Messenger No. 174 (December 2018)

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Telescopes and Instrumentation

2-7 (PDF)
E. Jehin et al.
The SPECULOOS Southern Observatory Begins its Hunt for Rocky Planets

DOI:
10.18727/0722-6691/5105
ADS BibCode:
2018Msngr.174....2J
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Jehin, E.; Gillon, M.; Queloz, D.; Delrez, L.; Burdanov, A.; Murray, C.; Sohy, S.; Ducrot, E.; Sebastian, D.; Thompson, S.; McCormac, J.; Almleaky, Y.; Burgasser, A.J.; Demory, B.-O.; de Wit, J.; Barkaoui, K.; Pozuelos, F.J.; Triaud, A.H.M.J.; Grootel, V.V.
AA(STAR Institute, University of Liège, Belgium) AB(Astrobiology Research Unit, University of Liège, Belgium; STAR Institute, University of Liège, Belgium) AC(Cavendish Laboratory, University of Cambridge, UK; University of Geneva, Switzerland) AD(Cavendish Laboratory, University of Cambridge, UK) AE(STAR Institute, University of Liège, Belgium) AF(Cavendish Laboratory, University of Cambridge, UK) AG(STAR Institute, University of Liège, Belgium) AH(STAR Institute, University of Liège, Belgium) AI(STAR Institute, University of Liège, Belgium) AJ(Cavendish Laboratory, University of Cambridge, UK) AK(Department of Physics, University of Warwick, UK) AL(Space and Astronomy Department, King Abdul Aziz University, Saudi Arabia) AM(Center for Astrophysics and Space Science, University of California San Diego, USA) AN(Center for Space and Habitability, University of Bern, Switzerland) AO(Department of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, USA) AP(Astrobiology Research Unit, University of Liège, Belgium; STAR Institute, University of Liège, Belgium) AQ(STAR Institute, University of Liège, Belgium) AR(School of Physics and Astronomy, University of Birmingham, UK) AS(STAR Institute, University of Liège, Belgium)
Abstract:
The SPECULOOS Southern Observatory (SSO), a new facility of four 1- metre robotic telescopes, began scientific operations at Cerro Paranal on 1 January 2019. The main goal of the SPECULOOS project is to explore approximately 1000 of the smallest (≤ 0.15 R), brightest (Kmag ≤ 12.5), and nearest (d ≤ 40 pc) very low mass stars and brown dwarfs. It aims to discover transiting temperate terrestrial planets well-suited for detailed atmospheric characterisation with future giant telescopes like ESO’s Extremely Large Telescope (ELT) and the NASA James Webb Telescope (JWST). The SSO is the core facility of SPECULOOS. The exquisite astronomical conditions at Cerro Paranal will enable SPECULOOS to detect exoplanets as small as Mars. Here, we briefly describe SPECULOOS, and present the features and performance of the SSO facility.
References:
Burdanov, A. et al. 2018, Handbook of Exoplanets, 1007; Delrez, L. et al. 2018a, Proceedings of the SPIE, 10700, 107001I Delrez, L. et al. 2018b, MNRAS, 455, 3577; McCormac, J. et al. 2013, PASP, 125, 548; Gillon, M. et al. 2011, European Physical Journal Web of Conferences, 11, 06002; Gillon, M. et al. 2016, Nature, 533, 221; Gillon, M. et al. 2017, Nature, 542, 456; Gillon, M. et al. 2018, Nature Astronomy, 2, 344; Grimm, S. et al. 2018, A&A, 613, A68; He, M. Y., Triaud, A. H. M. J. & Gillon, M. 2017, MNRAS, 464, 2687; Jehin, E. et al. 2011, The Messenger, 145, 2; Kaltenegger, L. & Traub, W. A. 2009, ApJ, 698, 51; Rodler, F. & López-Morales, M. 2014, ApJ, 781, 54; Wheatley, P. et al. 2018, MNRAS, 475, 4476
8-13 (PDF)
W. de Wit et al.
The Life and Times of AMBER: The VLTI’s Astronomical Multi-BEam combineR

DOI:
10.18727/0722-6691/5106
ADS BibCode:
2018Msngr.174....8W
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
de Wit, W.-J.; Wittkowski, M.; Rantakyrö, F.; Schöller, M.; Mérand, A.; Petrov, R.G.; Weigelt, G.; Malbet, F.; Massi, F.; Kraus, S.; Ohnaka, K.; Millour, F.; Lagarde, S.; Haubois, X.; Bourget, P.; Percheron, I.; Berger, J.-P.; Richichi, A.
AA(ESO) AB(ESO) AC(Gemini Observatory) AD(ESO) AE(ESO) AF(Université Côte d’Azur, France) AG(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AH(Institut de Planétologie et d’Astrophysique de Grenoble, France) AI(INAF–Osservatorio Astrofisico di Arcetri, Italy) AJ(University of Exeter, UK) AK(Universidad Católica del Norte, Chile) AL(Université Côte d’Azur, France) AM(Université Côte d’Azur, France) AN(ESO) AO(ESO) AP(ESO) AQ(Institut de Planétologie et d’Astrophysique de Grenoble, France) AR(INAF–Osservatorio Astrofisico di Arcetri, Italy)
Abstract:
The sharpest images on Paranal are produced by the beam-combining instruments of the Very Large Telescope Interferometer (VLTI). Currently, the VLTI is close to completing a transitional period, moving away from the first generation of instruments (AMBER, MIDI) and offering new instruments and subsystems to the community. In this article, we report on the life and achievements of the recently decommissioned, near-infrared beam combiner instrument AMBER, the most prolific optical interferometric instrument to date.
References:
Arroyo-Torres, B. et al. 2015, A&A, 575, 50; Baldwin, J. et al. 1996, A&A, 306, 13; Benisty, M. et al. 2010, A&A, 511, 75; Carciofi, A. et al. 2009, A&A, 504, 915; Chesneau, O. et al. 2007, A&A, 464, 119; Demory, B. O. et al. 2009, A&A, 505, 205; de Wit, W.-J. et al. 2014, The Messenger, 157, 50; Domiciano de Souza, M. et al. 2012, A&A, 545, 130; Gai, M. et al. 2004, SPIE, 5491, 528; Haguenauer, P. et al. 2008, SPIE, 7013, 7013C Jennison, R. 1958, MNRAS, 118, 276; Kraus, S. et al. 2008, A&A, 489, 1157; Kraus, S. et al. 2010, Nature, 466, 339; Le Bouquin, J. B. et al. 2009, A&A, 496, L1; Le Bouquin, J. B. et al. 2009, A&A, 498, 41; Malbet, F. et al. 2007, A&A, 464, 43; Malbet, F. et al. 2008, arXiv:0808.1315; Meilland, A. et al. 2007, A&A, 464, 59; Mérand, A. et al. 2014, SPIE, 9146, 9146J Ohnaka, K. et al. 2011, A&A, 529, 163; Ohnaka, K., Weigelt, G. & Hofmann, K.-H. 2017, Nature, 548, 310; Paresce, F. et al. 1996, The Messenger, 83, 14; Petrov, R. et al. 2007, A&A, 464, 1; Petrov, R. et al. 1998, The Messenger, 92, 11; Weigelt, G. et al. 2012, A&A, 541, L9; Weigelt, G. et al. 2016, A&A, 594, 106; Wittkowski, M. et al. 2008, A&A, 479, L21; Woillez, J. et al. 2015, The Messenger, 162, 16
14-17 (PDF)
T. Möller et al.
Modelling Data in CASA

DOI:
10.18727/0722-6691/5107
ADS BibCode:
2018Msngr.174...14M
Section:
Telescopes and Instrumentation
Author(s)/Affiliation(s):
Möller, T.; Schilke, P.; Hogerheijde, M.; Stewart, I.; Schaaf, R.; Harsono, D.
AA(University of Cologne, Germany) AB(University of Cologne, Germany) AC(Leiden University, the Netherlands; Allegro ALMA Regional Centre (ARC) Node, Leiden, the Netherlands; University of Amsterdam, the Netherlands) AD(Leiden University, the Netherlands; Allegro ALMA Regional Centre (ARC) Node, Leiden, the Netherlands) AE(Bonn University, Germany; German ARC Node, Argelander Institute for Astronomy, Bonn University, Germany) AF(Leiden University, the Netherlands; Allegro ALMA Regional Centre (ARC) Node, Leiden, the Netherlands)
Abstract:
The Common Astronomy Software Applications (CASA) package provides a powerful tool for post-processing Atacama Large Millimeter/submillimeter Array (ALMA) and Karl G. Jansky Very Large Array (VLA) observations, but contains only rudimentary functions for modelling the data. In order to derive physical parameters as well as information on the location and the kinematics of the emitting gas, modelling of the observed data is inescapable. Such modelling can take the form of inference — where physical parameters are inferred from the data — or forward modelling — where model calculations are used to produce synthetic observations for comparison with data. We present two interfaces that allow the use of modelling tools for both flavours from within CASA: the eXtended CASA Line Analysis Sofware Suite (XCLASS); and Adaptable Radiative Transfer Innovations for Submillimeter Telescopes (ARTIST).
References:
Allen, A., Li, Z.-Y. & Shu, F. H. 2003, ApJ, 599, 363; Bonnor, W. B. 1956, Zeitschrift für Astrophysik, 39, 143; Brinch, C. & Hogerheijde, M. R. 2010, A&A, 523, A25; Chiang, E. I. & Goldreich, P. 1997, ApJ, 490, 368; Dullemond, C. P., Dominik, C. & Natta, A. 2001, ApJ, 560, 957; Ebert, R. 1955, Zeitschrift für Astrophysik, 36, 222; Endres, C. P. et al. 2016, J. Mol. Spectrosc., 327, 95; Li, Z.-Y. & Shu, F. H. 1996, ApJ, 472, 211; Mamon, G. A., Glassgold, A. E. & Huggins, P. J. 1988, ApJ, 328, 797; McMullin, J. P. et al. 2007, Astronomical Data Analy- sis Software and Systems XVI (ASP Conf. Ser. 376), ed. Shaw, R. A., Hill, F. & Bell, D. J. (San Francisco, CA: ASP), 127; Mendoza, S., Tejeda, E. & Nagel, E. 2009, MNRAS, 393, 579; Möller, T., Endres, C. & Schilke, P. 2017, A&A, 598, A7; Möller, T. et al. 2013, A&A, 549, A21; Müller, H. S. P. et al. 2005, J. Mol. Struct., 742, 215; Padovani, M. et al. 2012, A&A, 543, A16; Pickett, H. M., Poynter, R. L. & Cohen, E. A. 1998, J. Quant. Spectr. Rad. Transf., 60, 883; Schöier, F. L. et al. 2005, A&A, 432, 369; Shu, F. H. 1977, ApJ, 214, 488; Ulrich, R. K. 1976, ApJ, 210, 377

Astronomical Science

19-23 (PDF)
S.M. Andrews et al.
ALMA Observations of the Epoch of Planet Formation

DOI:
10.18727/0722-6691/5108
ADS BibCode:
2018Msngr.174...19A
Section:
Astronomical Science
Author(s)/Affiliation(s):
Andrews, S.M.; Huang, J.; Pérez, L.M.; Isella, A.; Dullemond, C.P.; Kurtovic, N.T.; Guzmán, V.V.; Carpenter, J.M.; Wilner, D.J.; Zhang, S.; Zhu, Z.; Birnstiel, T.; Bai, X.-N.; Benisty, M.; Hughes, A.M.; Öberg, K.I.; Ricci, L.
AA(Harvard-Smithsonian Center for Astrophysics, Massachusetts, USA) AB(Harvard-Smithsonian Center for Astrophysics, Massachusetts, USA) AC(Universidad de Chile, Santiago, Chile) AD(Rice University, Houston, USA) AE(Universität Heidelberg, Germany) AF(Universidad de Chile, Santiago, Chile) AG(Joint ALMA Observatory, Santiago, Chile; Pontificia Universidad Católica de Chile, Santiago, Chile) AH(Joint ALMA Observatory, Santiago, Chile) AI(Harvard-Smithsonian Center for Astrophysics, Massachusetts, USA) AJ(University of Nevada, Las Vegas, USA) AK(University of Nevada, Las Vegas, USA) AL(Ludwig-Maximilians-Universität, Munich, Germany) AM(Institute for Advanced Study and Tsinghua Center for Astrophysics, Beijing, China) AN(Universidad de Chile, Santiago, Chile; Université Grenoble Alpes, CNRS, IPAG, France) AO(Wesleyan University, Middletown, USA) AP(Harvard-Smithsonian Center for Astrophysics, Massachusetts, USA) AQ(California State University, Northridge, USA)
Abstract:
Planetary systems form in the discs of gas and dust that orbit young stars. In the past few years, observations of these discs at (sub-)millimetre wavelengths with very fine angular resolution have started to uncover the hallmarks of small-scale substructures in the spatial distributions of their pebble-sized particles. These are some of the fundamental signatures of the planet formation epoch, since they trace localised concentrations of material that facilitate the formation of much larger planetary building blocks, and may themselves be created by young planets interacting with their birth environments.
References:
ALMA Partnership et al. 2015, ApJ Letters, 808, L3; Andrews, S. M. et al. 2011, ApJ, 732, 42; Andrews, S. M. et al. 2016, ApJ Letters, 820, L40; Andrews, S. M. et al. 2018, ApJ Letters, 869, L41; Avenhaus, H. et al. 2018, ApJ, 863, 44; Birnstiel, T. & Andrews, S. M. 2014, ApJ, 780, 153; Dullemond, C. P. et al. 2018, ApJ Letters, 869, L46; Guzmán, V. V. et al. 2018, ApJ Letters, 869, L48; Huang, J. et al. 2018a, ApJ Letters, 869, L42; Huang, J. et al. 2018b, ApJ Letters, 869, L43; Isella, A. et al. 2018, ApJ Letters, 869, L49; Kurtovic, N. T. et al. 2018, ApJ Letters, 869, L44; Pérez, L. M. et al. 2012, ApJ Letters, 760, L17; Pérez, L. M. et al. 2018, ApJ Letters, 869, L50; Pinilla, P. et al. 2012, A&A, 538, 114; Pinilla, P. et al. 2018, ApJ, 859, 32; Takeuchi, T. & Lin, D. N. C. 2002, ApJ, 581, 1344; Tripathi, A. et al. 2017, ApJ, 845, 44; Wiedenschilling, S. J. 1977, MNRAS, 180, 57; Zhang, S. et al. 2018, ApJ Letters, 869, L47
24-27 (PDF)
C. Evans et al.
A First Spectroscopic Census of the Dwarf Galaxy Leo P

DOI:
10.18727/0722-6691/5109
ADS BibCode:
2018Msngr.174...24E
Section:
Astronomical Science
Author(s)/Affiliation(s):
Evans, C.; Castro, N.; Gonzalez, O.; Garcia, M.; Bastian, N.; Cioni, M.-R.; Clark, S.; Davies, B.; Ferguson, A.; Kamann, S.; Lennon, D.; Patrick, L.; Vink, J.S.; Weisz, D.
AA(UKATC/STFC, Edinburgh, UK) AB(University of Michigan, USA; Leibniz-Institut für Astrophysik Potsdam, 
Germany 
) AC(UKATC/STFC, Edinburgh, UK) AD(Centro de Astrobiología (CSIC-INTA), Madrid, Spain) AE(Liverpool John Moores University, UK) AF(Leibniz-Institut für Astrophysik Potsdam, 
Germany 
) AG(Open University, Milton Keynes, UK) AH(Liverpool John Moores University, UK) AI(Institute for Astronomy, University of Edinburgh, UK) AJ(Liverpool John Moores University, UK) AK(ESAC, ESA, Madrid, Spain; IAC, Tenerife, Spain) AL(IAC, Tenerife, Spain; UKATC/STFC, Edinburgh, UK) AN(Armagh Observatory, UK) AO(University of California Berkeley, USA)
Abstract:
A longstanding quest in studies of luminous, massive stars has been to understand the role of environment on their evolution. The abundance of metals in their atmospheres has a significant impact on their physical properties, strongly influencing the feedback they have on their surroundings and the nature of their explosive deaths. To date we have been unable to study massive stars with metallicities below 10% that of the Sun. The low oxygen abundance (3% solar) and relative proximity (~1.6 Mpc) of Leo P, a low-luminosity dwarf galaxy discovered in 2013, provides a tantalising opportunity to investigate massive stars with near-primordial compositions. Here we introduce observations of Leo P with the Multi Unit Spectroscopic Explorer (MUSE) instrument on the VLT, which have revealed its spectroscopic content for the first time.
References:
Evans, C. et al. 2019, arxiv.org:1901.01295 Garcia, M. 2018, MNRAS, 474, L66; Giovanelli, R. et al. 2013, AJ, 146, 15; Gonzalez, O. A. & Battaglia, G. 2018, Proc. IAUS, 347, arXiv:1810.04422; Kamann, S., Wisotzki, L. & Roth, M. M. 2013, A&A, 549, A71; Lee, C. H. 2016, MNRAS, 461, L37; McQuinn, K. B. W. et al. 2013, AJ, 146, 145; McQuinn, K. B. W. et al. 2015, ApJ, 812, 158; Pflamm-Altenburg, J., Weidner, C. & Kroupa, P. 2007, ApJ, 671, 1550; Rhode, K. L. et al. 2013, AJ, 145, 149; Skillman, E. D. et al. 2013, AJ, 146, 3; Szécsi, D. et al. 2015, A&A, 581, A15
28-33 (PDF)
N.M. Förster Schreiber et al.
Witnessing the Early Growth and Life Cycle of Galaxies with KMOS3D

DOI:
10.18727/0722-6691/5110
ADS BibCode:
2018Msngr.174...28S
Section:
Astronomical Science
Author(s)/Affiliation(s):
Förster Schreiber, N.M.; Wilman, D.; Wisnioski, E.S.; Fossati, M.; Mendel, J.T.; Bender, R.; Genzel, R.; Beifiori, A.; Belli, S.; Brammer, G.; Burkert, A.; Chan, J.; Davies, R.I.; Davies, R.L.; Fabricius, M.; Galametz, A.; Herrera-Camus, R.; Lang, P.; Lutz, D.; Momcheva, I.; Naab, T.; Nelson, E.J.; Price, S.H.; Renzini, A.; Saglia, R.; Seitz, S.; Shimizu, T.; Sternberg, A.; Tacconi, L.J.; Tadaki, K.-i.; Übler, H.; van Dokkum, P.G.; Wuyts, S.
AA(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AB(Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany; Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AC(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia; ASTRO3D – ARC Centre for Excellence in All-Sky Astrophysics in 3D, Canberra, Australia) AD(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany; Department of Physics, Durham University, UK) AE(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany; Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia; ASTRO3D – ARC Centre for Excellence in All-Sky Astrophysics in 3D, Canberra, Australia) AF(Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany; Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AG(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Department of Physics and Astronomy, University of California, Berkeley, USA) AH(Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany; Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AI(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AJ(Cosmic Dawn Center, Niels Bohr Institute, University of Copenhagen, Denmark) AK(Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany; Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AL(Physics and Astronomy Department, University of California, Riverside, USA) AM(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AN(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AO(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany) AP(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany; Geneva Observatory, University of Geneva, Switzerland) AQ(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AR(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AS(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AT(Space Telescope Science Institute, Baltimore, USA) AU(Max-Planck-Institut für Astrophysik, Garching, Germany) AV(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Harvard-Smithsonian Center for Astrophysics, Cambridge, USA) AW(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) AX(INAF–Osservatorio Astronomico di Padova, Italy) AY(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany; Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany) AZ(Universitäts-Sternwarte, Ludwig-Maximilians-Universität, Munich, Germany) BA(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) BB(School of Physics and Astronomy, Tel Aviv University, Israel) BC(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) BD(National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan) BE(Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany) BF(Astronomy Department, Yale University, New Haven, USA) BG(Department of Physics, University of Bath, UK)
Abstract:
Near-infrared integral field unit (IFU) spectrographs are powerful tools for investigating galaxy evolution. We report on our recently completed multi- year KMOS3D survey of Hα, [N II] and [SII] line emission of galaxies at redshift z ~ 0.7–2.7 with the K-band Multi-Object Spectrograph (KMOS) at the Very Large Telescope (VLT). With deep observations of 745 targets spanning over two orders of magnitude in galaxy mass, five billion years of cosmic time, and all levels of star formation, KMOS3D provides an unparalleled population-wide census of spatially-resolved kinematics, star formation, outflows and nebular gas conditions. The dataset sheds new light on the physical mechanisms driving the early growth and lifecycle of galaxies, and provides a rich legacy for the astronomical community.
References:
Belli, S. et al. 2017, ApJ, 841, L6; Burkert, A. et al. 2016, ApJ, 826, 214; Förster Schreiber, N. M. et al. 2011, The Messenger, 145, 39; Förster Schreiber, N. M. et al. 2018, ApJ Suppl., 238, 21; Genzel, R. et al. 2011, ApJ, 733, 101; Genzel, R. et al. 2014, ApJ, 796, 7; Genzel, R. et al. 2017, Nature, 543, 397; Glazebrook, K. 2013, PASA, 30, 56; Krumholz, M. R. et al. 2018, MNRAS, 477, 2716; Lang, P. et al. 2014, ApJ, 788, 11; Lang, P. et al. 2017, ApJ, 840, 92; Momcheva, I. G. et al. 2016, ApJS, 255, 27; Tadaki, K. et al. 2017, ApJ, 834, 135; Übler, H. et al. 2017, ApJ, 842, 121; van der Wel, A. et al. 2014, ApJ, 788, 28; Whitaker, K. E. et al. 2014, ApJ, 795, 104; Wisnioski, E. S. et al. 2015, ApJ, 799, 209; Wisnioski, E. S. et al. 2018, ApJ, 855, 97; Wuyts, E. et al. 2016a, ApJ, 827, 74; Wuyts, S. et al. 2016b, ApJ, 831, 149
34-36 (PDF)
M. Bulla et al.
Shedding Light on the Geometry of Kilonovae

DOI:
10.18727/0722-6691/5111
ADS BibCode:
2018Msngr.174...34B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Bulla, M.; Covino, S.; Patat, F.; Kyutoku, K.; Maund, J.R.; Tanaka, M.; Toma, K.; Wiersema, K.; D’Avanzo, P.; Higgins, A.B.; Mundell, C.G.; Palazzi, E.
AA(Oskar Klein Centre, Department of Physics, Stockholm University, Sweden) AB(Istituto Nazionale di Astrofisica–Brera Astronomical Observatory, Merate, Italy) AC(ESO) AD(Theory Center, Institute of Particle and Nuclear Studies, KEK, Tsukuba, Japan; Department of Particle and Nuclear Physics, Sokendai, Tsukuba, Japan; Interdisciplinary Theoretical and Mathematical Sciences Program, RIKEN, Wako, Japan; Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Japan) AE(Department of Physics and Astronomy, University of Sheffield, UK) AF(Astronomical Institute, Tohoku University, Sendai, Japan; National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Mitaka, Japan) AG(Astronomical Institute, Tohoku University, Sendai, Japan; Frontier Research Institute for Interdisciplinary Sciences, Tohoku University, Sendai, Japan) AH(Department of Physics & Astronomy and Leicester Institute of Space & Earth Observation, University of Leicester, UK; University of Warwick, Coventry, UK) AI(Istituto Nazionale di Astrofisica–Brera Astronomical Observatory, Merate, Italy) AJ(Department of Physics & Astronomy and Leicester Institute of Space & Earth Observation, University of Leicester, UK) AK(Department of Physics, University of Bath, UK) AL(INAF–Astrophysics and Space Science Observatory, Bologna, Italy)
Abstract:
We present the first results of a campaign aimed at characterising the linear polarisation signals and thus the geometry of binary neutron star mergers (i.e., kilonovae). We carried out the first polarimetric observations of a kilonova called AT 2017gfo, using the FOcal Reducer/low dispersion Spectrograph 2 (FORS2). We predicted for the first time the polarisation signatures expected from kilonovae and highlighted the best strategy to detect linear polarisation in future events. Our studies demonstrate how the detection of polarisation will constrain crucial parameters of these systems, such as the inclination and composition, distribution and extent of the different components of the ejecta.
References:
Abbott, B. P. et al. 2017, Physics Review Letters, 119, 161101; Bulla, M. et al. 2018, Nature Astronomy, in press, arXiv:180904078; Covino, S. et al. 2017, Nature Astronomy, 1, 791

Astronomical News

38-40 (PDF)
S. Meakins et al.
ESO Conference Proceedings 2.0 at Zenodo

DOI:
10.18727/0722-6691/5112
ADS BibCode:
2018Msngr.174...38M
Section:
Astronomical News
Author(s)/Affiliation(s):
Meakins, S.; Gómez, M.E.; Bordelon, D.; Grothkopf, U.
AA(ESO) AB(ESO) AC(ESO) AD(ESO)
Abstract:
As of the past few years, ESO no longer publishes conference proceedings, mainly because of the large effort involved in their production and the relatively small impact of proceedings papers. In order to continue to preserve a record of ESO-hosted conferences, the ESO Library has implemented a system called "Conference Proceedings 2.0". Presentation slides and posters are made available through Zenodo, a CERN-developed platform for the permanent storage of digital research output, ensuring that content is citable, discoverable, and archived.
References:
Lisée, C., Larivière, V. & Archambault, E. 2008, Journal of the Association for Information Science and Technology, 59, 1776, DOI 10.1002/asi.20888; Nielsen, L. H. 2017, DOI 10.5281/zenodo.802100
40-43 (PDF)
R. Smiljanic et al.
Report on the ESO Workshop "A Revolution in Stellar Physics with Gaia and Large Surveys"

DOI:
10.18727/0722-6691/5113
ADS BibCode:
2018Msngr.174...40S
Section:
Astronomical News
Author(s)/Affiliation(s):
Smiljanic, R.; Hussain, G.; Pasquini, L.
AA(Nicolaus Copernicus Astronomical Center, PAN, Warsaw, Poland) AB(ESO) AC(ESO)
Abstract:
The exquisite astrometry and photometry of ESA’s Gaia satellite combined with data from other large photometric, spectroscopic, and asteroseismic stellar surveys are enabling a revolution in our understanding of stellar physics. The goal of this workshop was to bring together a diverse community working on or making use of various aspects of stellar physics. The discussions covered both recent advances in the field and expectations for when new data and surveys become available.
44-47 (PDF)
C.F. Manara et al.
Report on the ESO Workshop "Take a Closer Look: The Innermost Region of Protoplanetary Discs and its Connection to the Origin of Planets"

DOI:
10.18727/0722-6691/5114
ADS BibCode:
2018Msngr.174...44M
Section:
Astronomical News
Author(s)/Affiliation(s):
Manara, C.F.; Schneider, P.C.; Hussain, G.; Facchini, S.; Miotello, A.
AA(ESO) AB(Hamburg Observatory, Germany) AC(ESO) AD(ESO) AE(ESO)
Abstract:
About 150 scientists from all over the world convened at the ESO Headquarters to discuss the origin of close-in exoplanets and the properties of the inner regions of protoplanetary discs, where these planets are formed. In a cordial atmosphere, made possible by the collaborative attitude of the very diverse group of attendees, the discussion led to a deeper appreciation of the importance of several observing techniques and of advances in modelling to tackle key open questions. In addition, the participants had the chance to experience a special show at the ESO Supernova Planetarium & Visitor Centre, which highlighted the potential of this facility.
48-52 (PDF)
C. Chen et al.
Fellows at ESO

DOI:
10.18727/0722-6691/5115
ADS BibCode:
2018Msngr.174...48E
Section:
Astronomical News
Author(s)/Affiliation(s):
Chen, C.-C.; Gallenne, A.; Wylezalek, D.
AA(ESO) AB(ESO) AC(ESO)
53-54 (PDF)
X. Barcons, J. Spyromilio
Riccardo Giacconi (1931–2018)

DOI:
10.18727/0722-6691/5116
ADS BibCode:
2018Msngr.174...53B
Section:
Astronomical News
Author(s)/Affiliation(s):
Barcons, X.; Spyromilio, J.
AA(ESO) AB(ESO)
References:
Giacconi, R. 1993, The Messenger, 72, 1
55-55 (PDF)
ESO
Personnel Movements

ADS BibCode:
2018Msngr.174...55E
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO