Messenger No. 162 ( 2015)

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Telescopes and Instrumentation

2-8 (PDF)
M. Sterzik et al.
The Scientific Return of VLT Programmes

ADS BibCode:
2015Msngr.162....2S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Sterzik, M.; Dumas, C.; Grothkopf, U.; Kaufer, A.; Leibundgut, B.; Marteau, S.; Meakins, S.; Patat, F.; Primas, F.; Rejkuba, M.; Romaniello, M.; Stoehr, F.; Tacconi-Garman, L.; Vera, I.
AA(ESO) AB(TMT Observatory Corporation, Pasadena, USA) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO) AJ(ESO) AK(ESO) AL(ESO) AM(ESO) AN(ESO)
Abstract:
An in-depth analysis of the publications from 8414 distinct scheduled VLT observing programmes between April 1999 and March 2015 (Periods 63 to 94) is presented. The productivity by mode (Visitor or Service Mode) and type (Normal and Large, Guaranteed Time, Target of Opportunity, Director’s Discretionary Time) are examined through their publication records. We investigate how Service Mode rank classes impact the scientific return. Several results derive from this study: Large Programmes result in the highest productivity, whereas only about half of all scheduled observing programmes produce a refereed publication. Programmes that result in a publication yield on average two refereed papers. B rank class Service Mode Programmes appear to be slightly less productive. Follow-up studies will investigate in more detail the parameters that influence the productivity of the Observatory.
References:
Grothkopf, U. et al. 2007, The Messenger, 128, 62; Grothkopf, U. & Meakins, S. 2012, The Messenger, 147, 41; Primas, F. et al. 2014, The Messenger, 158, 8; Primas, F. et al. 2015, The Messenger, 161, 6; Silva, D. 2001, The Messenger, 105, 18
9-15 (PDF)
G. Lo Curto et al.
HARPS Gets New Fibres After 12 Years of Operations

ADS BibCode:
2015Msngr.162....9C
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Lo Curto, G.; Pepe, F.; Avila, G.; Boffin, H.; Bovay, S.; Chazelas, B.; Coffinet, A.; Fleury, M.; Hughes, I.; Lovis, C.; Maire, C.; Manescau, A.; Pasquini, L.; Rihs, S.; Sinclaire, P.; Udry, S.
AA(ESO) AB(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AC(ESO) AD(ESO) AE(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AF(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AG(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AH(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AI(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AJ(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AK(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AL(ESO) AM(ESO) AN(Université de Genève, Département d’Astronomie, Versoix, Switzerland) AO(ESO) AP(Université de Genève, Département d’Astronomie, Versoix, Switzerland)
Abstract:
In June 2015, as part of the HARPS Upgrade 2 Agreement signed in 2013 between ESO and Geneva University, a new set of non-circular (octagonal) optical fibres, with improved mode-scrambling capabilities, has been installed. The motivation for the exchange of the fibre link and the results from the commissioning tests are presented. The throughput of the instrument (+40% at 550 nm), its illumination uniformity and stability, and thus its radial velocity (RV) stability, are significantly improved. An RV offset correlated with the width of the stellar lines is found with the new fibres from observations of RV standards. As a result of this major upgrade, and once the laser frequency comb that is already assembled in the HARPS room is fully functional, we expect to reach an RV precision better than 0.5 m s–1 on bright stars.
References:
Baranne, A. et al. 1996, A&AS, 119, 373; Bouchy, F. et al. 2013, A&A, 549, A49; Chazelas, B. et al. 2010, Proc. SPIE, 7739E, 134; Chazelas, B. et al. 2012, Proc. SPIE, 8450E, 13; Cosentino, R. et al. 2012, Proc. SPIE, 8446E, 1V Lo Curto, G. et al. 2012, The Messenger, 149, 2; Lo Curto, G. et al. 2010, Proc. SPIE, 7735E, 33; Mayor, M. et al. 2003, The Messenger, 114, 20; Pepe, F. et al. 2002, A&A, 388, 682; Pepe, F. et al. 2002, The Messenger, 110, 9; Perruchot, S. et al. 2011, Proc. SPIE, 8151E, 37
16-18 (PDF)
J. Woillez et al.
VLTI: First Light for the Second Generation

ADS BibCode:
2015Msngr.162...16W
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Woillez, J.; Gonté, F.; Abad, J. A.; Abadie, S.; Abuter, R.; Accardo, M.; Acuña, M.; Alonso, J.; Andolfato, L.; Avila, G.; Barriga, P. J.; Beltran, J.; Berger, J.-P.; Bollados, C.; Bourget, P.; Brast, R.; Bristow, P.; Caniguante, L.; Castillo, R.; Conzelmann, R.; Cortes, A.; Delplancke, F.; Dell Valle, D.; Derie, F.; Diaz, A.; Donoso, R.; Duhoux, Ph.; Dupuy, C.; Elao, C.; Egner, S.; Fuenteseca, E.; Fernandez, R.; Gaytan, D.; Glindemann, A.; Gonzales, J.; Guisard, S.; Hagenauer, P.; Haimerl, A.; Heinz, V.; Henriquez, J. P.; van der Heyden, P.; Hubin, N.; Huerta, R.; Jochum, L.; Kirchbauer, J.-P.; Leiva, A.; Lévêque, S.; Lizon, J.-P.; Luco, F.; Mardones, P.; Mellado, A.; Mérand, A.; Osorio, J.; Ott, J.; Pallanca, L.; Pavez, M.; Pasquini, L.; Percheron, I.; Pirard, J.-F.; Phan, D. T.; Pineda, J. C.; Pino, A.; Poupar, S.; Ramírez, A.; Reinero, C.; Riquelme, M.; Romero, J.; Rivinius, Th.; Rojas, C.; Rozas, F.; Salgado, F.; Schöller, M.; Schuhler, N.; Siclari, W.; Stephan, C.; Tamblay, R.; Tapia, M.; Tristram, K.; Valdes, G.; de Wit, W.-J.; Wright, A.; Zins, G.
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(ESO) AQ(ESO) AR(ESO) AS(ESO) AT(ESO) AU(ESO) AV(ESO) AW(ESO) AX(ESO) AY(ESO) AZ(ESO) BA(ESO) BB(ESO) BC(ESO) BD(ESO) BE(ESO) BF(redlogix, Gilching, Germany) BG(ESO) BH(ESO) BI(ESO) BJ(ESO) BK(ESO) BL(ESO) BM(ESO) BN(ESO) BO(ESO) BP(ESO) BQ(ESO) BR(ESO) BS(ESO) BT(ESO) BU(ESO) BV(ESO) BW(ESO) BX(ESO) BY(ESO) BZ(ESO) CA(ESO) CB(redlogix, Gilching, Germany) CC(ESO) CD(ESO) CE(ESO) CF(ESO) CG(ESO) CH(ESO) CI(ESO) CJ(ESO) CK(ESO) CL(ESO) CM(ESO) CN(ESO) CO(MT Mecatronica SpA, Chile) CP(ESO) CQ(ESO) CR(ESO) CS(ESO) CT(ESO) CU(ESO) CV(ESO) CW(ESO) CX(ESO) CY(ESO) CZ(ESO) DA(ESO) DB(ESO) DC(ESO) DD(ESO)
Abstract:
The Very Large Telescope Interferometer (VLTI) stopped operation on 4 March 2015 with the objective of upgrading its infrastructure in preparation for the second generation VLTI instruments GRAVITY and MATISSE. A brief account of the eight bustling months it took our interferometer to metamorphose into its second generation, under the supervision of the VLTI Facility Project, is presented.
References:
Arsenault, R. et al. 2003, The Messenger, 112, 7; Dorn, R. et al. 2014, The Messenger, 156, 12; Eisenhauer, F. et al. 2011, The Messenger, 143, 16; Lopez, B. et al. 2014, The Messenger, 157, 5; Pepe, F. et al. 2013, The Messenger, 153, 6; Van Belle, G. T. et al. 2008, The Messenger, 134, 6; Zins, G. et al. 2011, The Messenger, 146, 12
19-23 (PDF)
P. Amico et al.
The First Component of the Adaptive Optics Facility Enters Operations: The Laser Traffic Control System on Paranal

ADS BibCode:
2015Msngr.162...19A
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Amico, P.; Santos, P.; Summers, D.; Duhoux, Ph.; Arsenault, R.; Bierwirth, Th.; Kuntschner, H.; Madec, P.-Y.; Prümm, M.; Rejkuba, M.
AA(ESO) AB(ESO) AC(Large Binocular Telescope Observatory, Tucson, Arizona, USA) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO; Informate) AJ(ESO)
Abstract:
The Laser Traffic Control System (LTCS) entered routine operations on 1 October 2015 at the Paranal Observatory as the first component of the Adaptive Optics Facility (AOF). LTCS allows the night operators to plan and execute the observations without having to worry about possible collisions between the AOF’s powerful laser beams and other telescopes with laser-sensitive instruments. LTCS provides observers with real-time information about ongoing collisions, predictive information for possible collisions and priority resolution between telescope pairs, where at least one telescope is operating a laser. LTCS is now deployed and embedded in the observatory’s operational environment, supporting high configurability of telescopes and instruments, right-of-way priority rules and interfacing with ESO’s observing tools for Service and Visitor Mode observations.
References:
Amico, P. et al. 2010, SPIE Proc., 7737-10; Lewis, S. et al. 2014, The Messenger, 155, 6; Summers, D. et al. 2003, SPIE Proc., 4839-57; Summers, D. et al. 2006, SPIE Proc., 6272; Summers, D. et al. 2012, SPIE Proc., 88474S-1, 2012
24-29 (PDF)
E. Hatziminaoglou et al.
The European ALMA Regional Centre Network: A Geographically Distributed User Support Model

ADS BibCode:
2015Msngr.162...24H
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Hatziminaoglou, E.; Zwaan, M.; Andreani, P.; Barta, M.; Bertoldi, F.; Brand, J.; Gueth, F.; Hogerheijde, M.; Maercker, M.; Massardi, M.; Muehle, S.; Muxlow, Th.; Richards, A.; Schilke, P.; Tilanus, R.; Vlemmings, W.; Afonso, J.; Messias, H.
AA(ESO) AB(ESO) AC(ESO) AD(Astronomical Institute of the Czech Academy of Sciences, Ondřejov, Czech Republic) AE(Argelander-Institut für Astronomie, University of Bonn, Germany) AF(INAF–Osservatorio di Radioastronomia, Bologna, Italy) AG(Institut de Radio Astronomie Millimétrique (IRAM), Grenoble, France) AH(University of Leiden, the Netherlands) AI(Onsala Space Observatory, Chalmers University of Technology, Sweden) AJ(INAF–Osservatorio di Radioastronomia, Bologna, Italy) AK(Argelander-Institut für Astronomie, University of Bonn, Germany) AL(Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester, United Kingdom) AM(Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester, United Kingdom) AN(I. Physikalisches Institut, Universität zu Köln, Germany) AO(University of Leiden, the Netherlands) AP(Onsala Space Observatory, Chalmers University of Technology, Sweden) AQ(Institute for Astrophysics and Space Science, Lisbon, Portugal) AR(Institute for Astrophysics and Space Science, Lisbon, Portugal)
Abstract:
In recent years there has been a paradigm shift from centralised to geographically distributed resources. Individual entities are no longer able to host or afford the necessary expertise in-house, and, as a consequence, society increasingly relies on widespread collaborations. Although such collaborations are now the norm for scientific projects, more technical structures providing support to a distributed scientific community without direct financial or other material benefits are scarce. The network of European ALMA Regional Centre (ARC) nodes is an example of such an internationally distributed user support network. It is an organised effort to provide the European ALMA user community with uniform expert support to enable optimal usage and scientific output of the ALMA facility. The network model for the European ARC nodes is described in terms of its organisation, communication strategies and user support.
References:
Andreani, P. & Zwaan, M. 2006, The Messenger, 126, 43; 2009, The virtual organisation, Economist, online edition, 23 November Huang, L. 2012, Mitigating the negative effects of geographically dispersed teams, (Irvine: University of California) Shaver, P. & van Dishoeck, E. 2002, The Messenger, 110, 44; Travica, B. 1997, in Gupta, J. N. D., Association for Information Systems, Proc. American Conference on Information Systems, Indianapolis, 417
30-35 (PDF)
F. Stoehr et al.
ALMA Cycle 0 Publication Statistics

ADS BibCode:
2015Msngr.162...30S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Stoehr, F.; Grothkopf, U.; Meakins, S.; Bishop, M.; Uchida, A.; Testi, L.; Iono, D.; Tatematsu, K.; Wootten, A.
AA(ESO) AB(ESO) AC(ESO) AD(National Radio Astronomy Observatory, Charlottesville, USA) AE(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan) AF(ESO) AG(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan) AH(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan) AI(National Radio Astronomy Observatory, Charlottesville, USA)
Abstract:
The scientific impact of a facility is the most important measure of its success. Monitoring and analysing the scientific return can help to modify and optimise operations and adapt to the changing needs of scientific research. The methodology that we have developed to monitor the scientific productivity of the ALMA Observatory, as well as the first results, are described. We focus on the outcome of the first cycle (Cycle 0) of ALMA Early Science operations. Despite the fact that only two years have passed since the completion of Cycle 0 and operations have already changed substantially, this analysis confirms the effectiveness of the underlying concepts. We find that ALMA is fulfilling its promise as a transformational facility for the observation of the Universe in the submillimetre.
References:
Meakins, S. et al. 2014, Proc. SPIE, 9149, 914926; Ness, J. U. et al. 2014, AN, 335, 210; Rots, A. H., Winkelman, S. L. & Becker, G. E. 2012, PASP, 124, 391

Astronomical Science

37-41 (PDF)
P. M. Weilbacher et al.
The Central Orion Nebula (M42) as seen by MUSE

ADS BibCode:
2015Msngr.162...37W
Section:
Astronomical Science
Author(s)/Affiliation(s):
Weilbacher, P. M.; Monreal-Ibero, A.; Mc Leod, A. F.; Ginsburg, A.; Kollatschny, W.; Sandin, C.; Wendt, M.; Wisotzki, L.; Bacon, R.
AA(Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany) AB(GEPI, Observatoire de Paris, PSL Research University, CNRS, Université Paris Diderot, Sorbonne Paris Cité, Meudon, France) AC(ESO) AD(ESO) AE(Institut für Astrophysik, Universität Göttingen, Germany) AF(Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany) AG(Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany; Institut für Physik und Astronomie, Universität Potsdam, Germany) AH(Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany) AI(CRAL, Observatoire de Lyon, Saint-Genis Laval, France)
Abstract:
The MUSE (Multi Unit Spectroscopic Explorer) instrument, an optical wide-field integral field spectrograph at the Very Large Telescope, has been operating successfully for about a year. Among the impressive sets of data collected during commissioning was a mosaic of the central Orion Nebula (M42), known as the Huygens region. During the past year, we have made the data ready for scientific use, and they are now publicly available to the community. An overview of the observations and their reduction, as well as two possible scientific applications, are presented.
References:
Bacon, R. et al. 2012, The Messenger, 147, 4; Bacon, R. et al. 2014, The Messenger, 157, 13; Baldwin, J. A. et al. 1991, ApJ, 374, 580; Mc Leod, A. F. et al. 2015, MNRAS, submitted O’Dell, C. R. & Wen, Z. 1994, ApJ, 436, 194; O’Dell, C. R. 2001, ARA&A, 39, 99; O’Dell, C. R. & Yusef-Zadeh, F. 2000, AJ, 136, 382; Ricci, L. et al. 2008, AJ, 136, 2136; Shields, G. A. 1990, ARA&A, 28, 525; Weilbacher, P. M. et al. 2012, Proc. SPIE, 8451, 84510B Weilbacher, P. M. et al. 2015, A&A, 582, A114; Vilchez, J. M. & Esteban, C. 1996, MNRAS, 280, 720
42-45 (PDF)
M. G. Petr-Gotzens et al.
Young Stellar Objects in the Orion B Cloud

ADS BibCode:
2015Msngr.162...42P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Petr-Gotzens, M. G.; Alcalá, J. M.; Spezzi, L.; Jørgensen, J. K.; Stanke, Th.; Lombardi, M.; Alves, J. F.
AA(ESO) AB(INAF Osservatorio Astronomico di Capodimonte, Napoli, Italy) AC(ESO; European Organization for the Exploitation of Meteorological Satellites (EUMETSAT), Darmstadt, Germany) AD(Niels Bohr Institute, University of Copenhagen, Denmark) AE(ESO) AF(Department of Physics, University of Milan, Italy; Harvard-Smithsonian Center for Astrophysics, Cambridge, USA) AG(Department of Astrophysics, University of Vienna, Austria)
Abstract:
Wide-field near-infrared imaging surveys offer an excellent opportunity to obtain spatially complete samples of young stars in nearby star-forming regions. By studying their spatial distribution and individual properties, the global star formation characteristics of a region can be established. Near-infrared wide-field imaging observations of a significantly large area in the Orion Molecular Cloud B, obtained with the VISTA telescope on Cerro Paranal are presented. On the basis of photometric selection criteria, we have identified 186 candidate young stellar objects that are associated with the stellar clusters NGC 2068 and NGC 2071, and with the stellar group around HH24-26. Overall, Orion B shows a lot of similarities in its star formation characteristics with other Galactic star-forming regions: a star formation efficiency of a few percent, a stellar mass distribution very similar to that of the Orion Trapezium cluster, and a high observed fraction of circumstellar discs.
References:
Baraffe, I. et al. 1998, A&A, 337, 403; Chabrier, G. et al. 2000, ApJ, 542, 464; Evans, N. J. et al. 2009, ApJS, 181, 321; Federrath, C. & Klessen, R. S. 2013, ApJ, 763, 51; Flaherty, K. M. & Muzerolle, J. 2008, AJ, 135, 966; Harvey, P. et al. 2007, ApJ, 663, 1149; Hatchell, J. et al. 2012, ApJ, 754, 104; Heiderman, A. et al. 2010, ApJ, 723, 1019; Lada, C. J. et al. 1991, ApJ, 371, 171; Lada, C. J. et al. 2010, ApJ, 724, 687; Megeath, S. T. et al. 2012, AJ, 144, 192; Muench, A. A. et al. 2002, ApJ, 573, 366; Petr-Gotzens, M. et al. 2011, The Messenger, 145, 29; Robin, A. C. et al. 2003, A&A, 409, 523; Spezzi, L. et al. 2015, A&A, 581, 140
46-50 (PDF)
K. Ohnaka et al.
Revealing the Complex Dynamics of the Atmospheres of Red Supergiants with the Very Large Telescope Interferometer

ADS BibCode:
2015Msngr.162...46O
Section:
Astronomical Science
Author(s)/Affiliation(s):
Ohnaka, K.; Weigelt, G.; Hofmann, K.-H.; Schertl, D.
AA(Instituto de Astronomía, Universidad Católica del Norte, Antofagasta, Chile) AB(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AC(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AD(Max-Planck-Institut für Radioastronomie, Bonn, Germany)
Abstract:
Massive stars lose a significant fraction of their initial mass when they evolve to red supergiants before they end their life in supernova explosions. The mass loss greatly affects their final fate. However, the mass loss from these dying supergiants is not yet understood well. Here we present our efforts to spatially resolve the dynamics of the atmospheres of red supergiants with the Very Large Telescope Interferometer (VLTI) and the AMBER instrument to clarify the physical mechanism behind the mass loss. The VLTI/AMBER’s combination of milliarcsecond spatial resolution and high spectral resolution allows us to spatially resolve stellar atmospheres and extract the dynamical information at each position over the star and the atmosphere — just like observations of the Sun.
References:
Arroyo-Torres, B. et al. 2015, A&A, 575, A50; Aurière, M. et al. 2010, A&A, 516, L2; Chiavassa, A. et al. 2011, A&A, 535, A22; Gilliland, R. L. & Dupree, A. K. 1996, ApJ, 463, L29; Harper, G. M. & Brown, A. 2006, ApJ, 646, 1179; Kervella, P. et al. 2011, A&A, 531, A117; Lim, J. et al. 1998, Nature, 392, 575; Lobel, A. & Dupree, A. K. 2001, ApJ, 558, 815; Montargès, M. et al. 2014, A&A, 572, A17; Ohnaka, K. et al. 2011, A&A, 529, A163; Ohnaka, K. et al. 2013, A&A, 555, A24; Ohnaka, K. 2014, A&A, 568, A17; Ohnaka, K. et al. 2015, A&A, 581, A127; Petrov, R. G. et al. 2007, A&A, 464, 1
51-55 (PDF)
S. Bagnulo et al.
Beyond Phase 3: The FORS1 Catalogue of Stellar Magnetic Fields

ADS BibCode:
2015Msngr.162...51.
Section:
Astronomical Science
Author(s)/Affiliation(s):
Bagnulo, S.; Landstreet, J. D.; Fossati, L.
AA(Armagh Observatory, College Hill, Armagh, United Kingdom) AB(Armagh Observatory, College Hill, Armagh, United Kingdom; University of Western Ontario, London, Canada) AC(Space Research Institute, Austrian Academy of Sciences, Graz, Austria)
Abstract:
Over the course of a decade of operations, more than 200 nights of telescope time have been granted for magnetic field measurements with the FORS1 instrument on the VLT. Motivated by some conflicting results published in the literature, we have studied the instrument characteristics and critically revised previous magnetic field detections obtained with FORS1. Our study has led to the publication of a catalogue of 1400 magnetic field measurements of a sample of 850 different stars, together with their intensity spectra. This catalogue includes nearly all the circular spectropolarimetric measurements taken during ten years of operation. Here we summarise some of the lessons learned from the analysis of the FORS1 stellar spectropolarimetric archive.
References:
Appenzeller, I. et al. 1998, The Messenger, 94, 1; Aurière, M. et al. 2010, A&A, 523, 40; Aznar Cuadrado, R. et al. 2004, A&A, 423, 1081; Bagnulo, S. et al. 2002, A&A, 389, 191; Bagnulo, S. et al. 2006, A&A, 450, 777; Bagnulo, S. et al. 2009, PASP, 121, 993; Bagnulo, S. et al. 2012, A&A, 538, 129; Bagnulo, S. et al. 2013, A&A, 559, 103; Bagnulo, S. et al. 2015, A&A, 583, A115; Hubrig, S. et al. 2006, AN, 327, 289; Hubrig, S. et al. 2009, The Messenger, 135, 21; Izzo, C. et al. 2010, SPIE, 7737, 7737-29; Jordan, S. et al. 2005, A&A, 432, 273; Jordan, S. et al. 2012, A&A, 542, 64; Landstreet, J. D. et al. 2009, A&A, 481, 465; Landstreet, J. D. et al. 2012, A&A, 541, A100; Landstreet, J. D. et al. 2014, A&A, 572, A113; Leone, F. et al. 2011, ApJ, 731, 33; Manso Sainz, R. 2011, ApJ, 731, L33; O’Toole, S. J. et al. 2005, A&A, 437, 227; Silvester, J. et al. 2009, MNRAS, 398, 1505; Shultz, M. et al. 2012, ApJ, 750, 2; Wade, G. A. et al. 2005, A&A, 442L, 31; Wade, G. A. et al. 2007, MNRAS, 376, 1145

Astronomical News

57-59 (PDF)
M. Arnaboldi et al.
Report on the ESO Workshop ''Rainbows on the Southern Sky: Science and Legacy Value of the ESO Public Surveys and Large Programmes''

ADS BibCode:
2015Msngr.162...57A
Section:
Astronomical News
Author(s)/Affiliation(s):
Arnaboldi, M.; Rejkuba, M.; Leibundgut, B.; Beccari, G.
AA(ESO) AB(ESO) AC(ESO) AD(ESO)
Abstract:
This was the third ESO workshop on the science from Large Programmes and the second on Public Surveys. By design, this workshop covered all areas of research in observational astronomy, providing a forum for the presentation of the most recent scientific results from these programmes and fostering discussions on the planned developments enabled by large and coherent time allocations on ESO telescopes. Several aspects of the legacy value of such programmes —technological, archival content, access to data, time domain and sociological — were evaluated and set a reference for future developments of ESO services to the community.
References:
Arnaboldi, M. & Rejkuba, M. 2012, The Messenger, 150, 67; Arnaboldi, M. et al. 2014, The Messenger, 156, 24; Mathys, G. & Leibundgut, B. 2009, The Messenger, 135, 53; Wagner, S. & Leibundgut, B. 2004, The Messenger, 115, 41
60-61 (PDF)
P. Kabath et al.
Report on the ESO/OPTICON/IAU Summer School ''Modern Instruments, their Science Case, and Practical Data Reduction''

ADS BibCode:
2015Msngr.162...60K
Section:
Astronomical News
Author(s)/Affiliation(s):
Kabath, P.; Dennefeld, M.; Gerbaldi, M.; Paunzen, E.; Karas, V.
AA(Astronomical Institute of Czech Academy of Sciences, Ondřejov, Czech Republic) AB(Institut d’Astrophysique de Paris, France) AC(Institut d’Astrophysique de Paris, France) AD(Department of Theoretical Physics and Astrophysics, Masaryk University Brno, Czech Republic) AE(Astronomical Institute of Czech Academy of Sciences, Ondřejov, Czech Republic)
Abstract:
The Astronomical Institute of the Czech Academy of Sciences organised, jointly with its local partners from Masaryk University, and international partners OPTICON, ESO and the IAU, a two-week practical training course in astronomy for young researchers. The summer school is briefly summarised: lectures covered a wide range of theoretical and observational topics and the emphasis of the practical work was on the analysis of archival data.
References:
Kabath, P. et al. 2014, The Messenger, 156, 58
62-63 (PDF)
G. Bono et al.
Report on the International PhD School ''Science and Technology with the E-ELT''

ADS BibCode:
2015Msngr.162...62B
Section:
Astronomical News
Author(s)/Affiliation(s):
Bono, G.; Hook, I.; Ramsay, S.
AA(Università di Roma Tor Vergata, Italy) AB(Lancaster University, United Kingdom) AC(ESO)
Abstract:
This international PhD school in the F. Lucchin cycle was the first to bring together Masters and PhD students with an interest in all aspects of the science and technology of the European Extremely Large Telescope (E-ELT). It was fitting that this school was held within a year of the project formally entering the construction phase. An overview of the topics covered during the school is presented.
64-64 (PDF)
E. Sani
Staff at ESO

ADS BibCode:
2015Msngr.162...64S
Section:
Astronomical News
Author(s)/Affiliation(s):
Sani, E.
AA(ESO)
64-67 (PDF)
M. Béthermin, K. Wang
Fellows at ESO

ADS BibCode:
2015Msngr.162...641
Section:
Astronomical News
Author(s)/Affiliation(s):
Béthermin, M.; Wang, K.
AA(ESO) AB(ESO)
67-67 (PDF)
ESO
Personnel Movements

ADS BibCode:
2015Msngr.162...67.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)