH(Centre for Astrophysics Research, University of Hertfordshire, Hatfield, United Kingdom) AI(Dipartimento di Astronomia, Università di Padova, Italy)
Abstract:
Photometry and long-slit spectroscopy are presented for 14 S0 and spiral galaxies of the Fornax, Eridanus and Pegasus clusters and the NGC 7582 group. The age, metallicity and α/Fe enhancement of the stellar population in the centres and their gradients are obtained using stellar population models with variable element abundance ratios. Most of the sample bulges display solar α/Fe enhancement, no gradient in age, and a negative gradient of metallicity. One of the bulges, that of NGC 1292, is a pseudobulge and the properties of its stellar population are consistent with a slow build-up within a scenario of secular evolution.
References:
Aguerri, J. A. L., Balcells, M. & Peletier, R. F. 2001, A&A, 367, 428; Bender, R., Saglia, R. P. & Gerhard, O. E. 1994, MNRAS, 269, 785 Binney, J. & Tremaine, S. 1987, Galactic Dynamics, (Princeton, NJ: Princeton Univ. Press), 747; Forbes, D. A. & Ponman, T. J. 1999, MNRAS, 309, 623; Gilmore, G. & Wyse, R. F. G 1998, AJ, 116, 748; Jablonka, P., Gorgas, J. & Goudfrooij, P. 2007, A&A, 474, 763 Kormendy, J. & Kennicutt, R. C. 2004, ARA&A, 42, 603; Mehlert, D., et al. 2003, A&A, 407, 423; Méndez-Abreu, J., et al. 2008, A&A, 478, 353 Moorthy, B. K. & Holtzman, J. A. 2006, MNRAS, 371, 583; Thomas, D., Maraston, C. & Bender, R. 2003, MNRAS, 339, 897

ADS BibCode:
2008Msngr.133...36M
Section:
Astronomical Science
Author(s)/Affiliation(s):
Meisenheimer, K.; Raban, D.; Tristram, K.; Schartmann, M.; Jaffe, W.; Röttgering, H.; Burtscher, L.
AA(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AB(Sterrewacht Leiden, the Netherlands) AC(Max-Planck-Institut für Astronomie, Heidelberg, Germany; Max-Planck-Institut für Radioastronomie, Bonn, Germany) AD(Max-Planck-Institut für Astronomie, Heidelberg, Germany; Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Universitäts-Sternwarte, München, Germany) AE(Sterrewacht Leiden, the Netherlands) AF(Sterrewacht Leiden, the Netherlands) AG(Max-Planck-Institut für Astronomie, Heidelberg, Germany)
Abstract:
Active Galactic Nuclei (AGN) are powered by accretion onto a supermassive black hole. The unified scheme for strongly accreting AGN postulates that the central engine is enshrouded by a doughnut-shaped structure of gas and dust – the so-called torus. We report observations with the MID-Infrared Interferometric Instrument (MIDI) at the VLT Interferometer, which resolve the tori in the nearest Seyfert 2 galaxies, and suggest a complex structure, consisting of a compact inner disc embedded in a patchy or filamentary outer torus. The prominent nearby radio galaxy Centaurus A, however, shows little sign of a torus. Instead, its mid-infrared emission is dominated by non-thermal radiation from the base of the radio jet. Thus, not all classes of AGN contain a thick torus.
References:
Antonucci, R. 1993, ARA&A, 31, 473; Gallimore, J. F., Baum, S. A. & O’Dea, C. P. 2004, ApJ, 613, 794. Jaffe, W., Meisenheimer, K., Röttgering, H., et al. 2004, Nature, 429, 47; Krolik, J. H. & Begelman, M. C. 1988, ApJ, 329, 702; Leinert, C., Graser, U., Richichi, A., et al. 2003, The Messenger, 112, 13; Meisenheimer, K., Tristram, K. R. W., Jaffe, W., et al. 2007, A&A, 471, 453; Nenkowa, M., Ivezi, Z. & Eliitzur, M. 2002, ApJL, 570, L9; Raban, D., Heijligers, B., Röttgering, H., et al. 2008a, A&A, in press (arXiv:0804.2395) Raban, D., Jaffe, W., Röttgering, H., et al. 2008b, MNRAS, in press Schartmann, M., Meisenheimer, K., Camenzind, M., et al. 2008, A&A, in press (arXiv:0802.2604) Tristram, K. R. W., Meisenheimer, K., Jaffe, W., et al. 2007, A&A, 474, 837

ADS BibCode:
2008Msngr.133...42S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Sullivan, M.; Balland, C.
AA(Department of Physics, University of Oxford, United Kingdom) AB(Laboratoire de Physique Nucléaire et des Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS) – Institut Nationale de Physique Nucléaire et de Physique des Particules (IN2P3), Universités Paris VI and Paris VII, France)
Abstract:
The accelerating Universe was one of the most surprising discoveries of 20th century science. The ‘dark energy’ that drives it lacks a compelling theoretical explanation, and has sparked an intense observational effort to understand its nature. Over the past five years, the Supernova Legacy Survey (SNLS) has made a concerted effort to gather 500 distant Type Ia Supernovae (SNe Ia), a sample of standard candles with the power to make a 5% statistical measurement of the dark energy’s equation of state. The SNLS sample also provides one of the most uniform sets of SNe Ia available, with a photometric and spectroscopic coverage allowing new insights into the physical nature of SN Ia progenitors. With the survey recently completed, we report on the latest science analysis, and the vital role that the ESO VLT has played in measuring these distant cosmic explosions.
References:
Appenzeller, I., et al. 1998, The Messenger, 94, 1; Astier, P., et al. 2006, A&A, 447, 31; Copeland, E. J., Sami, M. & Tsujikawa, S. 2006, International Journal of Modern Physics D, 15, 1753; Gallagher, J. S., et al. 2008, arXiv:0805.4360; Howell, D. A., et al. 2007, ApJL, 667, L37; Mannucci, F., Della Valle, M. & Panagia, N. 2006, MNRAS, 370, 773; Perlmutter, S., et al. 1997, ApJ, 483, 565; Perlmutter, S., et al. 1999, ApJ, 517, 565; Phillips, M. M. 1993, ApJL, 413, L105; Pritchet, C. J., Howell, D. A. & Sullivan, M. 2008, arXiv:0806.3729; Riess, A. G., et al. 1998, AJ, 116, 1009; Sullivan, M., et al. 2006, ApJ, 648, 868; Timmes, F. X., Brown, E. F. & Truran, J. W. 2003, ApJL, 590, L83

ADS BibCode:
2008Msngr.133...49B
Section:
Astronomical News
Author(s)/Affiliation(s):
Böcker, M.; Vogt, J.; Nolle-Gösser, T.
AA(ESO) AB(Deutsche Flugsicherung GmbH, Germany) AC(Technical University of Dortmund, Germany)
Abstract:
The ESO coordinated study “Optimising Performance, Health and Safety in High-Altitude Observatories” is based on a psychological approach using a questionnaire for data collection and assessment of high-altitude effects. During 2007 and 2008, data from 28 staff and visitors involved in APEX and ALMA were collected and analysed and the first results of the study are summarised. While there is a lot of information about biomedical changes at high altitude, relatively few studies have focussed on psychological changes, for example with respect to performance of mental tasks, safety consciousness and emotions. Both, biomedical and psychological changes are relevant factors in occupational safety and health. The results of the questionnaire on safety, health and performance issues demonstrate that the working conditions at high altitude are less detrimental than expected.
References:
Böcker, M. & Vogt, J. 2007, The Messenger, 127, 64; Fields, R. D. 2008, Scientific American, April/May 2008; Sakamoto, S., et al. 2003, ALMA Memo, 446; Vogt, J. 2002, in Lehrbuch der Umweltmedizin, W. Dott, et al., (Stuttgart: Wissenschaftliche Verlagsgesellschaft mbH), 479; Vogt, J., et al. 2004, International Journal of Emer- gency Mental Health, 6, 185; Vogt, J., Pennig, S. & Leonhardt, J. 2007, Air Traffic Control Quarterly, 15, 127; West, J. B. 1997, Aviation Space and Environmental Medicine, 68, 162; West, J. B. 2003, ALMA Memo, 477; West, J. B. 2004, The Observatory, 124, 1; Wu, T. et al. 2007, High Altitude Medicine & Biology, 8, 88

ADS BibCode:
2008Msngr.133...52L
Section:
Astronomical News
Author(s)/Affiliation(s):
Lehnert, M.; Breuck, C.D.; Kuntschner, H.; Zwaan, M.
AA(Laboratoire d’Etudes des Galaxies, Etoiles, Physique et Instrumentation (GEPI), Observatoire de Paris-Meudon, France) AB(ESO) AC(ESO) AD(ESO)
Abstract:
An overview of the ESO/Radionet workshop devoted to 3D optical/near-infrared and sub‑mm/radio observations of gas and stars in galaxies is presented. There will be no published proceedings but presentations are available at http://www.eso.org/sci/meetings/gal3D2008/program.html.
References:
Emsellem, E., et al. 2004, MNRAS, 352, 721; Genzel, R., et al. 2006, Nature, 442, 786; Riechers, D., et al. 2008, ApJL, submitted Walter, F., et al. 2008, ApJ, in press Young, L. M., Bureau, M. & Cappellari, M. 2008, ApJ, 676, 317

ADS BibCode:
2008Msngr.133...57M
Section:
Astronomical News
Author(s)/Affiliation(s):
Moorwood, A.
AA(ESO)

ADS BibCode:
2008Msngr.133...58D
Section:
Astronomical News
Author(s)/Affiliation(s):
Danziger, J.; Breysacher, J.
AA(Osservatorio Astronomico di Trieste, Italy) AB(Saubion, France)

ADS BibCode:
2008Msngr.133...58K
Section:
Astronomical News
Author(s)/Affiliation(s):
Kerber, F.; Hanuschik, R.; Kuntschner, H.
AA(ESO) AB(ESO) AC(ESO)

ADS BibCode:
2008Msngr.133...60A
Section:
Astronomical News
Author(s)/Affiliation(s):
Argandoña, G.; West, M.
AA(ESO) AB(ESO)

ADS BibCode:
2008Msngr.133...61B
Section:
Astronomical News
Author(s)/Affiliation(s):
Böcker, M.
AA(ESO)

ADS BibCode:
2008Msngr.133...61.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2008Msngr.133...63.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2008Msngr.133...64.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2008Msngr.133...65.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2008Msngr.133Q..66.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2008Msngr.133R..66.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)