DOI:
10.18727/0722-6691/5018
ADS BibCode:
2017Msngr.168....2Z
Section:
The Organisation
Author(s)/Affiliation(s):
de Zeeuw, T.; Comerón, F.; Tamai, R.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
The ceremony to seal the time capsule, signalling the beginning of construction of the dome and main telescope structure for the Extremely Large Telescope, took place at the Paranal Observatory on 26 May 2017, in the presence of the President of Chile, Michelle Bachelet and many international guests. Owing to high winds, the ceremony could not take place as planned on the levelled site on Cerro Armazones, but instead was held at the Paranal Residencia. A brief report of the event and its organisation is presented, and the welcome speech by the ESO Director General is included.

DOI:
10.18727/0722-6691/5019
ADS BibCode:
2017Msngr.168....8A
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Arsenault, R.; Madec, P.-Y.; Vernet, E.; Hackenberg, W.; La Penna, P.; Paufique, J.; Kuntschner, H.; Pirard, J.-F.; Kolb, J.; Hubin, N.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO) AJ(ESO)
Abstract:
All the Adaptive Optics Facility (AOF) subsystems are now in Paranal and the project team is working on commissioning activities on Unit Telescope 4 (UT4) of the Very Large Telescope. Excellent progress has been made; the new secondary mirror unit, the Deformable Secondary Mirror (DSM), was installed in October 2016 and UT4 is now operating routinely with the DSM in non-adaptive optics mode. The other modules of the AOF, the Ground Atmospheric Layer Adaptive optiCs for Spectroscopic Imaging (GALACSI), the 4 Laser Guide Star Facility (4LGSF) and the GRound-layer Adaptive optics Assisted by Lasers (GRAAL), have been installed and are being qualified. The coupling with the High Acuity Wide field K-band Imager (HAWK-I) and the Multi Unit Spectroscopic Explorer (MUSE) has been tested and all elements are functional and ready to proceed with their full commissioning. The goal for the AOF is to complete GALACSI wide-field mode technical commissioning by the end of summer 2017 and the GRAAL ground-layer adaptive optics mode by the end of the year.
References:
Amico, P. et al. 2015, The Messenger, 162, 19; Arsenault, R. et al. 2010, The Messenger, 142, 12; Arsenault, R. et al. 2013a, The Messenger, 151, 14; Arsenault, R. et al. 2013b, Third AO4ELT Conference, Florence, Italy Arsenault, R. et al. 2014a, Proc. SPIE, 9148, 914802; Arsenault, R. et al. 2014b, The Messenger, 156, 2; Arsenault, R. et al. 2016, The Messenger, 164, 2; Bonaccini Calia, D. et al. 2014, Proc. SPIE, 9148, 91483P Briguglio, R. et al. 2014, Proc. SPIE, 9148, 914845; Hackenberg, W. et al. 2014, Proc. SPIE, 9148, 91483O Holzlöhner, R. et al. 2008, Proc. SPIE, 7015, 701521; Holzlöhner, R. et al. 2010, A&A, 510, A20; Holzlöhner, R. et al. 2012, Proc. SPIE, 8447, 84470H Kuntschner, H. et al. 2012, Proc. SPIE, 8448, 844808; La Penna, P. et al. 2014, Proc. SPIE, 9148, 91482V Manetti, M. et al. 2014, Proc. SPIE, 9148, 91484G Paufique, J. et al. 2012, Proc. SPIE, 8447, 944738; Stuik, R. et al. 2012, Proc. SPIE, 8447, 84473L

DOI:
10.18727/0722-6691/5020
ADS BibCode:
2017Msngr.168...15A
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Arnaboldi, M.; Delmotte, N.; Gadotti, D.; Hilker, M.; Hussain, G.; Mascetti, L.; Micol, A.; Petr-Gotzens, M.; Rejkuba, M.; Retzlaff, J.; Ivison, R.; Leibundgut, B.; Romaniello, M.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(TERMA GmbH, Europahaus, Darmstadt, Germany) AG(ESO) AH(ESO) AI(ESO) AJ(ESO) AK(ESO) AL(ESO) AM(ESO)
Abstract:
The ESO Public Surveys on VISTA serve the science goals of the survey teams while increasing the legacy value of ESO programmes, thanks to their homogeneity and the breadth of their sky coverage in multiple bands. These projects address a variety of research areas: from the detection of planets via microlensing, to stars, the Milky Way and Local Group galaxies, to extragalactic astronomy, galaxy evolution, the high-redshift Universe and cosmology. In 2015, as the first generation of imaging surveys was nearing completion, a second call for Public Surveys was opened to define a coherent scientific programme for VISTA until the commissioning of the wide-field multi-fibre spectrograph, 4MOST, in 2020. This article presents the status of the Cycle 1 surveys as well as an overview of the seven new programmes in Cycle 2, including their science goals, coverage on the sky and observing strategies. We conclude with a forward look at the Cycle 2 data releases and the timelines for their release.
References:
Arnaboldi, M. et al. 1998, The Messenger, 93, 30; Arnaboldi, M. et al. 2007, The Messenger, 127, 28; Arnaboldi, M. et al. 2014, The Messenger, 156, 24; Capaccioli, M. & Schipani, P. 2011, The Messenger, 146, 2; Cirasuolo, M. et al. 2011, The Messenger, 145, 11 de Jong, R. 2011, The Messenger, 145, 14; Retzlaff, J. et al. 2016, SPIE, 9910, 09; Romaniello, M. et al. 2016, The Messenger, 163, 5; Sutherland, W. et al. 2015, A&A, 575, 27

DOI:
10.18727/0722-6691/5021
ADS BibCode:
2017Msngr.168...21H
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Hofmann, W.
AA(Max-Planck-Institut für Kernphysik, Heidelberg, Germany)
Abstract:
The Cherenkov Telescope Array (CTA) is a next-generation observatory for ground-based very-high-energy gamma-ray astronomy, using the imaging atmospheric Cherenkov technique to detect and reconstruct gamma-ray induced air showers. The CTA project is planning to deploy 19 telescopes on its northern La Palma site, and 99 telescopes on its southern site at Paranal, covering the 20 GeV to 300 TeV energy domain and offering vastly improved performance compared to currently operating Cherenkov telescopes. The combination of three different telescope sizes (23-, 12- and 4-metre) allows cost-effective coverage of the wide energy range. CTA will be operated as a user facility, dividing observation time between a guest observer programme and large Key Science Projects (KSPs), and the data will be made public after a one-year proprietary period. The history of the project, the implementation of the arrays, and some of the major science goals and KSPs, are briefly summarised.
References:
Acharya, B. S. et al. 2013, Astroparticle Physics, 43, 3; Bernlöhr, K. et al. 2013, Astroparticle Physics, 43, 171; Hillas, A. M. 2013, Astroparticle Physics, 43, 19

DOI:
10.18727/0722-6691/5022
ADS BibCode:
2017Msngr.168...28P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Paladini, C.; Klotz, D.; Sacuto, S.; Lagadec, E.; Wittkowski, M.; Richichi, A.; Hron, J.; Jorissen, A.; Groenewegen, M.A.T.; Kerschbaum, F.; Verhoelst, T.; Rau, G.; Olofsson, H.; Zhao-Geisler, R.; Matter, A.
AA(Institut d’Astronomie et d’Astrophysique, Université libre de Bruxelles, Belgium) AB(Department of Astrophysics, University of Vienna, Austria) AC(Department of Astrophysics, University of Vienna, Austria; Department of Physics and Astronomy, Division of Astronomy and Space Physics, University of Uppsala, Sweden) AD(Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Nice, France) AE(ESO) AF(National Astronomical Research Institute of Thailand, Chiang Mai, Thailand) AG(Department of Astrophysics, University of Vienna, Austria) AH(Institut d’Astronomie et d’Astrophysique, Université libre de Bruxelles, Belgium) AI(Koninklijke Sterrenwacht van België, Brussel, Belgium) AJ(Department of Astrophysics, University of Vienna, Austria) AK(Belgian Institute for Space Aeronomy, Brussels, Belgium) AL(Department of Astrophysics, University of Vienna, Austria) AM(Department of Earth and Space Sciences, Onsala Space Observatory, Sweden) AN(Department of Earth Sciences, National Taiwan Normal University, Taipei, Taiwan) AO(Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Nice, France)
Abstract:
The Mid-infrared Interferometric instrument (MIDI) at the Very Large Telescope Interferometer (VLTI) has been used to spatially resolve the dust-forming region of 14 asymptotic giant branch (AGB) stars with different chemistry (O-rich and C-rich) and variability types (Miras, semi-regular, and irregular variables). The main goal of the programme was to detect deviations from spherical symmetry in the dust-forming region of these stars. All the stars of the sample are well resolved with the VLTI, and five are asymmetric and O-rich. This finding contrasts with observations in the near-infrared, where the C-rich objects are found to be more asymmetric than the O-rich ones. The nature of the asymmetric structures so far detected (dusty discs versus blobs)remains uncertain and will require imaging on milli-arcsecond scales.
References:
Blasius, T. D. et al. 2012, MNRAS, 426, 4; Cox, N. L. J. et al. 2012, A&A, 537, A35; Cruzalèbes, P. et al. 2015, A&A, 446, 3277; Groenwegen, M. A. T. et al. 2011, A&A, 526, A162; Jones, D. & Boffin, H. 2017, NatAs, 1, 117; Karovicova, I. et al. 2011, A&A, 532, A134; Kervella, P. et al. 2014, A&A, 564, 88; Klotz, D. et al. 2012, Proc. SPIE, 8445, 84451; Le Bertre, T. 1993, A&AS, 97, 729
 Lykou, F. et al. 2015, A&A, 576, 46; Lopez, B. et al. 2006, Proc. SPIE, 6268, 62680; Maercker, M. et al. 2012, Nature, 490, 212; Ohnaka, K. et al. 2007, A&A, 484, 371; Paladini, C. et al. 2017, A&A, 600, 136; Ramstedt, S. et al. 2014, A&A, 570, 14; Rau, G. et al. 2017, A&A, 600, 92 van der Veen, W. E. C. J. & Habing, H. J. 1988, A&A, 194, 125

DOI:
10.18727/0722-6691/5023
ADS BibCode:
2017Msngr.168...32K
Section:
Astronomical Science
Author(s)/Affiliation(s):
Khorrami, Z.; Vakili, F.; Lanz, T.; Langlois, M.; Lagadec, E.; Meyer, M.R.; Gratton, R.; Beuzit, J.-L.; Mouillet, D.
AA(School of Physics and Astronomy, Cardiff University, United Kingdom; Université Côte d’Azur, OCA, CNRS, Lagrange, France) AB(School of Physics and Astronomy, Cardiff University, United Kingdom) AC(School of Physics and Astronomy, Cardiff University, United Kingdom) AD(Université de Lyon, Université Lyon 1, CNRS, CRAL UMR5574, Saint-Genis Laval, France; Université Aix Marseille, CNRS, Laboratoire d’Astrophysique de Marseille, UMR 7326, France) AE(School of Physics and Astronomy, Cardiff University, United Kingdom) AF(Institute for Astronomy, ETH Zurich, Switzerland; Department of Astronomy, University of Michigan, Ann Arbor, U.S.A.) AG(INAF — Astronomical Observatory of Padua, Italy) AH(Université Grenoble Alpes, CNRS, Institut de Planétologie et d’Astrophysique de Grenoble, France) AI(Université Grenoble Alpes, CNRS, Institut de Planétologie et d’Astrophysique de Grenoble, France)
Abstract:
The SPHERE extreme adaptive optics instrument was used to observe the central core of the Large Magellanic Cloud, R136, in the near-infrared. This challenging observation demonstrated the capabilities of SPHERE for imaging distant clusters. More than one thousand sources have been detected in Ks- and J-band images in the small field of view of IRDIS covering almost 2.7 × 3.1 pc of the core of R136. Based on isochrone fitting of the colour-magnitude diagram, ages of 1 and 1.5 Myr for the inner 3-arcsecond core and the outer core of R136 fit our data best. The mass function slope is –0.96 ± 0.22 over the mass range of 3 to 300 M_⊙. Using SPHERE data, we have gone one step further in partially resolving the core of R136, but this is certainly not the final step and higher resolution is still required.
References:
Beuzit, J.-L. et al. 2008, SPIE, 7014, 701418; Bressan, A. et al. 2012, MNRAS, 427, 127; Campbell, B. et al. 1992, AJ, 104, 1721; Campbell, M. A. et al. 2010, MNRAS, 405, 421; Cassinelli, J. P., Mathis, J. S. & Savage, B. D. 1981, Sci, 212, 1497; Grebel, E. K. & Chu, Y.-H. 2000, AJ, 119, 787; Crowther, P. A. et al. 2010, MNRAS, 408, 731; Crowther, P. A. et al. 2016, MNRAS, 458, 624; Diolaiti, E. et al. 2000, A&AS, 147, 335; Feitzinger, J. V. et al. 1980, A&A, 84, 50; Hunter, D. A., Shaya, E. J. & Holtzman, J. A. 1995, ApJ, 448, 179; Khorrami, Z. et al. 2016, A&A, 588, L7; Langlois, M. et al. 2014, SPIE, 9147, 91479P Sabbi, E. et al. 2012, ApJ, 754, L37; Savage, B. D. et al. 1983, ApJ, 273, 597; Weigelt, G. & Baier, G. 1985, A&A, 150, L18; Wünsch, R. et al. 2017, ApJ, 835, 60

DOI:
10.18727/0722-6691/5024
ADS BibCode:
2017Msngr.168...36H
Section:
Astronomical Science
Author(s)/Affiliation(s):
Harrison, C.; Swinbank, M.
AA(ESO; Centre for Extragalactic Astronomy, Durham University, United Kingdom) AB(Centre for Extragalactic Astronomy, Durham University, United Kingdom)
Abstract:
A sample of ~1000 high-redshift (z ~ 0.3–1.7) star-forming galaxies has been observed with three-dimensional spectroscopy using the KMOS and MUSE spectrographs in order to explore the dynamical properties of galaxies across cosmic time. A summary of the survey is presented along with one set of results that explores the relationship between the angular momentum of the star-forming gas and galaxy morphology. This work expands previous angular momentum studies that mostly focused on local galaxies, to cover the past 10 billion years of cosmic time.
References:
Bacon, R. et al. 2010, SPIE Conf. Ser., 7735, 8; Cortese, L. et al. 2016, MNRAS, 463, 170; Fall, M. S. & Romanowsky, A. J. 2013, ApJ, 769, 26; Harrison, C. M. et al. 2017, MNRAS, 467, 1965; Lagos, C. d. P. et al. 2017, MNRAS, 464, 3850; Mortlock, A. et al. 2013, MNRAS, 433, 1185; Schaye, J. et al. 2015, MNRAS, 446, 521; Sharples, R. et al. 2013, The Messenger, 151, 21; Stott, J. P. et al. 2016, MNRAS, 457, 1888; Swinbank, A. M. et al. 2017, MNRAS, 467, 3140

DOI:
10.18727/0722-6691/5025
ADS BibCode:
2017Msngr.168...40G
Section:
Astronomical Science
Author(s)/Affiliation(s):
Guzzo, L.; The Vipers Team
AA(Università degli Studi di Milano, Italy)
Abstract:
The VIMOS Public Extragalactic Redshift Survey (VIPERS) released its final set of nearly 90 000 galaxy redshifts in November 2016, together with a series of science papers that range from the detailed evolution of galaxies over the past 8 Gyr to the growth rate and the power spectrum of cosmological structures measured at about half the Hubble time. These are the results of a map of the distribution of galaxies and their properties which is unprecedented in its combination of large volume and detailed sampling at 0.5 < z < 1.2. In this article, the survey design and data properties are briefly summarised and an overview of the key scientific results published so far is provided. The VIPERS data, obtained within the framework of an ESO Large Programme over the equivalent of just under 55 nights at the Very Large Telescope, will remain the largest legacy of the VIMOS spectrograph and its still unsurpassed ability to reach target densities close to 10000 spectra per square degree.
References:
Alam, S. et al. 2015, ApJS, 219, 12 de la Torre, S. & Guzzo, L. 2012, MNRAS, 427, 327 de la Torre, S. & VIPERS Team 2013, A&A, 557, 54 de la Torre, S. & VIPERS Team 2017, A&A, submitted, arXiv:1612.05647; Colless, M. et al. 2001, MNRAS, 328, 1039; Cucciati, O. & VIPERS Team 2017, in press, arXiv:1611.07049; Davidzon, I. & VIPERS Team 2013, A&A, 558, 23; Eisenstein, D. et al. 2011, AJ, 142, 72; Ellis, R. S. et al. 2017, arXiv:1701.01976; Fritz, A. & VIPERS Team 2014, A&A, 563, 92; Gargiulo, A. & VIPERS Team 2017, A&A, in press, arXiv:1611.07047; Garilli, B. et al. 2012, PASP, 124, 1232; Garilli, B. et al. 2014, A&A, 562, 23; Granett, B. R. & VIPERS Team 2015, A&A, 583, 61; Guzzo, L. et al. 2008, Nature, 451, 541; Guzzo, L. & VIPERS Team 2013, The Messenger, 151, 41; Guzzo, L. & VIPERS Team 2014, A&A, 566, 108; Hawken, A. & VIPERS Team 2017, A&A, in press, arXiv:1611.07046; Haines, C. P. & VIPERS Team 2017, A&A, in press, arXiv:1611.07050; Kaiser, N. 1987, MNRAS, 227, 1; Krywult, J. & VIPERS Team 2017, A&A, 598, 120; Le Fèvre, O. et al. 2005, A&A, 439, 845; Lilly, S. J. et al. 2009, ApJS, 184, 218; Malavasi, N. & VIPERS Team 2017, MNRAS, 465, 3817; Micheletti, D. & VIPERS Team 2014, A&A, 570, 106; Moutard, T. & VIPERS Team 2016, A&A, 590, 102; Peacock, J. A. et al. 2001, Nature, 410, 169; Pezzotta, A. & VIPERS Team 2017, A&A, in press, arXiv:1612.05645; Planck Collaboration 2016, A&A, 594, 1; Rota, S. & VIPERS Team 2017, A&A, in press, arXiv:1612.05644; Scodeggio, M. & VIPERS Team 2017, A&A, in press, arXiv:1612.05648; Siudek, M. & VIPERS Team 2017, A&A, 597, 107; York, D. et al. 2000, AJ, 120, 1579

DOI:
10.18727/0722-6691/5026
ADS BibCode:
2017Msngr.168...49M
Section:
Astronomical News
Author(s)/Affiliation(s):
Merand, A.
AA(ESO)
Abstract:
The infrastructure of the Very Large Telescope Interferometer (VLTI) is in the process of being upgraded and second-generation interferometric instruments are entering service (GRAVITY) or under construction (MATISSE). The VLTI Community Days presented these developments and began a discussion with the community on the future of the VLTI. Prior to the VLTI Community Days, a short Winter School was held to introduce early stage researchers to VLTI observation and data reduction.

DOI:
10.18727/0722-6691/5027
ADS BibCode:
2017Msngr.168...50D
Section:
Astronomical News
Author(s)/Affiliation(s):
Dias, B.; Saviane, I.
AA(ESO) AB(ESO)
Abstract:
Chile hosts many world-leading expert groups working on stellar populations and stellar clusters. This field has undergone something of a revolution during the last decade with the advent of large photometric and spectroscopic surveys, and preparations for relevant new facilities are underway. A Chilean meeting on stellar populations and star clusters was therefore timely. The goal was to bring together experts in the field for discussion and to encourage collaboration. The workshop was open to all astronomers and advanced students, especially those in Chilean institutes, limited to a maximum of 50 participants in order to foster discussion.
References:
Bechtol, K. et al. 2015, ApJ, 807, 50; Bekki, K., Couch, W. J. & Drinkwater, M. J. 2001, ApJL, 552, 105; Besla, G. et al. 2007, ApJ, 668, 949; Brodie, J. P. & Strader, J. 2006, ARA&A, 44, 193; Dias, B. et al. 2016a, A&A, 590, 9; Dias, B. et al. 2016b, The Messenger, 165, 19; Dias, B. et al. 2016c, A&A, 591, 11; Diaz, J. & Bekki, K. 2011, MNRAS, 413, 2015; Fellhauer, M. & Kroupa, P. 2002, MNRAS, 330, 642; Geisler, D. et al. 2012, ApJL, 756, 40; Gratton, R. G., Carretta, E. & Bragaglia, A. 2012, A&ARv, 20, 50; Ivanov, V. D. et al. 2017, A&A, 600, 112; Koposov, S. E. et al. 2015, ApJ, 805, 130; Niederhofer, F. et al. 2017, MNRAS, 465, 4159; Salinas, R. et al. 2016, ApJL, 832, 14; Saviane, I. et al. 2012, A&A, 540, 27; Scannapieco, C. et al. 2011, MNRAS, 417, 154

DOI:
10.18727/0722-6691/5028
ADS BibCode:
2017Msngr.168...52E
Author(s)/Affiliation(s):
ESO

DOI:
10.18727/0722-6691/5029
ADS BibCode:
2017Msngr.168...53Z
Section:
Astronomical News
Author(s)/Affiliation(s):
de Zeeuw, T.; Gilmozzi, R.
AA(ESO) AB(ESO)
References:
Bignami, G. F. et al. 1983, ApJ, 272, L9; Bignami, G. F. & Caraveo, P. A. 1996, ARAA, 34, 331; Bignami, G. F. 2012, We are the Martians: Connect- ing Cosmology with Biology, (Milan: Springer Verlag Italia Srl) Bignami, G. F. & Sommariva, A. 2013, A Scenario for Interstellar Exploration and Its Financing, Springer Briefs in Space Development, (Milan: Springer Verlag Italia Srl) Bignami, G. F. 2014, Imminent Science: What Remains to be Discovered, (Milan: Springer Verlag Italia Srl)

ADS BibCode:
2017Msngr.168...54E
Section:
Astronomical News
Author(s)/Affiliation(s):
Popping, G.; Agnello, A.
AA(ESO) AB(ESO)

ADS BibCode:
2017Msngr.168...57E
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO

ADS BibCode:
2017Msngr.168...59E
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO