Messenger No. 180 (Quarter 2 | 2020)

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The Organisation

3-8 (PDF)
Ferrini, F., Wild, W.
The Cherenkov Telescope Array Observatory Comes of Age

DOI:
10.18727/0722-6691/5194
ADS BibCode:
2020Msngr.180....3F
Section:
The Organisation
Author(s)/Affiliation(s):
Ferrini, F.; Wild, W.
AA(CTAO, Heidelberg (DE) and Bologna (IT)) AB(CTAO, Heidelberg (DE) and Bologna (IT); ESO)
Abstract:
The Cherenkov Telescope Array (CTA) is the next-generation ground-based observatory for gamma-ray astronomy at very high energies. With up to 120 telescopes on two sites, CTA will be the world’s largest and most sensitive high-energy gamma-ray observatory covering the entire sky. It will consist of a northern array located at the Roque de los Muchachos astronomical observatory on the island of La Palma (Spain) and a southern array near the European Southern Observatory site at Paranal (Chile). Three classes of telescope spread over a large area are required to cover all of CTA’s very-high-energy range from 20 GeV to 300 TeV.
References:
Hofmann, W. 2017, The Messenger, 168, 21 The CTA Consortium 2018, arxiv:1709.07997

MOONS

10-17 (PDF)
Cirasuolo, M. et al.
MOONS: The New Multi-Object Spectrograph for the VLT

DOI:
10.18727/0722-6691/5195
ADS BibCode:
2020Msngr.180...10C
Section:
MOONS
Author(s)/Affiliation(s):
Cirasuolo, M.; Fairley, A.; Rees, P.; Gonzalez, O.A.; Taylor, W.; Maiolino, R.; Afonso, J.; Evans, C.; Flores, H.; Lilly, S.; Oliva, E.; Paltani, S.; Vanzi, L.; Abreu, M.; Accardo, M.; Adams, N.; Álvarez Méndez, D.; Amans, J.-P.; Amarantidis, S.; Atek, H.; Atkinson, D.; Banerji, M.; Barrett, J.; Barrientos, F.; Bauer, F.; Beard, S.; Béchet, C.; Belfiore, A.; Bellazzini, M.; Benoist, C.; Best, P.; Biazzo, K.; Black, M.; Boettger, D.; Bonifacio, P.; Bowler, R.; Bragaglia, A.; Brierley, S.; Brinchmann, J.; Brinkmann, M.; Buat, V.; Buitrago, F.; Burgarella, D.; Burningham, B.; Buscher, D.; Cabral, A.; Caffau, E.; Cardoso, L.; Carnall, A.; Carollo, M.; Castillo, R.; Castignani, G.; Catelan, M.; Cicone, C.; Cimatti, A.; Cioni, M.-R.L.; Clementini, G.; Cochrane, W.; Coelho, J.; Colling, M.; Contini, T.; Contreras, R.; Conzelmann, R.; Cresci, G.; Cropper, M.; Cucciati, O.; Cullen, F.; Cumani, C.; Curti, M.; Da Silva, A.; Daddi, E.; Dalessandro, E.; Dalessio, F.; Dauvin, L.; Davidson, G.; de Laverny, P.; Delplancke-Ströbele, F.; De Lucia, G.; Del Vecchio, C.; Dessauges-Zavadsky, M.; Di Matteo, P.; Dole, H.; Drass, H.; Dunlop, J.; Dünner, R.; Eales, S.; Ellis, R.; Enriques, B.; Fasola, G.; Ferguson, A.; Ferruzzi, D.; Fisher, M.; Flores, M.; Fontana, A.; Forchi, V.; Francois, P.; Franzetti, P.; Gargiulo, A.; Garilli, B.; Gaudemard, J.; Gieles, M.; Gilmore, G.; Ginolfi, M.; Gomes, J.M.; Guinouard, I.; Gutierrez, P.; Haigron, R.; Hammer, F.; Hammersley, P.; Haniff, C.; Harrison, C.; Haywood, M.; Hill, V.; Hubin, N.; Humphrey, A.; Ibata, R.; Infante, L.; Ives, D.; Ivison, R.; Iwert, O.; Jablonka, P.; Jakob, G.; Jarvis, M.; King, D.; Kneib, J.-P.; Laporte, P.; Lawrence, A.; Lee, D.; Li Causi, G.; Lorenzoni, S.; Lucatello, S.; Luco, Y.; Macleod, A.; Magliocchetti, M.; Magrini, L.; Mainieri, V.; Maire, C.; Mannucci, F.; Martin, N.; Matute, I.; Maurogordato, S.; McGee, S.; Mcleod, D.; McLure, R.; McMahon, R.; Melse, B.-T.; Messias, H.; Mucciarelli, A.; Nisini, B.; Nix, J.; Norberg, P.; Oesch, P.; Oliveira, A.; Origlia, L.; Padilla, N.; Palsa, R.; Pancino, E.; Papaderos, P.; Pappalardo, C.; Parry, I.; Pasquini, L.; Peacock, J.; Pedichini, F.; Pello, R.; Peng, Y.; Pentericci, L.; Pfuhl, O.; Piazzesi, R.; Popovic, D.; Pozzetti, L.; Puech, M.; Puzia, T.; Raichoor, A.; Randich, S.; Recio-Blanco, A.; Reis, S.; Reix, F.; Renzini, A.; Rodrigues, M.; Rojas, F.; Rojas-Arriagada, Á.; Rota, S.; Royer, F.; Sacco, G.; Sanchez-Janssen, R.; Sanna, N.; Santos, P.; Sarzi, M.; Schaerer, D.; Schiavon, R.; Schnell, R.; Schultheis, M.; Scodeggio, M.; Serjeant, S.; Shen, T.-C.; Simmonds, C.; Smoker, J.; Sobral, D.; Sordet, M.; Spérone, D.; Strachan, J.; Sun, X.; Swinbank, M.; Tait, G.; Tereno, I.; Tojeiro, R.; Torres, M.; Tosi, M.; Tozzi, A.; Tresiter, E.; Valenti, E.; Valenzuela Navarro, Á.; Vanzella, E.; Vergani, S.; Verhamme, A.; Vernet, J.; Vignali, C.; Vinther, J.; Von Dran, L.; Waring, C.; Watson, S.; Wild, V.; Willesme, B.; Woodward, B.; Wuyts, S.; Yang, Y.; Zamorani, G.; Zoccali, M.; Bluck, A.; Trussler, J.
AA(ESO) AB(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) AC(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) AD(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) AE(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) AF(Cavendish Laboratory, University of Cambridge, UK) AG(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) AH(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) AI(GEPI, Observatoire de Paris, PSL University, CNRS, France) AJ(Department of Physics, ETH Zurich, Switzerland) AK(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) AL(Department of Astronomy, University of Geneva, Versoix, Switzerland) AM(Pontificia Universidad Católica de Chile, Santiago, Chile) AN(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) AO(ESO) AP(Department of Physics, University of Oxford, UK) AQ(ESO) AR(GEPI, Observatoire de Paris, PSL University, CNRS, France) AS(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) AT(GEPI, Observatoire de Paris, PSL University, CNRS, France) AU(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) AV(Faculty of Engineering and Physical Sciences, University of Southampton, UK) AW(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) AX(Pontificia Universidad Católica de Chile, Santiago, Chile) AY(Pontificia Universidad Católica de Chile, Santiago, Chile) AZ(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) BA(Pontificia Universidad Católica de Chile, Santiago, Chile) BB(INAF, IASF-MI, Milano, Italy) BC(INAF – Astrophysics and Space Science Observatory Bologna, Italy) BD(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) BE(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) BF(INAF – Osservatorio Astronomico di Roma, Italy) BG(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) BH(Pontificia Universidad Católica de Chile, Santiago, Chile) BI(GEPI, Observatoire de Paris, PSL University, CNRS, France) BJ(Department of Physics, University of Oxford, UK) BK(INAF – Astrophysics and Space Science Observatory Bologna, Italy) BL(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) BM(Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Porto, Portugal) BN(ESO) BO(Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France) BP(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) BQ(Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France) BR(School of Physics Astronomy and Mathematics, University of Hertfordshire, UK) BS(Cavendish Laboratory, University of Cambridge, UK) BT(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) BU(GEPI, Observatoire de Paris, PSL University, CNRS, France) BV(Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Porto, Portugal) BW(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) BX(Department of Physics, ETH Zurich, Switzerland) BY(ESO) BZ(EPFL, Observatoire de Sauverny, Versoix, Switzerland) CA(Pontificia Universidad Católica de Chile, Santiago, Chile) CB(Institute of Theoretical Astrophysics, University of Oslo, Norway) CC(University of Bologna, Department of Physics and Astronomy (DIFA), Italy) CD(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CE(INAF – Astrophysics and Space Science Observatory Bologna, Italy) CF(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) CG(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) CH(STFC, Daresbury Laboratory, Sci-Tech Daresbury, UK) CI(Institut de Recherche en Astrophysique et Planétologie, Toulouse, France) CJ(Pontificia Universidad Católica de Chile, Santiago, Chile) CK(ESO) CL(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) CM(UCL Department of Space and Climate Physics, London, UK) CN(INAF – Astrophysics and Space Science Observatory Bologna, Italy) CO(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) CP(ESO) CQ(Cavendish Laboratory, University of Cambridge, UK) CR(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) CS(CEA, IRFU, DAp, AIM, Université Paris-Saclay, Université Paris Diderot, France) CT(INAF – Astrophysics and Space Science Observatory Bologna, Italy) CU(INAF – Osservatorio Astronomico di Roma, Italy) CV(Pontificia Universidad Católica de Chile, Santiago, Chile) CW(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) CX(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) CY(ESO) CZ(INAF – Osservatorio Astronomico di Trieste, Italy) DA(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) DB(Department of Astronomy, University of Geneva, Versoix, Switzerland) DC(GEPI, Observatoire de Paris, PSL University, CNRS, France) DD(Institut d’Astrophysique Spatiale, Orsay, Université Paris Sud, France) DE(Pontificia Universidad Católica de Chile, Santiago, Chile) DF(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) DG(Pontificia Universidad Católica de Chile, Santiago, Chile) DH(School of Physics and Astronomy, University of Cardiff, UK) DI(Dept of Physics & Astronomy, University College London, UK) DJ(Department of Physics, ETH Zurich, Switzerland) DK(GEPI, Observatoire de Paris, PSL University, CNRS, France) DL(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) DM(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) DN(Cavendish Laboratory, University of Cambridge, UK) DO(Pontificia Universidad Católica de Chile, Santiago, Chile) DP(INAF – Osservatorio Astronomico di Roma, Italy) DQ(ESO) DR(GEPI, Observatoire de Paris, PSL University, CNRS, France) DS(INAF, IASF-MI, Milano, Italy) DT(INAF, IASF-MI, Milano, Italy) DU(INAF, IASF-MI, Milano, Italy) DV(GEPI, Observatoire de Paris, PSL University, CNRS, France) DW(Astrophysics Research Group, Surrey University, UK) DX(Cavendish Laboratory, University of Cambridge, UK) DY(Department of Astronomy, University of Geneva, Versoix, Switzerland) DZ(Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Porto, Portugal) EA(GEPI, Observatoire de Paris, PSL University, CNRS, France) EB(ESO) EC(GEPI, Observatoire de Paris, PSL University, CNRS, France) ED(GEPI, Observatoire de Paris, PSL University, CNRS, France) EE(ESO) EF(Cavendish Laboratory, University of Cambridge, UK) EG(ESO) EH(GEPI, Observatoire de Paris, PSL University, CNRS, France) EI(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) EJ(ESO) EK(Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Porto, Portugal) EL(Observatoire Astronomique, Université de Strasbourg, France) EM(Pontificia Universidad Católica de Chile, Santiago, Chile) EN(ESO) EO(ESO) EP(ESO) EQ(EPFL, Observatoire de Sauverny, Versoix, Switzerland) ER(ESO) ES(Department of Physics, University of Oxford, UK) ET(Cavendish Laboratory, University of Cambridge, UK) EU(EPFL, Observatoire de Sauverny, Versoix, Switzerland) EV(GEPI, Observatoire de Paris, PSL University, CNRS, France) EW(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) EX(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) EY(INAF – Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy) EZ(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) FA(INAF – Osservatorio Astronomico di Padova, Italy) FB(Pontificia Universidad Católica de Chile, Santiago, Chile) FC(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) FD(INAF – Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy) FE(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) FF(ESO) FG(Department of Astronomy, University of Geneva, Versoix, Switzerland) FH(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) FI(Observatoire Astronomique, Université de Strasbourg, France) FJ(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) FK(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) FL(School of Physics and Astronomy, University of Birmingham, UK) FM(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) FN(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) FO(Cavendish Laboratory, University of Cambridge, UK) FP(GEPI, Observatoire de Paris, PSL University, CNRS, France) FQ(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) FR(University of Bologna, Department of Physics and Astronomy (DIFA), Italy) FS(INAF – Osservatorio Astronomico di Roma, Italy) FT(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) FU(Department of Physics, Durham University, UK) FV(Department of Astronomy, University of Geneva, Versoix, Switzerland) FW(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) FX(INAF – Astrophysics and Space Science Observatory Bologna, Italy) FY(Pontificia Universidad Católica de Chile, Santiago, Chile) FZ(ESO) GA(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) GB(Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Porto, Portugal) GC(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) GD(Cavendish Laboratory, University of Cambridge, UK) GE(ESO) GF(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) GG(INAF – Osservatorio Astronomico di Roma, Italy) GH(Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France) GI(Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China) GJ(INAF – Osservatorio Astronomico di Roma, Italy) GK(ESO) GL(INAF – Osservatorio Astronomico di Roma, Italy) GM(ESO) GN(INAF – Astrophysics and Space Science Observatory Bologna, Italy) GO(GEPI, Observatoire de Paris, PSL University, CNRS, France) GP(Pontificia Universidad Católica de Chile, Santiago, Chile) GQ(EPFL, Observatoire de Sauverny, Versoix, Switzerland) GR(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) GS(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) GT(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) GU(GEPI, Observatoire de Paris, PSL University, CNRS, France) GV(INAF – Osservatorio Astronomico di Padova, Italy) GW(GEPI, Observatoire de Paris, PSL University, CNRS, France) GX(Pontificia Universidad Católica de Chile, Santiago, Chile) GY(Pontificia Universidad Católica de Chile, Santiago, Chile) GZ(INAF, IASF-MI, Milano, Italy) HA(GEPI, Observatoire de Paris, PSL University, CNRS, France) HB(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) HC(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) HD(INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) HE(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) HF(Armagh Observatory & Planetarium, Armagh, Northern Ireland) HG(Department of Astronomy, University of Geneva, Versoix, Switzerland) HH(Liverpool John Moores University, UK) HI(Department of Astronomy, University of Geneva, Versoix, Switzerland) HJ(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) HK(INAF, IASF-MI, Milano, Italy) HL(School of Physical Sciences, The Open University, Milton Keynes, UK) HM(BlueShadows Ltda., Santiago, Chile) HN(EPFL, Observatoire de Sauverny, Versoix, Switzerland) HO(ESO) HP(Department of Physics, University of Lancaster, UK) HQ(Department of Astronomy, University of Geneva, Versoix, Switzerland) HR(EPFL, Observatoire de Sauverny, Versoix, Switzerland) HS(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) HT(Cavendish Laboratory, University of Cambridge, UK) HU(Department of Physics, Durham University, UK) HV(STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) HW(Instituto de Astrofísica e Ciências do Espaço and Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) HX(School of Physics and Astronomy, University of St Andrews, UK) HY(Pontificia Universidad Católica de Chile, Santiago, Chile) HZ(INAF – Astrophysics and Space Science Observatory Bologna, Italy) (INAF-Osservatorio Astrofisico di Arcetri, Florence, Italy) (Pontificia Universidad Católica de Chile, Santiago, Chile) (ESO) (Pontificia Universidad Católica de Chile, Santiago, Chile) (INAF – Astrophysics and Space Science Observatory Bologna, Italy) (GEPI, Observatoire de Paris, PSL University, CNRS, France) (EPFL, Observatoire de Sauverny, Versoix, Switzerland) (ESO) (INAF – Astrophysics and Space Science Observatory Bologna, Italy) (ESO) (Appleton Laboratory, STFC, Harwell Campus, UK) (STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) (STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) (School of Physics and Astronomy, University of St Andrews, UK) (STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) (STFC, UK Astronomy Technology Centre, Royal Observatory Edinburgh, UK) (Department of Physics, University of Bath, UK) (GEPI, Observatoire de Paris, PSL University, CNRS, France) (INAF – Astrophysics and Space Science Observatory Bologna, Italy) (Pontificia Universidad Católica de Chile, Santiago, Chile) (Cavendish Laboratory, University of Cambridge, UK) (Cavendish Laboratory, University of Cambridge, UK)
Abstract:
MOONS is the new Multi-Object Optical and Near-infrared Spectrograph currently under construction for the Very Large Telescope (VLT) at ESO. This remarkable instrument combines, for the first time, the collecting power of an 8-m telescope, 1000 fibres with individual robotic positioners, and both low- and high-resolution simultaneous spectral coverage across the 0.64–1.8 μm wavelength range. This facility will provide the astronomical community with a powerful, world-leading instrument able to serve a wide range of Galactic, extragalactic and cosmological studies. Construction is now proceeding full steam ahead and this overview article presents some of the science goals and the technical description of the MOONS instrument. More detailed information on the MOONS surveys is provided in the other dedicated articles in this Messenger issue.
References:
Rodrigues, M. et al. 2012, Proceedings of the SPIE, 8450E, 3HR
18-23 (PDF)
Gonzalez, O.A. et al.
MOONS Surveys of the Milky Way and its Satellites

DOI:
10.18727/0722-6691/5196
ADS BibCode:
2020Msngr.180...18G
Section:
MOONS
Author(s)/Affiliation(s):
Gonzalez, O.A.; Mucciarelli, A.; Origlia, L.; Schultheis, M.; Caffau, E.; Di Matteo, P.; Randich, S.; Recio-Blanco, A.; Zoccali, M.; Bonifacio, P.; Dalessandro, E.; Schiavon, R.P.; Pancino, E.; Taylor, W.; Valenti, E.; Rojas-Arriagada, Á.; Sacco, G.; Biazzo, K.; Bellazzini, M.; Cioni, M.-R.L.; Clementini, G.; Contreras Ramos, R.; de Laverny, P.; Evans, C.; Haywood, M.; Hill, V.; Ibata, R.; Lucatello, S.; Magrini, L.; Martin, N.; Nisini, B.; Sanna, N.; Cirasuolo, M.; Maiolino, R.; Afonso, J.; Lilly, S.; Flores, H.; Oliva, E.; Paltani, S.; Vanzi, L.
AA(UK Astronomy Technology Centre, Edinburgh, UK) AB(Università di Bologna, Italy; INAF – Astrophysics and Space Science Observatory Bologna, Italy) AC(INAF – Astrophysics and Space Science Observatory Bologna, Italy) AD(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) AE(GEPI, Observatoire de Paris, Université PSL, CNRS, France) AF(GEPI, Observatoire de Paris, Université PSL, CNRS, France) AG(INAF – Osservatorio Astrofisico di Arcetri, Italy) AH(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) AI(Pontificia Universidad Católica de Chile, Chile; Millennium Institute of Astrophysics, Chile) AJ(GEPI, Observatoire de Paris, Université PSL, CNRS, France) AK(INAF – Astrophysics and Space Science Observatory Bologna, Italy) AL(Liverpool John Moores University, UK) AM(INAF – Osservatorio Astrofisico di Arcetri, Italy) AN(UK Astronomy Technology Centre, Edinburgh, UK) AO(ESO) AP(Pontificia Universidad Católica de Chile, Chile; Millennium Institute of Astrophysics, Chile) AQ(INAF – Osservatorio Astrofisico di Arcetri, Italy) AR(INAF – Osservatorio Astronomico di Roma, Italy) AS(INAF – Astrophysics and Space Science Observatory Bologna, Italy) AT(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AU(INAF – Astrophysics and Space Science Observatory Bologna, Italy) AV(Pontificia Universidad Católica de Chile, Chile; Millennium Institute of Astrophysics, Chile) AW(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) AX(UK Astronomy Technology Centre, Edinburgh, UK) AY(GEPI, Observatoire de Paris, Université PSL, CNRS, France) AZ(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France) BA(Observatoire Astronomique, Université de Strasbourg, France) BB(INAF – Osservatorio Astronomico di Padova, Italy) BC(INAF – Osservatorio Astrofisico di Arcetri, Italy) BD(Observatoire Astronomique, Université de Strasbourg, France) BE(INAF – Osservatorio Astronomico di Roma, Italy) BF(INAF – Osservatorio Astrofisico di Arcetri, Italy) BG(ESO) BH(Department of Physics, Cavendish Laboratory, Cambridge, UK) BI(Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa, Portugal; Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) BJ(ETH Zurich, Switzerland) BK(GEPI, Observatoire de Paris, Université PSL, CNRS, France) BL(INAF – Osservatorio Astrofisico di Arcetri, Italy) BM(University of Geneva, Switzerland) BN(Pontificia Universidad Católica de Chile, Chile)
Abstract:
The study of resolved stellar populations in the Milky Way and other Local Group galaxies can provide us with a fossil record of their chemo-dynamical and star-formation histories over timescales of many billions of years. In the galactic components and stellar systems of the Milky Way and its satellites, individual stars can be resolved. Therefore, they represent a unique laboratory in which to investigate the details of the processes behind the formation and evolution of the disc and dwarf/irregular galaxies. MOONS at the VLT represents a unique combination of an efficient infrared multi-object spectrograph and a large-aperture 8-m-class telescope which will sample the cool stellar populations of the dense central regions of the Milky Way and its satellites, delivering accurate radial velocities, metallicities, and other chemical abundances for several millions of stars over its lifetime (see Cirasuolo et al., p. 10). MOONS will observe up to 1000 targets across a 25-arcminute field of view in the optical and near-infrared (0.6–1.8 µm) simultaneously. A high-resolution (R ~ 19700) setting in the H band has been designed for the accurate determination of stellar abundances such as alpha, light, iron-peak and neutron-capture elements.
References:
Bellazzini, M. et al. 2008, AJ, 136, 1147; Bensby, T. et al. 2017, A&A, 605, A89; Brown, T. M. et al. 2009, AJ, 137, 3172; Carrera, R. et al. 2011, AJ, 142, 61; Cioni, M.-R. L. et al. 2011, A&A, 527, 116; de Boer, T. J. L., Belokurov, V. & Koposov, S. 2015, MNRAS, 451, 3489; Dobbie, P. D. et al. 2014, MNRAS, 442, 1680; Erwin, P. & Debattista, V. P. 2017, MNRAS, 468, 2058; Gaia Collaboration, Helmi, A. et al. 2018, A&A, 616, A12; Haywood, M. et al. 2016, A&A, 593, A82 Ibata, R. A., Gilmore, G. & Irwin, M. J. 1994, Nature, 370, 194; Majewski, S. R. et al. 2003, ApJ, 599, 1082 Mucciarelli, A. et al. 2017, A&A, 605, 46; Nidever, D. et al. 2020, ApJ, 895, 88; Rojas-Arriagada, A. et al. 2019, A&A, 626, A16 Wegg, C., Gerhard, O. & Portail, M. 2015, MNRAS, 450, 4050
24-29 (PDF)
Maiolino, R. et al.
MOONRISE: The Main MOONS GTO Extragalactic Survey

DOI:
10.18727/0722-6691/5197
ADS BibCode:
2020Msngr.180...24M
Section:
MOONS
Author(s)/Affiliation(s):
Maiolino, R.; Cirasuolo, M.; Afonso, J.; Bauer, F.E.; Bowler, R.; Cucciati, O.; Daddi, E.; De Lucia, G.; Evans, C.; Flores, H.; Gargiulo, A.; Garilli, B.; Jablonka, P.; Jarvis, M.; Kneib, J.-P.; Lilly, S.; Looser, T.; Magliocchetti, M.; Man, Z.; Mannucci, F.; Maurogordato, S.; McLure, R.J.; Norberg, P.; Oesch, P.; Oliva, E.; Paltani, S.; Pappalardo, C.; Peng, Y.; Pentericci, L.; Pozzetti, L.; Renzini, A.; Rodrigues, M.; Royer, F.; Serjeant, S.; Vanzi, L.; Wild, V.; Zamorani, G.
AA(Kavli Institute for Cosmology, University of Cambridge, UK; Cavendish Laboratory, University of Cambridge, UK; Department of Physics and Astronomy, University College London, UK) AB(ESO) AC(Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa, Portugal; Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) AD(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile,; Millennium Institute of Astrophysics (MAS), Santiago, Chile; Space Science Institute, Boulder, USA) AE(Department of Physics, University of Oxford, UK) AF(INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Italy) AG(CEA, IRFU, DAp, AIM, Université Paris-Saclay, Université Paris Diderot, France) AH(INAF – Osservatorio Astronomico di Trieste, Italy) AI(UK Astronomy Technology Centre, Edinburgh, UK) AJ(GEPI, Observatoire de Paris, PSL University, CNRS, Meudon, France) AK(INAF, IASF-MI, Milano, Italy) AL(INAF, IASF-MI, Milano, Italy) AM(GEPI, Observatoire de Paris, PSL University, CNRS, Meudon, France; Physics Institute, Laboratoire d’Astrophysique, EPFL, Switzerland) AN(Department of Physics, University of Oxford, UK) AO(Physics Institute, Laboratoire d’Astrophysique, EPFL, Switzerland) AP(Department of Physics, ETH Zurich, Switzerland) AQ(Department of Physics, ETH Zurich, Switzerland) AR(INAF – IAPS, Roma, Italy) AS(Kavli Institute for Astronomy and Astrophysics, Peking University, China) AT(INAF – Osservatorio Astrofisico di Arcetri, Firenze, Italy) AU(Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Nice cedex 4, France) AV(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK) AW(Department of Physics, Durham University, UK) AX(Department of Astronomy, University of Geneva, Versoix, Switzerland; Cosmic Dawn Center (DAWN), Copenhagen, Denmark) AY(INAF – Osservatorio Astrofisico di Arcetri, Firenze, Italy) AZ(Department of Astronomy, University of Geneva, Versoix, Switzerland) BA(Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa, Portugal; Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Portugal) BB(Kavli Institute for Astronomy and Astrophysics, Peking University, China) BC(INAF – Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy) BD(INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Italy) BE(INAF – Osservatorio Astronomico di Padova, Italy) BF(Department of Physics, University of Oxford, UK; GEPI, Observatoire de Paris, PSL University, CNRS, Meudon, France) BG(GEPI, Observatoire de Paris, PSL University, CNRS, Meudon, France) BH(School of Physical Sciences, The Open University, Milton Keynes, UK) BI(Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile,) BJ(School of Physics and Astronomy, University of St Andrews, UK) BK(INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Italy)
Abstract:
The MOONS instrument possesses an exceptional combination of large multiplexing, high sensitivity, broad simultaneous spectral coverage (from optical to near-infrared bands), large patrol area and high fibre density. These properties provide the unprecedented potential of enabling, for the very first time, SDSS-like surveys around Cosmic Noon (z ~ 1–2.5), when the star formation rate in the Universe peaked. The high-quality spectra delivered by MOONS will sample the same nebular and stellar diagnostics observed in extensive surveys of local galaxies, providing an accurate and consistent description of the evolution of various physical properties of galaxies, and hence a solid test of different scenarios of galaxy formation and transformation. Most importantly, by spectroscopically identifying hundreds of thousands of galaxies at high redshift, the MOONS surveys will be capable of determining the environments in which primeval galaxies lived and will reveal how such environments affected galaxy evolution. In this article, we specifically focus on the main Guaranteed Time Observation (GTO) MOONS extragalactic survey, MOONRISE, by providing an overview of its scientific goals and observing strategy.
References:
Baldwin, J. A., Phillips, M. M. & Terlevich, R. 1981, PASP, 93, 5; Carnall, A. C. et al. 2019, submitted to MNRAS, arXiv:2001.11975; Cicone, C. et al. 2016, A&A, 588, A41; Citro, A. et al. 2016, A&A, 592, A19; Concas, A. et al. 2017, A&A, 606, A36; Concas, A. et al. 2019, A&A, 622, A188; Cullen, F. et al. 2019, MNRAS, 487, 2038; De Lucia, G. et al. 2017, MNRAS, 466, L88; Gallagher, R. et al. 2019, MNRAS, 485, 3409; Jarvis, M. et al. 2013, MNRAS, 428, 1281; Kashino, D. et al. 2019, ApJS, 241, 10; Laigle, C. et al. 2016, ApJS, 224, 24; Maiolino, R. & Mannucci, F. 2019, A&Arv, 27, 3; Mannucci, F. et al. 2010, MNRAS, 408, 2115; Merlin, E. et al. 2019, MNRAS, 430, 3309; Nayyeri, H. et al. 2017, ApJS, 228, 7; Nedelchev, B. et al. 2019, MNRAS, 486, 1608; Peng, Y. et al. 2010, ApJ, 721, 193; Pipino, A. et al. 2008, A&A, 484, 679; Springel, V. et al. 2005, Nature, 435, 629; Troncoso, P. et al. 2014, A&A, 563, A58; Trussler, J. et al. 2019, MNRAS, 491, 5406; Thomas, D. et al. 2010, MNRAS, 404, 1775; Vincenzo, F. et al. 2016, MNRAS, 458, 3466; Wild, V. et al. 2020, MNRAS, 494, 52

Astronomical Science

31-36 (PDF)
Béthermin, M. et al.
The ALPINE–ALMA [CII] Survey: Exploring the Dark Side of Normal Galaxies at the End of Reionisation

DOI:
10.18727/0722-6691/5198
ADS BibCode:
2020Msngr.180...31B
Section:
Astronomical Science
Author(s)/Affiliation(s):
Béthermin, M.; Dessauges-Zavadsky, M.; Faisst, A.L.; Ginolfi, M.; Gruppioni, C.; Jones, G.C.; Khusanova, Y.; Lemaux, B.; Capak, P.L.; Cassata, P.; Le Fèvre, O.; Schaerer, D.; Silverman, J.D.; Yan, L.; The Alpine collaboration
AA(Aix Marseille Université, CNRS, CNES, LAM, Marseille, France) AB(Département d’Astronomie, Université de Genève, Versoix, Switzerland) AC(IPAC, M/C 314-6, California Institute of Technology, Pasadena, USA) AD(Département d’Astronomie, Université de Genève, Versoix, Switzerland) AE(INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Italy) AF(Cavendish Laboratory, University of Cambridge, UK; Kavli Institute for Cosmology, University of Cambridge, UK) AG(Aix Marseille Université, CNRS, CNES, LAM, Marseille, France; Max-Planck-Institut für Astronomie, Heidelberg, Germany) AH(Department of Physics, University of California Davis, USA) AI(IPAC, M/C 314-6, California Institute of Technology, Pasadena, USA; The Cosmic Dawn Center (DAWN), University of Copenhagen, Denmark; Niels Bohr Institute, University of Copenhagen, Denmark) AJ(Dipartimento di Fisica e Astronomia, Università di Padova, Italy; INAF – Osservatorio Astronomico di Padova, Italy) AK(Aix Marseille Université, CNRS, CNES, LAM, Marseille, France) AL(Département d’Astronomie, Université de Genève, Versoix, Switzerland) AM(Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Kashiwa, Japan; Department of Astronomy, School of Science, The University of Tokyo, Japan) AN(The Caltech Optical Observatories, California Institute of Technology, Pasadena, USA)
Abstract:
Cold gas and cosmic dust are the fuel of star formation. ALPINE is an ALMA Large Programme which has built the first statistically representative sample of star-forming galaxies in the adolescent Universe by targeting emission from singly ionised carbon [CII] at 158 µm, which traces both emission from star-forming regions and molecular hydrogen gas clouds, and the thermal continuum from dust at the end of the epoch of reionisation (4.4 < z < 5.9). Observations by the ALPINE team have revealed that a significant fraction of the star formation at this epoch is already hidden by dust clouds. ALPINE observations have also shown how unruly these young galaxies were by finding a large fraction of mergers and ubiquitous gas outflows.
References:
Béthermin, M. et al. 2020, accepted by A&A, arxiv:2002.00962; Capak, P. L. et al. 2015, Nature, 522, 455; Cassata, P. et al. 2020, accepted by A&A, arxiv:2002.00967; De Looze, I. et al. 2014, A&A, 568, A62; Dessauges-Zavadsky, M. et al. 2020, submitted to A&A, arXiv:2004.10771 Faisst, A. L. et al. 2020, ApJS, 247, 61; Fudamoto, Y. et al. 2020, submitted to A&A, arXiv:2004.10760; Fujimoto, S. et al. 2020, submitted to ApJ, arxiv2003.00013; Ginolfi, M. et al. 2020a, A&A, 633, A90; Ginolfi, M. et al. 2020b, submitted to A&A, arXiv:2004.13737; Gruppioni, C. et al. 2020, submitted to A&A, arXiv:2006.04974; Hasinger, G. et al. 2018, ApJ, 858, 77; Jones, G. C. et al. 2020, MNRAS, 491, L18; Khusanova, Y. et al. 2020, submitted to A&A, arXiv:2007.08384; Le Fèvre, O. et al. 2020, accepted by A&A, arxiv:1910.09517; Le Fèvre, O. et al. 2015, A&A, 576, A79; Loiacono, F. et al. 2020, submitted to A&A, arXiv:2006.04837; Madau, P. & Dickinson, M. 2014, ARA&A, 52, 415; Schaerer, D. et al. 2020, accepted by A&A, arxiv:2002.00979
37-40 (PDF)
Triaud, A.H.M.J. et al.
A Rare Pair of Eclipsing Brown Dwarfs Identified by the SPECULOOS Telescopes

DOI:
10.18727/0722-6691/5199
ADS BibCode:
2020Msngr.180...37T
Section:
Astronomical Science
Author(s)/Affiliation(s):
Triaud, A.H.M.J.; Burgasser, A.J.; Burdanov, A.; Hodžić, V.K.; Alonso, R.; Bardalez Gagliuffi, D.; Delrez, L.; Demory, B.-O.; de Wit, J.; Ducrot, E.; Hessman, F.V.; Husser, T.-O.; Jehin, E.; Pedersen, P.P.; Queloz, D.; McCormac, J.; Murray, C.; Sebastian, D.; Thompson, S.; Van Grootel, V.; Gillon, M.
AA(School of Physics & Astronomy, University of Birmingham, UK) AB(Center for Astrophysics and Space Sciences, University of California, San Diego, La Jolla, USA) AC(Astrobiology Research Unit, Université de Liège, Belgium) AD(School of Physics & Astronomy, University of Birmingham, UK) AE(Instituto de Astrofísica de Canarias, La Laguna, Spain) AF(Department of Astrophysics, American Museum of Natural History, New York, USA) AG(Cavendish Laboratory, Cambridge, UK) AH(University of Bern, Center for Space and Habitability, Switzerland) AI(Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, USA) AJ(Astrobiology Research Unit, Université de Liège, Belgium) AK(Institut für Astrophysik, University of Göttingen, Germany) AL(Institut für Astrophysik, University of Göttingen, Germany) AM(Space Sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Belgium) AN(Cavendish Laboratory, Cambridge, UK) AO(Cavendish Laboratory, Cambridge, UK) AP(Department of Physics, University of Warwick, Coventry, UK) AQ(Cavendish Laboratory, Cambridge, UK) AR(Astrobiology Research Unit, Université de Liège, Belgium) AS(Cavendish Laboratory, Cambridge, UK) AT(Space Sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Belgium) AU(Astrobiology Research Unit, Université de Liège, Belgium)
Abstract:
Brown dwarfs — stellar objects unable to sustain hydrogen fusion in their cores because of their low masses — continuously cool over their lifetimes. Evolution models have been created to reproduce this behaviour, and to allow mass and age determination using their luminosity, temperatures, spectral types and other parameters. However, these models have not yet been fully validated or calibrated with observations. During a commissioning run of the SPECULOOS telescopes, we serendipitously discovered a rare double-line eclipsing binary, a member of the 45 Myr-old moving group Argus. This discovery permitted us to determine the masses, radii and ages of the brown dwarfs, and with their luminosities make a comparison to evolution models. The models reproduce these measurements remarkably well, although a measured offset in luminosity could result in systematic underestimation of brown dwarf masses by 20 to 30%. Calibrating these models is necessary as they are also used to infer the masses of young, directly imaged exoplanets such as those found at the VLT.
References:
Baraffe, I. et al. 2003, A&A, 402, 701; Baraffe, I. et al. 2015, A&A, 577, A42; Demory, B.-O. et al. 2009, A&A, 505, 205; Jehin, E. et al. 2018, The Messenger, 174, 2; Gagné, J. et al. 2015, ApJS, 219, 33. Gillon, M. et al. 2017, Nature, 542, 456; Gizis, J. E. 2002, ApJ, 575, 484; Hodžić, V. et al. 2019, MNRAS, 481, 5091; Hayashi, C. & Nakano, T. 1963, Prog. Th. Physics, 30, 460; Kumar, S. S. 1962, AJ, 67, 579; Luhman, K. L. 2014, ApJ, 786, 18; Stassun, K. G. et al. 2006, Nature, 440, 311; Torres, G. et al. 2010, Astron. Astrophys. Rev., 18, 67; Triaud, A. H. M. J. et al. 2020, Nature Astronomy, DOI 10.1038/s41550-020-1018-2

Astronomical News

42-45 (PDF)
Kemper, C.
Report on the ESO/ALMA Conference “ALMA 2019: Science Results and Cross-Facility Synergies”

DOI:
10.18727/0722-6691/5200
ADS BibCode:
2020Msngr.180...42K
Section:
Astronomical News
Author(s)/Affiliation(s):
Kemper, C.
AA(ESO)
Abstract:
The Atacama Large Millimeter/submillimeter Array (ALMA) is the largest and most sensitive millimetre/submillimetre array on the planet, with the highest spatial resolution. Since it began operating, ALMA has routinely been at the forefront of science in this wavelength regime, delivering ground-breaking discoveries. The ALMA 2019 science conference was organised as one of a series of meetings held at regular intervals for the worldwide ALMA community, the previous one being held in Indian Wells, USA in 2016. At the start of Cycle 7 of observations, the ALMA 2019 conference provided an opportunity for the community to reflect on the multitude of scientific results from the facility, with special emphasis on the results from the first rounds of ALMA Large Programmes, the long baselines and high-frequency capabilities, the new solar and very long baseline interferometry (VLBI) modes, as well as the synergy between ALMA and other observatories.
46-49 (PDF)
Pompei, E. et al.
Report on the ESO Summer School “La Silla Observing Summer School 2020”

DOI:
10.18727/0722-6691/5201
ADS BibCode:
2020Msngr.180...46P
Section:
Astronomical News
Author(s)/Affiliation(s):
Pompei, E.; Hartke, J.; Korhonen, H.; Mazzucchelli, C.; Navarrete, C.; Pala, A.F.; Sbordone, L.; Schmidtobreick, L.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO) AH(ESO)
Abstract:
The La Silla Observing Summer School was originally conceived with the goal of providing hands-on training in the use of telescopes and astronomical instruments for senior masters and young doctoral students. The third La Silla Summer School ran over two weeks and was hosted by ESO’s Office for Science and the La Silla Observatory. Twenty PhD and MSc students from several countries participated. They attended lectures on various observing modes and instrumentation but also on scientific presentations, time management, effective proposal writing, and career choices. For the hands-on part at the observatory, the students were supervised by seven ESO tutors. Four small research projects were offered, using three telescopes and four instruments. The students in each research group went through the full process of defining and discussing the observing strategies, conducting the observations, reducing and analysing the data and finally presenting the results to the scientific community at the ESO Vitacura offices. The next school is foreseen for the southern summer break of 2022.
References:
Andersen, J. et al. 1995, The Messenger, 79, 12; Arenou, F. et al. 2018, A&A, 616, A17; Baldwin, J. A., Phillips, M. M. & Terlevich, R. 1981, PASP, 93, 5; Bruch, A. 2017, New Astronomy, 57, 51 Buzzoni, B. et al. 1984, The Messenger, 38, 9; Di Stefano, R. 2010, ApJ, 712, 728D Gaia Collaboration et al. 2018, A&A, 616, A1; Mayor, M. et al. 2003, The Messenger, 114, 20; Moorwood, A., Cuby, J. G. & Lidman, C. 1998, The Messenger, 91, 9; Navarrete, C. et al. 2017, A&A, 604, 120; Pala, A. F. et al. 2020, MNRAS, 494, 3799; Sbordone, L. et al. 2014, A&A, 564, A109; Sbordone, L. et al. 2020, ATel, 13525
50-52 (PDF)
del P. Lagos, C. et al.
Report on the ESO Workshop “ESOz-2020: The Build-up of Galaxies through Multiple Tracers and Facilities”

DOI:
10.18727/0722-6691/5202
ADS BibCode:
2020Msngr.180...50L
Section:
Astronomical News
Author(s)/Affiliation(s):
del P. Lagos, C.; Robotham, A.S.G.; De Breuck, C.
AA(International Centre for Radio Astronomy Research, University of Western Australia, Perth, Australia) AB(ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)) AC(ESO)
Abstract:
We report on the second joint Australia–ESO conference, held in Perth, Australia, following the successful Sydney conference in 2019. The conference was supported by ESO, the Centre of Excellence ASTRO 3D, the International Centre for Radio Astronomy Research, Macquarie University, CSIRO Astronomy and Space Science (CASS), and the Galaxies Journal. The scientific organising committee (SOC) focused on a programme that highlighted the complementarity between ESO and Australian instruments and the science breakthroughs enabled by this combination. In terms of demographics, we followed the same strategies as the previous meeting to tackle unconscious bias, and this again resulted in a well- balanced programme in terms of gender, career stage and geography, proving its effectiveness. Given concerns about global warming and the COVID-19 pandemic, the local organising committee (LOC) allowed several talks to be delivered remotely, and we reflect on that experience here.
References:
Zafar, T., De Breuck, C. & Arnaboldi, M. 2019, The Messenger, 176, 48
53-55 (PDF)
Herenz, E.C., Mazzucchelli, C.
Fellows at ESO

DOI:
10.18727/0722-6691/5203
ADS BibCode:
2020Msngr.180...53E
Section:
Astronomical News
Author(s)/Affiliation(s):
Herenz, E.C.; Mazzucchelli, C.
AA(ESO) AB(ESO)
55-55 (PDF)
ESO
Personnel Movements

ADS BibCode:
2020Msngr.180...55E
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO