DOI:
10.18727/0722-6691/5117
ADS BibCode:
2019Msngr.175....3J
Section:
4MOST
Author(s)/Affiliation(s):
de Jong, R.S.; Agertz, O.; Berbel, A.A.; Aird, J.; Alexander, D.A.; Amarsi, A.; Anders, F.; Andrae, R.; Ansarinejad, B.; Ansorge, W.; Antilogus, P.; Anwand-Heerwart, H.; Arentsen, A.; Arnadottir, A.; Asplund, M.; Auger, M.; Azais, N.; Baade, D.; Baker, G.; Baker, S.; Balbinot, E.; Baldry, I.K.; Banerji, M.; Barden, S.; Barklem, P.; Barthélémy-Mazot, E.; Battistini, C.; Bauer, S.; Bell, C.P.M.; Bellido-Tirado, O.; Bellstedt, S.; Belokurov, V.; Bensby, T.; Bergemann, M.; Bestenlehner, J.M.; Bielby, R.; Bilicki, M.; Blake, C.; Bland-Hawthorn, J.; Boeche, C.; Boland, W.; Boller, T.; Bongard, S.; Bongiorno, A.; Bonifacio, P.; Boudon, D.; Brooks, D.; Brown, M.J.I.; Brown, R.; Brüggen, M.; Brynnel, J.; Brzeski, J.; Buchert, T.; Buschkamp, P.; Caffau, E.; Caillier, P.; Carrick, J.; Casagrande, L.; Case, S.; Casey, A.; Cesarini, I.; Cescutti, G.; Chapuis, D.; Chiappini, C.; Childress, M.; Christlieb, N.; Church, R.; Cioni, M.-R.L.; Cluver, M.; Colless, M.; Collett, T.; Comparat, J.; Cooper, A.; Couch, W.; Courbin, F.; Croom, S.; Croton, D.; Daguisé, E.; Dalton, G.; Davies, L.J.M.; Davis, T.; de Laverny, P.; Deason, A.; Dionies, F.; Disseau, K.; Doel, P.; Döscher, D.; Driver, S.P.; Dwelly, T.; Eckert, D.; Edge, A.; Edvardsson, B.; Youssoufi, D.E.; Elhaddad, A.; Enke, H.; Erfanianfar, G.; Farrell, T.; Fechner, T.; Feiz, C.; Feltzing, S.; Ferreras, I.; Feuerstein, D.; Feuillet, D.; Finoguenov, A.; Ford, D.; Fotopoulou, S.; Fouesneau, M.; Frenk, C.; Frey, S.; Gaessler, W.; Geier, S.; Fusillo, N.G.; Gerhard, O.; Giannantonio, T.; Giannone, D.; Gibson, B.; Gillingham, P.; González-Fernández, C.; Gonzalez-Solares, E.; Gottloeber, S.; Gould, A.; Grebel, E.K.; Gueguen, A.; Guiglion, G.; Haehnelt, M.; Hahn, T.; Hansen, C.J.; Hartman, H.; Hauptner, K.; Hawkins, K.; Haynes, D.; Haynes, R.; Heiter, U.; Helmi, A.; Aguayo, C.H.; Hewett, P.; Hinton, S.; Hobbs, D.; Hoenig, S.; Hofman, D.; Hook, I.; Hopgood, J.; Hopkins, A.; Hourihane, A.; Howes, L.; Howlett, C.; Huet, T.; Irwin, M.; Iwert, O.; Jablonka, P.; Jahn, T.; Jahnke, K.; Jarno, A.; Jin, S.; Jofre, P.; Johl, D.; Jones, D.; Jönsson, H.; Jordan, C.; Karovicova, I.; Khalatyan, A.; Kelz, A.; Kennicutt, R.; King, D.; Kitaura, F.; Klar, J.; Klauser, U.; Kneib, J.-P.; Koch, A.; Koposov, S.; Kordopatis, G.; Korn, A.; Kosmalski, J.; Kotak, R.; Kovalev, M.; Kreckel, K.; Kripak, Y.; Krumpe, M.; Kuijken, K.; Kunder, A.; Kushniruk, I.; Lam, M.I.; Lamer, G.; Laurent, F.; Lawrence, J.; Lehmitz, M.; Lemasle, B.; Lewis, J.; Li, B.; Lidman, C.; Lind, K.; Liske, J.; Lizon, J.-L.; Loveday, J.; Ludwig, H.-G.; McDermid, R.M.; Maguire, K.; Mainieri, V.; Mali, S.; Mandel, H.; Mandel, K.; Mannering, L.; Martell, S.; Martinez Delgado, D.; Matijevic, G.; McGregor, H.; McMahon, R.; McMillan, P.; Mena, O.; Merloni, A.; Meyer, M.J.; Michel, C.; Micheva, G.; Migniau, J.-E.; Minchev, I.; Monari, G.; Muller, R.; Murphy, D.; Muthukrishna, D.; Nandra, K.; Navarro, R.; Ness, M.; Nichani, V.; Nichol, R.; Nicklas, H.; Niederhofer, F.; Norberg, P.; Obreschkow, D.; Oliver, S.; Owers, M.; Pai, N.; Pankratow, S.; Parkinson, D.; Paschke, J.; Paterson, R.; Pecontal, A.; Parry, I.; Phillips, D.; Pillepich, A.; Pinard, L.; Pirard, J.; Piskunov, N.; Plank, V.; Plüschke, D.; Pons, E.; Popesso, P.; Power, C.; Pragt, J.; Pramskiy, A.; Pryer, D.; Quattri, M.; de Andrade Queiroz, A.B.; Quirrenbach, A.; Rahurkar, S.; Raichoor, A.; Ramstedt, S.; Rau, A.; Recio-Blanco, A.; Reiss, R.; Renaud, F.; Revaz, Y.; Rhode, P.; Richard, J.; Richter, A.D.; Rix, H.-W.; Robotham, A.S.G.; Roelfsema, R.; Romaniello, M.; Rosario, D.; Rothmaier, F.; Roukema, B.; Ruchti, G.; Rupprecht, G.; Rybizki, J.; Ryde, N.; Saar, A.; Sadler, E.; Sahlén, M.; Salvato, M.; Sassolas, B.; Saunders, W.; Saviauk, A.; Sbordone, L.; Schmidt, T.; Schnurr, O.; Scholz, R.-D.; Schwope, A.; Seifert, W.; Shanks, T.; Sheinis, A.; Sivov, T.; Skúladóttir, Á.; Smartt, S.; Smedley, S.; Smith, G.; Smith, R.; Sorce, J.; Spitler, L.; Starkenburg, E.; Steinmetz, M.; Stilz, I.; Storm, J.; Sullivan, M.; Sutherland, W.; Swann, E.; Tamone, A.; Taylor, E.N.; Teillon, J.; Tempel, E.; ter Horst, R.; Thi, W.-F.; Tolstoy, E.; Trager, S.; Traven, G.; Tremblay, P.-E.; Tresse, L.; Valentini, M.; van de Weygaert, R.; van den Ancker, M.; Veljanoski, J.; Venkatesan, S.; Wagner, L.; Wagner, K.; Walcher, C.J.; Waller, L.; Walton, N.; Wang, L.; Winkler, R.; Wisotzki, L.; Worley, C.C.; Worseck, G.; Xiang, M.; Xu, W.; Yong, D.; Zhao, C.; Zheng, J.; Zscheyge, F.; Zucker, D.
AA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AB(Lund Observatory, Lund University, Sweden) AC(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AD(Institute of Astronomy, University of Cambridge, UK) AE(Department of Physics, Durham University, UK) AF(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AG(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AH(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AI(Department of Physics, Durham University, UK) AJ(RAMS-CON, Assling, Germany) AK(Laboratoire de physique nucléaire et de hautes énergies, Paris, France) AL(Institut für Astrophysik, Georg-August Universität Göttingen, Germany) AM(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AN(Lund Observatory, Lund University, Sweden) AO(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AP(Institute of Astronomy, University of Cambridge, UK) AQ(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany; IRIDESCENCE, Paris, France) AR(ESO) AS(Australian Astronomical Optics — Macquarie, Sydney, Australia) AT(Australian Astronomical Optics — Macquarie, Sydney, Australia) AU(Kapteyn Instituut, Rijksuniversiteit Groningen, the Netherlands) AV(Astrophysics Research Institute, Liverpool John Moores University, UK) AW(Institute of Astronomy, University of Cambridge, UK) AX(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AY(Department of Physics and Astronomy, Uppsala universitet, Sweden) AZ(Laboratoire des Matériaux Avancés, Lyon, France) BA(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) BB(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BC(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BD(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BE(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) BF(Institute of Astronomy, University of Cambridge, UK) BG(Lund Observatory, Lund University, Sweden) BH(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BI(Physics and Astronomy, University of Sheffield, UK) BJ(Department of Physics, Durham University, UK) BK(Sterrewacht Leiden, Universiteit Leiden, the Netherlands) BL(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia) BM(Sydney Institute for Astronomy, University of Sydney, Australia) BN(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) BO(Nederlandse Onderzoekschool Voor Astronomie (NOVA), Leiden, the Netherlands; Sterrewacht Leiden, Universiteit Leiden, the Netherlands) BP(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) BQ(Laboratoire de physique nucléaire et de hautes énergies, Paris, France) BR(Osservatorio Astronomico di Roma, INAF, Italy) BS(GEPI, Observatoire de Paris, Université PSL, CNRS, France) BT(Centre de Recherche Astrophysique de Lyon, France) BU(Department of Physics and Astronomy, University College London, UK) BV(School of Physics and Astronomy, Monash University, Melbourne, Australia) BW(Australian Astronomical Optics — Macquarie, Sydney, Australia) BX(Hamburger Sternwarte, Universität Hamburg, Germany) BY(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BZ(Australian Astronomical Optics — Macquarie, Sydney, Australia) CA(Centre de Recherche Astrophysique de Lyon, France) CB(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) CC(GEPI, Observatoire de Paris, Université PSL, CNRS, France) CD(Centre de Recherche Astrophysique de Lyon, France) CE(Physics Department, Lancaster University, UK) CF(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) CG(Australian Astronomical Optics — Macquarie, Sydney, Australia) CH(School of Physics and Astronomy, Monash University, Melbourne, Australia) CI(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CJ(Osservatorio Astronomico di Trieste, INAF, Italy) CK(Centre de Recherche Astrophysique de Lyon, France) CL(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CM(School of Physics and Astronomy, University of Southampton, UK) CN(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) CO(Lund Observatory, Lund University, Sweden) CP(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CQ(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia) CR(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) CS(Institute of Cosmology and Gravitation, University of Portsmouth, UK) CT(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) CU(Department of Physics, Durham University, UK) CV(Australian Astronomical Observatory, Sydney, Australia; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia) CW(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) CX(Sydney Institute for Astronomy, University of Sydney, Australia) CY(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia) CZ(Centre de Recherche Astrophysique de Lyon, France) DA(Department of Physics, University of Oxford, UK) DB(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) DC(School of Mathematics and Physics, University of Queensland, Brisbane, Australia) DD(Observatoire de la Côte d’Azur, Nice, France) DE(Department of Physics, Durham University, UK) DF(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) DG(Centre de Recherche Astrophysique de Lyon, France) DH(Department of Physics and Astronomy, University College London, UK) DI(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) DJ(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) DK(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) DL(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) DM(Department of Physics, Durham University, UK) DN(Department of Physics and Astronomy, Uppsala universitet, Sweden) DO(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) DP(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) DQ(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) DR(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) DS(Australian Astronomical Optics — Macquarie, Sydney, Australia) DT(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) DU(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) DV(Lund Observatory, Lund University, Sweden) DW(Department of Physics and Astronomy, University College London, UK) DX(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) DY(Max-Planck-Institut für Astronomie, Heidelberg, Germany) DZ(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany; University of Helsinki, Finland) EA(Lund Observatory, Lund University, Sweden) EB(Department of Physics, Durham University, UK) EC(Max-Planck-Institut für Astronomie, Heidelberg, Germany) ED(Department of Physics, Durham University, UK) EE(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) EF(Max-Planck-Institut für Astronomie, Heidelberg, Germany) EG(Institut für Physik und Astronomie, Universität Potsdam, Germany) EH(Department of Physics, University of Warwick, UK) EI(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) EJ(Institute of Astronomy, University of Cambridge, UK) EK(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) EL(E. A. Milne Centre for Astrophysics, University of Hull, UK) EM(Australian Astronomical Optics — Macquarie, Sydney, Australia) EN(Institute of Astronomy, University of Cambridge, UK) EO(Institute of Astronomy, University of Cambridge, UK) EP(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) EQ(Ohio State University, Columbus, USA; Max-Planck-Institut für Astronomie, Heidelberg, Germany) ER(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) ES(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) ET(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) EU(Institute of Astronomy, University of Cambridge, UK) EV(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) EW(Max-Planck-Institut für Astronomie, Heidelberg, Germany; Dark Cosmology Centre, Københavns Universitet, Denmark) EX(Lund Observatory, Lund University, Sweden) EY(Institut für Astrophysik, Georg-August Universität Göttingen, Germany) EZ(Institute of Astronomy, University of Cambridge, UK) FA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) FB(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) FC(Department of Physics and Astronomy, Uppsala universitet, Sweden) FD(Kapteyn Instituut, Rijksuniversiteit Groningen, the Netherlands) FE(Department of Physics, Durham University, UK) FF(Institute of Astronomy, University of Cambridge, UK) FG(School of Mathematics and Physics, University of Queensland, Brisbane, Australia) FH(Lund Observatory, Lund University, Sweden) FI(School of Physics and Astronomy, University of Southampton, UK) FJ(Laboratoire des Matériaux Avancés, Lyon, France) FK(Physics Department, Lancaster University, UK) FL(ESO) FM(Australian Astronomical Optics — Macquarie, Sydney, Australia) FN(Institute of Astronomy, University of Cambridge, UK) FO(Lund Observatory, Lund University, Sweden) FP(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) FQ(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) FR(Institute of Astronomy, University of Cambridge, UK) FS(ESO) FT(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) FU(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) FV(Max-Planck-Institut für Astronomie, Heidelberg, Germany) FW(Centre de Recherche Astrophysique de Lyon, France) FX(Kapteyn Instituut, Rijksuniversiteit Groningen, the Netherlands) FY(Institute of Astronomy, University of Cambridge, UK) FZ(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) GA(Prime Optics, Eumundi, Queensland, Australia) GB(Lund Observatory, Lund University, Sweden) GC(Max-Planck-Institut für Astronomie, Heidelberg, Germany) GD(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) GE(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) GF(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) GG(Institute of Astronomy, University of Cambridge, UK) GH(Institute of Astronomy, University of Cambridge, UK) GI(Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain) GJ(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) GK(Australian Astronomical Optics — Macquarie, Sydney, Australia) GL(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) GM(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) GN(Institute of Astronomy, University of Cambridge, UK) GO(Observatoire de la Côte d’Azur, Nice, France) GP(Department of Physics and Astronomy, Uppsala universitet, Sweden) GQ(ESO; Centre de Recherche Astrophysique de Lyon, France) GR(School of Mathematics and Physics, Queen’s University Belfast, UK; University of Turku, Finland) GS(Max-Planck-Institut für Astronomie, Heidelberg, Germany) GT(Max-Planck-Institut für Astronomie, Heidelberg, Germany) GU(Australian Astronomical Optics — Macquarie, Sydney, Australia) GV(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) GW(Sterrewacht Leiden, Universiteit Leiden, the Netherlands) GX(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) GY(Lund Observatory, Lund University, Sweden) GZ(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) HA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) HB(Centre de Recherche Astrophysique de Lyon, France) HC(Australian Astronomical Optics — Macquarie, Sydney, Australia) HD(Max-Planck-Institut für Astronomie, Heidelberg, Germany) HE(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) HF(Institute of Astronomy, University of Cambridge, UK) HG(Department of Physics, Durham University, UK) HH(Australian Astronomical Observatory, Sydney, Australia; Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) HI(Department of Physics and Astronomy, Uppsala universitet, Sweden) HJ(Hamburger Sternwarte, Universität Hamburg, Germany) HK(ESO) HL(University of Sussex, Brighton, UK) HM(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) HN(Department of Physics and Astronomy, Macquarie University, Sydney, Australia) HO(School of Mathematics and Physics, Queen’s University Belfast, UK) HP(ESO) HQ(Australian Astronomical Optics — Macquarie, Sydney, Australia) HR(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) HS(Institute of Astronomy, University of Cambridge, UK) HT(Australian Astronomical Observatory, Sydney, Australia; International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) HU(School of Physics, University of New South Wales, Sydney, Australia) HV(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) HW(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) HX(Australian Astronomical Optics — Macquarie, Sydney, Australia) HY(Institute of Astronomy, University of Cambridge, UK) HZ(Lund Observatory, Lund University, Sweden) (Instituto de Física Corpuscular, Universidad de Valencia, Spain) (Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) (International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) (Laboratoire des Matériaux Avancés, Lyon, France) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Centre de Recherche Astrophysique de Lyon, France) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Institute of Astronomy, University of Cambridge, UK) (Institute of Astronomy, University of Cambridge, UK) (Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) (Nederlandse Onderzoekschool Voor Astronomie (NOVA), Dwingeloo, the Netherlands) (Max-Planck-Institut für Astronomie, Heidelberg, Germany) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Institute of Cosmology and Gravitation, University of Portsmouth, UK) (Institut für Astrophysik, Georg-August Universität Göttingen, Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Department of Physics, Durham University, UK) (International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) (University of Sussex, Brighton, UK) (Department of Physics and Astronomy, Macquarie University, Sydney, Australia) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (School of Mathematics and Physics, University of Queensland, Brisbane, Australia) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Centre de Recherche Astrophysique de Lyon, France) (Institute of Astronomy, University of Cambridge, UK) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Max-Planck-Institut für Astronomie, Heidelberg, Germany) (Laboratoire des Matériaux Avancés, Lyon, France) (ESO) (Department of Physics and Astronomy, Uppsala universitet, Sweden) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Institute of Astronomy, University of Cambridge, UK) (Physics Department, Technische Universität München, Germany) (International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) (Nederlandse Onderzoekschool Voor Astronomie (NOVA), Dwingeloo, the Netherlands) (Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) (University of Sussex, Brighton, UK) (ESO) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) (Department of Physics and Astronomy, Uppsala universitet, Sweden) (Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) (Observatoire de la Côte d’Azur, Nice, France) (ESO) (Lund Observatory, Lund University, Sweden) (Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) (Institut für Astrophysik, Georg-August Universität Göttingen, Germany) (Centre de Recherche Astrophysique de Lyon, France) (Institut für Astrophysik, Georg-August Universität Göttingen, Germany) (Max-Planck-Institut für Astronomie, Heidelberg, Germany) (International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) (Netherlands Institute for Space Research (SRON), Groningen, the Netherlands; Nederlandse Onderzoekschool Voor Astronomie (NOVA), Dwingeloo, the Netherlands) (ESO) (Department of Physics, Durham University, UK) (Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) (Torun Centre for Astronomy (TCfA), Nicolaus Copernicus University, Poland; Centre de Recherche Astrophysique de Lyon, France) (Lund Observatory, Lund University, Sweden) (ESO) (Max-Planck-Institut für Astronomie, Heidelberg, Germany) (Lund Observatory, Lund University, Sweden) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Sydney Institute for Astronomy, University of Sydney, Australia) (Department of Physics and Astronomy, Uppsala universitet, Sweden) (Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) (Laboratoire des Matériaux Avancés, Lyon, France) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Pontificia Universidad Católica de Chile, Santiago, Chile) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany; Cherenkov Telescope Array Observatory, Bologna, Italy) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) (Department of Physics, Durham University, UK) (Australian Astronomical Observatory, Sydney, Australia; CFHT, Kamuela, Hawaii, USA) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Max-Planck-Institut für Astronomie, Heidelberg, Germany) (School of Mathematics and Physics, Queen’s University Belfast, UK) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (University of Sussex, Brighton, UK) (Centre de Recherche Astrophysique de Lyon, France; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Department of Physics and Astronomy, Macquarie University, Sydney, Australia) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (School of Physics and Astronomy, University of Southampton, UK) (School of Physics and Astronomy, Queen Mary University of London, UK) (Institute of Cosmology and Gravitation, University of Portsmouth, UK) (Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) (Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia) (Laboratoire des Matériaux Avancés, Lyon, France) (Tartu Observatory, University of Tartu, Estonia; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Nederlandse Onderzoekschool Voor Astronomie (NOVA), Dwingeloo, the Netherlands) (Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) (Kapteyn Instituut, Rijksuniversiteit Groningen, the Netherlands) (Kapteyn Instituut, Rijksuniversiteit Groningen, the Netherlands) (Lund Observatory, Lund University, Sweden) (Department of Physics, University of Warwick, UK) (Centre de Recherche Astrophysique de Lyon, France) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Kapteyn Instituut, Rijksuniversiteit Groningen, the Netherlands) (ESO) (Kapteyn Instituut, Rijksuniversiteit Groningen, the Netherlands) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Institute of Astronomy, University of Cambridge, UK) (Netherlands Institute for Space Research (SRON), Groningen, the Netherlands; Kapteyn Instituut, Rijksuniversiteit Groningen, the Netherlands) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Institute of Astronomy, University of Cambridge, UK) (Institut für Physik und Astronomie, Universität Potsdam, Germany) (Max-Planck-Institut für Astronomie, Heidelberg, Germany) (XU-OSE, Heidelberg, Germany) (Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) (Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) (Australian Astronomical Optics — Macquarie, Sydney, Australia) (Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) (Department of Physics and Astronomy, Macquarie University, Sydney, Australia)
Abstract:
We introduce the 4-metre Multi-Object Spectroscopic Telescope (4MOST), a new high-multiplex, wide-field spectroscopic survey facility under development for the four-metre-class Visible and Infrared Survey Telescope for Astronomy (VISTA) at Paranal. Its key specifications are: a large field of view (FoV) of 4.2 square degrees and a high multiplex capability, with 1624 fibres feeding two low-resolution spectrographs (R = λ/Δλ ~ 6500), and 812 fibres transferring light to the high-resolution spectrograph (R ~ 20 000). After a description of the instrument and its expected performance, a short overview is given of its operational scheme and planned 4MOST Consortium science; these aspects are covered in more detail in other articles in this edition of The Messenger. Finally, the processes, schedules, and policies concerning the selection of ESO Community Surveys are presented, commencing with a singular opportunity to submit Letters of Intent for Public Surveys during the first five years of 4MOST operations.
References:
Guiglion, G. et al. 2019, The Messenger, 175, 17; Walcher, C. J. et al. 2019, The Messenger, 175, 12

DOI:
10.18727/0722-6691/5118
ADS BibCode:
2019Msngr.175...12W
Section:
4MOST
Author(s)/Affiliation(s):
Walcher, C.J.; Banerji, M.; Battistini, C.; Bell, C.P.M.; Bellido-Tirado, O.; Bensby, T.; Bestenlehner, J.M.; Boller, T.; Brynnel, J.; Casey, A.; Chiappini, C.; Christlieb, N.; Church, R.; Cioni, M.-R.L.; Croom, S.; Comparat, J.; Davies, L.J.M.; de Jong, R.S.; Dwelly, T.; Enke, H.; Feltzing, S.; Feuillet, D.; Fouesneau, M.; Ford, D.; Frey, S.; Gonzalez-Solares, E.; Gueguen, A.; Howes, L.; Irwin, M.; Klar, J.; Kordopatis, G.; Korn, A.; Krumpe, M.; Kushniruk, I.; Lam, M.I.; Lewis, J.; Lind, K.; Liske, J.; Loveday, J.; Mainieri, V.; Martell, S.; Matijevic, G.; McMahon, R.; Merloni, A.; Murphy, D.; Niederhofer, F.; Norberg, P.; Pramskiy, A.; Romaniello, M.; Robotham, A.S.G.; Rothmaier, F.; Ruchti, G.; Schnurr, O.; Schwope, A.; Smedley, S.; Sorce, J.; Starkenburg, E.; Stilz, I.; Storm, J.; Tempel, E.; Thi, W.-F.; Traven, G.; Valentini, M.; van den Ancker, M.; Walton, N.; Winkler, R.; Worley, C.C.
AA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AB(Institute of Astronomy, University of Cambridge, UK) AC(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AD(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AE(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AF(Lund Observatory, Lund University, Sweden) AG(Physics and Astronomy, University of Sheffield, UK) AH(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AI(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AJ(School of Physics and Astronomy, Monash University, Melbourne, Australia) AK(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AL(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AM(Lund Observatory, Lund University, Sweden) AN(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AO(Sydney Institute for Astronomy, University of Sydney, Australia) AP(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AQ(International Centre for Radio Astronomy Research / University of Western Australia, Perth, Australia) AR(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AS(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AT(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AU(Lund Observatory, Lund University, Sweden) AV(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AW(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AX(Lund Observatory, Lund University, Sweden) AY(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AZ(Institute of Astronomy, University of Cambridge, UK) BA(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) BB(Lund Observatory, Lund University, Sweden) BC(Institute of Astronomy, University of Cambridge, UK) BD(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BE(Observatoire de la Côte d’Azur, Nice, France) BF(Department of Physics and Astronomy, Uppsala universitet, Sweden) BG(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BH(Lund Observatory, Lund University, Sweden) BI(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BJ(Institute of Astronomy, University of Cambridge, UK) BK(Department of Physics and Astronomy, Uppsala universitet, Sweden) BL(Hamburger Sternwarte, Universität Hamburg, Germany) BM(University of Sussex, Brighton, UK) BN(ESO) BO(School of Physics, University of New South Wales, Sydney, Australia) BP(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BQ(Institute of Astronomy, University of Cambridge, UK) BR(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) BS(Institute of Astronomy, University of Cambridge, UK) BT(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BU(Department of Physics, Durham University, UK) BV(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) BW(ESO) BX(International Centre for Radio Astronomy Research / University of Western Australia, Perth, Australia) BY(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) BZ(Lund Observatory, Lund University, Sweden) CA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany; Cherenkov Telescope Array Observatory, Bologna, Italy) CB(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CC(Australian Astronomical Optics – Macquarie, Sydney, Australia) CD(Centre de Recherche Astrophysique de Lyon, France; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CE(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CF(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) CG(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CH(Tartu Observatory, University of Tartu, Estonia; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CI(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) CJ(Lund Observatory, Lund University, Sweden) CK(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CL(ESO) CM(Institute of Astronomy, University of Cambridge, UK) CN(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) CO(Institute of Astronomy, University of Cambridge, UK)
Abstract:
The 4MOST instrument is a multi-object spectrograph that will address Galactic and extragalactic science cases simultaneously by observing targets from a large number of different surveys within each science exposure. This parallel mode of operation and the survey nature of 4MOST require some distinct 4MOST- specific operational features within the overall operations model of ESO. The main feature is that the 4MOST Consortium will deliver, not only the instrument, but also contractual services to the user community, which is why 4MOST is also described as a facility. This white paper concentrates on information particularly useful to answering the forthcoming Call for Letters of Intent.

DOI:
10.18727/0722-6691/5119
ADS BibCode:
2019Msngr.175...17G
Section:
4MOST
Author(s)/Affiliation(s):
Guiglion, G.; Battistini, C.; Bell, C.P.M.; Bensby, T.; Boller, T.; Chiappini, C.; Comparat, J.; Christlieb, N.; Church, R.; Cioni, M.-R.L.; Davies, L.; Dwelly, T.; de Jong, R.S.; Feltzing, S.; Gueguen, A.; Howes, L.; Irwin, M.; Kushniruk, I.; Lam, M.I.; Liske, J.; McMahon, R.; Merloni, A.; Norberg, P.; Robotham, A.S.G.; Schnurr, O.; Sorce, J.G.; Starkenburg, E.; Storm, J.; Swann, E.; Tempel, E.; Thi, W.-F.; Worley, C.C.; Walcher, C.J.; The 4MOST Collaboration
AA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AB(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AC(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AD(Lund Observatory, Lund University, Sweden) AE(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AF(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AG(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AH(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AI(Lund Observatory, Lund University, Sweden) AJ(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AK(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) AL(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AM(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AN(Lund Observatory, Lund University, Sweden) AO(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AP(Lund Observatory, Lund University, Sweden) AQ(Institute of Astronomy, University of Cambridge, UK) AR(Lund Observatory, Lund University, Sweden) AS(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AT(Hamburger Sternwarte, Universität Hamburg, Germany) AU(Institute of Astronomy, University of Cambridge, UK) AV(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AW(Department of Physics, Durham University, UK) AX(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) AY(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany; Cherenkov Telescope Array Observatory, Bologna, Italy) AZ(Centre de Recherche Astrophysique de Lyon, France; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BB(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BC(Institute of Cosmology and Gravitation, University of Portsmouth, UK) BD(Tartu Observatory, University of Tartu, Estonia; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BE(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) BF(Institute of Astronomy, University of Cambridge, UK) BG(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany)
Abstract:
The current status of and motivation for the 4MOST survey strategy, as developed by the Consortium science team, are presented here. Key elements of the strategy are described, such as sky coverage, number of visits and total exposure times in different parts of the sky, and how to deal with different observing conditions. The task of organising the strategy is not simple, with many different surveys that have vastly different target brightnesses and densities, sample completeness levels, and signal-to-noise requirements. We introduce here a number of concepts that we will use to ensure all surveys are optimised. Astronomers who are planning to submit a Participating Survey proposal are strongly encouraged to read this article and any relevant 4MOST Survey articles in this issue of The Messenger such that they can optimally complement and benefit from the planned surveys of the 4MOST Consortium.

DOI:
10.18727/0722-6691/5120
ADS BibCode:
2019Msngr.175...23H
Section:
Surveys
Author(s)/Affiliation(s):
Helmi, A.; Irwin, M.; Deason, A.; Balbinot, E.; Belokurov, V.; Bland-Hawthorn, J.; Christlieb, N.; Cioni, M.-R.L.; Feltzing, S.; Grebel, E.K.; Kordopatis, G.; Starkenburg, E.; Walton, N.; Worley, C.C.
AA(Kapteyn Instituut, Rijksunversiteit Groningen, the Netherlands) AB(Institute of Astronomy, University of Cambridge, UK) AC(Department of Physics, Durham University, UK) AD(Kapteyn Instituut, Rijksunversiteit Groningen, the Netherlands) AE(Institute of Astronomy, University of Cambridge, UK) AF(Sydney Institute for Astronomy, University of Sydney, Australia) AG(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AH(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AI(Lund Observatory, Lund University, Sweden) AJ(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen- Institut, Germany) AK(Observatoire de la Côte d’Azur, Nice, France) AL(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AM(Institute of Astronomy, University of Cambridge, UK) AN(Institute of Astronomy, University of Cambridge, UK)
Abstract:
The goal of this survey is to study the formation and evolution of the Milky Way halo to deduce its assembly history and the 3D distribution of mass in the Milky Way. The combination of multi-band photometry, Gaia proper motion and parallax data, and radial velocities and the metallicity and elemental abundances obtained from low-resolution spectra of halo giants with 4MOST, will yield an unprecedented characterisation of the Milky Way halo and its interface with the thick disc. The survey will produce a volume- and magnitude- limited complete sample of giant stars in the halo. It will cover at least 10 000 square degrees of high Galactic latitude, and measure line-of-sight velocities with a precision of 1–2 km s^–1 as well as metallicities to within 0.2 dex.
References:
Belokurov, V. et al. 2006, ApJL, 642, L137; Belokurov, V. et al. 2018, MNRAS, 478, 611; Bland-Hawthorn, J. & Gerhard, O. 2016, ARA&A, 54, 529; Bonaca, A. et al. 2014, ApJ, 795, 94; Bonaca, A. et al. 2018, arXiv:1811.03631; Cooper, A. P. et al. 2010, MNRAS, 406, 744; Erkal, D. et al. 2016, MNRAS, 463, 102; Gaia Collaboration et al. 2018, A&A, 616, A1; Helmi, A. et al. 2018, Nature, 563, 85; Hayes, C. R. et al. 2018, ApJ, 852, 49; Malhan, K., Ibata, R. A. & Martin, N. F. 2018, MNRAS, 481, 3442; Sanderson, R. E., Helmi, A. & Hogg, D. W. 2015, ApJ, 801, 98; Xue, X.-X. et al. 2014, ApJ, 784, 170

DOI:
10.18727/0722-6691/5121
ADS BibCode:
2019Msngr.175...26C
Section:
Surveys
Author(s)/Affiliation(s):
Christlieb, N.; Battistini, C.; Bonifacio, P.; Caffau, E.; Ludwig, H.-G.; Asplund, M.; Barklem, P.; Bergemann, M.; Church, R.; Feltzing, S.; Ford, D.; Grebel, E.K.; Hansen, C.J.; Helmi, A.; Kordopatis, G.; Kovalev, M.; Korn, A.; Lind, K.; Quirrenbach, A.; Rybizki, J.; Skúladóttir, Á.; Starkenburg, E.
AA(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AB(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AC(GEPI, Observatoire de Paris, Université PSL, CNRS, France) AD(GEPI, Observatoire de Paris, Université PSL, CNRS, France) AE(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AF(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AG(Department of Physics and Astronomy, Uppsala universitet, Sweden) AH(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AI(Lund Observatory, Lund University, Sweden) AJ(Lund Observatory, Lund University, Sweden) AK(Lund Observatory, Lund University, Sweden) AL(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) AM(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AN(Kapteyn Instituut, Rijksunversiteit Groningen, the Netherlands) AO(Observatoire de la Côte d’Azur, Nice, France) AP(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AQ(Department of Physics and Astronomy, Uppsala universitet, Sweden) AR(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AS(Zentrum für Astronomie der Universität Heidelberg/Landessternwarte, Germany) AT(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AU(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AV(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany)
Abstract:
We will study the formation history of the Milky Way, and the earliest phases of its chemical enrichment, with a sample of more than 1.5 million stars at high galactic latitude. Elemental abundances of up to 20 elements with a precision of better than 0.2 dex will be derived for these stars. The sample will include members of kinematically coherent substructures, which we will associate with their possible birthplaces by means of their abundance signatures and kinematics, allowing us to test models of galaxy formation. Our target catalogue is also expected to contain 30 000 stars at a metallicity of less than one hundredth that of the Sun. This sample will therefore be almost a factor of 100 larger than currently existing samples of metal-poor stars for which precise elemental abundances are available (determined from high-resolution spectroscopy), enabling us to study the early chemical evolution of the Milky Way in unprecedented detail.
References:
Bastian, N. & Lardo, C. 2018, ARA&A, 56, 83; Casagrande, L. 2019, MNRAS, 482, 2770; De Lucia, G. & Helmi, A. 2008, MNRAS, 391, 14; Frebel, A. & Norris, J. E. 2015, ARA&A, 53, 631; Hansen, C. J. et al. 2015, AN, 336, 665; Helmi, A. et al. 2018, Nature, 563, 85; Hendricks, B. et al. 2014, ApJ, 785, 102; Ji, A. et al. 2016, ApJ, 830, 93; Koch, A. et al. 2013, A&A, 554, A5; Malhan, K. et al. 2018, MNRAS, 481, 3442; Martell, S. L. et al. 2011, A&A, 534, A136; Mashonkina, A. 2017, A&A, 608, A89; Nissen, P. E. & Schuster, W. J. 2010, A&A, 511, L10; Pillepich, A. et al. 2015, ApJ, 799, 184; Rybizki, J. et al. 2018, PASP, 130, 074101; Starkenburg, E. et al. 2017, MNRAS, 471, 2587; Tolstoy, E. et al. 2009, ARA&A, 47, 371

DOI:
10.18727/0722-6691/5122
ADS BibCode:
2019Msngr.175...30C
Section:
Surveys
Author(s)/Affiliation(s):
Chiappini, C.; Minchev, I.; Starkenburg, E.; Anders, F.; Fusillo, N.G.; Gerhard, O.; Guiglion, G.; Khalatyan, A.; Kordopatis, G.; Lemasle, B.; Matijevic, G.; de Andrade Queiroz, A.B.; Schwope, A.; Steinmetz, M.; Storm, J.; Traven, G.; Tremblay, P.-E.; Valentini, M.; Andrae, R.; Arentsen, A.; Asplund, M.; Bensby, T.; Bergemann, M.; Casagrande, L.; Church, R.; Cescutti, G.; Feltzing, S.; Fouesneau, M.; Grebel, E.K.; Kovalev, M.; McMillan, P.; Monari, G.; Rybizki, J.; Ryde, N.; Rix, H.-W.; Walton, N.; Xiang, M.; Zucker, D.; The 4MIDABLE-LR Team
AA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AB(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AC(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AD(Departament de Física Quàntica i Astrofísica, Universitat de Barcelona, Spain) AE(Department of Physics, University of Warwick, UK) AF(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AG(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AH(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AI(Observatoire de la Côte d’Azur, Nice, France) AJ(Zentrum für Astronomie der Universität Heidelberg / Astronomisches Rechen- Institut, Germany) AK(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AL(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AM(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AN(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AO(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AP(Lund Observatory, Lund University, Sweden) AQ(Department of Physics, University of Warwick, UK) AR(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AS(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AT(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AU(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AV(Lund Observatory, Lund University, Sweden) AW(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AX(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AY(Lund Observatory, Lund University, Sweden) AZ(Osservatorio Astronomico di Trieste, INAF, Italy) BA(Lund Observatory, Lund University, Sweden) BB(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BC(Zentrum für Astronomie der Universität Heidelberg / Astronomisches Rechen- Institut, Germany) BD(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BE(Lund Observatory, Lund University, Sweden) BF(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) BG(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BH(Lund Observatory, Lund University, Sweden) BI(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BJ(Institute of Astronomy, University of Cambridge, UK) BK(Max-Planck-Institut für Astronomie, Heidelberg, Germany) BL(Department of Physics and Astronomy, Macquarie University, Sydney, Australia)
Abstract:
The mechanisms of the formation and evolution of the Milky Way are encoded in the orbits, chemistry and ages of its stars. With the 4MOST MIlky way Disk And BuLgE Low-Resolution Survey (4MIDABLE-LR) we aim to study kinematic and chemical substructures in the Milky Way disc and bulge region with samples of unprecedented size out to larger distances and greater precision than conceivable with Gaia alone or any other ongoing or planned survey. Gaia gives us the unique opportunity for target selection based almost entirely on parallax and magnitude range, hence increasing the efficiency in sampling larger Milky Way volumes with well-defined and effective selection functions.
References:
Barbuy, B., Chiappini, C. & Gerhard, O. 2018, ARAA, 56, 223; Gaia collaboration, Brown, A. et al. 2018, A&A, 616, 1; Geier, S. et al. 2018, arXiv:1810.09321; Miglio, A. et al. 2017, Astronomische Nachrichten, 338, 644; Minchev, I. 2016, Astronomische Nachrichten, 337, 703; Minchev, I., Chiappini, C. & Martig, M. 2013, A&A, 558, A29; Schwope, A. 2018, A&A, 619, A62; Valentini, M. et al. 2018, arXiv:1808.08569

DOI:
10.18727/0722-6691/5123
ADS BibCode:
2019Msngr.175...35B
Section:
Surveys
Author(s)/Affiliation(s):
Bensby, T.; Bergemann, M.; Rybizki, J.; Lemasle, B.; Howes, L.; Kovalev, M.; Agertz, O.; Asplund, M.; Barklem, P.; Battistini, C.; Casagrande, L.; Chiappini, C.; Church, R.; Feltzing, S.; Ford, D.; Gerhard, O.; Kushniruk, I.; Kordopatis, G.; Lind, K.; Minchev, I.; McMillan, P.; Rix, H.-W.; Ryde, N.; Traven, G.
AA(Lund Observatory, Lund University, Sweden) AB(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AC(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AD(Zentrum für Astronomie der Universität Heidelberg / Astronomisches Rechen- Institut, Germany) AE(Lund Observatory, Lund University, Sweden) AF(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AG(Lund Observatory, Lund University, Sweden) AH(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AI(Department of Physics and Astronomy, Uppsala universitet, Sweden) AJ(Zentrum für Astronomie der Universität Heidelberg / Landessternwarte, Germany) AK(Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australia) AL(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AM(Lund Observatory, Lund University, Sweden) AN(Lund Observatory, Lund University, Sweden) AO(Lund Observatory, Lund University, Sweden) AP(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AQ(Lund Observatory, Lund University, Sweden) AR(Observatoire de la Côte d’Azur, Nice, France) AS(Max-Planck-Institut für Astronomie, Heidelberg, Germany; Department of Physics and Astronomy, Uppsala universitet, Sweden) AT(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AU(Lund Observatory, Lund University, Sweden) AV(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AW(Lund Observatory, Lund University, Sweden) AX(Lund Observatory, Lund University, Sweden)
Abstract:
The signatures of the formation and evolution of a galaxy are imprinted in its stars. Their velocities, ages, and chemical compositions present major constraints on models of galaxy formation, and on various processes such as the gas inflows and outflows, the accretion of cold gas, radial migration, and the variability of star formation activity. Understanding the evolution of the Milky Way requires large observational datasets of stars via which these quantities can be determined accurately. This is the science driver of the 4MOST MIlky way Disc And BuLgE High-Resolution (4MIDABLE-HR) survey: to obtain high-resolution spectra at < i>R ~ 20 000 and to provide detailed elemental abundances for large samples of stars in the Galactic disc and bulge. High data quality will allow us to provide accurate spectroscopic diagnostics of two million stellar spectra: precise radial velocities; rotation; abundances of many elements, including those that are currently only accessible in the optical, such as Li, s-, and r-process; and multi-epoch spectra for a sub-sample of stars. Synergies with complementary missions like Gaia and TESS will provide masses, stellar ages and multiplicity, forming a multi-dimensional dataset that will allow us to explore and constrain the origin and structure of the Milky Way.
References:
Antoja, T. et al. 2018, Nature, 561, 360; Barbuy, B. et al. 2018, ARA&A, 56, 223; Bensby, T. et al. 2011, ApJ, 735, L46; Bensby, T. et al. 2014, A&A, 562, A71; Bensby, T. et al. 2017, A&A, 605, A89; Bergemann, M. et al. 2014, A&A, 565, A89; Bergemann, M. et al. 2018, Nature, 555, 334; Grand, R. J. J. et al. 2018, MNRAS, 474, 3629; Hayden, M. R. et al. 2011, ApJ, 808, 132; Kushniruk, I. et al. 2017, A&A, 608, A73; Ness, M. et al. 2013, MNRAS, 430, 836; Renzini, A. et al. 2018, ApJ, 863, 16; Rix, H.-W. & Bovy, J. 2013, A&ARv, 21, 61; Schönrich, R. & Binney, J. 2009, MNRAS, 399, 3

DOI:
10.18727/0722-6691/5124
ADS BibCode:
2019Msngr.175...39F
Section:
Surveys
Author(s)/Affiliation(s):
Finoguenov, A.; Merloni, A.; Comparat, J.; Nandra, K.; Salvato, M.; Tempel, E.; Raichoor, A.; Richard, J.; Kneib, J.-P.; Pillepich, A.; Sahlén, M.; Popesso, P.; Norberg, P.; McMahon, R.; The 4MOST Collaboration
AA(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany; University of Helsinki, Finland) AB(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AC(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AD(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AE(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AF(Tartu Observatory, University of Tartu, Estonia; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AG(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) AH(Centre de Recherche Astrophysique de Lyon, France) AI(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) AJ(Max-Planck-Institut für Astronomie, Heidelberg, Germany) AK(Department of Physics and Astronomy, Uppsala universitet, Sweden) AL(Physics Department, Technische Universität München, Germany) AM(Department of Physics, Durham University, UK) AN(Institute of Astronomy, University of Cambridge, UK)
Abstract:
Groups and clusters of galaxies are a current focus of astronomical research owing to their role in determining the environmental effects on galaxies and the constraints they provide to cosmology. The eROSITA X-ray telescope on board the Spectrum Roentgen Gamma observatory will be launched in 2019 and will have completed eight scans of the full sky when 4MOST starts operating. The experiment will detect groups and clusters of galaxies through X-ray emission from the hot intergalactic medium. The purpose of the 4MOST eROSITA Galaxy Cluster Redshift Survey is to provide spectroscopic redshifts of the optical counterparts to the X-ray emission from 40 000 groups and clusters of galaxies so as to perform dynamical estimates of the total mass and to measure the properties of the member galaxies. The survey aims to obtain precise redshift measurements of the photometrically identified brightest cluster galaxies at redshift z > 0.7. At lower redshifts (z < 0.7) the programme aims to sample over 15 member galaxies per cluster and enable dynamical mass measurements to calibrate the clusters for cosmological experiments. At z < 0.2, eROSITA will also detect X-ray emission from galaxy groups and filaments. 4MOST spectroscopic data from the survey will be used for optical identification of galaxy groups down to eROSITA’s mass detection limits of 10¹³ M_⊙, as well as the detection of the largest filaments for pioneering studies of their X-ray emission.
References:
Albrecht, A. et al. 2006, arXiv:0609591; Bocquet, S. et al. 2016, MNRAS, 456, 2361; Capasso, R. et al. 2019, MNRAS, 482, 1043; Clerc, N. et al. 2016, MNRAS, 463, 4490; Comparat, J. et al. 2017, MNRAS, 469, 4157; Grandis, S. et al. 2018, arXiv:1810.10553; Merloni, A. et al. 2012, arXiv:1209.3114; Nicastro, F. et al. 2018, Nature, 558, 406; Pillepich, A. et al. 2018, MNRAS, 481, 613; Wilcox, H. et al. 2015, MNRAS, 452, 1171

DOI:
10.18727/0722-6691/5125
ADS BibCode:
2019Msngr.175...42M
Section:
Surveys
Author(s)/Affiliation(s):
Merloni, A.; Alexander, D.A.; Banerji, M.; Boller, T.; Comparat, J.; Dwelly, T.; Fotopoulou, S.; McMahon, R.; Nandra, K.; Salvato, M.; Croom, S.; Finoguenov, A.; Krumpe, M.; Lamer, G.; Rosario, D.; Schwope, A.; Shanks, T.; Steinmetz, M.; Wisotzki, L.; Worseck, G.
AA(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AB(Department of Physics, Durham University, UK) AC(Institute of Astronomy, University of Cambridge, UK) AD(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AE(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AF(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AG(Department of Physics, Durham University, UK) AH(Institute of Astronomy, University of Cambridge, UK) AI(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AJ(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AK(Sydney Institute for Astronomy, University of Sydney, Australia) AL(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany; University of Helsinki, Finland) AM(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AN(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AO(Department of Physics, Durham University, UK) AP(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AQ(Department of Physics, Durham University, UK) AR(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AS(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AT(Institut für Physik und Astronomie, Universität Potsdam, Germany)
Abstract:
X-ray and mid-infrared emission are signposts of the accretion of matter onto the supermassive black holes that reside at the centres of most galaxies. As a major step towards understanding accreting supermassive black holes and their role in the evolution of galaxies, we will use the 4MOST multi-object spectrograph to provide a highly complete census of active galactic nuclei over a large fraction of the extragalactic sky observed in X-rays by eROSITA that is visible to 4MOST. We will systematically follow up all eROSITA point-like extragalactic X-ray sources (mostly active galactic nuclei), and complement them with a heavily obscured active galactic nuclei selection approach using mid-infrared data from the Wide-field Infrared Survey Explorer (WISE). The X-ray and mid-infrared flux limits of eROSITA and WISE are well matched to the spectroscopic capabilities of a 4-metre-class telescope, allowing us to reach completeness levels of ~ 80–90% for all X-ray selected active galactic nuclei with fluxes f_{0.5–2 keV} > 10^–14 erg s^–1 cm^–2; this is about a factor of 30 deeper than the ROSAT all-sky survey. With these data we will determine the physical properties (redshift, luminosity, line emission strength, masses, etc.) of up to one million supermassive black holes, constrain their cosmic evolution and clustering properties, and explore the connection between active galactic nuclei and large-scale structure over redshifts 0 ≲ z ≲ 6.
References:
Aird, J. et al. 2015, MNRAS, 451, 1892; Alexander, D. M. & Hickox, R. C. 2012, NewAR, 56, 93; Banerji, M. et al. 2012, MNRAS, 427, 2275; Clerc, N. et al. 2018, A&A, 617, 92; Comparat, J. et al., MNRAS, submitted; Dwelly, T. et al. 2017, MNRAS, 469, 1065; Fotopolou, S. & Paltani, S. 2018, A&A, 619, 14; Harrison, C. M. 2017, Nature Astron., 1, 0165; Kolodzig, A. et al. 2013, A&A, 558, A90; Krumpe, M. et al. 2015, ApJ, 815, 21; Lam, A., Wright, E. & Malkan, M. 2018, MNRAS, 480, 451; Mateos, S. et al. 2012, MNRAS, 426, 3271; Menzel, M.-L. et al. 2016, MNRAS, 457, 110; Merloni, A. et al. 2012, arXiv:1209.3114; Reed, S. L. et al. 2017, MNRAS, 468, 4702; Risaliti, G. & Lusso, E. 2019, Nature Astronomy, in press; Shen, Y. 2013, Bulletin of the Astronomical Society of India, 41, 61

DOI:
10.18727/0722-6691/5126
ADS BibCode:
2019Msngr.175...46D
Section:
Surveys
Author(s)/Affiliation(s):
Driver, S.P.; Liske, J.; Davies, L.J.M.; Robotham, A.S.G.; Baldry, I.K.; Brown, M.J.I.; Cluver, M.; Kuijken, K.; Loveday, J.; McMahon, R.; Meyer, M.J.; Norberg, P.; Owers, M.; Power, C.; Taylor, E.N.; The WAVES Team
AA(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) AB(Hamburger Sternwarte, Universität Hamburg, Germany) AC(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) AD(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) AE(Astrophysics Research Institute, Liverpool John Moores University, UK) AF(School of Physics and Astronomy, Monash University, Melbourne, Australia) AG(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia) AH(Sterrewacht Leiden, Universiteit Leiden, the Netherlands) AI(University of Sussex, Brighton, UK) AJ(Institute of Astronomy, University of Cambridge, UK) AK(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) AL(Department of Physics, Durham University, UK) AM(Department of Physics and Astronomy, Macquarie University, Sydney, Australia) AN(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) AO(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia)
Abstract:
WAVES is designed to study the growth of structure, mass and energy on scales of ~ 1 kpc to ~ 10 Mpc over a 7 Gyr timeline. On the largest length scales (1–10 Mpc) WAVES will measure the structures defined by groups, filaments and voids, and their emergence over recent times. Comparisons with bespoke numerical simulations will be used to confirm, refine or refute the Cold Dark Matter paradigm. At intermediate length scales (10 kpc^–1 Mpc) WAVES will probe the size and mass distribution of galaxy groups, as well as the galaxy merger rates, in order to directly measure the assembly of dark matter halos and stellar mass. On the smallest length scales (1–10 kpc) WAVES will provide accurate distance and environmental measurements to complement high-resolution space-based imaging to study the mass and size evolution of galaxy bulges, discs and bars. In total, WAVES will provide a panchromatic legacy dataset of ~ 1.6 million galaxies, firmly linking the very low (z < 0.1) and intermediate (z ~ 0.8) redshift Universe.
References:
Alpaslan, M. et al. 2014, MNRAS, 438, 177; Bilicki, M. et al. 2018, A&A, 616, A69; Colless, M. et al. 2001, MNRAS, 328, 1039; Davies, L. J. M. et al. 2015, MNRAS, 452, 616; DESI Collaboration: Aghamousa, A. et al. 2016, arXiv:1611.00036; Driver, S. P. & Robotham, A. S. G. 2010, MNRAS, 407, 2131; Driver, S. P. et al. 2011, MNRAS, 413, 971; Elahi, P. et al. 2018, MNRAS, 475, 5338; Fall, S. M. & Efstathiou, G. 1980, MNRAS, 193, 189; Frenk, C. S. et al. 1988, ApJ, 327, 507; Ishiyama, T. et al. 2015, PASJ, 67, 61; Liske, J. et al. 2015, MNRAS, 452, 2087; Ludlow, A. et al. 2016, MNRAS, 460, 1214; Robotham, A. S. G. et al. 2011, MNRAS, 416, 2640; Springel, V. et al. 2005, Nature, 435, 629; York, D. G. et al. 2000, AJ, 120, 1579

DOI:
10.18727/0722-6691/5127
ADS BibCode:
2019Msngr.175...50R
Section:
Surveys
Author(s)/Affiliation(s):
Richard, J.; Kneib, J.-P.; Blake, C.; Raichoor, A.; Comparat, J.; Shanks, T.; Sorce, J.; Sahlén, M.; Howlett, C.; Tempel, E.; McMahon, R.; Bilicki, M.; Roukema, B.; Loveday, J.; Pryer, D.; Buchert, T.; Zhao, C.; The CRS Team
AA(Centre de Recherche Astrophysique de Lyon, France) AB(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) AC(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia) AD(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) AE(Max-Planck-Institut für extraterrestrische Physik, Garching, Germany) AF(Department of Physics, Durham University, UK) AG(Centre de Recherche Astrophysique de Lyon, France; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AH(Department of Physics and Astronomy, Uppsala universitet, Sweden) AI(International Centre for Radio Astronomy Research/University of Western Australia, Perth, Australia) AJ(Tartu Observatory, University of Tartu, Estonia; Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AK(Institute of Astronomy, University of Cambridge, UK) AL(Sterrewacht Leiden, Universiteit Leiden, the Netherlands) AM(Torun Centre for Astronomy (TCfA), Nicolaus Copernicus University, Poland; Centre de Recherche Astrophysique de Lyon, France) AN(University of Sussex, Brighton, UK) AO(University of Sussex, Brighton, UK) AP(Centre de Recherche Astrophysique de Lyon, France) AQ(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland)
Abstract:
The 4MOST Cosmology Redshift Survey (CRS) will perform stringent cosmological tests via spectroscopic clustering measurements that will complement the best lensing, cosmic microwave background and other surveys in the southern hemisphere. The combination of carefully selected samples of bright galaxies, luminous red galaxies, emission-line galaxies and quasars, totalling about 8 million objects over the redshift range z = 0.15 to 3.5, will allow definitive tests of gravitational physics. Many key science questions will be addressed by combining CRS spectra of these targets with data from current or future facilities such as the Large Synoptic Survey Telescope, the Square Kilometre Array and the Euclid mission.
References:
Bautista, J. E. et al. 2017, A&A, 603, 12; Clarkson, C. et al. 2008, Physical Review Letters, 101, 011301; Collett, T. E. 2015, ApJ, 811, 20; Comparat, J. et al. 2016, A&A, 592, 121; Howlett, C. et al. 2017, ApJ, 847, 128; Kirk, D. et al. 2015, MNRAS, 451, 4424; Newman, J. A. et al. 2015, Astroparticle Physics, 63, 81; Risaliti, G. & Lusso, E. 2018, Nature Astronomy, arXiv:1811.02590; Roukema, B. F. et al. 2015, MNRAS, 448, 1660; Wolz, L. et al. 2017, MNRAS, 470, 3220

DOI:
10.18727/0722-6691/5128
ADS BibCode:
2019Msngr.175...54C
Section:
Surveys
Author(s)/Affiliation(s):
Cioni, M.-.R.L.; Storm, J.; Bell, C.P.M.; Lemasle, B.; Niederhofer, F.; Bestenlehner, J.M.; El Youssoufi, D.; Feltzing, S.; González-Fernández, C.; Grebel, E.K.; Hobbs, D.; Irwin, M.; Jablonka, P.; Koch, A.; Schnurr, O.; Schmidt, T.; Steinmetz, M.
AA(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AB(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AC(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AD(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) AE(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AF(Physics and Astronomy, University of Sheffield, UK) AG(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AH(Lund Observatory, Lund University, Sweden) AI(Institute of Astronomy, University of Cambridge, UK) AJ(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) AK(Lund Observatory, Lund University, Sweden) AL(Institute of Astronomy, University of Cambridge, UK) AM(Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne, Switzerland) AN(Zentrum für Astronomie der Universität Heidelberg/Astronomisches Rechen-Institut, Germany) AO(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany; Cherenkov Telescope Array Observatory, Bologna, Italy) AP(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany) AQ(Leibniz-Institut für Astrophysik Potsdam (AIP), Germany)
Abstract:
The One Thousand and One Magellanic Fields (1001MC) survey aims to measure the kinematics and elemental abundances of many different stellar populations that sample the history of formation and interaction of the Magellanic Clouds. The survey will collect spectra of about half a million stars with G < 19.5 magnitudes (Vega) distributed over an area of about 1000 square degrees and will provide an invaluable dataset for a wide range of scientific applications.
References:
Bestenlehner, J. M. et al. 2014, A&A, 570, A38; Dobbie, P. D. et al. 2014, MNRAS, 442, 1663; Kallivayalil, N. et al. 2013, ApJ, 764, 161; Koposov, S. et al. 2018, MNRAS, 479, 5343; Kozlowski, S. et al. 2013, ApJ, 775, 92; Nicholls, C. P. et al. 2010, MNRAS, 405, 1770; Nidever, D. et al. 2019, ApJ, submitted Niederhofer, F. et al. 2018, A&A, 613, L8; Richter, P. et al. 2013, ApJ, 772, 111; Rubele, S. et al. 2018, MNRAS, 478, 501; Sana, H. et al. 2013, A&A, 550, A107

DOI:
10.18727/0722-6691/5129
ADS BibCode:
2019Msngr.175...58S
Section:
Surveys
Author(s)/Affiliation(s):
Swann, E.; Sullivan, M.; Carrick, J.; Hoenig, S.; Hook, I.; Kotak, R.; Maguire, K.; McMahon, R.; Nichol, R.; Smartt, S.
AA(Institute of Cosmology and Gravitation, University of Portsmouth, UK) AB(School of Physics and Astronomy, University of Southampton, UK) AC(Physics Department, Lancaster University, UK) AD(School of Physics and Astronomy, University of Southampton, UK) AE(Physics Department, Lancaster University, UK) AF(School of Mathematics and Physics, Queen’s University Belfast, UK; University of Turku, Finland) AG(School of Mathematics and Physics, Queen’s University Belfast, UK) AH(Institute of Astronomy, University of Cambridge, UK) AI(Institute of Cosmology and Gravitation, University of Portsmouth, UK) AJ(School of Mathematics and Physics, Queen’s University Belfast, UK)
Abstract:
The Time-Domain Extragalactic Survey (TiDES) is focused on the spectro-scopic follow-up of extragalactic optical transients and variable sources selected from forthcoming large sky surveys such as that from the Large Synoptic Survey Telescope (LSST). TiDES contains three sub-surveys: (i) spectroscopic observations of supernova- like transients; (ii) comprehensive follow-up of transient host galaxies to obtain redshift measurements for cosmological applications; and (iii) repeat spectroscopic observations to enable the reverberation mapping of active galactic nuclei. Our simulations predict we will be able to classify transients down to r = 22.5 magnitudes (AB) and, over five years of 4MOST operations, obtain spectra for up to 30 000 live transients to redshift z ~ 0.5, measure redshifts for up to 50 000 transient host galaxies to z ~ 1 and monitor around 700 active galactic nuclei to z ~ 2.5.
References:
Balland, C. et al. 2009, A&A, 507, 85; Childress, M. et al. 2017, MNRAS, 472, 273; DES Collaboration et al. 2018, ApJL, arXiv:1811.02374; Goldstein, D. A. et al. 2018, ApJS, submitted King, A. L. et al. 2015, MNRAS, 453, 1701; Lochner, M. et al. 2016, ApJS, 225, 31; Mandelbaum, R. et al. 2018, arXiv:1809.01669; Shen, Y. et al. 2016, ApJ, 818, 30; Smartt, S. J. et al. 2017, Nature, 551, 75; Watson, D. et al. 2011, ApJ, 740, 49

DOI:
10.18727/0722-6691/5130
ADS BibCode:
2019Msngr.175...63P
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO Phase 1 Project Team;
AA(ESO)

DOI:
10.18727/0722-6691/5131
ADS BibCode:
2019Msngr.175...63E
Section:
Astronomical News
Author(s)/Affiliation(s):
Sedaghati, E.; Miotello, A.
AA(ESO) AB(ESO)

DOI:
10.18727/0722-6691/5132
ADS BibCode:
2019Msngr.175...66E
Section:
Astronomical News
Author(s)/Affiliation(s):
Zhang, Z.-Y.
AA(ESO)

ADS BibCode:
2019Msngr.175...67E
Section:
Astronomical News
Author(s)/Affiliation(s):
ESO

ADS BibCode:
2019Msngr.175...69E
Section:
Annual Index
Author(s)/Affiliation(s):
ESO