Messenger No. 163 ( 2016)

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The Organisation

2-3 (PDF)
N. Gube, T. de Zeeuw
The Signing of the ALMA Trilateral Agreement

ADS BibCode:
2016Msngr.163....2G
Section:
The Organisation
Author(s)/Affiliation(s):
Gube, N.; de Zeeuw, T.
AA(ESO) AB(ESO)

Telescopes and Instrumentation

5-9 (PDF)
M. Romaniello et al.
The Growth of the User Community of the La Silla Paranal Observatory Science Archive

ADS BibCode:
2016Msngr.163....5R
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Romaniello, M.; Arnaboldi, M.; Da Rocha, C.; De Breuck, C.; Delmotte, N.; Dobrzycki, A.; Fourniol, N.; Freudling, W.; Mascetti, L.; Micol, A.; Retzlaff, J.; Sterzik, M.; Vera Sequeiros, I.; Vuong De Breuck, M.
AA(ESO) AB(ESO) AC(TERMA GmbH, Germany) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(TERMA GmbH, Germany) AJ(ESO) AK(ESO) AL(ESO) AM(ESO) AN(TERMA GmbH, Germany)
Abstract:
The archive of the La Silla Paranal Observatory has grown steadily into a powerful science resource for the ESO astronomical community. Established in 1998, the Science Archive Facility (SAF) stores both the raw data generated by all ESO instruments and selected processed (science-ready) data. The growth of the SAF user community is analysed through access and publication statistics. Statistics are presented for archival users, who do not contribute to observing proposals, and contrasted with regular and archival users, who are successful in competing for observing time. Archival data from the SAF contribute to about one paper out of four that use data from ESO facilities. This study reveals that the blend of users constitutes a mixture of the traditional ESO community making novel use of the data and of a new community being built around the SAF.
References:
Arnaboldi, M. & Retzlaff, J. 2011, The Messenger, 146, 45; Arnaboldi, M. et al. 2014, The Messenger, 156, 24; Freudling, W. et al. 2013, A&A, 559, A96; Pirenne, B. et al. 1998, The Messenger, 93, 20; Primas, F. et al. 2015, The Messenger, 161, 6; Romaniello, M. et al. 2016, The Messenger, in prep.
10-11 (PDF)
H. Boffin et al.
FORS2 Rotating Flat Field Systematics Fixed — Recent Exchange of FORS LADC Prisms Improves the Long-known Flat-fielding Problem

ADS BibCode:
2016Msngr.163...10B
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Boffin, H.; Moehler, S.; Freudling, W.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
For many years the FORS2 instrument has suffered from artefacts in the flat fields caused by surface inhomogeneities on the longitudinal atmospheric dispersion corrector (LADC) that affected high-precision photometric and spectroscopic measurements. Recently, the FORS LADC prisms were exchanged, and our analysis of a large number of flat fields shows that this exchange has resulted in a significant decrease in the level of small-scale artefacts.
References:
Bean, J. L., Miller-Ricci Kempton, E. & Homeier, D. 2010, Nature, 468, 669; Boffin, H. M. J. et al. 2015, The Messenger, 159, 6; Bramich, D. et al. 2012, The Messenger, 149, 12; Coccato, L. et al. 2014, MNRAS, 438, 1256; Moehler, S. et al. 2010, PASP, 122, 93; Sedaghati, E. et al. 2015, A&A, 576, L11
12-13 (PDF)
B. Carry, J. Berthier
A Simpler Procedure for Specifying Solar System Objects in Phase 2

ADS BibCode:
2016Msngr.163...12C
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Carry, B.; Berthier, J.
AA(IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ Paris 06, Université Lille, France; Laboratoire Lagrange, Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, France) AB(IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ Paris 06, Université Lille, France)
Abstract:
Observations of Solar System objects in Service Mode require a special procedure. Observers preparing Observing Blocks must submit a detailed ephemerides file for each target for the whole duration of the observability period, which can sometimes be the entire ESO Period. These ephemerides files are ASCII files and follow a strict format, compatible with the VLT parameter file format. We present a simple web service that is now available to replace the former two-step process.
References:
Berthier, J. et al. 2009, European Planetary Science Congress 2009, 676; Berthier, J. et al. 2006, ADASS, ASP Conference Series, 351, ed. Gabriel, C., Ponz, D. & Enrique, S., 367; Bonnarel, F. et al. 2000, A&AS, 143, 33; Bulirsch, R. & Stoer, J. 1966, Numerische Mathematik, 8, 1; Fienga, A. et al. 2014, Scientific notes Lainey, V., Arlot, J. E. & Vienne, A. 2004, A&A, 427, 371; Lainey, V., Dehant, V. & Patzold, M. 2007, A&A, 465, 1075; Lainey, V., Duriez, L. & Vienne, A. 2004, A&A, 420, 1171; Laskar, J. & Jacobson, R. A. 1987, A&A, 188, 212; Le Guyader, C. 1993, A&A, 272, 687; Stoer, J. & Bulirsch, R. 1980, Introduction to numerical analysis, (New York: Springer) Thuillot, W. et al. 2005, BAAS, 37, 638; Vienne, A. & Duriez, L. 1995, A&A, 297, 588

Astronomical Science

15-20 (PDF)
S. Wedemeyer
New Eyes on the Sun — Solar Science with ALMA

ADS BibCode:
2016Msngr.163...15W
Section:
Astronomical Science
Author(s)/Affiliation(s):
Wedemeyer, S.
AA(University of Oslo, Norway)
Abstract:
In Cycle 4, which starts in October 2016, the Atacama Large Millimeter/submillimeter Array (ALMA) will be open for regular observations of the Sun for the first time. ALMA’s impressive capabilities have the potential to revolutionise our understanding of our host star, with far-reaching implications for our knowledge about stars in general. The radiation emitted at ALMA wavelengths originates mostly from the chromosphere — a complex and dynamic layer between the photosphere and the corona that is prominent during solar eclipses. Despite decades of intensive research, the chromosphere is still elusive due to its complex nature and the resulting challenges to its observation. ALMA will change the scene substantially by opening up a new window on the Sun, promising answers to long-standing questions.
References:
De Pontieu, B. et al. 2007, Science, 318, 1574; Edlén, B. 1943, Zeitschrift für Astrophysik, 22, 30; Emslie, A. G. et al. 2005, Journal of Geophysical Research (Space Physics), 110, A9, 11103; Hawley, S. L. & Pettersen, B. R. 1991, ApJ, 378, 725; Maehara, H. et al. 2012, Nature, 485, 478; Schrijver, C. J. 1987, A&A, 172, 111; Vial, J.-C. & Engvold, O. 2015, A&SS Library, Vol. 415, (Switzerland: Springer International Publishing) Wedemeyer, S. et al. 2015, SSRv, Online First
21-25 (PDF)
M. Schöller et al.
The Central Role of FORS1/2 Spectropolarimetric Observations for the Progress of Stellar Magnetism Studies

ADS BibCode:
2016Msngr.163...21S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Schöller, M.; Hubrig, S.; Ilyin, I.; Steffen, M.; Briquet, M.; Kholtygin, A. F.
AA(ESO) AB(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AC(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AD(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AE(Institut d’Astrophysique et de Géophysique, Université de Liège, Belgium; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AF(Astronomical Institute, St Petersburg State University, Russia)
Abstract:
The spectropolarimetric mode of the FOcal Reducer and low dispersion Spectrographs (FORS), which was first implemented in FORS1, and then moved to FORS2 seven years ago, has made it possible to probe the presence of magnetic fields in stars of different spectral classes at almost all stages of stellar evolution. While in the early days of FORS1, many of the observations were related to magnetic Ap/Bp stars and their progenitor Herbig Ae/Be stars, recent spectropolarimetric studies with FORS2 have involved more challenging targets, such as massive O- and B-type stars in clusters and in the field, very fast rotating massive stars with magnetospheres, Wolf–Rayet stars and central stars of planetary nebulae. The role of FORS observations for stellar magnetic field measurements is summarised and improvements in the measurement technique are described.
References:
Bagnulo, S. et al. 2015a, A&A, 583, A115; Bagnulo, S. et al. 2015b, The Messenger, 162, 51; Castro, N. et al. 2015, A&A, 581, A81; Hubrig, S. et al. 2006, MNRAS, 369, L61; Hubrig, S. et al. 2010, Astron. Nachr., 331, 361; Hubrig, S. et al. 2009, The Messenger, 135, 21; Hubrig, S. et al. 2011a, ApJ, 726, L5; Hubrig, S. et al. 2011b, A&A, 525, L4; Hubrig, S. et al. 2013, A&A, 551, A33; Hubrig, S. et al. 2015, MNRAS, 447, 1885; Hubrig, S. et al. 2016, MNRAS, in press Jordan, S. et al. 2012, A&A, 542, A64; Karitskaya, E. A. et al. 2010, IBVS, 5950, 1; Morel, T. et al. 2014, The Messenger, 157, 27; Nazé, Y. et al. 2010, A&A, 520, A59; Oskinova, L. M. et al. 2014, NatCo, 5E4024; Steffen, M. et al. 2014, A&A, 570, A88; Wade, G. A. et al. 2007, MNRAS, 376, 1145; Wade, G. A. et al. 2012, MNRAS, 419, 2459; Walborn, N. R. 1973, AJ, 78, 1067
26-29 (PDF)
R. Cartier et al.
The QUEST–La Silla AGN Variability Survey

ADS BibCode:
2016Msngr.163...26C
Section:
Astronomical Science
Author(s)/Affiliation(s):
Cartier, R.; Lira, P.; Coppi, P.; Sánchez, P.; Arévalo, P.; Bauer, F. E.; Muñoz, R. R.
AA(School of Physics & Astronomy, University of Southampton, United Kingdom) AB(Departamento de Astronomia, Universidad de Chile, Chile) AC(Department of Astronomy, Yale University, USA) AD(Departamento de Astronomia, Universidad de Chile, Chile) AE(Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Chile) AF(Instituto de Astrofísica, Pontifícia Universidad Católica de Chile, Chile; Space Institute, University of Tennessee, Tullahoma, USA) AG(Departamento de Astronomia, Universidad de Chile, Chile)
Abstract:
It is widely believed that supermassive black holes reside at the centres of every massive galaxy. When actively accreting they are known as Active Galactic Nuclei (AGNs). Most commonly, their presence is exposed by the radiation generated by the accretion of matter toward their centres. This radiation can show dramatic flux variations on timescales from minutes to years that can be observed across the full electromagnetic spectrum from X-ray to radio wavelengths. Although the exact origin of AGN variability remains unclear, such variability can be used as an efficient tool to find them and to understand the origin and demographics of flux variations. To this end, we have undertaken an AGN variability survey using the QUEST camera on the ESO 1.0-metre Schmidt Telescope at La Silla. The QUEST–La Silla AGN Variability Survey aims to discover thousands of new AGNs, and provide highly sampled light curves to study the ultraviolet/optical flux variations to a limiting magnitude of r ~ 21.5 mag.
References:
Baltay, C. et al. 2007, PASP, 119, 1278; Cartier, R. et al. 2015, ApJ, 810, 164; Cartier, R. et al. 2016, in prep. Fan, X. 1999, AJ, 177, 2528; Jarvis, M. J. et al. 2013, MNRAS, 428, 1281; McCracken, H. J. et al. 2012, A&A, 544, 156; Rabinowitz, D. et al. 2012, AJ, 144, 140; Sanchez, P. et al. 2016, in prep. Schmidt, M. & Green, R. F. 1983, ApJ, 269, 352
32-34 (PDF)
V. D. Ivanov et al.
Towards a Fundamental Astrometric Reference System behind the Magellanic Clouds: Spectroscopic Confirmation of New Quasar Candidates Selected in the Near-infrared

ADS BibCode:
2016Msngr.163...32I
Section:
Astronomical Science
Author(s)/Affiliation(s):
Ivanov, V. D.; Cioni, M.-R. L.; Bekki, K.; de Grijs, R.; Emerson, J.; Gibson, B. K.; Kamath, D.; van Loon, J. Th.; Piatti, A. E.; For, B.-Q.
AA(ESO) AB(Universität Potsdam, Institut für Physik und Astronomie, Germany; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany; University of Hertfordshire, Physics Astronomy and Mathematics, United Kingdom) AC(ICRAR, The University of Western Australia, Crawley, Australia) AD(Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China; Department of Astronomy, Peking University, Beijing, China; International Space Science Institute –Beijing, China) AE(School of Physics and Astronomy, Queen Mary University of London, United Kingdom) AF(E. A. Milne Centre for Astrophysics, Department of Physics & Mathematics, University of Hull, United Kingdom) AG(Instituut voor Sterrenkunde, K. U. Leuven, Belgium) AH(Lennard-Jones Laboratories, Keele University, United Kingdom) AI(Observatorio Astronómico, Universidad Nacional de Córdoba, Argentina; Consejo Nacional de Investigaciones Científicas y Técnicas, Buenos Aires, Argentina) AJ(ICRAR, The University of Western Australia, Crawley, Australia)
Abstract:
Quasi-stellar objects (quasars) located behind nearby galaxies provide an excellent absolute reference system for astrometric studies, but they are difficult to identify because of fore- and background contamination. We have embarked on a programme to expand the quasar reference system behind the Large and Small Magellanic Clouds, the Magellanic Bridge and Magellanic Stream. Hundreds of quasar candidates were selected, based on their near-infrared colours and variability properties from the ESO VISTA Magellanic Clouds (VMC) Public Survey. A subset of 49 objects was followed up with optical spectroscopy with FORS2. We confirmed the quasar nature of 37 objects (34 new identifications) that span a redshift range from z ~ 0.5 to 4.1.
References:
Appenzeller, I. et al. 1998, The Messenger, 94, 1; Cioni, M.-R. L. et al. 2011, A&A, 527, 116; Cioni, M.-R. L. et al. 2013, A&A, 549, A29; Cross, N. J. G. et al. 2012, A&A, 548, 119; Dalton, G. B. et al. 2006, SPIE Conf. Ser., 6269, 30; Emerson, J. et al. 2006, The Messenger, 126, 41; Ivanov, V. et al. 2016, A&A, in press, arXiv:1510.05504; Irwin, M. J. et al. 2004, SPIE Conf. Ser., 5493, 411; Kozlowski, S. et al. 2013, ApJ, 775, 92; Vanden Berk, D. E. et al. 2001, AJ, 122, 549
35-38 (PDF)
C. Harrison et al.
The KMOS AGN Survey at High Redshift (KASHz)

ADS BibCode:
2016Msngr.163...35H
Section:
Astronomical Science
Author(s)/Affiliation(s):
Harrison, C.; Alexander, D.; Mullaney, J.; Stott, J.; Swinbank, M.; Arumugam, V.; Bauer, F.; Bower, R.; Bunker, A.; Sharples, R.
AA(Centre for Extragalactic Astronomy, Durham University, United Kingdom) AB(Centre for Extragalactic Astronomy, Durham University, United Kingdom) AC(Department of Physics and Astronomy, University of Sheffield, United Kingdom) AD(Astrophysics, Department of Physics, University of Oxford, United Kingdom; Centre for Extragalactic Astronomy, Durham University, United Kingdom) AE(Institute for Computational Cosmology, Durham University, United Kingdom; Centre for Extragalactic Astronomy, Durham University, United Kingdom) AF(ESO) AG(Instituo de Astrofisica, Pontifica Universidad Catolica de Chile, Santiago, Chile; Millenium Institute of Astrophysics, Santiago, Chile; Space Science Institute, Boulder, Colorado, USA) AH(Institute for Computational Cosmology, Durham University, United Kingdom; Centre for Extragalactic Astronomy, Durham University, United Kingdom) AI(Astrophysics, Department of Physics, University of Oxford, United Kingdom; Kavli Institute for the Physics and Mathematics of the Universe, The University of Toyko, Japan) AJ(Centre for Advanced Instrumentation, Durham University, United Kingdom)
Abstract:
The KMOS AGN Survey at High Redshift (KASHz) is an extensive observational programme to obtain spatially resolved spectroscopy of distant galaxies that host rapidly growing supermassive black holes (i.e., active galactic nuclei [AGN]). By exploiting the unique capabilities of KMOS we will spatially resolve the ionised gas kinematics in around 200 such galaxies. A fundamental prediction of galaxy formation models is that AGN inject considerable energy into their host galaxies and ultimately destroy or remove star-forming material via outflows. However, until now, observational constraints of this prediction have been limited to only a small number of distant galaxies. KASHz will provide the strongest constraints to date on the prevalence, properties and impact of ionised outflows in the host galaxies of distant AGN. The survey is described and our first results presented.
References:
Aird, J. et al. 2010, MNRAS, 401, 2531; Bower, R. & Bureau, M. 2014, The Messenger, 157, 38; Cano-Díaz, M. et al. 2012, A&A, 537, L8; Cicone, C. et al. 2014, A&A, 562, A21; Cresci, G. et al. 2015, ApJ, 708, 419; Ganguly, R. & Brotherton, M. S. 2008, ApJ, 692, 758; Harrison, C. M. et al. 2014, MNRAS, 441, 3306; Harrison, C. M. et al. 2016, MNRAS, 456, 1195; Madau, P. & Dickinson, M. 2014, ARA&A, 52, 415; Mullaney, J. et al. 2013, MNRAS, 433, 622; Rupke, D. S. N. & Veilleux, S. 2013, ApJ, 768, 75; Schaye, J. et al. 2015, MNRAS, 446, 521; Sharples, R. et al. 2013, The Messenger, 151, 21; Stott, J. et al. 2016, MNRAS, submitted Vogelsberger, M. et al. 2014, MNRAS, 444, 1518; Wisnioski, E. et al. 2015, ApJ, 799, 209

Astronomical News

40-42 (PDF)
L. L. Christensen et al.
Light Phenomena over the ESO Observatories I: Airglow

ADS BibCode:
2016Msngr.163...40C
Section:
Astronomical News
Author(s)/Affiliation(s):
Christensen, L. L.; Noll, S.; Horálek, P.
AA(ESO) AB(Institute for Astro- and Particle Physics, University of Innsbruck, Austria) AC(ESO)
Abstract:
Airglow, the faint light emitted by the Earth’s atmosphere, has in recent years been frequently photographed in large field images taken at ESO’s observatories. The nature of the airglow is briefly described and example images are shown, capturing the variety of the displays.
References:
Hanuschik, R. W. 2003, A&A, 407, 1157; Hathaway, D. H. 2015, Living Rev. Solar Phys., 12, 4; Heirtzler, J. R. 2002, JASTP, 64, 1701; Khomich, V. Y. et al. 2008, Airglow as an Indicator of Upper Atmospheric Structure and Dynamics, (Berlin: Springer) McLennan, 1928, Bakerian Lecture. The Aurora and Its Spectrum, Royal Society Proc. A, 120, 785; Noll, S. et al. 2012, A&A, 543, A92; Noll, S. et al. 2014, A&A, 567, A25; Noll, S. et al. 2015a, Atmospheric Chemistry and Physics, 15, 3647; Noll, S. et al. 2015b, ACPD, 15, 30793; Patat, F. 2004, The Messenger, 115, 18; Patat, F. 2008, A&A, 481, 575; Roach, F. E. & Gordon, J. L. 1973, The Light of the Night Sky, (Dordrecht: Reidel) Rousselot, P. et al. 2000, A&A, 354, 1134; Taylor, M. J. et al. 1997, JGR, 102, 26283
43-45 (PDF)
P. Horálek et al.
Light Phenomena over the ESO Observatories II: Red Sprites

ADS BibCode:
2016Msngr.163...43H
Section:
Astronomical News
Author(s)/Affiliation(s):
Horálek, P.; Christensen, L. L.; Bór, J.; Setvák, M.
AA(ESO) AB(ESO) AC(Research Centre of Astronomy and Earth Sciences, GGI, Hungarian Academy of Sciences, Budapest, Hungary) AD(Czech Hydrometeorological Institute, Prague, Czech Republic)
Abstract:
A rare atmospheric phenomenon, known as red sprites, was observed and captured on camera from the La Silla Observatory. This event signalled the first time that these extremely short-lived flashes of red light, originating in the Earth’s upper atmosphere, were photographed from a major astronomical observatory. Further images of red sprites from the La Silla Paranal Observatory sites are presented and the nature of red sprites is discussed.
References:
Boccippio, D. J. et al. 1995, Science, 269, 1088; Bór, J. 2013, J. Atmospheric & Solar-Terrestrial Physics, 92, 151; Fishman, G. J. et al. 1994, Science, 264, 1313; Franz, R. C., Nemzek, R. J. & Winckler, J. R. 1990, Science, 249, 4964, 48; Jehl, A., Farges, T. & Blanc, E. 2013, J. Geophysical Research: Space Phys., 116, 454; Marshall, R. A. & Inan, U. S. 2007, Geophysical Research Letters, 34, L05806; Pasko, V. P., Yair, Y. & Kuo, C.-L. 2012, Space Sci. Rev., 168, 475; Siefring, C. L. et al. 2010, J. Geophysical Research, 115, A00E57; Siingh, D. et al. 2012, Space Sci. Rev., 169, 73; Yair, Y. et al. 2009, J. Geophysical Research, 114, E09002; Yair, Y. et al. 2013, J. Atmospheric & Solar-Terrestrial Physics, 102, 140
46-49 (PDF)
M. Romaniello et al.
Report on the ESO–ESA Workshop ''Science Operations 2015: Science Data Management''

ADS BibCode:
2016Msngr.163...46R
Section:
Astronomical News
Author(s)/Affiliation(s):
Romaniello, M.; Arviset, C.; Leibundgut, B.; Lennon, D.; Sterzik, M.
AA(ESO) AB(ESAC, Villafranca de Castillo, Madrid, Spain) AC(ESO) AD(ESAC, Villafranca de Castillo, Madrid, Spain) AE(ESO)
Abstract:
During four intense days, more than 100 astronomers, software engineers, science operation and data management experts gathered for the second installment of the ESO–ESA workshop series “Science Operations: Working together in support of science”. Two years ago, the inaugural meeting of the series at the European Space Astronomy Centre in Madrid provided an overview of all of the different aspects of Science Operations. This year’s gathering was focused on science data management, and an overview of the presentations and a summary of the discussions is provided.
References:
Primas, F. & Hanowski, N. 2013, The Messenger, 154, 67
50-51 (PDF)
R. Laing, A. Richards
Report on ''European Radio Interferometry School 2015''

ADS BibCode:
2016Msngr.163...50L
Section:
Astronomical News
Author(s)/Affiliation(s):
Laing, R.; Richards, A.
AA(ESO) AB(Jodrell Bank Centre for Astrophysics, University of Manchester, United Kingdom)
Abstract:
The sixth European Interferometry School (ERIS2015) was held at ESO for the first time. As usual the school was aimed at graduate students and early-career postdocs, but this year the emphasis was on enhanced wide-bandwidth interferometers covering metre to submillimetre wavebands. More than 100 participants attended ERIS2015. The topics of the school are briefly described here. They covered a wide range, from an introduction to radio interferometric techniques through packages for data reduction and analysis to hands-on workshop sessions and proposal writing.
51-52 (PDF)
L. Humphreys et al.
The AstroMundus–ESO Connection

ADS BibCode:
2016Msngr.163...51H
Section:
Astronomical News
Author(s)/Affiliation(s):
Humphreys, L.; Hussain, G.; Biggs, A.; Lu, H.-Y.; Emsellem, E.; De Cia, A.; Lavail, A.; Spyromilio, J.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO)
Abstract:
The AstroMundus Programme is an E+ Erasmus Mundus Joint Masters Degree course in astronomy and astrophysics offered by a consortium of European universities and research institutes. In 2014 and 2016, AstroMundus Masters students visited ESO and participated in proposal-writing sessions, during which groups of students speed-wrote complete ALMA proposals, before presenting them to a pseudo Time Allocation Committee providing on-the-spot feedback. The AstroMundus visit of 25–26 January 2016 is described.
References:
ALMA Partnership, Brogan, C. et al. 2015, ApJ, 808, L3; Oberg, K. et al. 2015, Nature, 520, 198; Maiolino, R. et al. 2015, MNRAS, 452, 54
53-54 (PDF)
T. de Zeeuw et al.
Gert Finger Becomes Emeritus Physicist

ADS BibCode:
2016Msngr.163...53Z
Section:
Astronomical News
Author(s)/Affiliation(s):
de Zeeuw, T.; Lucuix, C.; Péron, M.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
Gert Finger has retired after almost 33 years service and he has been made the first Emeritus Physicist at ESO. An appreciation of some of his many achievements in the development of infrared instrumentation and detector controllers is given. A retirement party for Gert Finger was held in February 2016.
References:
Finger, G. et al. 2014, Proc. SPIE, 9148, 914817; Moorwood, A. et al. 1986, The Messenger, 44, 19; Moorwood, A., Moneti, A. & Gredel, R. 1991, The Messenger, 63, 77; Primas, F., Casali, M. & Walsh, J. 2010, The Messenger, 141, 50
54-57 (PDF)
M. McClure et al.
Fellows at ESO

ADS BibCode:
2016Msngr.163...54.
Section:
Astronomical News
Author(s)/Affiliation(s):
McClure, M.; Milli, J.; Ginsburg, A.
AA(ESO) AB(ESO) AC(ESO)
57-57 (PDF)
ESO
Personnel Movements

ADS BibCode:
2016Msngr.163...57.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
58-58 (PDF)
ESO
ESO Studentship Programme 2016/2017

ADS BibCode:
2016Msngr.163...58.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

60-63 (PDF)
ESO
Annual Index 2015

ADS BibCode:
2016Msngr.163...60.
Author(s)/Affiliation(s):
ESO
AA(ESO)