Messenger No. 164 (June 2016)

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Telescopes and Instrumentation

2-7 (PDF)
R. Arsenault et al.
Adaptive Optics Facility Status Report: When First Light Is Produced Rather Than Captured

ADS BibCode:
2016Msngr.164....2A
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Arsenault, R.; Madec, P.-Y.; Vernet, E.; Hackenberg, W.; Bonaccini Calia, D.; La Penna, P.; Paufique, J.; Kuntschner, H.; Pirard, J.-F.; Sarazin, M.; Haguenauer, P.; Hubin, N.; Vera, I.
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)
Abstract:
First light for the 4 Laser Guide Star Facility (4LGSF) took place in Paranal on 26 April 2016 with four laser units in operation for the first time. A combined test with the first laser guide star unit and the Ground Layer Adaptive optics Assisted by Lasers (GRAAL) instrument in October 2015 demonstrated the whole acquisition sequence of the Adaptive Optics Facility (AOF). Many tools that will support the operation of the AOF for science observations have meanwhile been implemented. GALACSI was granted Provisional Acceptance in Europe in April 2016, completing the system tests and qualification in Garching of the adaptive optics modules GRAAL and GALACSI (Ground Atmospheric Layer Adaptive Optics for Spectroscopic Imaging), their real-time computers and the deformable secondary mirror (DSM). Results of tests both in the laboratory and on sky are presented. The installation of the DSM and GALACSI will be completed by early 2017, to be followed by commissioning of all AOF systems.
References:
Amico, P. et al. 2015, The Messenger, 162, 19; Arsenault, R. et al. 2010, The Messenger, 142, 12; Arsenault, R. et al. 2013, The Messenger, 151, 14; Arsenault, R. et al. 2013, in AO4ELT Conference – Adaptive Optics for Extremely Large Telescopes, Florence, Italy, May 2013; Arsenault, R. et al. 2014, The Messenger, 156, 2; Arsenault, R. et al. 2014, Proc. SPIE, 9148; Bonaccini Calia, D. et al. 2014, Proc. SPIE, 9148; Briguglio, R. et al. 2014, Proc. SPIE, 9148; Hackenberg, W. et al. 2014, Proc. SPIE, 9148; Holzlöhner, R. et al. 2008, Proc. SPIE, 7015; Holzlöhner, R. et al. 2010, A&A, 510, A20; Holzlöhner, R. et al. 2012, Proc. SPIE, 8447; Kuntschner, H. et al. 2012, Proc. SPIE, 8448; La Penna, P. et al. 2014, Proc. SPIE, 9148; Manetti, M. et al. 2014, Proc. SPIE, 9148; Paufique, J. et al. 2012, Proc. SPIE, 8447; Stuik, R. et al. 2012, Proc. SPIE, 8447
8-9 (PDF)
N. Fourniol et al.
A Fruitful Collaboration between ESO and the Max Planck Computing and Data Facility

ADS BibCode:
2016Msngr.164....8F
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Fourniol, N.; Zampieri, S.; Panea, M.
AA(ESO) AB(ESO) AC(Max Planck Computing and Data Facility, Garching, Germany)
Abstract:
The ESO Science Archive Facility (SAF), contains all La Silla Paranal Observatory raw data, as well as, more recently introduced, processed data created at ESO with state-of-the-art pipelines or returned by the astronomical community. The SAF has been established for over 20 years and its current holding exceeds 700 terabytes. An overview of the content of the SAF and the preservation of its content is provided. The latest development to ensure the preservation of the SAF data, provision of an independent backup copy of the whole SAF at the Max Planck Computing and Data Facility in Garching, is described.
References:
Arnaboldi, M. et al. 2014, The Messenger, 156, 24; Romaniello, M. et al. 2016a, in prep. Romaniello, M. et al. 2016b, The Messenger, 163, 5; Wicenec, A. et al. 2007, The Messenger, 129, 27
10-13 (PDF)
C. Martayan et al.
Solar Activity-driven Variability of Instrumental Data Quality

ADS BibCode:
2016Msngr.164...10M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Martayan, C.; Smette, A.; Hanuschik, R.; van Der Heyden, P.; Mieske, S.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO)
Abstract:
The unexplained variability of the data quality from Very Large Telescope instruments and the frequency of power cuts have been investigated. Origins for the variability in ambient temperature variations, software, data reduction pipelines and internal to hardware could be discarded. The most probable cause appears to be correlated with the evolution of the cosmic ray rate, and also with solar and terrestrial geomagnetic activity. We report on the consequences of such variability and describe how the observatory infrastructure, instruments and data are affected.
References:
Forbush, S. E. 1937, PhRv, 51, 1108; Forbush, S. E. 1938, PhRv, 54, 975; Vernet, J. et al. 2011, A&A, 536A, 105
14-16 (PDF)
D. Asmus et al.
Science Verification for the VISIR Upgrade

ADS BibCode:
2016Msngr.164...14A
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Asmus, D.; van den Ancker, M.; Ivanov, V.; Käufl, H.-U.; Kerber, F.; Leibundgut, B.; Mehner, A.; Momany, Y.; Pantin, E.; Tristram, K. R. W.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(INAF – Osservatorio Astronomico di Padova, Italy) AI(Laboratoire AIM, CEA/DSM – CNRS – Université Paris Diderot, IRFU/SAp, Gif sur Yvette, France) AJ(ESO)
Abstract:
The Very Large Telescope spectrometer and imager for the mid-infrared (VISIR) was upgraded in 2015 with new detectors and several new modes were added. Science Verification (SV) is carried out for new ESO instruments as well as for substantial upgrades to existing instruments. Sparse aperture masking and coronagraphy in the mid infrared have now been added to VISIR’s capabilities and during SV these new observational modes, together with the recommissioned burst mode, were used to demonstrate the observational capabilities of the instrument. The SV process for VISIR is briefly described and some results from the successful observations are presented. All SV data are publicly available.
References:
Käufl, H. U. et al. 2015, The Messenger, 159, 15; Kerber, F. et al. 2014, MNRAS, 439, 247; Kerber, F., Querel, R. R. & Neureiter, B. 2015, J. Phys., Conf. Ser., 595, 012017; Sanchez-Bermudez, J. et al. 2016, A&A, 588, A117; Vehoff, S. et al. 2010, A&A, 520, 78

Astronomical Science

18-22 (PDF)
S. Kamann et al.
A Stellar Census in NGC 6397 with MUSE

ADS BibCode:
2016Msngr.164...18K
Section:
Astronomical Science
Author(s)/Affiliation(s):
Kamann, S.; Husser, T.-O.; Wendt, M.; Bacon, R.; Brinchmann, J.; Dreizler, S.; Emsellem, E.; Krajnović, D.; Monreal-Ibero, A.; Roth, M. M.; Weilbacher, P. M.; Wisotzki, L.
AA(Institut für Astrophysik, Universität Göttingen, Germany) AB(Institut für Astrophysik, Universität Göttingen, Germany) AC(Institut für Physik und Astronomie, Universität Potsdam, Germany; Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany) AD(CRAL, Observatoire de Lyon, Saint-Genis Laval, France) AE(Sterrewacht Leiden, Universiteit Leiden, the Netherlands; Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, Portugal) AF(Institut für Astrophysik, Universität Göttingen, Germany) AG(ESO; CRAL, Observatoire de Lyon, Saint-Genis Laval, France) AH(Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany) AI(GEPI, Observatoire de Paris, PSL Research University, CNRS, Université Paris Diderot, Sorbonne Paris Cité, Meudon, France) AJ(Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany) AK(Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany) AL(Leibniz-Institut für Astrophysik (AIP), Potsdam, Germany)
Abstract:
The new and powerful integral-field spectrograph on the VLT, the Multi- Unit Spectroscopic Explorer (MUSE), was designed to search for distant galaxies to an unprecedented depth, but it is also capable of opening new science windows on the Galaxy. To demonstrate this capability, the globular cluster NGC 6397 was observed during the commissioning of MUSE in August 2014. We outline how the analysis of this unique dataset allowed us to assemble the largest spectroscopic sample of stars in a globular cluster to date. We also highlight the scientific applications that benefit from such MUSE data.
References:
Anderson, J. et al. 2008, AJ, 135, 2055; Bacon, R. et al. 2012, The Messenger, 147, 4; Bacon, R. et al. 2014, The Messenger, 157, 13; Harris, W. E. et al. 1996, AJ, 112, 1487; Husser, T.-O. et al. 2016, A&A, 588, 148; Kamann, S. et al. 2013, A&A, 549, 71; Kamann, S. et al. 2016, A&A, 588, 149; Korn, A. J. et al. 2007, ApJ, 671, 402; Noyola, E. et al. 2010, ApJ, 719, 60; Stetson, P. B. 1987, PASP, 99, 191; Ströbele, S. et al. 2012, Proc. SPIE, 8447, 844737; van der Marel, R. et al. 2010, ApJ, 710, 1063; Weilbacher, P. M. et al. 2012, Proc. SPIE, 8451, 84510B
23-26 (PDF)
S. K. Randall et al.
Pulsating Hot Subdwarfs in Omega Centauri

ADS BibCode:
2016Msngr.164...23R
Section:
Astronomical Science
Author(s)/Affiliation(s):
Randall, S. K.; Calamida, A.; Fontaine, G.; Monelli, M.; Bono, G.; Alonso, M. L.; Van Grootel, V.; Brassard, P.; Chayer, P.; Catelan, M.; Littlefair, S.; Dhillon, V. S.; Marsh, T. R.
AA(ESO) AB(Space Telescope Science Institute, Baltimore, USA) AC(Département de Physique, Université de Montréal, Canada) AD(Instituto de Astrofisica de Canarias, Tenerife, Spain) AE(Universita di Roma “Tor Vergata”, Department of Physics, Rome, Italy; INAF – Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) AF(Pontificia Universidad Catolica de Chile, Santiago, Chile) AG(Institut d’Astrophysique et de Géophysique de l’Université de Liège, Belgium) AH(Département de Physique, Université de Montréal, Canada) AI(Space Telescope Science Institute, Baltimore, USA) AJ(Pontificia Universidad Catolica de Chile, Santiago, Chile) AK(Department of Physics and Astronomy, University of Sheffield, United Kingdom) AL(Department of Physics and Astronomy, University of Sheffield, United Kingdom; Instituto de Astrofisica de Canarias, Tenerife, Spain) AM(Department of Physics, University of Warwick, Coventry, United Kingdom)
Abstract:
We recently discovered the first globular cluster hot subdwarf pulsators in Omega Centauri (ω Cen). These stars were initially thought to belong to the class of rapidly pulsating subdwarf B stars, which are well established among the field star population and have become showcases for asteroseismology. However, our spectroscopic analysis revealed the ω Cen variables to be significantly hotter than expected, indicating that they form a new class of subdwarf O pulsators clustered around 50 000 K, not known among the field star population. Non-adiabatic pulsation modelling suggests that the driver for the pulsations occurs via the same iron opacity mechanism that is at work in the rapidly pulsating subdwarf B stars.
References:
Ahmad, A. & Jeffery, C. S. 2005, A&A, 437, 51; Brown, T. M. et al. 2013, ApJ, 777, L22; Castellani, V. et al. 2007, ApJ, 663, 1021; Charpinet, S. et al. 1996, ApJ, 471, L103; Charpinet, S., Fontaine, G. & Brassard, P. 1997, ApJ, 483, L123; Fontaine, G. et al. 2012, A&A, 539, A12; Green, E. M. et al. 2003, ApJ, 583, 31; Johnson, C. et al. 2014, ASP Conf. Ser., 481, 153; Kilkenny, D. et al. 1997, MNRAS, 285, 640; Randall, S. K. et al. 2011, ApJ, 737, 27; Randall, S. K. et al. 2016, A&A, 589, 1; Schuh, S. et al. 2005, ASPC, 334, 530; Woudt, P. A. et al. 2006, MNRAS, 371, 149
27-33 (PDF)
C. Adami et al.
First Results from the XXL Survey and Associated Multi-wavelength Programmes

ADS BibCode:
2016Msngr.164...27A
Section:
Astronomical Science
Author(s)/Affiliation(s):
Adami, C.; Pierre, M.; Baran, N.; Eckert, D.; Fotopoulou, S.; Giles, P. A.; Koulouridis, E.; Lidman, C.; Lieu, M.; Mantz, A. B.; Pacaud, F.; Pompei, E.; Smolčić, V.; Ziparo, F.; XXL Team
AA(Aix Marseille Université, CNRS, LAM UMR 7326, Marseille, France) AB(Laboratoire AIM, CEA/DSM/IRFU/SAp, CEA Saclay, Gif-sur-Yvette, France) AC(Department of Physics, University of Zagreb, Croatia) AD(Department of Astronomy, University of Geneva, Versoix, Switzerland) AE(Department of Astronomy, University of Geneva, Versoix, Switzerland) AF(H. H. Wills Physics Laboratory, University of Bristol, United Kingdom) AG(Laboratoire AIM, CEA/DSM/IRFU/SAp, CEA Saclay, Gif-sur-Yvette, France) AH(Australian Astronomical Observatory, North Ryde, Australia) AI(School of Physics & Astronomy, University of Birmingham, United Kingdom) AJ(Department of Astronomy and Astrophysics, University of Chicago, USA) AK(Argelander Institut für Astronomie, Universität Bonn, Germany) AL(ESO) AM(Department of Physics, University of Zagreb, Croatia) AN(Department of Astronomy and Astrophysics, University of Chicago, USA) AO(XXL Team: http://irfu.cea.fr/xxl/members)
Abstract:
The XXL survey has mapped two extragalactic regions of 25 square degrees, using 10 ks XMM observations down to a point source sensitivity of ~ 5 × 10–15 erg s–1 cm–2 in the 0.5–2 keV band. It is the largest XMM project approved to date (> 6 Ms in total). The two fields have been or will be observed by several ground- and space-based facilities from ultra-violet to radio wavelengths. Besides the imaging, the spectroscopic follow-up is of special interest and ESO has contributed through Large Programmes and dedicated allocations. As of December 2015, ~ 450 new galaxy clusters are detected to z ~ 1.5–2, as well as more than 22 000 active galactic nuclei (AGN) to z ~ 4. The main goal of the project is to constrain the dark energy equation of state using clusters of galaxies. This survey will have lasting legacy value for cluster scaling laws and studies of AGNs and the X-ray background. The first XXL scientific results are summarised.
References:
Clerc, N. et al. 2012, MNRAS, 423, 3561; Clerc, N. et al. 2012, MNRAS, 423, 3545; Driver, S. P. et al. 2016, MNRAS, 455, 3911; Hinshaw, G. et al. 2013, ApJS, 208, 19; Le Brun, V. et al. 2014, MNRAS, 441, 1270; Le Fèvre, O. et al. 2005, A&A, 439, 845; Guzzo, L. et al. 2014, A&A, 566, 108; Hinshaw, G. et al. 2013, ApJS, 208, 19; XXL Survey: I. Pierre, M. et al. 2016, A&A, 592, A1; XXL Survey: II. Pacaud, F. et al. 2016, A&A, 592, A2; XXL Survey: III. Giles, P. A. et al. 2016, A&A, 592, A3; XXL Survey: IV. Lieu, M. et al. 2016, A&A, 592, A4; XXL Survey: V. Mantz, A. B. et al. 2016, ApJ, 794, 157; XXL Survey: VI. Fotopoulou, S. et al. 2016, A&A, 592, A5; XXL Survey: VII. Pompei, E. et al. 2016, A&A, 592, A6; XXL Survey: VIII. Adami, C. et al. 2016, A&A, 592, A7; XXL Survey: IX. Baran, N. et al. 2016, A&A, 592, A8; XXL Survey: X. Ziparo, F. et al. 2016, A&A, 592, A9; XXL Survey: XI. Smolčić, V. et al. 2016, A&A, 592, A10; XXL Survey: XII. Koulouridis, E. et al. 2016, A&A, 592, A11; XXL Survey. XIII. Eckert, D. et al. 2016, A&A, 592, A12; XXL Survey XIV. Lidman, C. et al. 2016, PASA, 33, 1
36-40 (PDF)
A. van der Wel et al.
The LEGA-C Survey: The Physics of Galaxies 7 Gyr Ago

ADS BibCode:
2016Msngr.164...36W
Section:
Astronomical Science
Author(s)/Affiliation(s):
van der Wel, A.; Noeske, K.; Bezanson, R.; Pacifici, C.; Gallazzi, A.; Franx, M.; Muñoz-Mateos, J.-C.; Bell, E. F.; Brammer, G.; Charlot, S.; Chauké, P.; Labbé, I.; Maseda, M. V.; Muzzin, A.; Rix, H.-W.; Sobral, D.; van de Sande, J.; van Dokkum, P. G.; Wild, V.; Wolf, C.
AA(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AB(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AC(Steward Observatory, University of Arizona, Tucson, USA) AD(Goddard Space Flight Center, Greenbelt, USA) AE(INAF–Osservatorio Astrofisico di Arcetri, Firenze, Italy) AF(Leiden Observatory, Leiden University, the Netherlands) AG(ESO) AH(Department of Astronomy, University of Michigan, Ann Arbor, USA) AI(Space Telescope Science Institute, Baltimore, USA) AJ(Institut d’Astrophysique de Paris, France) AK(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AL(Leiden Observatory, Leiden University, the Netherlands) AM(Leiden Observatory, Leiden University, the Netherlands) AN(Institute of Astronomy, University of Cambridge, UK) AO(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AP(Department of Physics, Lancaster University, UK; Leiden Observatory, Leiden University, the Netherlands) AQ(Sydney Institute for Astronomy, University of Sydney, Australia) AR(Department of Astronomy, Yale University, New Haven, USA) AS(School of Physics and Astronomy, University of St. Andrews, UK) AT(Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australia)
Abstract:
The LEGA-C (Large Early Galaxy Census) survey is made possible by the refurbishment of the Very Large Telescope VIsible and Multi Object Spectrograph (VIMOS) instrument and the implementation by ESO of a new generation of large spectroscopic surveys. The goal is to obtain high-quality continuum spectra of thousands of galaxies with redshifts up to z = 1, with which key physical parameters that were previously inaccessible can be measured. These include star formation histories and dynamical masses, which greatly improve our insight into how galaxies form and evolve. This article coincides with the first public data release of fully reduced and calibrated spectra.
References:
Conselice, C. et al. 2011, MNRAS, 417, 2770; Franx, M. et al. 2008, ApJ, 688, 770; Gallazzi, A. et al. 2005, MNRAS, 362, 41; Le Fèvre, O. et al. 2005, A&A, 439, 845; Lilly, S. et al. 2007, ApJS, 172, 70; Madau, P. et al. 1996, MNRAS, 283, 1388; McCracken, H. J. et al. 2012, A&A, 544, 156; Scoville, N. J. et al. 2007, ApJS, 172, 1; van der Wel, A. et al. 2014a, ApJ, 792, 6L van der Wel, A. et al. 2014b, ApJ, 788, 28; van der Wel, A. et al. 2016, ApJS, 223, 29
41-43 (PDF)
I. Oteo et al.
ALMACAL: Exploiting ALMA Calibrator Scans to Carry Out a Deep and Wide (Sub)millimetre Survey, Free of Cosmic Variance

ADS BibCode:
2016Msngr.164...41O
Section:
Astronomical Science
Author(s)/Affiliation(s):
Oteo, I.; Zwaan, M.; Ivison, R.; Smail, I.; Biggs, A.
AA(Institute for Astronomy, University of Edinburgh, United Kingdom; ESO) AB(ESO) AC(ESO; Institute for Astronomy, University of Edinburgh, United Kingdom) AD(Centre for Extragalactic Astronomy, Department of Physics, Durham University, United Kingdom; Institute for Computational Cosmology, Department of Physics, Durham University, United Kingdom) AE(ESO)
Abstract:
We present the latest results from ALMACAL, a novel, wide and deep (sub-)millimetre survey that exploits ALMA calibration data that comes for free during science observations. Combining compatible data acquired during multiple visits to many ALMA calibrators, sufficiently low noise levels can be reached to detect faint dusty star-forming galaxies (DSFGs). As of April 2016, we have analysed data for more than 240 calibrators, reaching noise levels as low as ~10 µJy beam−1, at sub-arcsecond spatial resolution. We have found 15 DSFGs, some less luminous than the sources detected by the deepest far-infrared surveys. Future analyses will deliver larger samples, free of cosmic variance, with redshifts determined via detection of multiple (sub-)millimetre lines, and dust emission imaged at milliarcsecond spatial resolution. The combination of area and depth reached by ALMACAL is unlikely to be surpassed by any other ALMA (sub-)millimetre survey.
References:
Béthermin, M. et al. 2011, A&A, 529, 4; Cai, Z.-Y. et al. 2013, ApJ, 768, 21; Casey, C. M. et al. 2014, PhR, 541, 45; da Cunha, E. et al. 2013, ApJ, 765, 9D Decarli, R. et al. 2014, ApJ, 782, 78; Fomalont, E. et al. 2014, The Messenger, 155, 19; Fujimoto, S. et al. 2016, ApJS, 222, 1; Hatsukade, B. et al. 2013, ApJL, 769, L27; Hatsukade, B. et al. 2016, PASJ, 34; Karim, A. et al. 2013, MNRAS, 432, 2; Lagos, C. del P. et al. 2011, MNRAS, 418, 1649; Muller, S. et al. 2014, A&A, 566, 112; Ono, Y. et al. 2014, ApJ, 795, 5; Oteo, I. et al. 2013, A&A, 554, 3; Oteo, I. et al. 2016, ApJ, 822, 36; Pearson, T. J. & Readhead, A. C. S. 1984, ARA&A, 22, 97; Popping, G. et al. 2016, arXiv:1602.02761P Simpson, J. M. et al. 2015, ApJ, 807, 128; Smail, I., Ivison, R. & Blain, A. W. 1997, ApJ, 490, L5; Swinbank, A. M. et al. 2014, MNRAS, 438, 1267; Weiss, A. et al. 2009, ApJ, 705, 45

Astronomical News

45-47 (PDF)
P. Horálek et al.
Light Phenomena over the ESO Observatories III: Zodiacal Light

ADS BibCode:
2016Msngr.164...45H
Section:
Astronomical News
Author(s)/Affiliation(s):
Horálek, P.; Christensen, L. L.; Nesvorný, D.; Davies, R.
AA(ESO) AB(ESO) AC(Dept. of Space Studies, Southwest Research Institute, Boulder, USA) AD(ESO)
Abstract:
The zodiacal light is often seen at the ESO observatories in the hours after sunset and before sunrise. The origin of the zodiacal light is described and recent research briefly summarised. Some fine images of the zodiacal light from Paranal and La Silla, including the full extent of the night sky are presented.
References:
Christensen, L. L., Noll, S. & Horálek, P. 2016, The Messenger, 163, 38; Dermott, S. F. et al. 1994, Nature, 369, 719; Dermott, S. F. et al. 1984, Nature, 312, 505; Ertel, S. et al. 2015, The Messenger, 159, 24; Guess, A. W. 1962, AJ, 135, 855; Horálek, P. et al. 2016, The Messenger, 163, 41; Jones, M. H., Bewsher, D. & Brown, D. S. 2013, Science, 342, 960; Lebreton, J. et al. 2013, A&A, 555, A146; Low, F. J. et al. 1984, AJ, 278, L15; Marion, L. et al. 2014, A&A, 570, A127; Nesvorný, D. et al. 2003, ApJ, 591, 486; Nesvorný, D. et al. 2010, ApJ, 713, 816; Reach, W. T. et al. 1995, Nature, 374, 521; Rowan-Robinson, M. & May, B. 2013, MNRAS, 429, 2894; Schulz, R. et al. 2015, Nature, 515, 216
47-49 (PDF)
M. Dennefeld et al.
The First NEON School in La Silla

ADS BibCode:
2016Msngr.164...47D
Section:
Astronomical News
Author(s)/Affiliation(s):
Dennefeld, M.; Melo, C.; Selman, F.
AA(Institut d’Astrophysique de Paris, CNRS, and Université P. et M. Curie, Paris, France) AB(ESO) AC(ESO)
Abstract:
The NEON Observing Schools have long provided PhD students with practical experience in the preparation, execution and reduction of astronomical observations, primarily at northern observatories. The NEON School was held in Chile for the first time, with observations being conducted at La Silla. The school was attended by 20 students, all from South America, and observations were performed with two telescopes, including the New Technology Telescope. A brief description of the school is presented and the observing projects and their results are described.
References:
Chalabaev, A. & D’Odorico, S. 1988, The Messenger, 53, 11
50-51 (PDF)
P. Ballester
Report on the ESO Data Simulation Workshop

ADS BibCode:
2016Msngr.164...50B
Section:
Astronomical News
Author(s)/Affiliation(s):
Ballester, P.
AA(ESO)
Abstract:
The role of simulated data is increasing rapidly across all phases of instrumentation projects, from design to scientific exploitation. The many commonalities among ESO instruments, their reduction software and archival products, makes it especially worthwhile to exchange knowledge between their instrument teams. The data simulation workshop was the first of its kind to bring together the ESO instrument simulator community and a brief overview of the workshop is presented. The participants expressed strong interest in continuing to exchange knowledge in this area.
References:
Bristow, P. et al. 2010, Proc. SPIE, 7735, 271; Jarno, A. et al. 2012, Proc. SPIE, 8449, 84490A Leschinski, K. et al. 2016, Proc. ASP Conf. Ser. ADASS XXV, in press Li Causi, G. et al. 2014, Proc. SPIE, 9147, 64-1; Noll, S. et al. 2012, A&A, 543, A92; Schmalzl, E. et al. 2012, Proc. SPIE, 8449, 1P
52-53 (PDF)
J. Spyromilio, R. Holzlöhner
Retirement of Lothar Noethe

ADS BibCode:
2016Msngr.164...52S
Section:
Astronomical News
Author(s)/Affiliation(s):
Spyromilio, J.; Holzlöhner, R.
AA(ESO) AB(ESO)
Abstract:
Lothar Noethe retired in April after 33 years at ESO. An appreciation of his contributions is presented, in particular his pioneering work in active optics and his role in the commissioning of the NTT and VLT.
References:
Holzlöhner, R. et al. 2014, SPIE, 9151, 2I Karban, R. et al. 2008, Proc. SPIE, 7017, #1I Madsen, C. 2012, The Jewel on the Mountaintop, (London: Wiley-VCH) Noethe, L. et al. 1986, SPIE, 628, 285N Noethe, L. 2002, Progress in Optics, 43, 1; Sarazin, M. 1989, The Messenger, 56, 8; Wilson, R. 1989, The Messenger, 56, 1; Wilson, R. 2003, The Messenger, 113, 2
54-57 (PDF)
K. Immer et al.
Fellows at ESO

ADS BibCode:
2016Msngr.164...54.
Section:
Astronomical News
Author(s)/Affiliation(s):
Immer, K.; Johnston, E.; Kerzendorf, W.
AA(ESO) AB(ESO) AC(ESO)
57-57 (PDF)
ESO
Personnel Movements

ADS BibCode:
2016Msngr.164...57.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)
58-58 (PDF)
ESO
ESO Fellowship Programme 2016/2017

ADS BibCode:
2016Msngr.164...58.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)