DOI:
10.18727/0722-6691/5000
ADS BibCode:
2017Msngr.167....2S
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Stoehr, F.; Manning, A.; Moins, C.; Jenkins, D.; Lacy, M.; Leon, S.; Muller, E.; Nakanishi, K.; Matthews, B.; Gaudet, S.; Murphy, E.; Ashitagawa, K.; Kawamura, A.
AA(ESO) AB(ESO) AC(ESO) AD(Canadian Astronomical Data Centre (CADC), National Research Council of Canada, Victoria, Canada) AE(National Radio Astronomy Observatory (NRAO), Charlottesville, USA) AF(Joint ALMA Observatory (JAO), Vitacura, Santiago, Chile) AG(National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences, Tokyo, Japan) AH(National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences, Tokyo, Japan) AI(National Research Council of Canada, Victoria, Canada) AJ(Canadian Astronomical Data Centre (CADC), National Research Council of Canada, Victoria, Canada) AK(National Radio Astronomy Observatory (NRAO), Charlottesville, USA) AL(National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences, Tokyo, Japan) AM(National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences, Tokyo, Japan)
Abstract:
Science archives help to maximise the scientific return of astronomical facilities. After placing science archives into a slightly larger context, we describe the current status and capabilities of the ALMA Science Archive. We present the design principles and technology employed for three main contexts: query; result set display; and data download. A summary of the ALMA data flow is also presented as are access statistics to date.
References:
Bonnarel, F. et al. 2000, A&A, 143, 33; Boch, T. & Fernique, P. 2014, ASPC, 485, 277; Dieleman, S. et al. 2015, MNRAS, 450, 1441; Grothkopf, U. & Meakins, S. 2015, ASP, 492, 63; Romaniello, M. et al. 2016, The Messenger, 163, 5; Rosolowsky, E. et al. 2015, ASPC, 495, 121; Stoehr, F. et al. 2012, ASPC, 461, 697; Stoehr, F. et al. 2014, SPIE, 9149, 914902; Stoehr, F. et al. 2015, The Messenger, 162, 30; Stoehr, F. et al. 2016, arXiv:1611.09625; Stoehr, F. 2017, ASPC, in preparation Teuben, P. et al. 2015, ASPC, 495, 305; Wicenec, A. et al. 2001, The Messenger, 106, 11; Wicenec, A. & Knudstrup, J. 2007, The Messenger, 129, 27

DOI:
10.18727/0722-6691/5001
ADS BibCode:
2017Msngr.167....7H
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Humphreys, L.; Biggs, A.; Immer, K.; Laing, R.; Liu, H. B.; Marconi, G.; Mroczkowski, T.; Testi, L.; Yagoubov, P.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO) AI(ESO)
Abstract:
ALMA Band 5 (163–211 GHz) was recently commissioned and Science Verification (SV) observations were obtained in the latter half of 2016. A primary scientific focus of this band is the H₂O line at 183.3 GHz, which can be observed around 15% of the time when the precipitable water vapour is sufficiently low (< 0.5 mm). Many more lines are covered in Band 5 and can be observed for over 70% of the time on Chajnantor, requiring similar restrictions to those for ALMA Bands 4 and 6. Examples include the H₂¹⁸O line at 203 GHz, some of the bright (3–2) lines of singly and doubly deuterated forms of formaldehyde, the (2–1) lines of HCO⁺, HCN, HNC, N₂H⁺ and several of their isotopologues. A young star-forming region near the centre of the Milky Way, an evolved star also in our Galaxy, and a nearby ultraluminous infrared galaxy (ULIRG) were observed as part of the SV process and the data are briefly described. The reduced data, along with imaged data products, are now public and demonstrate the power of ALMA for high-resolution studies of H₂O and other molecules in a variety of astronomical targets.
References:
Belitsky, V. et al. 2017, A&A, in preparation Belloche, A. et al. 2013, A&A, 559, 147; Billade, B. et al. 2012, IEEE Trans. Terahertz Science Technology, 2, 208; Cernicharo, J. et al. 2006, ApJ, 646, L49; Galametz, M. et al. 2016, MNRAS, 462, L36; Immer, K. et al. 2016, The Messenger, 165, 13; König, S. et al. 2017, A&A, submitted, arXiv:1612.07668; Wittkowski, M. et al. 2012, A&A, 540, 12

DOI:
10.18727/0722-6691/5002
ADS BibCode:
2017Msngr.167...11B
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
De Breuck, C.; Testi, L.; Immer, K.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
The workshop provided an overview of the wide range of results from the first two years of science operations with the ALMA Band 5 (163–211 GHz) receiver in the Swedish ESO PI Instrument for APEX (SEPIA) ahead of the ALMA Cycle 5 call for proposals, when the Band 5 receivers will be offered for the first time. The frequency range of the Band 5 receiver has never been fully covered by existing receivers; the talks presented at the workshop illustrate the importance of several lines in this frequency range that provide crucial diagnostics of the interstellar medium.
References:
Belitsky, V. et al. 2017, A&A, in preparation Billade, B. et al. 2012, IEEE Trans. Terahertz Science Technology, 2, 208; Galametz, M. et al. 2016, MNRAS, 462, L36; Immer, K. et al. 2016, The Messenger, 165, 13; König, S. et al. 2016, A&A, submitted, arXiv:1612.07668; Molinari, S. et al. 2016, ApJ, 826, 8; Oteo, I. et al. 2017, ApJ, submitted, arXiv:1701.05901; Strandet, M. et al. 2016, ApJ, 822, 80

DOI:
10.18727/0722-6691/5003
ADS BibCode:
2017Msngr.167...16P
Section:
Astronomical Science
Author(s)/Affiliation(s):
Popescu, M.; Licandro, J.; Morate, D.; de León, J.; Nedelcu, D. A.
AA(Astronomical Institute of the Romanian Academy, Bucharest, Romania; IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ Paris 06, Université de Lille, France) AB(Instituto de Astrofísica de Canarias (IAC), La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) AC(Instituto de Astrofísica de Canarias (IAC), La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) AD(Instituto de Astrofísica de Canarias (IAC), La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain) AE(Astronomical Institute of the Romanian Academy, Bucharest, Romania; IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ Paris 06, Université de Lille, France)
Abstract:
We have carried out a serendipitous search for Solar System objects imaged by the VISTA Hemisphere Survey (VHS) and have identified 230 375 valid detections for 39 947 objects. This information is available in three catalogues, entitled MOVIS. The distributions of the data in colour-colour plots show clusters identified with the different taxonomic asteroid types. Diagrams that use (Y–J) colour separate the spectral classes more effectively than any other method based on colours. In particular, the end-class members A-, D-, R-, and V-types occupy well-defined regions and can be easily identified. About 10 000 asteroids were classified taxonomically using a probabilistic approach. The distribution of basaltic asteroids across the Main Belt was characterised using the MOVIS colours: 477 V-type candidates were found, of which 244 are outside the Vesta dynamical family.
References:
Cross, N. J. G. et al. 2012, A&A, 548, A119; DeMeo, F. E. et al. 2009, Icarus, 202, 160; DeMeo, F. E. et al. 2015, Asteroids IV, University of Arizona Press, 13; Licandro, J. et al. 2016, A&A, submitted McMahon, R. G. et al. 2013, The Messenger, 154, 35; Popescu, M. et al. 2016a, A&A, 591, A115; Popescu, M. et al. 2016b, in preparation

DOI:
10.18727/0722-6691/5004
ADS BibCode:
2017Msngr.167...20K
Section:
Astronomical Science
Author(s)/Affiliation(s):
Kervella, P.; Montargès, M.; Richards, A. M. S.; Homan, W.; Decin, L.; Lagadec, E.; Ridgway, S. T.; Perrin, G.; McDonald, I.; Ohnaka, K.
AAPierre Kervella,) AB Miguel Montargès) AC Anita M. S. Richards) AD Ward Homan) AE Leen Decin) AF Eric Lagadec) AG Stephen T. Ridgway) AH Guy Perrin) AI Iain McDonald) AJ Keiichi Ohnaka)
Abstract:
The impact of the dramatic terminal phases of the lives of Sun-like stars on their orbiting planets is currently uncertain. Observations with NAOS CONICA and SPHERE/ZIMPOL in 2014–2015 have revealed that the nearby red giant star L₂ Puppis is surrounded by an almost edge-on disc of dust and gas. We have observed several remarkable features in L₂ Pup: plumes, spirals, and a secondary source (L₂ Pup B) which is embedded in the disc at a projected separation of 2 au. ALMA observations have allowed us to measure a mass of 0.659 ± 0.043 M⊙ for the central star. This indicates that L₂ Pup is a close analogue of the future Sun at an age of 10 Gyr. We also estimate the mass of L₂ Pup B to be 12 ± 16 M_Jup, implying that it is likely a planet or a brown dwarf. L₂ Pup therefore offers us a remarkable preview of the distant future of our Solar System.
References:
Bedding, T. R. et al. 2002, MNRAS, 337, 79; Dullemond, C. P. 2012, Astrophysics Source Code Library, 1202.015; Eisenhauer, F. et al. 2011, The Messenger, 143, 16; Homan, W. et al. 2017, A&A, submitted Kervella, P. et al. 2014a, A&A, 564, A88; Kervella, P. et al. 2014b, A&A, 572, A7; Kervella, P. et al. 2015, A&A, 578, A77; Kervella, P. et al. 2016, A&A, 596, A92; Khouri, T. et al. 2016, A&A, 591, A70; Lopez, B. et al. 2014, The Messenger, 157, 5; Millour, F. et al. 2016, Proc. SPIE, 9907, 99073; Ohnaka, K., Weigelt, G. & Hofmann, K.-H. 2016, A&A, 589, A91; Ohtomo, Y. et al. 2014, Nature Geoscience, 7, 25; Sparks, W. B. et al. 2008, AJ, 135, 605; van Leeuwen, F. 2007, A&A, 474, 653; Veras, D. 2016, Royal Society Open Science, 3, 150571; Wiesemeyer, H. et al. 2009, A&A, 498, 801

DOI:
10.18727/0722-6691/5005
ADS BibCode:
2017Msngr.167...26S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Spyromilio, J.; Leibundgut, B.; Fransson, C.; Larsson, J.; Migotto, K.; Girard, J.
AA(ESO) AB(ESO) AC(Department of Astronomy, The Oskar Klein Centre, Stockholm University, Sweden) AD(Department of Astronomy, The Oskar Klein Centre, Stockholm University, Sweden) AE(Department of Astronomy, The Oskar Klein Centre, Stockholm University, Sweden) AF(ESO)
Abstract:
Thirty years on, SN 1987A continues to develop and, over the last decade in particular, has: revealed the presence of a large centrally concentrated reservoir of dust; shown the presence of molecular species within the ejecta; expanded such that the ejecta structure is angularly resolved; begun the destruction of the circumstellar ring and transitioned to being dominated by energy sources external to the ejecta. We are participating in a live experiment in the creation of a supernova remnant and here the recent progress is briefly overviewed. Exciting developments can be expected as the ejecta and the reverse shock continue their interaction, the X-rays penetrate into the cold molecular core and we observe the return of the material into the interstellar medium. We anticipate that the nature of the remnant of the leptonisation event in the centre will also be revealed.
References:
Boggs, S. E. et al. 2015, Science, 348, 670; Culhane, M. & McCray, R. 1995, ApJ, 455, 335; Danziger, I. J. 1987, Proc. ESO Workshop on SN 1987, ESO, Garching Frank, K. A. et al. 2016, ApJ, 829, 40; Fransson, C. & Chevalier, R. A. 1987, ApJ, 322, 15; Fransson, C. et al. 2007, The Messenger, 127, 44; Fransson, C. et al. 2015, ApJ, 806, L19; Fransson, C. et al. 2016, ApJ, 821, 5; Grebenev, S. A. et al. 2012, Nature, 490, 373; Indebetouw, R. et al. 2014, ApJ, 782, L2; Jerkstrand, A. et al. 2011, A&A, 530, A45; Kamenetzky, J. et al. 2013, ApJL, 773, L34; Kjaer, K. et al. 2010, A&A, 517, 51; Lakićević, M. et al. 2012, A&A, 541, L1; Larsson, J. et al. 2011, Nature, 474, 484; Larsson, J. et al. 2016, ApJ, 833, 147; Matsuura, M. et al. 2011, Science, 333, 6047; Matsuura, M. et al. 2015, ApJ, 800, 50; McCray, R. & Fransson, C. 2016, ARAA, 54, 19; Orlando, S. et al. 2015, ApJ, 810, 168; Potter, T. M. et al. 2009, ApJ, 705, 261; Zanardo, G. et al. 2014, ApJ, 796, 82

DOI:
10.18727/0722-6691/5006
ADS BibCode:
2017Msngr.167...31M
Section:
Astronomical Science
Author(s)/Affiliation(s):
McLure, R.; Pentericci, L.; the VANDELS team
AA(Institute for Astronomy, University of Edinburgh, Royal Observatory Edinburgh, United Kingdom) AB(INAF, Osservatorio Astronomico di Roma, Monteporzio, Italy)
Abstract:
VANDELS is a new ESO spectroscopic Public Survey targeting the high-redshift Universe. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the survey is obtaining ultra-deep optical spectroscopy of around 2100 galaxies in the redshift interval 1.0 < z < 7.0, with 85% of its targets selected to be at z ≥ 3. The fundamental aim of the survey is to provide the high signal-to-noise spectra necessary to measure key physical properties such as stellar population ages, metallicities and outflow velocities from detailed absorption-line studies. By targeting two extragalactic survey fields with superb multi-wavelength imaging data, VANDELS will produce a unique legacy dataset for exploring the physics underpinning high-redshift galaxy evolution.
References:
Bradshaw, E. J. et al. 2013, MNRAS, 433, 194; Brammer, G. B. et al. 2012, ApJS, 200, 13; Conselice, C. J. 2014, ARA&A, 52, 291; Daddi, E. et al. 2009, ApJL, 695, L176; de Barros, A. L. F. et al. 2014, A&A, 563, 81; Dekel, A. et al. 2009, 457, 451; Fabian, A. C. 2012, ARA&A, 50, 455; Fontana, A. et al. 2014, A&A, 570, 11; Garilli, B. et al. 2012, PASP, 124, 1232; González, V. et al. 2014, ApJ, 781, 34; Grogin, N. A. et al. 2011, ApJS, 197, 35; Guzzo, L. et al. 2014, A&A, 566, 108; Le Fèvre, O. et al. 2005, A&A, 439, 845; Le Fèvre, O. et al. 2015, A&A, 576, 79; Lilly, S. et al. 2007, ApJS, 172, 70; Mannucci, F. et al. 2010, MNRAS, 408, 211; Madau, P. & Dickinson, M. 2014, ARA&A, 52, 415; Noeske, K. G. et al. 2007, ApJL, 660, L47; Pentericci, L. et al. 2014, ApJ, 793, 113; Rogers, A. B. et al. 2014, MNRAS, 440, 3714; Shapley, A. E. et al. 2003, ApJ, 588, 65; Somerville, R. S. & Davé, R. 2015, ARA&A, 53, 51; Steidel, C. C. et al. 2016, ApJ, 826, 159; Williams, R. J. et al. 2009, ApJ, 691, 1879

DOI:
10.18727/0722-6691/5007
ADS BibCode:
2017Msngr.167...37S
Section:
Astronomical News
Author(s)/Affiliation(s):
Smette, A.; Kerber, F.; Kaufer, A.
AA(ESO) AB(ESO) AC(ESO)
Abstract:
The participants at the 2017 ESO Calibration Workshop shared their experiences and the challenges encountered in calibrating VLT second-generation instruments and the upgraded first-generation instruments, and discussed improvements in the characterisation of the atmosphere and data reduction. A small group of ESO participants held a follow-up retreat and identified possible game changers in the future operations of the La Silla Paranal Observatory: feedback on the proposals is encouraged.
References:
Kaufer, A. & Kerber, F. (eds.) 2007, Proc. ESO Instrument Calibration Workshop, ESO Astrophysics Symposia, Springer Kausch, W. et al. 2015, A&A, 576, 78; Kerber, F. et al. 2012, The Messenger, 148, 9; Kerber, F. et al. 2014, The Messenger, 155, 17; Smette, A. et al. 2015, A&A, 576, 77

DOI:
10.18727/0722-6691/5008
ADS BibCode:
2017Msngr.167...39P
Section:
Astronomical News
Author(s)/Affiliation(s):
Primas, F.; Guinot, G.; Strandberg, L.
AA(ESO) AB(CERN, European Organization for Nuclear Research, Geneva, Switzerland) AC(NordForsk, Oslo, Sweden)
Abstract:
In their role as observers on the EU Gender Equality Network in the European Research Area (GENERA) project, funded under the Horizon 2020 framework, CERN, ESO and NordForsk joined forces and organised a Gender in Physics Day at the CERN Globe of Science and Innovation. The one-day conference aimed to examine innovative activities promoting gender equality, and to discuss gender-oriented policies and best practice in the European Research Area (with special emphasis on intergovernmental organisations), as well as the importance of building solid networks. The event was very well attended and was declared a success. The main highlights of the meeting are reported.

DOI:
10.18727/0722-6691/5009
ADS BibCode:
2017Msngr.167...42D
Section:
Astronomical News
Author(s)/Affiliation(s):
Dias, B.; Milli, J.
AA(ESO) AB(ESO)
Abstract:
The Python programming language is becoming very popular within the astronomical community. Python is a high-level language with multiple applications including database management, handling FITS images and tables, statistical analysis, and more advanced topics. Python is a very powerful tool both for astronomical publications and for observatory operations. Since the best way to learn a new programming language is through practice, we therefore organised a two-day hands-on workshop to share expertise among ESO colleagues. We report here the outcome and feedback from this pilot event.

DOI:
10.18727/0722-6691/5010
ADS BibCode:
2017Msngr.167...45.
Section:
Astronomical News
Author(s)/Affiliation(s):
Sybilska, A.; De Cia, A.; Lillo Box, J.
AA(ESO) AB(ESO) AC(ESO)

ADS BibCode:
2017Msngr.167...48.
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO
AA(ESO)

ADS BibCode:
2017Msngr.167...49.
Section:
Annual Index
Author(s)/Affiliation(s):
ESO
AA(ESO)