ADS BibCode:
2007Msngr.129....2S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Siringo, G.; Weiss, A.; Kreysa, E.; Schuller, F.; Kovacs, A.; Beelen, A.; Esch, W.; Gemünd, H.-P.; Jethava, N.; Lundershausen, G.; Menten, K. M.; Güsten, R.; Bertoldi, F.; De Breuck, C.; Nyman, L.-Å.; Haller, E.; Beeman, J.
AA(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AB(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AC(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AD(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AE(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AF(Max-Planck-Institut für Radioastronomie, Bonn, Germany & Institut d’Astrophysique Spatiale, Université Paris-Sud, Paris, France) AG(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AH(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AI(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AJ(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AK(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AL(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AM(Argelander-Institut für Astronomie, Universität Bonn, Germany) AN(ESO) AO(ESO) AP(Lawrence Berkeley National Laboratory, Berkeley, California, USA) AQ(Lawrence Berkeley National Laboratory, Berkeley, California, USA)
Abstract:
In May 2007, the Large APEX Bolometer Camera LABOCA was commissioned as a facility instrument on the APEX 12-m submillimetre telescope located at an altitude of 5100 m in northern Chile. The new 870-μm bolometer camera, in combination with the high efficiency of APEX and the excellent atmospheric transmission at the site, offers unprecedented capability in mapping submillimetre continuum emission. An overview of LABOCA and the prospects for science are presented.
References:
Baars J. W. M. et al. 1987, A&A 175, 319
Booth R. S. et al. 1989, A&A 216, 315
Chapman S. C. et al. 2005, ApJ 622, 722
Nyman L.-Å. 2001, The Messenger 106, 40
Güsten R. et al. 2006, A&A 454L, 13
Ivison R. J. et al. 2000, MNRAS 315, 209
Kreysa E. et al. 2002, AIPC 616, 262
Reichertz L. A. et al. 2001, A&A 379, 735
Weferling B. et al. 2002, A&A 383, 1088

ADS BibCode:
2007Msngr.129....8M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Marchetti, E.; Brast, R.; Delabre, B.; Donaldson, R.; Fedrigo, E.; Frank, C.; Hubin., N.; Kolb, J.; Lizon, J.-L.; Marchesi, M.; Oberti, S.; Reiss, R.; Santos, J.; Soenke, C.; Tordo, S.; Baruffolo, A.; Bagnara, P.; The CAMCAO Consortium
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO) AJ(ESO) AK(ESO) AL(ESO) AM(ESO) AN(ESO) AO(ESO) AP(INAF – Astronomical Observatory of Padova, Italy) AQ(INAF – Astronomical Observatory of Padova, Italy) AR(Universidade de Lisboa, Portugal)
Abstract:
The aim of the Multi-Conjugate Adaptive Optics Demonstrator (MAD) is to correct for atmospheric turbulence over a field of view which is much larger than the one typically covered by the exist-ing adaptive optics systems installed on 8-m-class telescopes. After a long period of testing at the ESO premises, MAD was installed at the VLT early in 2007 in order to evaluate its correction performance. Here we present the MAD project and the recent results obtained during the on-sky testing at the VLT UT3 telescope Melipal.
References:
Beckers J. M. 1988, in ESO conference “Very Large
Telescopes and their instrumentation”,
ed. M.-H. Hulrich, 693
Gilmozzi R. and Spyromilio J. 2007, The Messenger
127, 11
Hartkopf W. I., McAlister H. A. and Mason B. D.
2001, AJ 122, 3480
Marchetti E. et al. 2006, SPIE 6272, 21M
Ragazzoni R., Marchetti E. and Rigaut F. 1999,
A&A 342, L53
Ragazzoni R., Marchetti E. and Valente G. 2000,
Nature 403, 54
Ragazzoni R., Farinato J. and Marchetti E. 2000,
SPIE 4007, 1076
Vernet-Viard E. et al. 2005, Opt. Eng. 44, 6601

ADS BibCode:
2007Msngr.129...14S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Saviane, I.; Piirola, V.; Bagnulo, S.; Monaco, L.; Hutsemekers, D.; Katajainen, S.; Lehto, H.; Vornanen, T.; Berdyugin, A.; Hakala, P.
AA(ESO) AB(Tuorla Observatory, University of Turku Piikkiö, Finland & Vatican Observatory, Città del Vaticano, Rome, Italy) AC(Armagh Observatory, Armagh, Northern Ireland) AD(ESO) AE(University of Liège, Belgium) AF(Tuorla Observatory, University of Turku Piikkiö, Finland) AG(Tuorla Observatory, University of Turku Piikkiö, Finland) AH(Tuorla Observatory, University of Turku Piikkiö, Finland) AI(Tuorla Observatory, University of Turku Piikkiö, Finland) AJ(Tuorla Observatory, University of Turku Piikkiö, Finland)
Abstract:
Starting from period P79, circular polarimetry measurements can be carried out with EFOSC2 at the ESO 3.6-m telescope. Here we describe the motivations behind the upgrade of the instrument, and a few results from the commissioning runs are used to show the excellent performance of the new polarimetry unit.
References:
Andronov I. L., Baklanov A. V. and Burwitz V. 2006,
A&A 452, 941
Angel J. R. P. and Landstreet J. D. 1974, ApJ 191,
457
Bagnulo S. et al. 2001, The Messenger 104, 32
Bagnulo S. et al. 2006, A&A 450, 777
Cropper M. 1990, Space Sci. Rev. 54, 195
Landstreet J. D. and Angel J. R. P. 1971, ApJ 165,
L67
Landstreet J. D. 1980, AJ 85, 611
Rana V. R. et al. 2005, ApJ 625, 351
Schmidt G. D., Liebert J. and Stockman H. S. 1995,
ApJ 441, 414
Staubert R. et al. 2003, A&A 407, 987
West S. C. 1989, ApJ 345, 511

ADS BibCode:
2007Msngr.129...18I
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Ihle, G.; Montano, N.; Tamai, R.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
After rotating for more than 30 years, the dome support wheels for the ESO 3.6-m telescope started to degrade, resulting in a shutdown in October 2006. The engineering process of reshaping the track and gradual replacement of the supporting wheels is described. The rotation of the dome is now returning to its original efficiency.

ADS BibCode:
2007Msngr.129...21K
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Kerber, F.; Saitta, F.; Bristow, P.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
We have studied the properties of wavelength calibration sources for the near- IR arm of X-shooter. In a novel approach we are combining laboratory measurements from a Fourier Transform Spectrometer (FTS), and literature data, with simulated data derived from a physi- cal model of X-shooter. The sources studied are pen ray lamps filled with the noble gases Ne, Ar, Kr, and Xe and Th-Ar hollow cathode lamps. As a product we provide a quantitative order by order analysis of the expected properties of the calibration lamps during X-shooter operations. Based on these we give recommendations for the selection of the best combination of lamps. The combination of laboratory measurements and instrument modeling provides a powerful tool for future instrument development.
References:
Engleman R. Jr., Hinkle K. H. and Wallace L. 2003,
JQSRT 78
Hinkle K. H. et al. 2001, PASP 113, 548
Kerber F. et al. 2007, in “The Future of Photometric,
Spectrophotometric and Polarimetric Standardization”,
ed. C. Sterken, ASP Conf. Ser. 364, 461
Palmer B. A. and Engleman R. 1983, LANL 9615
Saloman E. B. 2004, J. Phys. Chem. Ref. Data 33,
765
Sansonetti C. J. and Greene M. M. 2007,
Phys. Scr. 75, 577
Sansonetti C. J., Blackwell M. M. and Saloman E. B.
2004, J. Res. Natl. Inst. Stand. Technol. 109, 371
Whaling W., Anderson W. H. C. and Carle M. T.
2002, J. Res. Natl. Inst. Stand. Technol. 107, 149

ADS BibCode:
2007Msngr.129...24A
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Araujo-Hauck, Constanza; Pasquini, Luca; Manescau, Antonio; Udem, Thomas; Hänsch, Theodor W.; Holzwarth, Ronald; Sizmann, Andreas; Dekker, Hans; D'Odorico, Sandro; Murphy, Michael T.
AA(ESO) AB(ESO) AC(ESO) AD(Max-Planck Institute for Quantum Optics, Garching, Germany) AE(Max-Planck Institute for Quantum Optics, Garching, Germany) AF(Max-Planck Institute for Quantum Optics, Garching, Germany & Menlo Systems GmbH, Martinsried, Germany) AG(Menlo Systems GmbH, Martinsried, Germany) AH(ESO) AI(ESO) AJ(Institute of Astronomy, University of Cambridge, United Kingdom)
Abstract:
A new technique for precise wavelength calibration of high-resolution spectrographs using frequency combs has recently been proposed. After introducing the basic concepts and advantages of this technique, we describe the ongoing development between ESO and the Max-Planck Institute for Quantum Optics for a novel wavelength calibration system that aims, within three years, to construct a laboratory demonstrator.
References:
Araujo-Hauck C. et al. 2007, in Proceedings of
the 2007 ESO Instrument Calibration Workshop,
ESO Astrophysics Symposia Series, in press
Grazian A. et al. 2007, A&A, submitted
Hoogland S. et al. 2005, IEEE Photonics Technology
Letters 17, 267
Liske J. et al. 2007, MNRAS, submitted
Lovis C. et al. 2006, Proc. SPIE 6269, 62690P
Murphy M. T. et al. 2007, MNRAS, submitted,
astro-ph/0703622
Pasquini L. et al. (CODEX Team) 2006, in “The scientific
requirements for ELTs”, Proceedings of IAU
Symposium 232, eds. P. Whitelock, M. Dennefeld,
and B. Leibundgut, Cambridge, 193
Santos N., Pasquini L. and Romaniello M. (eds.)
2007, “Precision Spectroscopy in Astrophysics”,
Proceedings of the Aveiro Conference, Springer,
in press
Udem T., Holzwarth R. and Hänsch T. W. 2002,
Nature 416, 233

ADS BibCode:
2007Msngr.129...27W
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Wicenec, A.; Knudstrup, J.
AA(ESO) AB(ESO)
Abstract:
Considerations of the technical feasibility and the cost implications of a disk-based archiving system to store digital observations coming from the ever growing suite of ESO telescopes and instruments began in 2000. The so-called Next Generation Archiving System (NGAS) started archiving data in a prototype system in 2001. Now the second generation of NGAS hardware has been installed in the new ESO data centre and about 98% of all data since 1998 have been migrated onto disks hosted on NGAS computers. In addition all data currently produced by ESO instruments is directly archived onto NGAS hosts both in La Silla and Paranal. Currently the ESO archive keeps about 125 TB of data online and the system has been scaled up to cope with the next data wave coming from VISTA and OmegaCAM.
References:
More detailed information on NGAS is available at
http://www.eso.org/projetcs/ngas
Dusseault L. (ed.) 2007, RFC 4918, http://www.ietf.
org/rfc/rfc4918.txt
Graham M. et al. 2007, VOSpace service specification,
Version 1.01, http://www.ivoa.net/Documents/
latest/VOSpace.html
Harrison P. et al. 2006, in “Astronomical Data Analysis
Software and Systems XV”, ASP Conference
Series
351, 402
Schroeder B. and Gibson G. A. 2007, presented at
the 5th USENIX conference, http://www.cs.cmu.
edu/bianca/fast07.pdf
Wicenec A. and Pirenne B. 2000, The Next Generation
of Science Archive Storage, http://www.eso.
org/projects/ngas/ngas-whitepaper.pdf
Wicenec A., Knudstrup J. and Johnston S. 2001,
The Messenger 106, 11

ADS BibCode:
2007Msngr.129...33S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Spiering, C.
AA(DESY – Deutsches Elektronen-Synchrotron)
Abstract:
Astroparticle physics has evolved as an interdisciplinary field at the intersec- tion of particle physics, astronomy and cosmology. Over the last two decades, it has moved from infancy to technological maturity and is now envisaging projects on the 100 M€ scale. This price tag requires international coordination, cooperation and convergence to a few flagship projects. The Roadmap Committee of ApPEC (Astroparticle Physics European Coordination) has recently released a roadmap covering the next ten years. ApPEC is a corporation of European funding agencies promoting astroparticle physics.
References:
Aharonian F. 2007, Science 315, 70
Baudis L. 2005, astro-ph/0511805
de Bellefon A. et al. 2006, hep-ex/0607026
Halzen F. 2007, Science 315, 66
Hong J., Rowan S. and Sathyaprkash B. 2005,
gr-qc/0501007
Olinto A. 2007, Science 135, 68
Sadoulet B. 2007, Science 315, 61
Watson A. 2005, astro-ph/0511800
Voelk H. 2006, astro-ph/0603501
Vogl P. 2006, hep-ph/0611243
Waxman E. 2007, Science 315, 63

ADS BibCode:
2007Msngr.129...38F
Section:
Astronomical Science
Author(s)/Affiliation(s):
Fox, A. J.; Petitjean, P.; Ledoux, C.; Srianand, R.
AA(Institut d'Astrophysique de Paris, Université Pierre et Marie Curie, Paris, France) AB(Institut d'Astrophysique de Paris, Université Pierre et Marie Curie, Paris, France & LERMA, Observatoire de Paris, France) AC(ESO) AD(Inter-University Centre for Astronomy and Astrophysics – IUCAA, Ganesh Khind, Pune, India)
Abstract:
The neutral discs of high-redshift galaxies give rise to the Damped Lyman-a (DLA) systems seen in the spectra of background quasars. We show for the first time that a hot phase of gas is present in DLAs, observable in the absorption lines of five-times-ionised oxygen. This plasma phase, which could harbour a considerable fraction of all the metals produced by star formation at these epochs, can be explained as the feedback from star formation taking place in the neutral discs.
References:
Bouché N. et al. 2007, MNRAS 378, 525
Bouwens R. J. et al. 2004, ApJ 616, L79
Davé R. et al. 2001, ApJ 552, 473
Fox A. et al. 2007a, A&A 465, 171
Fox A. et al. 2007b, A&A, in press,
astro-ph/0707.4065
Gnat O. and Sternberg A. 2007, ApJS 168, 213
Ledoux C. et al. 2006, A&A 457, 71
Prochaska J. X. et al. 2005, ApJ 635, 123
Rauch M. 1998, ARA&A 36, 267
Wolfe A. M. et al. 2005, ARA&A 43, 861

ADS BibCode:
2007Msngr.129...42F
Section:
Astronomical Science
Author(s)/Affiliation(s):
Falomo, R.; Treves, A.
AA(INAF – Osservatorio Astronomico di Padova, Italy) AB(Università dell'Insubria, Como, Italy)
Abstract:
BL Lacertae objects are active galactic nuclei dominated by non-thermal continuum emission and characterised by absence or extreme weakness of emission lines. These properties in several cases hinder the determination of their distance and thus the assessment of the properties of the class. High signal-to-noise optical spectra of these sources obtained with the VLT help to overcome these difficulties and allow one to obtain new redshifts and set stringent limits on the distance for pure lineless objects.
References:
Aharonian F. et al. 2006, A&A 448, L19
Albert J. et al. 2007, ApJ 654, L119
Blandford R. D. and Rees M. J. 1978, in Pittsburgh
Conference on BL Lac Objects, ed. A. M. Wolfe,
University Pittsburgh Press, 328
Falomo R. and Treves A. 1990, PASP 102, 1120
Sbarufatti B. et al. 2005a, AJ 129, 599
Sbarufatti B., Treves A. and Falomo R. 2005b,
ApJ 635, 173
Sbarufatti B. et al. 2006, AJ 132, 1
Scarpa R. et al. 2000, ApJ 532, 740
Urry C. M. et al. 2000, ApJ 532, 816

ADS BibCode:
2007Msngr.129...45T
Section:
Astronomical Science
Author(s)/Affiliation(s):
Treister, E.; Gawiser, E.; van Dokkum, P.; Lira, P.; Urry, M.; The Musyc Collaboration
AA(ESO) AB(Rutgers, State University of New Jersey, Piscataway, New Jersey, USA) AC(Yale University, New Haven, Connecticut, USA) AD(Universidad de Chile, Santiago de Chile, Chile) AE(Yale University, New Haven, Connecticut, USA) AF(The Musyc Collaboration)
Abstract:
We present results from the MUSYC survey, which images a total of 1.2 square degrees spread over four fields in UBVRIz;K down to the spectroscopic limit, R ~ 25, K ~ 22 (AB). A significant fraction of the survey area has also been imaged by Chandra, XMM, GALEX, HST-ACS, near-infrared (JH), Spitzer-IRAC+MIPS, VLA, and ATCA. The main goals of this survey include the study of galaxy formation and evolution, Active Galactic Nuclei (AGN) and Galactic structure.
References:
Gawiser E. et al. 2006a, ApJS 162, 1
Gawiser E. et al. 2006b, ApJ 642, L13
Kriek M. et al. 2006, ApJ 649, L71
Kriek M. et al. 2007, ApJ, in press, astro-ph/0611724
Marchesini D. et al. 2007, ApJ 656, 45
Quadri R. et al. 2007a, ApJ 654, 138
Quadri R. et al. 2007b, AJ, in press,
astro-ph/0612612
Van Dokkum P. G. et al. 2006, ApJ 638, L59
Virani S. et al. 2006, AJ 131, 2373
Webb T. M. A. et al. 2006, ApJ 636, L17

ADS BibCode:
2007Msngr.129...49H
Section:
Astronomical Science
Author(s)/Affiliation(s):
Hilker, M.; Baumgardt, H.; Infante, L.; Drinkwater, M.; Evstigneeva, E.; Gregg, M.
AA(ESO) AB(Argelander-Institut für Astronomie, Universität Bonn, Germany) AC(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago de Chile, Chile) AD(Department of Physics, University of Queensland, Brisbane, Australia) AE(Department of Physics, University of Queensland, Brisbane, Australia) AF(Department of Physics, University of California, Davis, California, USA)
Abstract:
High-resolution spectra from the Ultraviolet and Visual Echelle Spectrograph (UVES) were used to derive internal velocity dispersions of Ultracompact Dwarf galaxies (UCDs) in the Fornax cluster of galaxies. The velocity dispersions, together with highly spatially resolved luminosity profiles from Hubble Space Telescope imaging (ACS camera), allowed us to derive the dynamical masses of the UCDs. We show that the mass-to-light ratios of UCDs in Fornax are consistent with those expected for pure stellar populations. No dark matter contribution is needed. Thus, these UCDs seem to be the result of star-cluster formation processes within galaxies, rather than being compact dwarf galaxies formed in dark-matter halos.
References:
Bekki K. et al. 2003, MNRAS 344, 399
Drinkwater M. J. et al. 2003, Nature 423, 519
Evstigneeva E. A. et al. 2007, AJ 133, 1722
Fellhauer M. and Kroupa P. 2006, MNRAS 367, 1577
Hilker M. et al. 2007, A&A 463, 119
Hilker M. et al. 1999, A&AS 134, 75
Maraston C. 2005, MNRAS 362, 799
Mieske S., Hilker M. and Infante L. 2004, A&A 418,
445
Mieske S. et al. 2006, AJ 131, 2442
Phillipps S. et al. 2001, ApJ 560, 201
van der Marel R. P. and Franx M. 1993, ApJ 407, 525

ADS BibCode:
2007Msngr.129...53C
Section:
Astronomical Science
Author(s)/Affiliation(s):
Crowther, Paul A.; Hadfield, Lucy J.
AA(University of Sheffield, United Kingdom) AB(University of Sheffield, United Kingdom)
Abstract:
Wolf-Rayet (WR) stars are the chemical-ly evolved descendents of O stars, such that they trace massive star formation. Here we present results of recent VLT/FORS surveys of WR stars in near- by spiral and irregular galaxies and consider individual WR stars as progenitors of Type Ib/c core-collapse supernovae. Young massive clusters hosting large WR populations may be used as templates for high-redshift Lyman break galaxies.
References:
Chandar R. et al. 2004, ApJ 604, 153
Crockett R. M. et al. 2007, MNRAS, in press,
arXiv:0706.0500
Crowther P. A. 2007, ARA&A 45, 177
Crowther P. A. and Hadfield L. J. 2006, A&A 449,
711
Crowther P. A. et al. 2002, A&A 392, 653
Crowther P. A. et al. 2007, A&A 469, L31
Eldridge J. and Vink J. 2006, A&A 452, 295
Hadfield L. J. and Crowther P. A. 2006, MNRAS 368,
1822
Hadfield L. J. and Crowther P. A. 2007, MNRAS,
in press, arXiv:0708.2039
Hadfield L. J. et al. 2005, A&A 439, 265
Hammer F. et al. 2006, A&A 454, 103
Hjorth J. et al. 2003, Nature 423, 847
Kennicutt R. C. 1998, ARA&A 36, 189
MacFadyen A. and Woosley S. 1999, ApJ 524, 262
Mokiem M. R. et al. 2007, A&A, in press,
arXiv:0708.2042
Schild H. et al. 2003, A&A 397, 859
Shapley A. et al. 2003, ApJ 347, 127
Smartt S. et al. 2004, Sci 303, 499
Testor G. and Schild H. 1993, The Messenger 72, 31
Vazquez G. A. et al. 2007, ApJ 663, 995

ADS BibCode:
2007Msngr.129...58P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Protopapa, S.; Herbst, T.; Böhnhardt, H.
AA(Max-Planck Institute for Solar System Research, Lindau, Germany) AB(Max-Planck Institute for Astronomy, Heidelberg, Germany) AC(Max-Planck Institute for Solar System Research, Lindau, Germany)
Abstract:
We present new reflectance spectra of Pluto and Triton taken with the ESO adaptive optics instrument NACO at the VLT and covering the wavelength range 1 5 µm. Apart from known and expected absorption bands from methane ice, our data reveal new absorption bands centred around 4.0 µm and 4.6 µm never detected before. The latter absorption could be related to the presence of CO ice at the body surfaces. Charon's spectrum is also measured in the wavelength range 1 4 µm, for the first time simultaneously with, but isolated from, that of Pluto. The non-detection of Pluto's moonlets (unknown at the time of observation) in acquisition images of Pluto-Charon provides a lower limit of 18.8 mag for the K-band brightness of Hydra and Nix.
References:
Brown M. E. and Calvin W. M. 2000, Science 287,
107
Buie M. W. and Grundy W. M. 2000, Icarus 148, 324
Cruikshank D. P. et al. 1993, Science 261, 742
Douté S. et al. 1999, Icarus 142, 421
Grundy W. M., Buie M. W. and Spencer J. R. 2002,
AJ 124, 2273
Olkin C. B. et al. 2007, AJ 133, 420
Owen T. C. et al. 1993, Science 261, 745
Palumbo M. E. and Strazzulla G. 1993, A&A 269, 568
Quirico E. et al. 1999, Icarus 139, 159
Weaver H. A. et al. 2006, Nature 439, 943

ADS BibCode:
2007Msngr.129...62A
Section:
Astronomical News
Author(s)/Affiliation(s):
Avila, G.; Burwitz, V.; Guirao, C.; Rodriguez, J.; Shida, R.; Baade, D.
AA(ESO) AB(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AC(ESO) AD(ESO) AE(ESO & ST-ECF) AF(ESO)
Abstract:
BACHES is a low-cost, light-weight echelle spectrograph suitable for observations of bright stars coupled with small telescopes up to 35 cm (14?) in diameter. The resolving power reaches 19000 in a continuous spectral range between 390 and 750 nm. The throughput of the instrument including the telescope and detector is 11% peak at 500 nm. With this efficiency spectra of stars of visual magnitude 5 can be obtained in 15 min exposure with a S/N of 50. One of the goals of the instrument is to monitor the spectral variability of Balmer emission lines in Be stars.
References:
Avila G. et al. 1999, Proc. IAU Coll. 173, 235
Kaye T. et al. 2006, J. Br. Astron. Assoc. 116, 2
Pollmann E. 2007, IAU Inf. Bull. Var. Stars, 5778
For a list of spectroscopy amateur web sites see
for example: http://www.astroman.fsnet.co.uk/
players.htm

ADS BibCode:
2007Msngr.129...64F
Section:
Astronomical News
Author(s)/Affiliation(s):
Fosbury, Robert A. E.; De Breuck, Carlos; Mainieri, Vincenzo; Robertson, Gordon; Vernet, Joël
AA(ST-ECF, ESO) AB(ESO) AC(ESO) AD(ESO & University of Sydney, Australia) AE(ESO)
Abstract:
While the radio-loud, obscured quasars (the radio galaxies) have been known and studied for decades, new and sensitive X-ray and mid-infrared surveys are now beginning to reveal large numbers of their radio-quiet counterparts beyond the local Universe. Consequent- ly, we are approaching the compilation of a relatively complete census of AGN of all types covering a large fraction of cosmic time. This is revealing a remarkably intimate connection between the supermassive black hole and its host galaxy. The workshop reported here was designed to explore the results of these rapid observational developments and the nature of the relationships between the stellar and AGN components.
References:
Baldwin J., Phillips M. and Terlevich R. 1981,
PASP 93, 5
Kauffmann G. et al. 2003, MNRAS 341, 54
Kewley L. et al. 2002, ApJS 142, 35
Kewley L. et al. 2006, MNRAS 372, 961
Spoon H. et al. 2006, in “Astrochemistry: Recent
Successes and Current Challenges”, eds. D. C.
Lis, G. A. Blake and E. Herbst, IAU Symposium
231, 281
Spoon H. et al. 2007, ApJ 654, L49
Conference web site: http://www.eso.org/agnii2007

ADS BibCode:
2007Msngr.129...69K
Section:
Astronomical News
Author(s)/Affiliation(s):
Kissler-Patig, M.; Wilson, T.; Bastian, N.; D'Antona, F.; de Grijs, R.; Froebrich, D.; Galliano, E.; Grosbøl, P.; Johnson, K.; Keto, E.; Klessen, R.; Megeath, T.; Rejkuba, M.; Steinacker, J.; Zinnecker, H.
AA(ESO) AB(ESO) AC(University College London, United Kingdom) AD(Osservatorio di Roma, Italy) AE(University of Sheffield, United Kingdom) AF(University of Kent, United Kingdom) AG(Universidad de Chile, Santiago de Chile, Chile) AH(ESO) AI(University of Virginia, Charlottesville, Virginia, USA) AJ(Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts, USA) AK(Universität Heidelberg, Germany) AL(University of Toledo, Ohio, USA) AM(ESO) AN(Max-Planck Institute for Astronomy, Heidelberg, Germany) AO(Astrophysikalisches Institut Potsdam, Germany)
Abstract:
The Workshop “12 Questions on Star and Massive Star Cluster Formation” was held in Garching from 3 to 6 July 2007. The programme was set up to allow long (and fruitful) discussions around several questions connecting the formation of stars and star clusters. Here we summarise some of the discussions, and encourage interest- ed readers to download the contributions from http://www.eso.org/star07.

ADS BibCode:
2007Msngr.129...72.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
The workshop will take place a few weeks after the UKIRT Infrared Deep Sky Survey (UKIDSS) large Third Data Release (DR3). The purpose of the workshop is to provide a forum, bringing together European astronomers working on (or planning to work on) UKIDSS data, to hear about science being undertaken with UKIDSS, and to share knowledge gained in working with the data and ideas for exploiting the archive efficiently, in an informal atmosphere. The emphasis will be on work in progress. The workshop will include science and technical talks, and tutorials, as well as a summary of the current status of the surveys, and an opportunity to discuss the future direction.

ADS BibCode:
2007Msngr.129...73.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2007Msngr.129...73P
Section:
Astronomical News
Author(s)/Affiliation(s):
Primas, F.; Nass, P.; Hainaut, O.; Sterzik, M.
AA(ESO) AB(ESO) AC(ESO) AD(ESO)
Abstract:
As stated in the ESO Call for Proposals, targets and constraints requested at time of proposal submission (i.e. at Phase 1) are binding, because once the proposals have been evaluated by the Observing Proposal Committee, the requested targets and constraints become one of the major inputs to finalise and optimise the scheduling of the telescopes. However, part of the success of an observatory comes also from the ability to balance operational efficiency (hence rules and procedures) and scientific return. In other words, target and/or instrument set-up changes are allowed also after Phase 1, but only after they have been carefully scrutinised. Their approval is subject to the following conditions:

ADS BibCode:
2007Msngr.129...74.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
Nearly a decade ago astronomers from two competing teams announced that they had found evidence for an accelerated cosmic expansion. The Gruber Prize in Cosmology 2007 honours this achievement and has been awarded to two groups: the Supernova Cosmology Project team, led by Saul Perlmutter (Lawrence Berkeley Laboratory), and the High-z Supernova Search Team, led by Brian Schmidt (Australian National University). Their results were based on the observations of distant Type Ia supernovae and were obtained with the major telescopes at the time (Riess et al. 1998, AJ 116, 1009; Perlmutter et al. 1999, ApJ 517, 565). Both teams used the 3.6-m telescope and the NTT to contribute photometry and spectroscopic classifications of the supernovae. Four people at ESO were directly involved in the two teams and are recognised as co-recipients of the Gruber Prize. Isobel Hook (now at Oxford University) and Chris Lidman (ESO Chile) were ESO Fellows when they contributed to the work of the Super- nova Cosmology Project, while Jason Spyromilio and Bruno Leibundgut (both ESO Garching) participated in the High-z Supernova Search Team.

ADS BibCode:
2007Msngr.129...74H
Section:
Astronomical News
Author(s)/Affiliation(s):
Hook, R.; The Scisoft Team
AA(ST-ECF, ESO)
Abstract:
The Scisoft bundle is a collection of astronomical software intended mostly for ESO users but which is also distributed to other interested parties. It includes most of the packages needed by working observational astronomers, with emphasis on those widely used for handling optical and infrared data sets. Scisoft is installed on almost all the scientific computers running Linux at ESO Garching and widely at the ESO sites in Chile. More complete details can be found on the Scisoft web pages at http:// www.eso.org/scisoft.

ADS BibCode:
2007Msngr.129...75.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
Steffen Mieske; Julia Scharwächter

ADS BibCode:
2007Msngr.129...76.
Author(s)/Affiliation(s):
ESO
AA(ESO)