Messenger No. 165 (September 2016)

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Telescopes and Instrumentation

2-9 (PDF)
F. Patat
Gender Systematics in Telescope Time Allocation at ESO

ADS BibCode:
2016Msngr.165....2P
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Patat, F.
AA(ESO)
Abstract:
The results of a comprehensive statistical analysis of gender systematics in the time allocation process at ESO are presented. The sample on which the study is based includes more than 13 000 Normal and Short proposals, submitted by about 3000 principal investigators (PI) over eight years. The genders of PIs, and of the panel members of the Observing Programmes Committee (OPC), were used, together with their career level, to analyse the grade distributions and the proposal success rates. Proposals submitted by female PIs show a significantly lower probability of being allocated time. The proposal success rates (defined as number of top ranked runs over requested runs) are 16.0 ± 0.6% and 22.0 ± 0.4% for females and males, respectively. To a significant extent the disparity is related to different input distributions in terms of career level. The seniority of male PIs is significantly higher than that of female PIs, with only 34% of the female PIs being professionally employed astronomers (compared to 53% for male PIs). A small, but statistically significant, gender-dependent behaviour is measured for the OPC referees: both genders show the same systematics, but they are larger for males than females. The PI female/male fraction is very close to 30/70; although far from parity, the fraction is higher than that observed, for instance, among IAU membership.
References:
Cesarsky, C. & Walker, H. 2010, Astronomy & Geophysics, 51, 2.33 Goldin, C. & Cecilia, R. 2000, The American Economic Review, 90, 715 Patat, F. & Hussain, G. A. J. 2013, in Organizations, People and Strategies in Astronomy, Vol. 2, ed. Heck, A., (Duttlenheim: Venngeist), 231 Primas, F. et al. 2015, The Messenger, 161, 5 Reid, I. N. 2014, PASP, 126, 923
10-12 (PDF)
R. G. West et al.
The Next Generation Transit Survey Becomes Operational at Paranal

ADS BibCode:
2016Msngr.165...10W
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
West, R. G.; Pollacco, D.; Wheatley, P.; Goad, M.; Queloz, D.; Rauer, H.; Watson, C.; Udry, S.; Bannister, N.; Bayliss, D.; Bouchy, F.; Burleigh, M.; Cabrera, J.; Chaushev, A.; Chazelas, B.; Crausaz, M.; Csizmadia, S.; Eigmüller, P.; Erikson, A.; Genolet, L.; Gillen, E.; Grange, A.; Günther, M.; Hodgkin, S.; Kirk, J.; Lambert, G.; Louden, T.; McCormac, J.; Metrailler, L.; Neveu, M.; Smith, A.; Thompson, A.; Raddi, R.; Walker, S. R.; Jenkins, J.; Jordán, A.
AA(Dept. of Physics, University of Warwick, United Kingdom) AB(Dept. of Physics, University of Warwick, United Kingdom) AC(Dept. of Physics, University of Warwick, United Kingdom) AD(Dept. of Physics and Astronomy, University of Leicester, United Kingdom) AE(Institute of Astronomy, University of Cambridge, United Kingdom) AF(Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, Berlin, Germany) AG(Astrophysics Research Centre, Queen’s University Belfast, United Kingdom) AH(Observatoire de Genève, Sauverny, Switzerland) AI(Dept. of Physics and Astronomy, University of Leicester, United Kingdom) AJ(Observatoire de Genève, Sauverny, Switzerland) AK(Observatoire de Genève, Sauverny, Switzerland) AL(Dept. of Physics and Astronomy, University of Leicester, United Kingdom) AM(Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, Berlin, Germany) AN(Dept. of Physics and Astronomy, University of Leicester, United Kingdom) AO(Observatoire de Genève, Sauverny, Switzerland) AP(Observatoire de Genève, Sauverny, Switzerland) AQ(Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, Berlin, Germany) AR(Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, Berlin, Germany) AS(Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, Berlin, Germany) AT(Observatoire de Genève, Sauverny, Switzerland) AU(Institute of Astronomy, University of Cambridge, United Kingdom) AV(Dept. of Physics and Astronomy, University of Leicester, United Kingdom) AW(Institute of Astronomy, University of Cambridge, United Kingdom) AX(Institute of Astronomy, University of Cambridge, United Kingdom) AY(Dept. of Physics, University of Warwick, United Kingdom) AZ(ASTELCO Systems GmbH, Martinsried, Germany) BA(Dept. of Physics, University of Warwick, United Kingdom) BB(Dept. of Physics, University of Warwick, United Kingdom) BC(Observatoire de Genève, Sauverny, Switzerland) BD(Observatoire de Genève, Sauverny, Switzerland) BE(Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, Berlin, Germany) BF(Astrophysics Research Centre, Queen’s University Belfast, United Kingdom) BG(Dept. of Physics, University of Warwick, United Kingdom) BH(Dept. of Physics, University of Warwick, United Kingdom) BI(Departamento de Astronomía, Universidad de Chile, Santiago, Chile) BJ(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile)
Abstract:
A new facility dedicated to the discovery of exoplanets has commenced science operations at Paranal. The Next-Generation Transit Survey (NGTS) will deliver photometry at a precision unprecedented for a ground-based wide-field survey, enabling the discovery of dozens of transiting exoplanets of the size of Neptune or smaller around bright stars. NGTS is briefly described and the survey prospects are outlined.
References:
Berta-Thompson, Z. K. et al. 2015, Nature, 527, 204 Gillon, M. et al. 2016, Nature, 533, 221 Jehin, E. 2011, The Messenger, 145, 2 Wilson, D. M. et al. 2008, ApJ, 675, L113
13-17 (PDF)
K. Immer et al.
SEPIA — A New Instrument for the Atacama Pathfinder Experiment (APEX) Telescope

ADS BibCode:
2016Msngr.165...13I
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Immer, K.; Belitsky, V.; Olberg, M.; De Breuck, C.; Conway, J.; Montenegro-Montes, F. M.; Perez-Beaupuits, J.-P.; Torstensson, K.; Billade, B.; De Beck, E.; Ermakov, A.; Ferm, S.-E.; Fredrixon, M.; Lapkin, I.; Meledin, D.; Pavolotsky, A.; Strandberg, M.; Sundin, E.; Arumugam, V.; Galametz, M.; Humphreys, E.; Klein, T.; Adema, J.; Barkhof, J.; Baryshev, A.; Boland, W.; Hesper, R.; Klapwijk, T. M.
AA(ESO) AB(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AC(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AD(ESO) AE(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AF(ESO) AG(ESO) AH(ESO) AI(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AJ(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AK(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AL(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AM(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AN(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AO(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AP(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AQ(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AR(Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, Sweden) AS(ESO) AT(ESO) AU(ESO) AV(ESO) AW(Kapteyn Astronomical Institute, University of Groningen, the Netherlands) AX(Kapteyn Astronomical Institute, University of Groningen, the Netherlands) AY(Kapteyn Astronomical Institute, University of Groningen, the Netherlands; SRON Netherlands Institute for Space Research, Groningen, the Netherlands) AZ(Leiden Observatory, Leiden University, the Netherlands; Netherlands Research School for Astronomy, Leiden, the Netherlands) BA(Kapteyn Astronomical Institute, University of Groningen, the Netherlands) BB(Kavli Institute of Nanoscience, Delft University of Technology, the Netherlands)
Abstract:
The Swedish-ESO PI receiver for APEX (SEPIA) was installed at the APEX telescope in 2015. This instrument currently contains ALMA Band 5 (157–212 GHz) and Band 9 (600–722 GHz) receivers. Commissioning and science verification for Band 5 have been successfully completed but are still ongoing for Band 9. The SEPIA instrument is briefly described and the commissioning of the Band 5 receiver and results from the first science observations are presented.
References:
Baryshev, A. M. et al. 2015, A&A, 577, A129 Billade, B. et al. 2012, IEEE Trans. Terahertz Science and Technology, 2, 208 Cheung, A. C. et al. 1969, Nature, 221, 626 Galametz, M. et al. 2016, MNRAS, 462, 36 González-Alfonso, E. et al. 1998, A&A, 334, 1016 González-Alfonso, E. et al. 1999, ApJ, 525, 845 Humphreys, E. M. L. et al. 2016, arXiv:1608.00258 Klein, B. et al. 2012, A&A, 542, 3 Molinari, S. et al. 2016, ApJL, 826, 8 Olofsson, H. et al. 1998, A&A, 329, 1059 Pardo, J. R. et al. 2001, IEEE Trans. on Antennas and Propagation, 49, 1683 Strandet, M. L. et al. 2016, ApJ, 822, 80 van Dishoeck, E. et al. 2011, PASP, 123, 138

Astronomical Science

19-21 (PDF)
B. Dias et al.
Globular Clusters and the Milky Way Connected by Chemistry

ADS BibCode:
2016Msngr.165...19D
Section:
Astronomical Science
Author(s)/Affiliation(s):
Dias, B.; Saviane, I.; Barbuy, B.; Held, E. V.; Da Costa, G.; Ortolani, S.; Gullieuszik, M.
AA(ESO) AB(ESO) AC(Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Brazil) AD(Research School of Astronomy & Astrophysics, Australian National University, Australia) AE(Dipartimento di Fisica e Astronomia, Università di Padova, Italy; INAF, Osservatorio Astronomico di Padova, Italy) AF(INAF, Osservatorio Astronomico di Padova, Italy)
Abstract:
There are two ways to study galaxy formation and evolution: one is to observe a large number of galaxies at a variety of redshifts, the other is to observe in detail just a few nearby galaxies. The precision achievable by the latter method enables the galactic history, including the formation and early evolution, to be studied. Globular clusters provide targets for the second method. We show how the chemical content of Milky Way globular clusters can be used to place them on a timeline charting the history of our Galaxy. The results suggest that different α-elements trace different processes of Milky Way chemical evolution.
References:
Appenzeller, I. et al. 1998, The Messenger, 94, 1 Carretta, E. et al. 2009, A&A, 508, 695 Dias, B. et al. 2015, A&A, 573, 13 Dias, B. et al. 2016, A&A, 590, 9 Eggen, O. J., Lynden-Bell, D. & Sandage, A. R. 1962, ApJ, 136, 748 Gratton, R., Sneden, C. & Carretta, E. 2004, ARA&A, 42, 385 Gratton, R., Carretta, E. & Bragaglia, A. 2012, A&ARv, 20, 50 Harris, W. E. 1996, AJ, 112, 1487 (2010 edition) Matteucci, F. & Recchi, S. 2001, ApJ, 558, 351 McWilliam, A. 2016, PASA, submitted, arXiv:1607.05299 Mellinger, A. 2009, PASP, 121, 1180 Pagel, B. E. J. 1997, Nucleosynthesis and Chemical Evolution of Galaxies, CUP Pasquini, L. et al. 2002, The Messenger, 110, 1 Pritzl, B. J., Venn, K. A. & Irwin, M. 2005, AJ, 130, 2140 Saviane, I., Held, E. V. & Da Costa, G. S. et al. 2012, The Messenger, 149, 23 Searle, L. & Zinn, R. 1978, ApJ, 225, 3
22-26 (PDF)
A. F. McLeod et al.
Connecting the Dots: MUSE Unveils the Destructive Effect of Massive Stars

ADS BibCode:
2016Msngr.165...22M
Section:
Astronomical Science
Author(s)/Affiliation(s):
McLeod, A. F.; Ginsburg, A.; Klaassen, P.; Mottram, J.; Ramsay, S.; Testi, L.
AA(ESO) AB(ESO) AC(UK Astronomy Technology Centre, Edinburgh, United Kingdom) AD(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AE(ESO) AF(ESO; INAF Osservatorio di Arcetri, Florence, Italy)
Abstract:
Throughout their entire lives, massive stars have a substantial impact on their surroundings, such as via protostellar outflows, stellar winds, ionising radiation and supernovae. Conceptually this is well understood, but the exact role of feedback mechanisms on the global star formation process and the stellar environment, as well as their dependence on the properties of the star-forming regions, are yet to be understood in detail. Observational quantification of the various feedback mechanisms is needed to precisely understand how high mass stars interact with and shape their environment, and which feedback mechanisms dominate under given conditions. We analysed the photo-evaporative effect of ionising radiation from massive stars on their surrounding molecular clouds using MUSE integral field data. This allowed us to determine the mass-loss rate of pillar-like structures (due to photo-evaporation) in different environments, and relate it to the ionising power of nearby massive stars. The resulting correlation is the first observational quantification of the destructive effect of ionising radiation from massive stars.
References:
Bertoldi, F. 1989, ApJ, 346, 735 Evans, C. J. et al. 2005, A&A, 437, 467 Gritschneder, M. et al. 2010, ApJ, 723, 971 Hartigan, P. et al. 2015, AJ, 149, 101 Hester, J. J. et al. 1996, AJ, 111, 2349 Lefloch, B. & Lazareff, B. 1994, A&A, 289, 559 Martins, F. et al. 2005, A&A, 436, 1049 McLeod, A. F. et al. 2015, MNRAS, 450, 1057 McLeod, A. F. et al. 2016, MNRAS, in press, arXiv:1608.00005 Melena, N. W. et al. 2008, AJ, 135, 878 Sankrit, R. & Hester, J. J. 2000, AJ, 535, 847 Smith, N. et al. 2010, MNRAS, 405, 1153 Tremblin, P. et al. 2012, A&A, 538, A31
27-33 (PDF)
F. Schuller et al.
From ATLASGAL to SEDIGISM: Towards a Complete 3D View of the Dense Galactic Interstellar Medium

ADS BibCode:
2016Msngr.165...27U
Section:
Astronomical Science
Author(s)/Affiliation(s):
Schuller, F.; Urquhart, J.; Bronfman, L.; Csengeri, T.; Bontemps, S.; Duarte-Cabral, A.; Giannetti, A.; Ginsburg, A.; Henning, T.; Immer, K.; Leurini, S.; Mattern, M.; Menten, K.; Molinari, S.; Muller, E.; Sánchez-Monge, A.; Schisano, E.; Suri, S.; Testi, L.; Wang, K.; Wyrowski, F.; Zavagno, A.
AA(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AB(Centre for Astrophysics and Planetary Science, University of Kent, United Kingdom; Max-Planck-Institut für Radioastronomie, Bonn, Germany) AC(University of Chile, Departamento de Astronomía, Chile) AD(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AE(Laboratoire d’Astrophysique de Bordeaux, University of Bordeaux, France) AF(School of Physics, University of Exeter, United Kingdom) AG(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AH(ESO) AI(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AJ(ESO) AK(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AL(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AM(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AN(INAF, Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy) AO(National Astronomical Observatory of Japan, Tokyo, Japan) AP(University of Cologne, I. Physikalisches Institut, Germany) AQ(INAF, Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy) AR(University of Cologne, I. Physikalisches Institut, Germany) AS(ESO) AT(ESO) AU(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AV(Laboratoire d’Astrophysique de Marseille, France)
Abstract:
The ATLASGAL survey has provided the first unbiased view of the inner Galactic Plane at sub-millimetre wavelengths. This is the largest ground-based survey of its kind to date, covering 420 square degrees at a wavelength of 870 µm. The reduced data, consisting of images and a catalogue of > 104 compact sources, are available from the ESO Science Archive Facility through the Phase 3 infrastructure. The extremely rich statistics of this survey initiated several follow-up projects, including spectroscopic observations to explore molecular complexity and high angular resolution imaging with the Atacama Large Millimeter/submillimeter Array (ALMA), aimed at resolving individual protostars. The most extensive follow-up project is SEDIGISM, a 3D mapping of the dense interstellar medium over a large fraction of the inner Galaxy. Some notable results of these surveys are highlighted.
References:
Beaumont, C. N. & Williams, J. P. 2010, ApJ, 709, 791 Brand, J. & Blitz, L. 1993, A&A, 275, 67 Colombo, D. et al. 2015, MNRAS, 454, 2067 Contreras, Y. et al. 2013, A&A, 549, A45 Csengeri, T. et al. 2014, A&A, 565, A75 Csengeri, T. et al. 2016a, A&A, 585, A104 Csengeri, T. et al. 2016b, A&A, 586, A149 Giannetti, A. et al. 2014, A&A, 570, A65 Giannetti, A. et al. 2015, A&A, 580, L7 Heyer, M. & Dame, T. M. 2015, ARA&A, 53, 583 Jackson, J. M. et al. 2006, ApJS, 163, 145 Kendrew, S. et al. 2016, ApJ, 825, 142 Li, G.-X. et al. 2016, A&A, 591, A5 Molinari, S. et al. 2010, A&A, 518, L100 Schuller, F. et al. 2009, A&A, 504, 415 Schuller, F. et al. 2016, submitted to A&A Siringo, G. et al. 2009, A&A, 497, 945 Sousbie, T. 2011, MNRAS, 414, 350 Urquhart, J. et al. 2014a, A&A, 568, A41 Urquhart, J. et al. 2014b, MNRAS, 443, 1555 Wang, K. et al. 2015, MNRAS, 450, 4043 Wang, K. et al. 2016, ApJS, in press, arXiv:1607.06452 Wienen, M. et al. 2012, A&A, 544, A146 Wienen, M. et al. 2015, A&A, 579, A91
34-37 (PDF)
G. B. Brammer et al.
Ultra-deep K-band Imaging of the Hubble Frontier Fields

ADS BibCode:
2016Msngr.165...34B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Brammer, G. B.; Marchesini, D.; Labbé, I.; Spitler, L.; Lange-Vagle, D.; Barker, E. A.; Tanaka, M.; Fontana, A.; Galametz, A.; Ferré-Mateu, A.; Kodama, T.; Lundgren, B.; Martis, N.; Muzzin, A.; Stefanon, M.; Toft, S.; van der Wel, A.; Vulcani, B.; Whitaker, K. E.
AA(Space Telescope Science Institute, Baltimore, USA
) AB(Physics and Astronomy Department, Tufts University, Medford, USA
) AC(Leiden Observatory, Leiden University, the Netherlands) AD(Department of Physics & Astronomy, Macquarie University, Sydney, Australia; Australian Astronomical Observatory, North Ryde, Australia
) AE(Space Telescope Science Institute, Baltimore, USA
; Physics and Astronomy Department, Tufts University, Medford, USA
) AF(Space Telescope Science Institute, Baltimore, USA
) AG(National Astronomical Observatory of Japan, Tokyo, Japan
) AH(INAF, Osservatorio Astronomico di Roma, Monteporzio, Italy) AI(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AJ(Subaru Telescope, Hilo, USA) AK(National Astronomical Observatory of Japan, Tokyo, Japan
) AL(Department of Astronomy, University of Wisconsin, Madison, USA
) AM(Physics and Astronomy Department, Tufts University, Medford, USA
) AN(Kavli Institute for Cosmology, Cambridge University, United Kingdom) AO(Leiden Observatory, Leiden University, the Netherlands) AP(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Denmark) AQ(Max-Planck-Institut für Astronomie Heidelberg, Germany
) AR(School of Physics, University of Melbourne, Australia
) AS(Department of Astronomy, University of Massachusetts Amherst, USA
; Hubble Fellow)
Abstract:
We have recently completed a deep near-infrared imaging survey with the High Acuity Wide Field K-band Imager (HAWK-I), nicknamed KIFF (Ks-band Imaging of the Frontier Fields). KIFF provides ultra-deep images of six fields around massive galaxy clusters that have also recently been observed with the Hubble and Spitzer Space Telescopes as part of the Frontier Fields programme. Each of the KIFF mosaics is among the deepest Ks-band images ever obtained, and, with a boost from strong gravitational lensing by the galaxy clusters, they will be used to reveal the stellar populations of galaxies seen only a few hundred million years after the Big Bang. Fully reduced images are made available to the community through the Phase 3 infrastructure of the ESO Science Archive Facility.
References:
Bouwens, R. J. et al. 2013, ApJL, 765, L16 Brammer, G. B. et al. 2016, ApJS, in press, arXiv:1606.07450 Franx, M. et al. 2003, ApJL, 587, L79 Labbé, I. et al. 2005, ApJL, 624, L81 Lotz, J. M. et al. 2016, ApJ, submitted, arXiv:1605.06567 Fontana, A. et al. 2006, A&A, 459, 745 Fontana, A. et al. 2014, A&A, 570, A11 Fontana, A. et al. 2014b, The Messenger, 155, 42 Muzzin, A. et al. 2009, ApJ, 701, 1839 van Dokkum, P. G. et al. 2006, ApJL, 638, L59

Astronomical News

39-43 (PDF)
R. Ellis
Report on the ESO/MPA/MPE/Excellence Cluster/LMU and TUM Munich Joint Conference ''Discs in Galaxies''

ADS BibCode:
2016Msngr.165...39E
Section:
Astronomical News
Author(s)/Affiliation(s):
Ellis, R.
AA(ESO)
Abstract:
The annual Munich Joint Astronomy Conference brought together observers and theorists studying the full range of cosmic environments and epochs where discs play a role in shaping the structural assembly history of galaxies. Considerable progress is being made in interpreting the past history of the Milky Way and Andromeda through massive stellar imaging and spectroscopic campaigns. This is being augmented with interferometric studies of gaseous discs in nearby galaxies with exquisite angular resolution. Integral field spectrographs are providing resolved data for star-forming and quiescent galaxies to redshifts of three. This explosion of new data is being interpreted with high resolution numerical simulations in order to understand the physical processes which govern the stability, formation and disruption of early discs, and how star formation is regulated in the context of various feedback processes. Selected highlights of the progress reported at the conference are presented.
References:
Belfiore, F. et al. 2016, MNRAS, 461, 3111 Hayden, M. R. et al. 2015, ApJ, 808, 132 Schinnerer, E. et al. 2013, ApJ, 779, 42 Vogelsberger, M. et al. 2014, MNRAS, 444, 1518
44-44 (PDF)
P. Padovani
Report on the ESO Workshop ''Active Galactic Nuclei: what’s in a name?''

ADS BibCode:
2016Msngr.165...44P
Section:
Astronomical News
Author(s)/Affiliation(s):
Padovani, P.
AA(ESO)
Abstract:
The workshop was aimed at presenting a multi-wavelength picture of active galactic nuclei. The contents of the workshop are here briefly summarised; a review article synthesising the invited reviews, presentations and discussions is in preparation.
45-46 (PDF)
P. Ballester, Dennefeld M.
Report on the ESO/OPTICON ''Instrumentation School on Use and Data Reduction of X-shooter and KMOS''

ADS BibCode:
2016Msngr.165...45B
Section:
Astronomical News
Author(s)/Affiliation(s):
Ballester, P.; Dennefeld M.
AA(ESO) AB(Institut d’Astrophysique de Paris, CNRS, and Université P. et M. Curie, Paris, France)
Abstract:
The NEON Archive Schools have since 1999 provided opportunities for young researchers to gain practical experience of the reduction and analysis of archive data. Twenty-four participants from 17 nationalities gathered to learn about the end-to-end cycle of observation proposal, data reduction and archive usage for X-shooter and KMOS. A brief description of the school is presented and the content of the main sessions is described.
References:
Dennefeld, M., Melo, C. & Selman, F. 2016, The Messenger, 164, 47 Freudling, W. et al. 2013, A&A, 559, A96
47-48 (PDF)
R. Laing et al.
Report on the ''ALMA Developers’ Workshop''

ADS BibCode:
2016Msngr.165...47L
Section:
Astronomical News
Author(s)/Affiliation(s):
Laing, R.; Mroczkowski, T.; Testi, L.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
A workshop was recently held in Gothenburg to discuss the ALMA Development Programme for the period 2015–2030. The main aims were to inform the European and international communities about progress on current development projects, to solicit new ideas and to discuss priorities for the future. This contribution summarises the outcomes of the workshop.
49-51 (PDF)
R. Visser et al.
Fellows at ESO

ADS BibCode:
2016Msngr.165...49.
Section:
Astronomical News
Author(s)/Affiliation(s):
Visser, R.; Watson, L.; Asmus, D.
AA(ESO) AB(ESO) AC(ESO)
52-52 (PDF)
ESO
ESO Studentship Programme 2016 — 2nd Call

ADS BibCode:
2016Msngr.165...52.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
53-53 (PDF)
ESO
Personnel Movements

ADS BibCode:
2016Msngr.165...53.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)