Author: "Max-Planck-Institut für Astrophysik (MPA)" / Topic: astrophysics::cosmology and extragalactic astrophysics - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Max-Planck-Institut für Astrophysik (MPA)"' showing total 107 results

Start Over Author "Max-Planck-Institut für Astrophysik (MPA)" Topic astrophysics::cosmology and extragalactic astrophysics

107 results on '"Max-Planck-Institut für Astrophysik (MPA)"'

1. The Fourteenth Data Release of the Sloan Digital Sky Survey:First Spectroscopic Data from the Extended Baryon Oscillation Spectroscopic Survey and from the Second Phase of the Apache Point Observatory Galactic Evolution Experiment

Author: Abolfathi , Bela, Aguado , D. S., Aguilar , Gabriela, Prieto , Carlos Allende, Almeida , Andres, Ananna , Tonima Tasnim, Anders , Friedrich, Anderson , Scott F., Andrews , Brett H., Anguiano , Borja, Aragon-Salamanca , Alfonso, Argudo-Fernandez , Maria, Armengaud , Eric, Ata , Metin, Aubourg , Eric, Avila-Reese , Vladimir, Badenes , Carles, Bailey , Stephen, Balland , Christophe, Barger , Kathleen A., Barrera-Ballesteros , Jorge, Bartosz , Curtis, Bastien , Fabienne, Bates , Dominic, Baumgarten , Falk, Bautista , Julian, Beaton , Rachael, Beers , Timothy C., Belfiore , Francesco, Bender , Chad F., Bernardi , Mariangela, Bershady , Matthew A., Beutler , Florian, Bird , Jonathan C., Bizyaev , Dmitry, Blanc , Guillermo A., Blanton , Michael R., Blomqvist , Michael, Bolton , Adam S., Boquien , Médéric, Borissova , Jura, Bovy , Jo, Diaz , Christian Andres Bradna, Brandt , William Nielsen, Brinkmann , Jonathan, Brownstein , Joel R., Bundy , Kevin, Burgasser , Adam J., Burtin , Etienne, Busca , Nicolás G., Canas , Caleb I., Cano-Diaz , Mariana, Cappellari , Michele, Carrera , Ricardo, Casey , Andrew R., Sodi , Bernardo Cervantes, Chen , Yanping, Cherinka , Brian, Chiappini , Cristina, Choi , Peter Doohyun, Chojnowski , Drew, Chuang , Chia-Hsun, Chung , Haeun, Clerc , Nicolas, Cohen , Roger E., Comerford , Julia M., Comparat , Johan, Nascimento , Janaina Correa do, da Costa , Luiz, Cousinou , Marie-Claude, Covey , Kevin, Crane , Jeffrey d., Cruz-Gonzalez , Irene, Cunha , Katia, Ilha , Gabriele da Silva, Damke , Guillermo J., Darling , Jeremy, Davidson Jr. , James W., Dawson , Kyle, Lizaola , Miguel Angel C. de Icaza, de la Macorra , Axel, De La Torre , Sylvain, De Lee , Nathan, Agathe , Victoria de Sainte, Machado , Alice Deconto, Dell'Agli , Flavia, Delubac , Timothée, Diamond-Stanic , Aleksandar M., Donor , John, Downes , Juan Jose, Drory , Niv, Bourboux , Hélion du Mas des, Duckworth , Christopher J., Dwelly , Tom, Dyer , Jamie, Ebelke , Garrett, Eigenbrot , Arthur Davis, Eisenstein , Daniel J., Elsworth , Yvonne P., Emsellem , Eric, Eracleous , Mike, Erfanianfar , Ghazaleh, Escoffier , Stéphanie, Fan , Xiaohui, Alvar , Emma Fernandez, Fernandez-Trincado , J. G., Cirolini , Rafael Fernando, Feuillet , Diane, Finoguenov , Alexis, Fleming , Scott W., Font-Ribera , Andreu, Freischlad , Gordon, Frinchaboy , Peter, Fu , Hai, Chew , Yilen Gomez Maqueo, Galbany , Lluis, Perez , Ana E. Garcia, Garcia-Dias , R., García-Hernández , D. A., Oehmichen , Luis Alberto Garma, Gaulme , Patrick, Gelfand , Joseph, Gil-Marin , Hector, Gillespie , Bruce A., Goddard , Daniel, Hernandez , Jonay I. Gonzalez, Gonzalez-Perez , Violeta, Grabowski , Kathleen, Green , Paul J., Grier , Catherine J., Gueguen , Alain, Guo , Hong, Guy , Julien, Hagen , Alex, Hall , Patrick, Harding , Paul, Hasselquist , Sten, Hawley , Suzanne, Hayes , Christian R., Hearty , Fred, Hekker , Saskia, Hernández , Jesús, Toledo , Hector Hernandez, Hogg , David W., Holley-Bockelmann , Kelly, Holtzman , Jon, Hou , Jiamin, Hsieh , Bau-Ching, Hunt , Jason A. S., Hutchinson , Timothy A., Hwang , Ho Seong, Angel , Camilo Eduardo Jimenez, Johnson , Jennifer A., Jones , Amy, Jönsson , Henrik, Jullo , Eric, Khan , Fahim Sakil, Kinemuchi , Karen, Kirkby , David, Kirkpatrick IV , Charles C., Kitaura , Francisco-Shu, Knapp , Gillian R., Kneib , Jean-Paul, Kollmeier , Juna A., Lacerna , Ivan, Lane , Richard R., Lang , Dustin, Law , David R., Goff , Jean-Marc Le, Lee , Young-Bae, Li , Hongyu, Li , Cheng, Lian , Jianhui, Liang , Yu, Lima , Marcos, Lin , Lihwai, Long , Dan, Lucatello , Sara, Lundgren , Britt, Mackereth , J. Ted, MacLeod , Chelsea L., Mahadevan , Suvrath, Maia , Marcio Antonio Geimba, Majewski , Steven, Manchado , Arturo, Maraston , Claudia, Mariappan , Vivek, Marques-Chaves , Rui, Masseron , Thomas, Masters , Karen L., Mcdermid , Richard M., McGreer , Ian D., Melendez , Matthew, Meneses-Goytia , Sofia, Merloni , Andrea, Merrifield , Michael R., Meszaros , Szabolcs, Meza , Andres, Minchev , Ivan, Minniti , Dante, Prieto , Carlos, Ananna , Tonima, Anderson , Scott, Andrews , Brett, Aragón-Salamanca , Alfonso, Argudo-Fernández , Maria, Barger , Kathleen, Beers , Timothy, Bender , Chad, Bershady , Matthew, Bird , Jonathan, Blanc , Guillermo, Blanton , Michael, Bolton , Adam, Andres , Christian, Diaz , Bradna, Brandt , William, Brownstein , Joel, Burgasser , Adam, Busca , Nicolás, Cañas , Caleb, Cano-Díaz , Mariana, Casey , Andrew, Sodi , Bernardo, Choi , Peter, 10 , Davidson, Angel , Miguel, De Icaza Lizaola , C, De Sainte , Victoria, 72 , Agathe, Machado , Alice, Dell 'agli , Flavia, Diamond-Stanic , Aleksandar, Downes , Juan, du Mas des Bourboux , Hélion, Duckworth , Christopher, Davis Eigenbrot , Arthur, Eisenstein , Daniel, Elsworth , Yvonne, Fernández Alvar , Emma, Fernández-Trincado , J., Cirolini , Rafael, Fleming , Scott, Gómez , Yilen, Chew , Maqueo, Galbany , Lluís, García Pérez , Ana, Alberto , Luis, Oehmichen , Garma, Gil-Marín , Héctor, Gillespie , Bruce, González Hernández , Jonay, Green , Paul, Grier , Catherine, Hayes , Christian, Toledo , Hector, Hogg , David, Hunt , Jason, Hutchinson , Timothy, Hwang , Ho, Jimenez Angel , Camilo, Johnson , Jennifer, Fahim , Sakil, Kirkpatrick , Charles, 94 , Iv, Knapp , Gillian, Kollmeier , Juna, Lane , Richard, Law , DAvid, Le Goff , Jean-Marc, Macleod , Chelsea, Antonio , Marcio, Maia , Geimba, Masters , Karen, Mueller , Eva-Maria, Muller-Sanchez , Francisco, Muna , Demitri, Muñoz , Ricardo, Myers , Adam, Nair , Preethi, Nandra , Kirpal, Ness , Melissa, Newman , Jeffrey, Nichol , Robert, Nidever , David, Nitschelm , Christian, Noterdaeme , Pasquier, O 'connell , Julia, Oelkers , Ryan, Oravetz , Audrey, Oravetz , Daniel, Aquino Ortíz , Erik, Osorio , Yeisson, Pace , Zach, Padilla , Nelson, Palanque-Delabrouille , Nathalie, Palicio , Pedro, Pan , Hsi-An, Pan , Kaike, Parikh , Taniya, Pâris , Isabelle, Park , Changbom, Peirani , Sebastien, Pellejero-Ibanez , Marcos, Penny , Samantha, Percival , Will, Perez-Fournon , Ismael, Petitjean , Patrick, Pieri , Matthew, Pinsonneault , Marc, Pisani , Alice, Prada , Francisco, Prakash , Abhishek, Bárbara De Andrade Queiroz , Anna, Raddick , M, Raichoor , Anand, Rembold , Sandro, Richstein , Hannah, Riffel , Rogemar, Riffel , Rogério, Rix , Hans-Walter, Robin , Annie, Torres , Sergio, Román-Zúñiga , Carlos, Ross , Ashley, Rossi , Graziano, Ruan , John, Ruggeri , Rossana, Ruiz , Jose, Salvato , Mara, Sánchez , Ariel, Sanchez , Sebastian, Sanchez Almeida , Jorge, Sánchez-Gallego , José, Antonio , Felipe, Rojas , Santana, Santiago , Basílio, Schiavon , Ricardo, Schimoia , Jaderson, Schlafly , Edward, Schlegel , David, Schneider , Donald, Schuster , William, Schwope , Axel, Seo , Hee-Jong, Serenelli , Aldo, Shen , Shiyin, Shen , Yue, Shetrone , Matthew, Shull , Michael, Aguirre , Silva, Simon , Joshua, Skrutskie , Mike, Slosar , Anže, Smethurst , Rebecca, Smith , Verne, Sobeck , Jennifer, Somers , Garrett, Souter , Barbara, Souto , Diogo, Spindler , Ashley, Stark , David, Stassun , Keivan, Steinmetz , Matthias, Stello , Dennis, Storchi-Bergmann , Thaisa, Streblyanska , Alina, Stringfellow , Guy, Suárez , Genaro, Sun , Jing, Szigeti , Laszlo, Taghizadeh-Popp , Manuchehr, talbot , michael, Tang , Baitian, Tao , Charling, Tayar , Jamie, Tembe , Mita, Teske , Johanna, Aniruddha R. , Thakar, Daniel , Thomas, Tissera , Patricia, Tojeiro , Rita, Tremonti , Christy, Troup , Nicholas W., Urry , Meg, Valenzuela , O., van den Bosch , Remco, Vargas-González , Jaime, Magaña , Mariana Vargas, Vazquez , Jose Alberto, Villanova , Sandro, Vogt , Nicole, Wake , David, Wang , Yuting, Weaver , Benjamin Alan, Weijmans , Anne-Marie, Weinberg , David H., Westfall , Kyle B., Whelan , David G., Wilcots , Eric, Wild , Vivienne, Williams , Rob A., Wilson , John, Wood-Vasey , W.M., Wylezalek , Dominika, Xiao , Ting, Yan , Renbin, Yang , Meng, Ybarra , Jason E., Yèche , Christophe, Zakamska , Nadia, Zamora , Olga, Zarrouk , Pauline, Zasowski , Gail, Zhang , Kai, Zhao , Chang, Zhao , Gong-Bo, Zheng , Zheng, Zhou , Zhi-Min, Zhu , Guangtun, Zinn , Joel C., Zou , Hu, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astrophysical Sciences [Princeton], Princeton University, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Université Paris Diderot - Paris 7 (UPD7), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, European Southern Observatory (ESO), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Departamento de Matemáticas [Madrid], Universidad Autónoma de Madrid (UAM), Department of Physics and Astronomy [Nashville], Vanderbilt University [Nashville], Korea Institute for Advanced Study (KIAS), Sainsbury Laboratory Cambridge University (SLCU), University of Cambridge [UK] (CAM), Wuhan University [China], Equipe de Recherche sur l’Utilisation des Données Individuelles en lien avec la Théorie Economique (ERUDITE), Université Paris-Est Marne-la-Vallée (UPEM)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), Institute of Astronomy [Cambridge], Max-Planck-Institut für Astrophysik (MPA), Department of Physics and Astronomy [Rochester], University of Rochester [USA], Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Inflammation, Tissus épithéliaux et Cytokines (LITEC), Université de Poitiers, Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques (REHSEIS (UMR_7596)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Universidad Politécnica de Madrid (UPM), Universidad de Jaén (UJA), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), University of Edinburgh, Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], Alfred P. Sloan Foundation, Department of Energy (US), University of Utah, AVL, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Astronomy and Astrophysics ( PENNSYLVANIA STATE UNIVERSITY ), PennState University [Pennsylvania] ( PSU ), Université Paris Diderot - Paris 7 ( UPD7 ), University of Pennsylvania [Philadelphia], Laboratoire d'Astrophysique de Marseille ( LAM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Aix Marseille Université ( AMU ) -Centre National d'Etudes Spatiales ( CNES ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), California Institute of Technology ( CALTECH ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, University of Oxford [Oxford]-University of Oxford [Oxford], Imaging Diagnostic Center, Nanfang Hospital Guangzhou, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid ( UAM ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Carnegie Institution of Washington, AUTRES, Département de Physique des Particules (ex SPP) ( DPP ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, School of Physics and Astronomy, University of Birmingham [Birmingham], European Southern Observatory ( ESO ), Département de Physique Nucléaire (ex SPhN) ( DPHN ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Max-Planck-Institut für Astronomie ( MPIA ), STScI, University of California [Irvine] ( UCI ), ISO Data Centre ( ESA - Espagne ), European Space Agency ( ESA ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Lagrange de Paris, Sorbonne Universités, Research Institute of Forest Resource Information Techniques, Chinese Academy of Forestry, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Korea Institute for Advanced Study ( KIAS ), Department of Astronomy ( Ohio State University ), Ohio State University [Columbus] ( OSU ), Institute of Infection, Immunity & Inflammation, University of Glasgow, Sainsbury Laboratory Cambridge, University of Cambridge [UK] ( CAM ), Equipe de Recherche sur l’Utilisation des Données Individuelles en lien avec la Théorie Economique ( ERUDITE ), Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ) -Université Paris-Est Marne-la-Vallée ( UPEM ), Institute of Physics, Universidade de Brasilia [Brasília] ( UnB ), Department of Chemical and Biomolecular Engineering, University of California [Berkeley], Max-Planck-Institut für Astrophysik ( MPA ), Bioinformatics and Functional Genomics Research Group, Cancer Research Center (IBMCC-CIC, CSIC-USAL), University of Wisconsin-Madison [Madison], Texas Tech University Health Sciences Center, Texas Tech University [Lubbock] ( TTU ), Institute for Astronomy ( IfA ), University of Hawaii, Research Institute of Organic Agriculture ( FiBL ), Dept. of Physics, Princess Margaret Hospital, University of Toronto-Princess Margaret Hospital, J. A. Baker Institute, Cornell University, The Observatories of the Carnegie Institution for Science, Economics, Bangor, Physics Department, Carnegie Mellon University [Pittsburgh] ( CMU ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Inflammation, Tissus épithéliaux et Cytokines ( LITEC ), School of Physics, Korea Institute for Advanced Study, Korea Institute for Advanced Study-Korea Institute for Advanced Study, Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques ( REHSEIS ), Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Universidad Politécnica de Madrid ( UPM ), Universidad de Jaén ( UJA ), Institute of Space Sciences [Barcelona] ( ICE-CSIC ), Spanish National Research Council [Madrid] ( CSIC ), Department of Physics and Astronomy - Stellar Astrophysics Centre, Department of Physics, The Leverhulme Trust, University of St Andrews. School of Physics and Astronomy, University of St Andrews. Centre for Contemporary Art, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Département de Physique des Particules (ex SPP) (DPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universidad Autonoma de Madrid (UAM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), University of California [Irvine] (UCI), University of California-University of California, ISO Data Centre (ESA - Espagne), European Space Agency (ESA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Universidade de Brasilia [Brasília] (UnB), University of Wisconsin-Madison, Texas Tech University [Lubbock] (TTU), Institute for Astronomy [Honolulu] (IfA), University of Hawai'i [Honolulu] (UH), Research Institute of Organic Agriculture (FiBL), University of Toronto, Bangor University, Carnegie Mellon University [Pittsburgh] (CMU), Recherches Epistémologiques et Historiques sur les Sciences Exactes et les Institutions Scientifiques (REHSEIS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Université Paris-Est Marne-la-Vallée (UPEM), Research Institute of Organic Agriculture - Forschungsinstitut für biologischen Landbau (FiBL), Cornell University [New York], Carnegie Observatories, Carnegie Institution for Science [Washington], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Astrophysics, E-SCIENCE, 01 natural sciences, HISTORIES, TARGET SELECTION, Observatory, QB Astronomy, 010303 astronomy & astrophysics, R2C, QC, media_common, QB, Physics, CATALOGS, Point (typography), ~DC~, Astrophysics::Instrumentation and Methods for Astrophysics, 520 Astronomie und zugeordnete Wissenschaften, atlases, GALAXIES, X-RAY SURVEYS, BDC, Astrophysics - Instrumentation and Methods for Astrophysics, METALLICITY, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], TELESCOPE, media_common.quotation_subject, astro-ph.GA, Phase (waves), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Data-driven, Data cube, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, 0103 physical sciences, ddc:530, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysics, DAS, 115 Astronomy, Space science, Catalogues, 530 Physik, Astrophysics - Astrophysics of Galaxies, Galaxy, Baryon, QC Physics, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), ddc:520, catalogs, astro-ph.IM, SDSS-IV MANGA
Abstract: Open Access. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI., The fourth generation of the Sloan Digital Sky Survey (SDSS-IV) has been in operation since 2014 July. This paper describes the second data release from this phase, and the 14th from SDSS overall (making this Data Release Fourteen or DR14). This release makes the data taken by SDSS-IV in its first two years of operation (2014-2016 July) public. Like all previous SDSS releases, DR14 is cumulative, including the most recent reductions and calibrations of all data taken by SDSS since the first phase began operations in 2000. New in DR14 is the first public release of data from the extended Baryon Oscillation Spectroscopic Survey; the first data from the second phase of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE-2), including stellar parameter estimates from an innovative data-driven machine-learning algorithm known as ¿The Cannon¿ and almost twice as many data cubes from the Mapping Nearby Galaxies at APO (MaNGA) survey as were in the previous release (N = 2812 in total). This paper describes the location and format of the publicly available data from the SDSS-IV surveys. We provide references to the important technical papers describing how these data have been taken (both targeting and observation details) and processed for scientific use. The SDSS web site (www.sdss.org) has been updated for this release and provides links to data downloads, as well as tutorials and examples of data use. SDSS-IV is planning to continue to collect astronomical data until 2020 and will be followed by SDSS-V. © 2018. The American Astronomical Society.., Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org.
Published: 2018

2. Cosmological model parameter dependence of the matter power spectrum covariance from the DEUS-PUR Cosmo simulations

Author: Pier Stefano Corasaniti, Yann Rasera, Shankar Agarwal, Linda Blot, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, symbols.namesake, 0103 physical sciences, Statistical physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, Matter power spectrum, Spectral density, Astronomy and Astrophysics, Covariance, Universe, Redshift, Space and Planetary Science, Dark energy, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: Future galaxy surveys will provide accurate measurements of the matter power spectrum across an unprecedented range of scales and redshifts. The analysis of these data will require one to accurately model the imprint of non-linearities of the matter density field. In particular, these induce a non-Gaussian contribution to the data covariance that needs to be properly taken into account to realise unbiased cosmological parameter inference analyses. Here, we study the cosmological dependence of the matter power spectrum covariance using a dedicated suite of N-body simulations, the Dark Energy Universe Simulation - Parallel Universe Runs (DEUS-PUR) {\it Cosmo}. These consist of 512 realizations for 10 different cosmologies where we vary the matter density $\Omega_m$, the amplitude of density fluctuations $\sigma_8$, the reduced Hubble parameter $h$ and a constant dark energy equation of state $w$ by approximately $10\%$. We use these data to evaluate the first and second derivatives of the power spectrum covariance with respect to a fiducial $\Lambda$CDM cosmology. We find that the variations can be as large as $150\%$ depending on the scale, redshift and model parameter considered. By performing a Fisher matrix analysis we explore the impact of different choices in modelling the cosmological dependence of the covariance. Our results suggest that fixing the covariance to a fiducial cosmology can significantly affect the recovered parameter errors and that modelling the cosmological dependence of the variance while keeping the correlation coefficient fixed can alleviate the impact of this effect., Comment: 12 pages, 11 figures, replaced to match the version published on MNRAS. Data available at https://cosmo.obspm.fr/public-datasets/
Published: 2020

3. The 16th Data Release of the Sloan Digital Sky Surveys : First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra

Author: Romina Ahumada, Carlos Allende Prieto, Andrés Almeida, Friedrich Anders, Scott F. Anderson, Brett H. Andrews, Borja Anguiano, Riccardo Arcodia, Eric Armengaud, Marie Aubert, Santiago Avila, Vladimir Avila-Reese, Carles Badenes, Christophe Balland, Kat Barger, Jorge K. Barrera-Ballesteros, Sarbani Basu, Julian Bautista, Rachael L. Beaton, Timothy C. Beers, B. Izamar T. Benavides, Chad F. Bender, Mariangela Bernardi, Matthew Bershady, Florian Beutler, Christian Moni Bidin, Jonathan Bird, Dmitry Bizyaev, Guillermo A. Blanc, Michael R. Blanton, Médéric Boquien, Jura Borissova, Jo Bovy, W. N. Brandt, Jonathan Brinkmann, Joel R. Brownstein, Kevin Bundy, Martin Bureau, Adam Burgasser, Etienne Burtin, Mariana Cano-Díaz, Raffaella Capasso, Michele Cappellari, Ricardo Carrera, Solène Chabanier, William Chaplin, Michael Chapman, Brian Cherinka, Cristina Chiappini, Peter Doohyun Choi, S. Drew Chojnowski, Haeun Chung, Nicolas Clerc, Damien Coffey, Julia M. Comerford, Johan Comparat, Luiz da Costa, Marie-Claude Cousinou, Kevin Covey, Jeffrey D. Crane, Katia Cunha, Gabriele da Silva Ilha, Yu Sophia Dai, Sanna B. Damsted, Jeremy Darling, James W. Davidson, Roger Davies, Kyle Dawson, Nikhil De, Axel de la Macorra, Nathan De Lee, Anna Bárbara de Andrade Queiroz, Alice Deconto Machado, Sylvain de la Torre, Flavia Dell’Agli, Hélion du Mas des Bourboux, Aleksandar M. Diamond-Stanic, Sean Dillon, John Donor, Niv Drory, Chris Duckworth, Tom Dwelly, Garrett Ebelke, Sarah Eftekharzadeh, Arthur Davis Eigenbrot, Yvonne P. Elsworth, Mike Eracleous, Ghazaleh Erfanianfar, Stephanie Escoffier, Xiaohui Fan, Emily Farr, José G. Fernández-Trincado, Diane Feuillet, Alexis Finoguenov, Patricia Fofie, Amelia Fraser-McKelvie, Peter M. Frinchaboy, Sebastien Fromenteau, Hai Fu, Lluís Galbany, Rafael A. Garcia, D. A. García-Hernández, Luis Alberto Garma Oehmichen, Junqiang Ge, Marcio Antonio Geimba Maia, Doug Geisler, Joseph Gelfand, Julian Goddy, Violeta Gonzalez-Perez, Kathleen Grabowski, Paul Green, Catherine J. Grier, Hong Guo, Julien Guy, Paul Harding, Sten Hasselquist, Adam James Hawken, Christian R. Hayes, Fred Hearty, S. Hekker, David W. Hogg, Jon A. Holtzman, Danny Horta, Jiamin Hou, Bau-Ching Hsieh, Daniel Huber, Jason A. S. Hunt, J. Ider Chitham, Julie Imig, Mariana Jaber, Camilo Eduardo Jimenez Angel, Jennifer A. Johnson, Amy M. Jones, Henrik Jönsson, Eric Jullo, Yerim Kim, Karen Kinemuchi, Charles C. Kirkpatrick IV, George W. Kite, Mark Klaene, Jean-Paul Kneib, Juna A. Kollmeier, Hui Kong, Marina Kounkel, Dhanesh Krishnarao, Ivan Lacerna, Ting-Wen Lan, Richard R. Lane, David R. Law, Jean-Marc Le Goff, Henry W. Leung, Hannah Lewis, Cheng Li, Jianhui Lian, Lihwai Lin, Dan Long, Penélope Longa-Peña, Britt Lundgren, Brad W. Lyke, J. Ted Mackereth, Chelsea L. MacLeod, Steven R. Majewski, Arturo Manchado, Claudia Maraston, Paul Martini, Thomas Masseron, Karen L. Masters, Savita Mathur, Richard M. McDermid, Andrea Merloni, Michael Merrifield, Szabolcs Mészáros, Andrea Miglio, Dante Minniti, Rebecca Minsley, Takamitsu Miyaji, Faizan Gohar Mohammad, Benoit Mosser, Eva-Maria Mueller, Demitri Muna, Andrea Muñoz-Gutiérrez, Adam D. Myers, Seshadri Nadathur, Preethi Nair, Kirpal Nandra, Janaina Correa do Nascimento, Rebecca Jean Nevin, Jeffrey A. Newman, David L. Nidever, Christian Nitschelm, Pasquier Noterdaeme, Julia E. O’Connell, Matthew D. Olmstead, Daniel Oravetz, Audrey Oravetz, Yeisson Osorio, Zachary J. Pace, Nelson Padilla, Nathalie Palanque-Delabrouille, Pedro A. Palicio, Hsi-An Pan, Kaike Pan, James Parker, Romain Paviot, Sebastien Peirani, Karla Peña Ramŕez, Samantha Penny, Will J. Percival, Ismael Perez-Fournon, Ignasi Pérez-Ràfols, Patrick Petitjean, Matthew M. Pieri, Marc Pinsonneault, Vijith Jacob Poovelil, Joshua Tyler Povick, Abhishek Prakash, Adrian M. Price-Whelan, M. Jordan Raddick, Anand Raichoor, Amy Ray, Sandro Barboza Rembold, Mehdi Rezaie, Rogemar A. Riffel, Rogério Riffel, Hans-Walter Rix, Annie C. Robin, A. Roman-Lopes, Carlos Román-Zúñiga, Benjamin Rose, Ashley J. Ross, Graziano Rossi, Kate Rowlands, Kate H. R. Rubin, Mara Salvato, Ariel G. Sánchez, Laura Sánchez-Menguiano, José R. Sánchez-Gallego, Conor Sayres, Adam Schaefer, Ricardo P. Schiavon, Jaderson S. Schimoia, Edward Schlafly, David Schlegel, Donald P. Schneider, Mathias Schultheis, Axel Schwope, Hee-Jong Seo, Aldo Serenelli, Arman Shafieloo, Shoaib Jamal Shamsi, Zhengyi Shao, Shiyin Shen, Matthew Shetrone, Raphael Shirley, Víctor Silva Aguirre, Joshua D. Simon, M. F. Skrutskie, Anže Slosar, Rebecca Smethurst, Jennifer Sobeck, Bernardo Cervantes Sodi, Diogo Souto, David V. Stark, Keivan G. Stassun, Matthias Steinmetz, Dennis Stello, Julianna Stermer, Thaisa Storchi-Bergmann, Alina Streblyanska, Guy S. Stringfellow, Amelia Stutz, Genaro Suárez, Jing Sun, Manuchehr Taghizadeh-Popp, Michael S. Talbot, Jamie Tayar, Aniruddha R. Thakar, Riley Theriault, Daniel Thomas, Zak C. Thomas, Jeremy Tinker, Rita Tojeiro, Hector Hernandez Toledo, Christy A. Tremonti, Nicholas W. Troup, Sarah Tuttle, Eduardo Unda-Sanzana, Marica Valentini, Jaime Vargas-González, Mariana Vargas-Magaña, Jose Antonio Vázquez-Mata, M. Vivek, David Wake, Yuting Wang, Benjamin Alan Weaver, Anne-Marie Weijmans, Vivienne Wild, John C. Wilson, Robert F. Wilson, Nathan Wolthuis, W. M. Wood-Vasey, Renbin Yan, Meng Yang, Christophe Yèche, Olga Zamora, Pauline Zarrouk, Gail Zasowski, Kai Zhang, Cheng Zhao, Gongbo Zhao, Zheng Zheng, Guangtun Zhu, Hu Zou, Department of Physics, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional Autónoma de México (UNAM), Department of Astrophysical Sciences [Princeton], Princeton University, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Department of Astronomy, Yale University [New Haven], University of Notre Dame [Indiana] (UND), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], University of Wisconsin-Madison, Texas Tech University Health Sciences Center, Texas Tech University [Lubbock] (TTU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), California Institute of Technology (CALTECH), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford [Oxford]-University of Oxford [Oxford], Center for Astrophysics and Space Sciences [La Jolla] (CASS), University of California [San Diego] (UC San Diego), University of California-University of California, Department of Psychology, St John's University, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Lowell Observatory [Flagstaff], Observatorio Nacional [Rio de Janeiro], Vernalis (R&D) Ltd, Special Care Dentistry, UCLH Eastman Dental Hospital, University of Utah, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad de La Laguna [Tenerife - SP] (ULL), University of Virginia [Charlottesville], University of Wyoming (UW), School of Physics and Astronomy, University of Birmingham [Birmingham], Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Arizona State University [Tempe] (ASU), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Max-Planck-Institut für Astronomie (MPIA), Texas Christian University (TCU), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UCI), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), New York University [New York] (NYU), NYU System (NYU), Research Institute of Forest Resource Information Techniques, Chinese Academy of Forestry, New Mexico State University, Pennsylvania State University (Penn State), Penn State System, Princess Margaret Hospital, University of Toronto, Cognition, Langues, Langage, Ergonomie (CLLE-ERSS), École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J)-Université Bordeaux Montaigne-Centre National de la Recherche Scientifique (CNRS), J. A. Baker Institute, Cornell University [New York], Institute of Infection, Immunity & Inflammation, University of Glasgow, Sainsbury Laboratory Cambridge University (SLCU), University of Cambridge [UK] (CAM), Ecole Polytechnique Fédérale de Lausanne (EPFL), Carnegie Observatories, Carnegie Institution for Science [Washington], Institute of Science and Technology [Austria] (IST Austria), Universidad de Atacama, Department of Chemical and Biomolecular Engineering, Universidad de Antofagasta, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Institute of cosmology and gravitation, University of Portsmouth, Institut d'Astronomie et d'Astrophysique [Bruxelles] (IAA), Université libre de Bruxelles (ULB), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max-Planck-Institut für Astrophysik (MPA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département des Sciences et Gestion de l'Environnement/Océanologie [Liège], Université de Liège, Universidad Andrés Bello [Santiago] (UNAB), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Montana State University (MSU), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Institut Lagrange de Paris, Sorbonne Université (SU), The Wellcome Trust Centre for Human Genetics [Oxford], University of Oxford [Oxford], Liverpool John Moores University (LJMU), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Chinese Academy of Sciences [Beijing] (CAS), McDonald Observatory, University of Texas at Austin [Austin], Astronomy Centre, University of Sussex, Department of Physics and Astronomy [Aarhus], Aarhus University [Aarhus], University of Washington [Seattle], Vanderbilt University [Nashville], Stellar Astrophysics Centre [Aarhus] (SAC), University of Colorado [Boulder], Laboratoire de Biochimie Médicale (LBM), CHU Rouen, Normandie Université (NU)-Normandie Université (NU), University of St Andrews [Scotland], Instituto de Astronomıa, universidad catolica del Norte, Institut d'Astrophysique et de Géophysique [Liège], Laboratoire de Physique des Solides (LPS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Department of Computer Science and Engineering [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Dunlap Institute for Astronomy and Astrophysics [Toronto], World Bank, State Key Laboratory in Computer Science [Beijing] (SKLCS), Institute of Software Chinese Academy of Sciences [Beijing], Nanjing University of Information Science and Technology (NUIST), Laboratoire de Chimie - UMR5182 (LC), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon)-Institut de Chimie du CNRS (INC), Johns Hopkins University (JHU), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Pennsylvania, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Oxford-University of Oxford, University of California (UC)-University of California (UC), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM), University of Virginia, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), University of California [Irvine] (UC Irvine), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Bordeaux Montaigne (UBM)-Centre National de la Recherche Scientifique (CNRS), Carnegie Institution for Science, Institute of Science and Technology [Klosterneuburg, Austria] (IST Austria), Harvard University-Smithsonian Institution, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Oxford, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Ahumada R., Prieto C.A., Almeida A., Anders F., Anderson S.F., Andrews B.H., Anguiano B., Arcodia R., Armengaud E., Aubert M., Avila S., Avila-Reese V., Badenes C., Balland C., Barger K., Barrera-Ballesteros J.K., Basu S., Bautista J., Beaton R.L., Beers T.C., Benavides B.I.T., Bender C.F., Bernardi M., Bershady M., Beutler F., Bidin C.M., Bird J., Bizyaev D., Blanc G.A., Blanton M.R., Boquien M., Borissova J., Bovy J., Brandt W.N., Brinkmann J., Brownstein J.R., Bundy K., Bureau M., Burgasser A., Burtin E., Cano-Diaz M., Capasso R., Cappellari M., Carrera R., Chabanier S., Chaplin W., Chapman M., Cherinka B., Chiappini C., Doohyun Choi P., Chojnowski S.D., Chung H., Clerc N., Coffey D., Comerford J.M., Comparat J., Da Costa L., Cousinou M.-C., Covey K., Crane J.D., Cunha K., Ilha G.D.S., Dai Y.S., Damsted S.B., Darling J., Davidson J.W., Davies R., Dawson K., De N., De La Macorra A., De Lee N., Queiroz A.B.D.A., Deconto Machado A., De La Torre S., Dell'Agli F., Du Mas Des Bourboux H., Diamond-Stanic A.M., Dillon S., Donor J., Drory N., Duckworth C., Dwelly T., Ebelke G., Eftekharzadeh S., Davis Eigenbrot A., Elsworth Y.P., Eracleous M., Erfanianfar G., Escoffier S., Fan X., Farr E., Fernandez-Trincado J.G., Feuillet D., Finoguenov A., Fofie P., Fraser-Mckelvie A., Frinchaboy P.M., Fromenteau S., Fu H., Galbany L., Garcia R.A., Garcia-Hernandez D.A., Oehmichen L.A.G., Ge J., Maia M.A.G., Geisler D., Gelfand J., Goddy J., Gonzalez-Perez V., Grabowski K., Green P., Grier C.J., Guo H., Guy J., Harding P., Hasselquist S., Hawken A.J., Hayes C.R., Hearty F., Hekker S., Hogg D.W., Holtzman J.A., Horta D., Hou J., Hsieh B.-C., Huber D., Hunt J.A.S., Chitham J.I., Imig J., Jaber M., Angel C.E.J., Johnson J.A., Jones A.M., Jonsson H., Jullo E., Kim Y., Kinemuchi K., Kirkpatrick Iv C.C., Kite G.W., Klaene M., Kneib J.-P., Kollmeier J.A., Kong H., Kounkel M., Krishnarao D., Lacerna I., Lan T.-W., Lane R.R., Law D.R., Le Goff J.-M., Leung H.W., Lewis H., Li C., Lian J., Lin L., Long D., Longa-Peña P., Lundgren B., Lyke B.W., Ted Mackereth J., Macleod C.L., Majewski S.R., Manchado A., Maraston C., Martini P., Masseron T., Masters K.L., Mathur S., McDermid R.M., Merloni A., Merrifield M., Meszaros S., Miglio A., Minniti D., Minsley R., Miyaji T., Mohammad F.G., Mosser B., Mueller E.-M., Muna D., Muñoz-Gutierrez A., Myers A.D., Nadathur S., Nair P., Nandra K., Do Nascimento J.C., Nevin R.J., Newman J.A., Nidever D.L., Nitschelm C., Noterdaeme P., O'Connell J.E., Olmstead M.D., Oravetz D., Oravetz A., Osorio Y., Pace Z.J., Padilla N., Palanque-Delabrouille N., Palicio P.A., Pan H.-A., Pan K., Parker J., Paviot R., Peirani S., Ramrez K.P., Penny S., Percival W.J., Perez-Fournon I., Perez-Rafols I., Petitjean P., Pieri M.M., Pinsonneault M., Poovelil V.J., Povick J.T., Prakash A., Price-Whelan A.M., Raddick M.J., Raichoor A., Ray A., Rembold S.B., Rezaie M., Riffel R.A., Riffel R., Rix H.-W., Robin A.C., Roman-Lopes A., Roman-Zuñiga C., Rose B., Ross A.J., Rossi G., Rowlands K., Rubin K.H.R., Salvato M., Sanchez A.G., Sanchez-Menguiano L., Sanchez-Gallego J.R., Sayres C., Schaefer A., Schiavon R.P., Schimoia J.S., Schlafly E., Schlegel D., Schneider D.P., Schultheis M., Schwope A., Seo H.-J., Serenelli A., Shafieloo A., Shamsi S.J., Shao Z., Shen S., Shetrone M., Shirley R., Aguirre V.S., Simon J.D., Skrutskie M.F., Slosar A., Smethurst R., Sobeck J., Sodi B.C., Souto D., Stark D.V., Stassun K.G., Steinmetz M., Stello D., Stermer J., Storchi-Bergmann T., Streblyanska A., Stringfellow G.S., Stutz A., Suarez G., Sun J., Taghizadeh-Popp M., Talbot M.S., Tayar J., Thakar A.R., Theriault R., Thomas D., Thomas Z.C., Tinker J., Tojeiro R., Toledo H.H., Tremonti C.A., Troup N.W., Tuttle S., Unda-Sanzana E., Valentini M., Vargas-Gonzalez J., Vargas-Magaña M., Vazquez-Mata J.A., Vivek M., Wake D., Wang Y., Weaver B.A., Weijmans A.-M., Wild V., Wilson J.C., Wilson R.F., Wolthuis N., Wood-Vasey W.M., Yan R., Yang M., Yeche C., Zamora O., Zarrouk P., Zasowski G., Zhang K., Zhao C., Zhao G., Zheng Z., Zhu G., Zou H., Alfred P. Sloan Foundation, and Department of Energy (US)
Subjects: Optical telescopes, SAMPLE, Astrophysics, 01 natural sciences, Astronomi, astrofysik och kosmologi, Infrared astronomy, Observatory, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, REDSHIFT 0.8, redshift surveys, stellar spectral lines, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Astronomy databases, Redshift surveys, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, stellar properties, CATALOG, astro-ph.CO, astronomy databases, Data release, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], infrared astonomy, TELESCOPE, astro-ph.GA, media_common.quotation_subject, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galactic abundances, Stellar properties, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, DISTANCES, Stellar spectral lines, 010308 nuclear & particles physics, Astronomy and Astrophysics, optical telescopes, 115 Astronomy, Space science, Galaxy, GALAXY, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], STELLAR, 13. Climate action, Space and Planetary Science, Sky, [SDU]Sciences of the Universe [physics], galactic abundances, MILKY, astro-ph.IM, SDSS-IV MANGA
Abstract: This paper documents the 16th data release (DR16) from the Sloan Digital Sky Surveys (SDSS), the fourth and penultimate from the fourth phase (SDSS-IV). This is the first release of data from the Southern Hemisphere survey of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2); new data from APOGEE-2 North are also included. DR16 is also notable as the final data release for the main cosmological program of the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and all raw and reduced spectra from that project are released here. DR16 also includes all the data from the Time Domain Spectroscopic Survey and new data from the SPectroscopic IDentification of ERosita Survey programs, both of which were co-observed on eBOSS plates. DR16 has no new data from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey (or the MaNGA Stellar Library "MaStar"). We also preview future SDSS-V operations (due to start in 2020), and summarize plans for the final SDSS-IV data release (DR17)., Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org.
Published: 2020

4. Double X/Peanut Structures in Barred Galaxies -Insights from an N -body Simulation

Author: Francesca Fragkoudi, Sergey Khoperskov, Francoise Combes, Paola Di Matteo, Bogdan C Ciambur, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Leibniz-Institut für Astrophysik Potsdam (AIP), and Russian Academy of Sciences [Moscow] (RAS)
Subjects: N-body simulation, Bar (music), Milky Way, kinematics and dynamics, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Projection (linear algebra), structure -galaxies, 0103 physical sciences, galaxies, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Galactic Center, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Dark matter halo, evolution -galaxies, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), bulges -galaxies
Abstract: Boxy, peanut- or X-shaped "bulges" are observed in a large fraction of barred galaxies viewed in, or close to, edge-on projection, as well as in the Milky Way. They are the product of dynamical instabilities occurring in stellar bars, which cause the latter to buckle and thicken vertically. Recent studies have found nearby galaxies that harbour two such features arising at different radial scales, in a nested configuration. In this paper we explore the formation of such double peanuts, using a collisionless N-body simulation of a pure disc evolving in isolation within a live dark matter halo, which we analyse in a completely analogous way to observations of real galaxies. In the simulation we find a stable double configuration consisting of two X/peanut structures associated to the same galactic bar - rotating with the same pattern speed - but with different morphology, formation time, and evolution. The inner, conventional peanut-shaped structure forms early via the buckling of the bar, and experiences little evolution once it stabilises. This feature is consistent in terms of size, strength and morphology, with peanut structures observed in nearby galaxies. The outer structure, however, displays a strong X, or "bow-tie", morphology. It forms just after the inner peanut, and gradually extends in time (within 1 to 1.5 Gyr) to almost the end of the bar, a radial scale where ansae occur. We conclude that, although both structures form, and are dynamically coupled to, the same bar, they are supported by inherently different mechanisms., Comment: 12 pages, 11 figures
Published: 2020

5. Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi

Author: William J. Chaplin, Aldo M. Serenelli, Andrea Miglio, Thierry Morel, J. Ted Mackereth, Fiorenzo Vincenzo, Hans Kjeldsen, Sarbani Basu, Warrick H. Ball, Amalie Stokholm, Kuldeep Verma, Jakob Rørsted Mosumgaard, Victor Silva Aguirre, Anwesh Mazumdar, Pritesh Ranadive, H. M. Antia, Yveline Lebreton, Joel Ong, Thierry Appourchaux, Timothy R. Bedding, Jørgen Christensen-Dalsgaard, Orlagh Creevey, Rafael A. García, Rasmus Handberg, Daniel Huber, Steven D. Kawaler, Mikkel N. Lund, Travis S. Metcalfe, Keivan G. Stassun, Michäel Bazot, Paul G. Beck, Keaton J. Bell, Maria Bergemann, Derek L. Buzasi, Othman Benomar, Diego Bossini, Lisa Bugnet, Tiago L. Campante, Zeynep Çelik Orhan, Enrico Corsaro, Lucía González-Cuesta, Guy R. Davies, Maria Pia Di Mauro, Ricky Egeland, Yvonne P. Elsworth, Patrick Gaulme, Hamed Ghasemi, Zhao Guo, Oliver J. Hall, Amir Hasanzadeh, Saskia Hekker, Rachel Howe, Jon M. Jenkins, Antonio Jiménez, René Kiefer, James S. Kuszlewicz, Thomas Kallinger, David W. Latham, Mia S. Lundkvist, Savita Mathur, Josefina Montalbán, Benoit Mosser, Andres Moya Bedón, Martin Bo Nielsen, Sibel Örtel, Ben M. Rendle, George R. Ricker, Thaíse S. Rodrigues, Ian W. Roxburgh, Hossein Safari, Mathew Schofield, Sara Seager, Barry Smalley, Dennis Stello, Róbert Szabó, Jamie Tayar, Nathalie Themeßl, Alexandra E. L. Thomas, Roland K. Vanderspek, Walter E. van Rossem, Mathieu Vrard, Achim Weiss, Timothy R. White, Joshua N. Winn, Mutlu Yıldız, European Commission, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Generalitat de Catalunya, Chaplin W.J., Serenelli A.M., Miglio A., Morel T., Mackereth J.T., Vincenzo F., Kjeldsen H., Basu S., Ball W.H., Stokholm A., Verma K., Mosumgaard J.R., Silva Aguirre V., Mazumdar A., Ranadive P., Antia H.M., Lebreton Y., Ong J., Appourchaux T., Bedding T.R., Christensen-Dalsgaard J., Creevey O., Garcia R.A., Handberg R., Huber D., Kawaler S.D., Lund M.N., Metcalfe T.S., Stassun K.G., Bazot M., Beck P.G., Bell K.J., Bergemann M., Buzasi D.L., Benomar O., Bossini D., Bugnet L., Campante T.L., Orhan Z.C., Corsaro E., Gonzalez-Cuesta L., Davies G.R., Di Mauro M.P., Egeland R., Elsworth Y.P., Gaulme P., Ghasemi H., Guo Z., Hall O.J., Hasanzadeh A., Hekker S., Howe R., Jenkins J.M., Jimenez A., Kiefer R., Kuszlewicz J.S., Kallinger T., Latham D.W., Lundkvist M.S., Mathur S., Montalban J., Mosser B., Bedon A.M., Nielsen M.B., Ortel S., Rendle B.M., Ricker G.R., Rodrigues T.S., Roxburgh I.W., Safari H., Schofield M., Seager S., Smalley B., Stello D., Szabo R., Tayar J., Themessl N., Thomas A.E.L., Vanderspek R.K., van Rossem W.E., Vrard M., Weiss A., White T.R., Winn J.N., Yildiz M., Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Department of Psychology, St John's University, Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), School of Physics and Astronomy, University of Birmingham [Birmingham], Centre Européen de Recherche et de Formation Avancée en Calcul Scientifique (CERFACS), Danish AsteroSeismology Centre (DASC), Aarhus University [Aarhus], Department of Astronomy, Yale University [New Haven], Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Sydney Institute for Astronomy (SIfA), The University of Sydney, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Research institute of Computer Vision and Robotics [Girona] (VICOROB), Universitat de Girona (UdG), Department of Physics and Astronomy [Aarhus], Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), NASA Ames Research Center (ARC), Centre for Automation and Robotics (CAR), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad Politécnica de Madrid (UPM), Kiepenheuer-Institut für Sonnenphysik (KIS), Stellar Astrophysics Centre [Aarhus] (SAC), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), High Altitude Observatory (HAO), National Center for Atmospheric Research [Boulder] (NCAR), Département des Sciences et Gestion de l'Environnement/Océanologie [Liège], Université de Liège, Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), High Speed Networks Laboratory, Dept. of Telecommunications and Media Informatics, Budapest University of Technology and Economics [Budapest] (BME), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Observatoire de Paris, Université Paris sciences et lettres (PSL), Ege Üniversitesi, CERFACS [Toulouse], Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidad Politécnica de Madrid (UPM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), PSL Research University (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Milky Way, Population, GAIA, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, CHEMICAL-COMPOSITION, Q1, 01 natural sciences, Asteroseismology, 0103 physical sciences, QB460, Satellite galaxy, STELLAR HALOES, Astrophysics::Solar and Stellar Astrophysics, 10. No inequality, education, 010303 astronomy & astrophysics, QB600, QC, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Dwarf galaxy, QB, Physics, [PHYS]Physics [physics], education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ACCRETION HISTORY, Astronomy and Astrophysics, DISC, Astrophysics - Astrophysics of Galaxies, Galaxy, MODEL, Stars, Astrophysics - Solar and Stellar Astrophysics, DARK-MATTER HALOES, ROTATION, Halo, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SOLAR-LIKE OSCILLATIONS, QB799
Abstract: This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). et al., Over the course of its history, the Milky Way has ingested multiple smaller satellite galaxies. Although these accreted stellar populations can be forensically identified as kinematically distinct structures within the Galaxy, it is difficult in general to date precisely the age at which any one merger occurred. Recent results have revealed a population of stars that were accreted via the collision of a dwarf galaxy, called Gaia–Enceladus, leading to substantial pollution of the chemical and dynamical properties of the Milky Way. Here we identify the very bright, naked-eye star ν Indi as an indicator of the age of the early in situ population of the Galaxy. We combine asteroseismic, spectroscopic, astrometric and kinematic observations to show that this metal-poor, alpha-element-rich star was an indigenous member of the halo, and we measure its age to be 11.0±0.7 (stat) ±0.8 (sys) billion years. The star bears hallmarks consistent with having been kinematically heated by the Gaia–Enceladus collision. Its age implies that the earliest the merger could have begun was 11.6 and 13.2 billion years ago, at 68% and 95% confidence, respectively. Computations based on hierarchical cosmological models slightly reduce the above limits., J.M. acknowledge support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, grant agreement number 772293). A.M.S. is partially supported by the Spanish Government (ESP2017-82674-R) and Generalitat de Catalunya (2017-SGR-1131). T.L.C. acknowledges support from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement number 792848 (PULSATION). K.J.B., S.H., J.S.K. and N.T. are supported by the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement number 338251 (StellarAges). E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement number 664931. L.G.-C. acknowledges support from the MINECO FPI-SO doctoral research project SEV-2015-0548-17-2 and predoctoral contract BES-2017-082610. S.M. acknowledges support from the Spanish ministry through the Ramon y Cajal fellowship number RYC-2015-17697. This work was supported by FEDER through COMPETE2020 (POCI-01-0145-FEDER-030389. A.M.B. acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No 749962 (project THOT).
Published: 2020

6. Complex molecular gas kinematics in the inner 5 kpc of 4C12.50 as seen by ALMA

Author: M. Papachristou, Francoise Combes, Kalliopi Dasyra, P. Salomé, C. M. Fotopoulou, National and Kapodistrian University of Athens (NKUA), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, National Observatory of Athens (NOA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Chaire Galaxies et cosmologie, and Collège de France (CdF (institution))
Subjects: Infrared, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Doubly ionized oxygen, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, infrared: galaxies, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Luminous infrared galaxy, ISM: kinematics and dynamics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, line: profiles, Atacama Large Millimeter Array, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Stars, ISM: jets and outflows, Radiation pressure, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: nuclei
Abstract: The nearby system 4C12.50, also known as IRAS 13451+1217 and PKS 1345+12, is a merger of gas-rich galaxies with infrared and radio activity. It has a perturbed interstellar medium (ISM) and a dense configuration of gas and dust around the nucleus. The radio emission at small (∼100 pc) and large (∼100 kpc) scales, as well as the large X-ray cavity in which the system is embedded, are indicative of a jet that could have affected the ISM. We carried out observations of the CO(1−0), (3−2), and (4−3) lines with the Atacama Large Millimeter Array (ALMA) to determine basic properties (i.e., extent, mass, and excitation) of the cold molecular gas in this system, including its already-known wind. The CO emission reveals the presence of gaseous streams related to the merger, which result in a small (∼4 kpc-wide) disk around the western nucleus. The disk reaches a rotational velocity of 200 km s−1, and has a mass of 3.8(±0.4) × 109 M⊙. It is truncated at a gaseous ridge north of the nucleus that is bright in [O III]. Regions with high-velocity CO emission are seen at signal-to-noise ratios of between 3 and 5 along filaments that radially extend from the nucleus to the ridge and that are bright in [O III] and stellar emission. A tentative wind detection is also reported in the nucleus and in the disk. The molecular gas speed could be as high as 2200 km s−1 and the total wind mass could be as high as 1.5(±0.1) × 109 M⊙. Energetically, it is possible that the jet, assisted by the radiation pressure of the active nucleus or the stars, accelerated clouds inside an expanding bubble.
Published: 2019

7. 4MOST Consortium Survey 2: The Milky Way Halo High-Resolution Survey

Author: Christlieb, N., Battistini, C., Bonifacio, P., Caffau, E., Ludwig, H., Asplund, M., Barklem, P., Bergemann, M., Church, R., Feltzing, S., Ford, D., Grebel, E., Hansen, C., Helmi, A., Kordopatis, G., Kovalev, M., Korn, A., Lind, K., Quirrenbach, A., Rybizki, J., Skúladóttir, Á., Starkenburg, E., Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], Department of Physics and Astronomy [Uppsala], Uppsala University, Lund Observatory, Lund University [Lund], Departament Llenguatges i Sistemes Informatics, Universitat Politècnica de Catalunya [Barcelona] (UPC), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, and Astronomy
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
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., Comment: Part of the 4MOST issue of The Messenger, published in preparation of 4MOST Community Workshop, see http://www.eso.org/sci/meetings/2019/4MOST.html
Published: 2019
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8. The Detailed Science Case for the Maunakea Spectroscopic Explorer, 2019 edition

Author: The MSE Science Team, Babusiaux, Carine, Bergemann, Maria, Burgasser, Adam, Ellison, Sara, Haggard, Daryl, Huber, Daniel, Kaplinghat, Manoj, Li, Ting, Marshall, Jennifer, Martell, Sarah, McConnachie, Alan, Percival, Will, Robotham, Aaron, Shen, Yue, Thirupathi, Sivarani, Tran, Kim-Vy, Yeche, Christophe, Yong, David, Adibekyan, Vardan, Aguirre, Victor Silva, Angelou, George, Asplund, Martin, Balogh, Michael, Banerjee, Projjwal, Bannister, Michele, Barría, Daniela, Battaglia, Giuseppina, Bayo, Amelia, Bechtol, Keith, Beck, Paul G., Beers, Timothy C., Bellinger, Earl P., Berg, Trystyn, Bestenlehner, Joachim M., Bilicki, Maciej, Bitsch, Bertram, Bland-Hawthorn, Joss, Bolton, Adam S., Boselli, Alessandro, Bovy, Jo, Bragaglia, Angela, Buzasi, Derek, Caffau, Elisabetta, Cami, Jan, Carleton, Timothy, Casagrande, Luca, Cassisi, Santi, Catelan, Márcio, Chang, Chihway, Cortese, Luca, Damjanov, Ivana, Davies, Luke J. M., de Grijs, Richard, de Rosa, Gisella, Deason, Alis, di Matteo, Paola, Drlica-Wagner, Alex, Erkal, Denis, Escorza, Ana, Ferrarese, Laura, Fleming, Scott W., Font-Ribera, Andreu, Freeman, Ken, Gänsicke, Boris T., Gabdeev, Maksim, Gallagher, Sarah, Gandolfi, Davide, García, Rafael A., Gaulme, Patrick, Geha, Marla, Gennaro, Mario, Gieles, Mark, Gilbert, Karoline, Gordon, Yjan, Goswami, Aruna, Greco, Johnny P., Grillmair, Carl, Guiglion, Guillaume, Hénault-Brunet, Vincent, Hall, Patrick, Handler, Gerald, Hansen, Terese, Hathi, Nimish, Hatzidimitriou, Despina, Haywood, Misha, Santisteban, Juan V. Hernández, Hillenbrand, Lynne, Hopkins, Andrew M., Howlett, Cullan, Hudson, Michael J., Ibata, Rodrigo, Ilić, Dragana, Jablonka, Pascale, Ji, Alexander, Jiang, Linhua, Juneau, Stephanie, Karakas, Amanda, Karinkuzhi, Drisya, Kim, Stacy Y., Kong, Xu, Konstantopoulos, Iraklis, Krogager, Jens-Kristian, Lagos, Claudia, Lallement, Rosine, Laporte, Chervin, Lebreton, Yveline, Lee, Khee-Gan, Lewis, Geraint F., Lianou, Sophia, Liu, Xin, Lodieu, Nicolas, Loveday, Jon, Mészáros, Szabolcs, Makler, Martin, Mao, Yao-Yuan, Marchesini, Danilo, Martin, Nicolas, Mateo, Mario, Melis, Carl, Merle, Thibault, Miglio, Andrea, Mohammad, Faizan Gohar, Molaverdikhani, Karan, Monier, Richard, Morel, Thierry, Mosser, Benoit, Nataf, David, Necib, Lina, Neilson, Hilding R., Newman, Jeffrey A., Nierenberg, A. M., Nord, Brian, Noterdaeme, Pasquier, O'Dea, Chris, Oshagh, Mahmoudreza, Pace, Andrew B., Palanque-Delabrouille, Nathalie, Pandey, Gajendra, Parker, Laura C., Pawlowski, Marcel S., Peter, Annika H. G., Petitjean, Patrick, Petric, Andreea, Placco, Vinicius, Popović, Luka Č., Price-Whelan, Adrian M., Prsa, Andrej, Ravindranath, Swara, Rich, R. Michael, Ruan, John, Rybizki, Jan, Sakari, Charli, Sanderson, Robyn E., Schiavon, Ricardo, Schimd, Carlo, Serenelli, Aldo, Siebert, Arnaud, Siudek, Malgorzata, Smiljanic, Rodolfo, Smith, Daniel, Sobeck, Jennifer, Starkenburg, Else, Stello, Dennis, Szabó, Gyula M., Szabo, Robert, Taylor, Matthew A., Thanjavur, Karun, Thomas, Guillaume, Tollerud, Erik, Toonen, Silvia, Tremblay, Pier-Emmanuel, Tresse, Laurence, Tsantaki, Maria, Valentini, Marica, Van Eck, Sophie, Variu, Andrei, Venn, Kim, Villaver, Eva, Walker, Matthew G., Wang, Yiping, Wang, Yuting, Wilson, Michael J., Wright, Nicolas, Xu, Siyi, Yildiz, Mutlu, Zhang, Huawei, Zwintz, Konstanze, Anguiano, Borja, Bedell, Megan, Chaplin, William, Collet, Remo, Cuillandre, Jean-Charles, Duc, Pierre-Alain, Flagey, Nicolas, Hermes, JJ, Hill, Alexis, Kamath, Devika, Laychak, Mary Beth, Małek, Katarzyna, Marley, Mark, Sheinis, Andy, Simons, Doug, Sousa, Sérgio G., Szeto, Kei, Ting, Yuan-Sen, Vegetti, Simona, Wells, Lisa, Babas, Ferdinand, Bauman, Steve, Bosselli, Alessandro, Côté, Pat, Colless, Matthew, Comparat, Johan, Courtois, Helene, Crampton, David, Croom, Scott, Davies, Luke, Denny, Kelly, Devost, Daniel, Driver, Simon, Fernandez-Lorenzo, Mirian, Guhathakurta, Raja, Han, Zhanwen, Higgs, Clare, Hill, Vanessa, Ho, Kevin, Hopkins, Andrew, Hudson, Mike, Isani, Sidik, Jarvis, Matt, Johnson, Andrew, Jullo, Eric, Kaiser, Nick, Kneib, Jean-Paul, Koda, Jun, Koshy, George, Mignot, Shan, Murowinski, Rick, Newman, Jeff, Nusser, Adi, Pancoast, Anna, Peng, Eric, Peroux, Celine, Pichon, Christophe, Poggianti, Bianca, Richard, Johan, Salmon, Derrick, Seibert, Arnaud, Shastri, Prajval, Smith, Dan, Sutaria, Firoza, Tao, Charling, Taylor, Edwar, Tully, Brent, van Waerbeke, Ludovic, Vermeulen, Tom, Walker, Matthew, Willis, Jon, Willot, Chris, Withington, Kanoa, International Max Planck Research School for Astronomy and Cosmic Physics (University of Heidelberg), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Center for Astrophysics and Space Sciences [La Jolla] (CASS), University of California [San Diego] (UC San Diego), University of California-University of California, Cognition, Langues, Langage, Ergonomie (CLLE-ERSS), École pratique des hautes études (EPHE)-Université Toulouse - Jean Jaurès (UT2J)-Université Bordeaux Montaigne-Centre National de la Recherche Scientifique (CNRS), Technicolor R & I [Cesson Sévigné], Technicolor, University of Edinburgh, University of Texas-Pan American (UTPA), University of Texas-Pan, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Australian National University (ANU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Max-Planck-Institut für Astronomie (MPIA), Lund Observatory, Lund University [Lund], Anglo-Australian Observatory (AAO), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], Department of Physics and Astronomy [London, ON], University of Western Ontario (UWO), National Research Council of Canada (NRC), STScI, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, University of Cambridge [UK] (CAM), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), State Key Laboratory of Fine Chemicals, Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), School of Physics and Astronomy, University of Birmingham [Birmingham], Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Sciences, Philosophie, Histoire (SPHERE UMR 7219), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [UCLA Los Angeles], University of California [Los Angeles] (UCLA), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], High Speed Networks Laboratory, Dept. of Telecommunications and Media Informatics, Budapest University of Technology and Economics [Budapest] (BME), Laboratoire Interdisciplinaire Carnot de Bourgogne (LICB), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, College of Life Sciences, Peking Univertsity, Department of Mathematics [UCLA], Department of Psychology, St John's University, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Herzberg Institute of Astrophysics, Department of electronic engineering, Chang Gung University, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), The Open Group Research Institute (TOGRI), Université Joseph Fourier - Grenoble 1 (UJF), École normale supérieure - Paris (ENS Paris), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), MSE Science Team, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J)-Université Bordeaux Montaigne-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Cambridge], Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Sciences, Philosophie, Histoire (SPHERE (UMR_7219)), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Bourgogne (UB), University of California (UC)-University of California (UC), École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Bordeaux Montaigne (UBM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Universität Heidelberg [Heidelberg] = Heidelberg University, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interdisciplinaire Carnot de Bourgogne (ICB), Peking University [Beijing], Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Universidad Autónoma de Madrid (UAM), École normale supérieure - Paris (ENS-PSL), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Lebreton, Yveline
Subjects: [PHYS]Physics [physics], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, [PHYS] Physics [physics], [SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: (Abridged) The Maunakea Spectroscopic Explorer (MSE) is an end-to-end science platform for the design, execution and scientific exploitation of spectroscopic surveys. It will unveil the composition and dynamics of the faint Universe and impact nearly every field of astrophysics across all spatial scales, from individual stars to the largest scale structures in the Universe. Major pillars in the science program for MSE include (i) the ultimate Gaia follow-up facility for understanding the chemistry and dynamics of the distant Milky Way, including the outer disk and faint stellar halo at high spectral resolution (ii) galaxy formation and evolution at cosmic noon, via the type of revolutionary surveys that have occurred in the nearby Universe, but now conducted at the peak of the star formation history of the Universe (iii) derivation of the mass of the neutrino and insights into inflationary physics through a cosmological redshift survey that probes a large volume of the Universe with a high galaxy density. MSE is positioned to become a critical hub in the emerging international network of front-line astronomical facilities, with scientific capabilities that naturally complement and extend the scientific power of Gaia, the Large Synoptic Survey Telescope, the Square Kilometer Array, Euclid, WFIRST, the 30m telescopes and many more., 9 chapters, 301 pages, 100 figures. This version of the DSC is a comprehensive update of the original version, released in 2016, which can be downloaded at arXiv:1606.00043. A detailed summary of the design of MSE is available in the MSE Book 2018, available at arXiv:1810.08695
Published: 2019

9. Planck ’s dusty GEMS

Author: Canameras, R., Yang, C., Nesvadba, N. P. H., Beelen, A., Kneissl, R., Koenig, S., Le Floc’h, E., Limousin, M., Malhotra, S., Omont, A., Scott, D., Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Guangzhou Marine Geological Survey, Ministry of Land and Resources (MLR), Cavendish Laboratory, University of Cambridge [UK] (CAM), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], submillimeter: galaxies, galaxies: high-redshift, galaxies: star formation, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, galaxies: ISM, ISM: molecules
Abstract: 19 pages, 10 figures, 4 tables, accepted for publication in A&A; International audience; We present ALMA, NOEMA, and IRAM-30 m/EMIR observations of the high-density tracer molecules HCN, HCO + , and HNC in three of the brightest lensed dusty star-forming galaxies at z ≃ 3–3.5, part of the Planck ’s Dusty Gravitationally Enhanced subMillimetre Sources (GEMS), with the aim of probing the gas reservoirs closely associated with their exceptional levels of star formation. We obtained robust detections of ten emission lines between J up = 4 and 6, as well as several additional upper flux limits. In PLCK_G244.8+54.9, the brightest source at z = 3.0, the HNC(5–4) line emission at 0.1″ resolution, together with other spatially-integrated line profiles, suggests comparable distributions of dense and more diffuse gas reservoirs, at least over the most strongly magnified regions. This rules out any major effect from differential lensing. This line is blended with CN(4–3) and in this source, we measure a HNC(5–4)/CN(4–3) flux ratio of 1.76 ±0. 86. Dense-gas line profiles generally match those of mid- J CO lines, except in PLCK_G145.2+50.8, which also has dense-gas line fluxes that are relatively lower, perhaps due to fewer dense cores and more segregated dense and diffuse gas phases in this source. The HCO + /HCN ≳ 1 and HNC/HCN ∼ 1 line ratios in our sample are similar to those of nearby ultraluminous infrared galaxies (ULIRGs) and consistent with photon-dominated regions without any indication of important mechanical heating or active galactic nuclei feedback. We characterize the dense-gas excitation in PLCK_G244.8+54.9 using radiative transfer models assuming pure collisional excitation and find that mid- J HCN, HCO + , and HNC lines arise from a high-density phase with an H 2 density of n ∼ 10 5 –10 6 cm −3 , although important degeneracies hinder a determination of the exact conditions. The three GEMS are consistent with extrapolations of dense-gas star-formation laws derived in the nearby Universe, adding further evidence that the extreme star-formation rates observed in the most active galaxies at z ∼ 3 are a consequence of their important dense-gas contents. The dense-gas-mass fractions traced by HCN/[CI] and HCO + /[CI] line ratios are elevated, but not exceptional as compared to other lensed dusty star-forming galaxies at z > 2, and they fall near the upper envelope of local ULIRGs. Despite the higher overall gas fractions and local gas-mass surface densities observed at high redshift, the dense-gas budget of rapidly star-forming galaxies seems to have evolved little between z ∼ 3 and z ∼ 0. Our results favor constant dense-gas depletion times in these populations, which is in agreement with theoretical models of star formation.
Published: 2018

10. A new algorithm for optimizing the wavelength coverage for spectroscopic studies: Spectral Wavelength Optimization Code (swoc)

Author: G. Ruchti, Karin Lind, Camilla Juul Hansen, R. S. de Jong, Andreas Koch, Andreas Korn, Elisabetta Caffau, Luca Sbordone, Olivier Schnurr, Sofia Feltzing, Lund Observatory, Lund University [Lund], Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Space Physics [Uppsala], Uppsala University, and European Organization for Nuclear Research (CERN)
Subjects: [PHYS]Physics [physics], Physics, Mode (statistics), FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Set (abstract data type), Wavelength, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, 0103 physical sciences, Code (cryptography), Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Spectrograph, Algorithm, ComputingMilieux_MISCELLANEOUS, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The past decade and a half has seen the design and execution of several ground-based spectroscopic surveys, both Galactic and Extra-galactic. Additionally, new surveys are being designed that extend the boundaries of current surveys. In this context, many important considerations must be done when designing a spectrograph for the future. Among these is the determination of the optimum wavelength coverage. In this work, we present a new code for determining the wavelength ranges that provide the optimal amount of information to achieve the required science goals for a given survey. In its first mode, it utilizes a user-defined list of spectral features to compute a figure-of-merit for different spectral configurations. The second mode utilizes a set of flux-calibrated spectra, determining the spectral regions that show the largest differences among the spectra. Our algorithm is easily adaptable for any set of science requirements and any spectrograph design. We apply the algorithm to several examples, including 4MOST, showing the method yields important design constraints to the wavelength regions., Comment: 27 pages, 4 figures, accepted to MNRAS
Published: 2016

11. The Gaia -ESO Survey: Properties of newly discovered Li-rich giants

Author: C. Régulo, Giovanni Carraro, Luca Sbordone, Amelia Bayo, Rafael A. García, E. Franciosini, Thierry Morel, X. Fu, Arnas Drazdauskas, Thomas Bensby, Alejandra Recio-Blanco, Laura Magrini, B. Mosser, Angela Bragaglia, Savita Mathur, Simone Zaggia, L. Prisinzano, L. Morbidelli, R. de Assis Peralta, Lorenzo Monaco, A. C. Lanzafame, Antonio Frasca, Sofia Randich, M. T. Costado, Paula Jofre, V. Adibekyan, P. de Laverny, Karin Lind, Andreas J. Korn, Rodolfo Smiljanic, Grazina Tautvaisiene, L. Pasquini, Elena Pancino, Thomas Masseron, Marica Valentini, S. G. Sousa, Saskia Hekker, Antonella Vallenari, Josefina Montalbán, Gerard Gilmore, D. Feuillet, Carmela Lardo, Sofia Feltzing, Sarah L. Martell, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Matériaux divisés, interfaces, réactivité, électrochimie (MADIREL), Aix Marseille Université (AMU)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Space Science Institute [Boulder] (SSI), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), School of Physics and Astronomy, University of Birmingham [Birmingham], Dipartimento di Scienze e Tecnologie Aerospaziali - Politecnico, Politecnico di Milano [Milan] (POLIMI), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astronomico di Padova (OAPD), Department of Astronomy and Space Physics [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Smiljanic R., Franciosini E., Bragaglia A., Tautvaisiene G., Fu X., Pancino E., Adibekyan V., Sousa S.G., Randich S., Montalban J., Pasquini L., Magrini L., Drazdauskas A., Garcia R.A., Mathur S., Mosser B., Regulo C., De Assis Peralta R., Hekker S., Feuillet D., Valentini M., Morel T., Martell S., Gilmore G., Feltzing S., Vallenari A., Bensby T., Korn A.J., Lanzafame A.C., Recio-Blanco A., Bayo A., Carraro G., Costado M.T., Frasca A., Jofre P., Lardo C., De Laverny P., Lind K., Masseron T., Monaco L., Morbidelli L., Prisinzano L., Sbordone L., Zaggia S., ITA, USA, GBR, FRA, DEU, ESP, AUS, BEL, CHL, DNK, LTU, POL, PRT, SWE, CHE, Universidade do Porto = University of Porto, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Gilmore, Gerard [0000-0003-4632-0213], Apollo - University of Cambridge Repository, Osservatorio Astronomico di Bologna (OABO), Universidade do Porto [Porto], Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional de Colombia, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Fisica Nucleare [Milano] (INFN), and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: barium stars, k-giant, Astrophysics, Stars: late-type, GALACTIC BULGE, mass-loss, 7. Clean energy, 01 natural sciences, LITHIUM ENRICHMENT, Bulge, Planet, Asymptotic giant branch, EVOLVED STARS, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, K-GIANT, [PHYS]Physics [physics], open clusters, red giants, LATE-TYPE STARS, Evolution [Stars], Red-giant branch, evolved stars, Stars: evolution, Astrophysics - Solar and Stellar Astrophysics, late-type [Stars], chemical-composition, Astrophysics::Earth and Planetary Astrophysics, Stars: abundance, stars: abundances, late-type stars, FOS: Physical sciences, Abundances [Stars], Astrophysics::Cosmology and Extragalactic Astrophysics, galactic bulge, CHEMICAL-COMPOSITION, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Infrared excess, 010308 nuclear & particles physics, Astronomy and Astrophysics, MASS-LOSS, BARIUM STARS, Accretion (astrophysics), lithium enrichment, RED GIANTS, Stars, Stars: abundances, Space and Planetary Science, 13. Climate action, OPEN CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Open cluster
Abstract: Aims. We report 20 new lithium-rich giants discovered within the Gaia-ESO Survey, including the first Li-rich giant with an evolutionary stage confirmed by CoRoT (Convection, Rotation and planetary Transits) data. We present a detailed overview of the properties of these 20 stars., Methods. Atmospheric parameters and abundances were derived in model atmosphere analyses using medium-resolution GIRAFFE or high-resolution UVES (Ultraviolet and Visual Echelle Spectrograph) spectra. These results are part of the fifth internal data release of the Gaia-ESO Survey. The Li abundances were corrected for non-local thermodynamical equilibrium effects. Other stellar properties were investigated for additional peculiarities (the core of strong lines for signs of magnetic activity, infrared magnitudes, rotational velocities, chemical abundances, and Galactic velocities). We used Gaia DR2 parallaxes to estimate distances and luminosities., Results. The giants have A(Li) > 2.2 dex. The majority of them (14 of 20 stars) are in the CoRoT fields. Four giants are located in the field of three open clusters, but are not members. Two giants were observed in fields towards the Galactic bulge, but likely lie in the inner disc. One of the bulge field giants is super Li-rich with A(Li) = 4.0 dex., Conclusions. We identified one giant with infrared excess at 22 mu m. Two other giants, with large v sin i, might be Li-rich because of planet engulfment. Another giant is found to be barium enhanced and thus could have accreted material from a former asymptotic giant branch companion. Otherwise, in addition to the Li enrichment, the evolutionary stages are the only other connection between these new Li-rich giants. The CoRoT data confirm that one Li-rich giant is at the core-He burning stage. The other giants are concentrated in close proximity to the red giant branch luminosity bump, the core-He burning stages, or the early-asymptotic giant branch. This is very clear from the Gaia-based luminosities of the Li-rich giants. This is also seen when the CoRoT Li-rich giants are compared to a larger sample of 2252 giants observed in the CoRoT fields by the Gaia-ESO Survey, which are distributed throughout the red giant branch in the T-eff-log g diagram. These observations show that the evolutionary stage is a major factor for the Li enrichment in giants. Other processes, such as planet accretion, contribute at a smaller scale.
Published: 2018

12. Low-frequency radio absorption in Cassiopeia A

Author: M. Arias, J. Vink, F. de Gasperin, P. Salas, J. B. R. Oonk, R. J. van Weeren, A. S. van Amesfoort, J. Anderson, R. Beck, M. E. Bell, M. J. Bentum, P. Best, R. Blaauw, F. Breitling, J. W. Broderick, W. N. Brouw, M. Brüggen, H. R. Butcher, B. Ciardi, E. de Geus, A. Deller, P. C. G. van Dijk, S. Duscha, J. Eislöffel, M. A. Garrett, J. M. Grießmeier, A. W. Gunst, M. P. van Haarlem, G. Heald, J. Hessels, J. Hörandel, H. A. Holties, A. J. van der Horst, M. Iacobelli, E. Juette, A. Krankowski, J. van Leeuwen, G. Mann, D. McKay-Bukowski, J. P. McKean, H. Mulder, A. Nelles, E. Orru, H. Paas, M. Pandey-Pommier, V. N. Pandey, R. Pekal, R. Pizzo, A. G. Polatidis, W. Reich, H. J. A. Röttgering, H. Rothkaehl, D. J. Schwarz, O. Smirnov, M. Soida, M. Steinmetz, M. Tagger, S. Thoudam, M. C. Toribio, C. Vocks, M. H. D. van der Wiel, R. A. M. J. Wijers, O. Wucknitz, P. Zarka, P. Zucca, API (FNWI), High Energy Astrophys. & Astropart. Phys (API, FNWI), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), LOFAR, Astronomy, Astronomical Institute Anton Pannekoek, University of Amsterdam, SRON Netherlands Institute for Space Research (SRON), Leiden Observatory, Netherlands Institute for Radio Astronomy (ASTRON), GeoForschungsZentrum (GFZ), Max-Planck-Institut für Astronomie (MPIA), University of Technology Sydney, 15 Broadway, Ultimo, NSW 2007, Australia, University of Edinburgh, Leibniz-Institut für Astrophysik Potsdam (IAP), University of Hamburg, Gojenbergsweg 112, 21029, Hamburg, Germany, Mount Stromlo Observatory, Australian National University, Max-Planck-Institut für Astrophysik (MPA), Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Thüringer Landessternwarte, Tautenburg Observatory, JBCA School of Physics and Astronomy, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), CSIRO Astronomy and Space Science, Department of Astrophysics, Radboud University Nijmegen, PO Box 9010, 6500 GL, Nijmegen, The Netherlands, George Washington University, Astronomisches Institut der Ruhr-Universitat Bochum, Universitaetsstrasse 150, 44780, Bochum, Germany, University of Warmia and Mazury [Olsztyn], Department of Physics and Technology, University of Tromso, Tromso, Norway, Department of Physics and Astronomy, University of Missouri, Center for Information Technology, University of Groningen (CIT), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Poznan University of Technology, Space Research Center, Polish Academy of Sciences (Torun), Universität Bielefeld = Bielefeld University, Department of Physics and Electronics, Rhodes University, Astronomical Observatory, Jagiellonian University, Department of Physics and Electrical Engineering, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Electromagnetics, Center for Wireless Technology Eindhoven, EM for Radio Science Lab, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Centre National de la Recherche Scientifique ( CNRS ) -Université d'Orléans ( UO ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS Lyon ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: TI-44, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astronomy, radio continuum: general, Astrophysics, 7. Clean energy, 01 natural sciences, supernova remnants / radiation mechanisms: general / radio continuum, Astrophysics::Solar and Stellar Astrophysics, individual, Ejecta, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, SUPERNOVA REMNANT CASSIOPEIA, general [radiation mechanisms], ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, ABSOLUTE SPECTRUM, supernova remnants [ISM], Radius, Supernova, EJECTA, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, general [radio continuum], Astrophysics - High Energy Astrophysical Phenomena, Cas A / ISM, individual: Cas A [supernovae], supernovae, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, radiation mechanisms: general, LARGE ARRAY, Astrophysics::Cosmology and Extragalactic Astrophysics, Low frequency, Astronomy & Astrophysics, ACCELERATION, Radio spectrum, VDP::Matematikk og Naturvitenskap: 400::Fysikk: 430::Astrofysikk, astronomi: 438, 0103 physical sciences, 3-DIMENSIONAL STRUCTURE, Astrophysics::Galaxy Astrophysics, EXPLOSION, 010308 nuclear & particles physics, Astronomy and Astrophysics, LOFAR, Cassiopeia A, VDP::Mathematics and natural science: 400::Physics: 430::Astrophysics, astronomy: 438, supernovae: individual: Cas A, 13. Climate action, Space and Planetary Science, general, EMISSION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CAS-A
Abstract: Cassiopeia A is one of the best-studied supernova remnants. Its shocked ejecta emits brightly in radio and X-rays. Its unshocked ejecta can be studied through infrared emission, the radio-active decay of $^{44}$Ti, and low frequency free-free absorption due to cold gas internal to the shell. Free-free absorption is affected by the mass, geometry, temperature, and ionisation conditions in the absorbing gas. Observations at the lowest radio frequencies constrain a combination of these properties. We use LOFAR LBA observations at 30-77 MHz and L-band VLA observations to compare $u-v$-matched images with a common resolution of 17". We simultaneously fit, per pixel, for the emission measure and the ratio of the emission from the unabsorbed front of the shell versus the absorbed back of the shell. We explore the effects that low temperatures and a high degree of clumping can have on the derived physical properties, such as mass and density. We also compile published radio flux measurements, fit for the absorption processes that occur in the radio band, and consider how they affect the secular decline of the source. We find a mass in the unshocked ejecta of $M = 2.95 \pm {0.48} \,M_{\odot}$ for an assumed gas temperature of $T=100$ K. This estimate is reduced for colder gas temperatures and if the ejecta are clumped. We measure the reverse shock to have a radius of $114$" $\pm $6". We also find that a decrease in the amount of mass in the unshocked ejecta (as more and more material meets the reverse shock and heats up) cannot account for the observed low frequency behaviour of the secular decline rate. To reconcile our low frequency absorption measurements with models that predict little mass in the unshocked ejecta we need the ejecta to be very clumped, or the temperature in the cold gas to be low ($\sim10$ K). Both conditions can jointly contribute to the high absorption., Accepted for publication in A&A v2: including the DOI, language edits
Published: 2018

13. Accurate effective temperatures of the metal-poor benchmark stars HD 140283, HD 122563, and HD 103095 from CHARA interferometry

Author: Gail Schaefer, Andrea Chiavassa, Denis Mourard, Luca Casagrande, Karin Lind, O. L. Creevey, Thomas Nordlander, Martin Asplund, Gerry Gilmore, I. Karovicova, Daniel Huber, Paula Jofre, Timothy R. White, Ulrike Heiter, Michael J. Ireland, Markus Wittkowski, F. Thévenin, Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Uppsala], Uppsala University, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Research School of Astronomy and Astrophysics [Canberra] (RSAA), Australian National University (ANU), Sydney Institute for Astronomy (SIfA), The University of Sydney, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Georgia State University, University System of Georgia (USG), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), European Southern Observatory (ESO), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Gilmore, Gerard [0000-0003-4632-0213], and Apollo - University of Cambridge Repository
Subjects: individual: HD140283 [stars], stars: individual: HD140283, FOS: Physical sciences, individual: HD122563 [stars], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Set (abstract data type), surveys, HIPPARCOS, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, stars: individual: HD122563, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Chara, Physics, biology, 010308 nuclear & particles physics, Astronomy and Astrophysics, biology.organism_classification, interferometric [techniques], 3. Good health, Stars, Interferometry, STELLAR, Astrophysics - Solar and Stellar Astrophysics, techniques: interferometric, 13. Climate action, Space and Planetary Science, stars: individual: HD103095, standards, Benchmark (computing), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], individual: HD103095 [stars], SYSTEM
Abstract: Large stellar surveys of the Milky Way require validation with reference to a set of "benchmark" stars whose fundamental properties are well-determined. For metal-poor benchmark stars, disagreement between spectroscopic and interferometric effective temperatures has called the reliability of the temperature scale into question. We present new interferometric measurements of three metal-poor benchmark stars, HD 140283, HD 122563, and HD 103095, from which we determine their effective temperatures. The angular sizes of all the stars were determined from observations with the PAVO beam combiner at visible wavelengths at the CHARA array, with additional observations of HD 103095 made with the VEGA instrument, also at the CHARA array. Together with photometrically derived bolometric fluxes, the angular diameters give a direct measurement of the effective temperature. For HD 140283 we find {\theta}_LD = 0.324+/-0.005 mas, Teff = 5787+/-48 K; for HD 122563, {\theta}_LD = 0.926+/-0.011 mas, Teff = 4636+/-37 K; and for HD 103095 {\theta}_LD = 0.595+/-0.007 mas, Teff = 5140+/-49 K. Our temperatures for HD 140283 and HD 103095 are hotter than the previous interferometric measurements by 253 K and 322 K, respectively. We find good agreement between our temperatures and recent spectroscopic and photometric estimates. We conclude some previous interferometric measurements have been affected by systematic uncertainties larger than their quoted errors., Comment: 5 pages, 2 figures
Published: 2018

14. The Gaia-ESO Survey: Lithium enrichment histories of the Galactic thick and thin disc

Author: Giovanni Carraro, Paolo Donati, Gražina Tautvaišienė, Carmela Lardo, Sarah L. Martell, L. Morbidelli, Donatella Romano, X. Fu, Carlos Abia, Ettore Flaccomio, Laura Magrini, Y. Chorniy, Angela Bragaglia, S. G. Sousa, Rodolfo Smiljanic, Emilio J. Alfaro, Georges Kordopatis, Andreas J. Korn, E. Delgado Mena, Arnas Drazdauskas, Paula Jofre, Luca Sbordone, Alessandro Bressan, Sofia Randich, Lorenzo Monaco, Amelia Bayo, Karin Lind, B. Tang, A. C. Lanzafame, Antonio Frasca, Francesco Damiani, Simone Zaggia, Elena Pancino, Thomas Bensby, Alessio Mucciarelli, European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, European Science Foundation, Ministerio de Economía y Competitividad (España), European Commission, Fundação para a Ciência e a Tecnologia (Portugal), Ministry of Science and Higher Education (Poland), Fu, X., Romano, D., Bragaglia, A., Mucciarelli, A., Lind, K., Delgado Mena, E., Sousa, S.G., Randich, S., Bressan, A., Sbordone, L., Martell, S., Korn, A.J., Abia, C., Smiljanic, R., Jofré, P., Pancino, E., Tautvaišiene, G., Tang, B., Magrini, L., Lanzafame, A.C., Carraro, G., Bensby, T., Damiani, F., Alfaro, E.J., Flaccomio, E., Morbidelli, L., Zaggia, S., Lardo, C., Monaco, L., Frasca, A., Donati, P., Drazdauskas, A., Chorniy, Y., Bayo, A., Kordopatis, G., School of Earth and Space Sciences, Peking University [Beijing], INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Padova (OAPD), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Astronomy and Space Physics [Uppsala], Uppsala University, Dpto. Fisica Teorica y del Cosmos, Universidad de Granada (UGR), INAF - Osservatorio Astrofisico di Catania (OACT), University of Turin, Ecole Polytechnique Fédérale de Lausanne (EPFL), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Galaxy: abundances, Galaxy: disk, Stars: abundances, Astronomy and Astrophysics, Space and Planetary Science, Stars: abundance, Metallicity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Astronomi, astrofysik och kosmologi, Big Bang nucleosynthesis, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, abundances [Galaxy], Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Galaxy: abundance, [SDU]Sciences of the Universe [physics], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), abundances [Stars], Astrophysics::Earth and Planetary Astrophysics, Formation and evolution of the Solar System, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], disk [Galaxy], Main sequence
Abstract: Lithium abundance in most of the warm metal-poor main sequence stars shows a constarnt plateau (A(Li) ~ 2.2 dex) and then the upper envelope of the lithium vs. metallicity distribution increases as we approach solar metallicity. Meteorites, which carry information about the chemical composition of the interstellar medium (ISM) at the solar system formation time, show a lithium abundance A(Li) ~ 3.26 dex. This pattern reflects the Li enrichment history of the ISM during the Galaxy lifetime. After the initial Li production in big bang nucleosynthesis, the sources of the enrichment include asymptotic giant branch (AGB) stars, low-mass red giants, novae, type II supernovae, and Galactic cosmic rays. The total amount of enriched Li is sensitive to the relative contribution of these sources. Thus different Li enrichment histories are expected in the Galactic thick and thin disc. We investigate the main sequence stars observed with UVES in Gaia-ESO Survey iDR4 catalogue and find a Li-anticorrelation independent of [Fe/H], T, and log(g). Since in stellar evolution different α enhancements at the same metallicity do not lead to a measurable Li abundance change, the anticorrelation indicates that more Li is produced during the Galactic thin disc phase than during the Galactic thick disc phase. We also find a correlation between the abundance of Li and s-process elements Ba and Y, and they both decrease above the solar metallicity, which can be explained in the framework of the adopted Galactic chemical evolution models.© ESO 2018., This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188. B-3002 and 193. B-0936. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. Data used her were obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell' Istruzione, dell' Universita' e della Ricerca (MIUR) in the form of the grant >Premiale VLT 2012>. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. This research has made use of the TOPCAT catalogue handling and plotting tool (Taylor 2005, 2017); of the Simbad database and the VizieR catalogue access tool, CDS, Strasbourg, France (Ochsenbein et al. 2000); and of NASA's Astrophysics Data System. X. F acknowledges helpful discussions with Nikos Prantzos and Paolo Molaro, and thanks Zhiyu Zhang for the help on MCMC calculations. E. D. M. and S. G. S. acknowledge the support from Fundacao para a Ciencia e a Tecnologia (FCT) through national funds and from FEDER through COMPETE2020 by the following grants: UID/FIS/04434/2013 & POCI-01-0145-FEDER-007672, PTDC/FIS-AST/1526/2014 & POCI-01-0145-FEDER-016886, and PTDC/FIS-AST/7073/2014 & POCI-01-0145-FEDER-016880. E. D. M. and S. G. S. also acknowledge the support from FCT through Investigador FCT contracts IF/00849/2015/CP1273/CT003 and IF/00028/2014/CP1215/CT0002. C. A. acknowledges to the Spanish grant AYA2015-63588-P within the European Founds for Regional Development (FEDER). A. K. and T. B. acknowledge the project grant >The New Milky Way> from the Knut and Alice Wallenberg Foundation. R. S. acknowledges support from the Polish Ministry of Science and Higher Education.
Published: 2018

15. A catalog of polychromatic bulge-disk decompositions of ~ 17.600 galaxies in CANDELS

Author: Paola Dimauro, D. Tuccillo, David C. Koo, B. Häußler, Mariangela Bernardi, A. Cattaneo, Dale D. Kocevski, Helena Domínguez-Sánchez, Guillermo Barro, Fernando Buitrago, Marc Huertas-Company, Sandra M. Faber, Emanuele Daddi, Fernando Caro, Aldo Rodríguez-Puebla, Mara Salvato, Francesco Shankar, Joel R. Primack, Anton M. Koekemoer, Christoph T. Lee, Simona Mei, Berta Margalef-Bentabol, Pablo G. Pérez-González, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Department of Physics, University of California [Santa Cruz] (UCSC), University of California-University of California, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Max-Planck-Institut für Astrophysik (MPA), École des Mines de Paris, Space Telescope Science Institute (STSci), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Pennsylvania, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Centre de Morphologie Mathématique (CMM), and Mines Paris - PSL (École nationale supérieure des mines de Paris)
Subjects: Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, galaxies: fundamental parameters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, galaxies: bulges, Redshift, Galaxy, Large sample, Space and Planetary Science, Bulge, galaxies: high-redshift, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Surface brightness, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Understanding how bulges grow in galaxies is critical step towards unveiling the link between galaxy morphology and star-formation. To do so, it is necessary to decompose large sample of galaxies at different epochs into their main components (bulges and disks). This is particularly challenging, especially at high redshifts, where galaxies are poorly resolved. This work presents a catalog of bulge-disk decompositions of the surface brightness profiles of ~17.600 H-band selected galaxies in the CANDELS fields (F160W, Comment: 18 pages, 18 figures, 3 table, submitted to MNRAS after the first referee's report
Published: 2018
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16. Radial migration in a stellar galactic disc with thick components

Author: P. Di Matteo, A. Halle, Misha Haywood, Francoise Combes, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Chaire Galaxies et cosmologie, and Collège de France (CdF (institution))
Subjects: Angular momentum, Bar (music), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Gravitational potential, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, [PHYS]Physics [physics], Physics, Spiral galaxy, 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, Amplitude, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: stellar content, galaxies: structure, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We study how migration affects stars of a galaxy with a thin stellar disc and thicker stellar components. The simulated galaxy has a strong bar and lasting spiral arms. We find that the amplitude of the churning (change in angular momentum) is similar for thin and thick components, and of limited amplitude, and that stars of all components can be trapped at the corotation of the bar. At the exception of those stars trapped at the corotation, we find that stars that are far from their initial guiding radius are more likely so due to blurring rather than churning effects. We compare the simulation to orbits integration with a fixed gravitational potential rotating at a constant speed. In the latter case, stars trapped at corotation are churned periodically outside and inside the corotation radius, with a zero net average. However, as the bar speed of the simulated galaxy decreases and its corotation radius increases, stars trapped at corotation for several Gyrs can be churned outwards on average. We study the location of extreme migrators (stars experimenting the largest churning) and find that extreme migrators come from regions on the leading side of the effective potential local maxima., Comment: Accepted for publication in Astronomy and Astrophysics (acceptance date: 06/03/18),15 pages, 22 figures
Published: 2018
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17. Ionised gas structure of 100 kpc in an over-dense region of the galaxy group COSMOS-Gr30 at z ~ 0.7

Author: David Carton, Leindert Boogaard, Marcella Carollo, Sebastiano Cantalupo, Genevieve Soucail, Stephen Hamer, Peter M. Weilbacher, Thierry Contini, Léo Michel-Dansac, Hayley Finley, R. A. Marino, Johan Richard, Davor Krajnović, Roland Bacon, Benoît Epinat, Adrien Guérou, Wolfram Kollatschny, Jarle Brinchmann, Lutz Wisotzki, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Leiden Observatory [Leiden], Universiteit Leiden, Institut de recherche en astrophysique et planétologie (IRAP), European Southern Observatory (ESO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Computer Science [ETH Zürich] (D-INFK), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut für Astrophysik [Göttingen], Georg-August-University = Georg-August-Universität Göttingen, Leibniz-Institut für Astrophysik Potsdam (AIP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden [Leiden], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Georg-August-University [Göttingen], Epinat, B, Contini, T, Finley, H, Boogaard, L, Guerou, A, Brinchmann, J, Carton, D, Michel-Dansac, L, Bacon, R, Cantalupo, S, Carollo, M, Hamer, S, Kollatschny, W, Krajnovic, D, Marino, R, Richard, J, Soucail, G, Weilbacher, P, and Wisotzki, L
Subjects: Active galactic nucleus, Absorption spectroscopy, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Galaxies: kinematics and dynamic, galaxies: groups: general, galaxies: high-redshift, Ionization, Galaxy group, 0103 physical sciences, Tidal force, galaxies: interactions, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Line (formation), Physics, evolution, intergalactic medium, galaxies: high-redshift [galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Galaxies: interaction, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: evolution
Abstract: We report the discovery of a 10^4 kpc^2 gaseous structure detected in [OII] in an over-dense region of the COSMOS-Gr30 galaxy group at z~0.725 thanks to deep MUSE Guaranteed Time Observations. We estimate the total amount of diffuse ionised gas to be of the order of (~5+-3)x10^10 Msun and explore its physical properties to understand its origin and the source(s) of the ionisation. The MUSE data allow the identification of a dozen of group members embedded in this structure from emission and absorption lines. We extracted spectra from small apertures defined for both the diffuse ionised gas and the galaxies. We investigated the kinematics and ionisation properties of the various galaxies and extended gas regions thanks to line diagnostics (R23, O32 and [OIII]/H\beta) available within the MUSE wavelength range. We compared these diagnostics to photo-ionisation models and shock models. The structure is divided in two kinematically distinct sub-structures. The most extended sub-structure of ionised gas is likely rotating around a massive galaxy and displays filamentary patterns linking some galaxies. The second sub-structure links another massive galaxy hosting an Active Galactic Nucleus to a low mass galaxy but also extends orthogonally to the AGN host disk over ~35 kpc. This extent is likely ionised by the AGN itself. The location of small diffuse regions in the R23 vs. O32 diagram is compatible with photo-ionisation. However, the location of three of these regions in this diagram (low O32, high R23) can also be explained by shocks, which is supported by their large velocity dispersions. One edge-on galaxy shares the same properties and may be a source of shocks. Whatever the hypothesis, the extended gas seems to be non primordial. We favour a scenario where the gas has been extracted from galaxies by tidal forces and AGN triggered by interactions between at least the two sub-structures., Comment: 21 pages, 12 figures, 3 tables, accepted for publication in A&A (27 October 2017)
Published: 2018

18. The Gaia-ESO Survey: Churning through the Milky Way

Author: Carmela Lardo, Sofia Feltzing, Vanessa Hill, Laura Magrini, Amelia Bayo, Gerard Gilmore, P. de Laverny, S. Mikolaitis, Paula Jofre, A. Hourihane, E. Franciosini, Michael R. Hayden, Alejandra Recio-Blanco, Elena Pancino, Georges Kordopatis, Thomas Bensby, E. Stonkute, G. G. Sacco, Sofia Randich, Karin Lind, Angela Bragaglia, M. T. Costado, L. Morbidelli, Maria Bergemann, Sergey E. Koposov, A. C. Lanzafame, Jack Lewis, Guillaume Guiglion, Tomaž Zwitter, Andrew R. Casey, Lorenzo Monaco, C. C. Worley, Agence Nationale de la Recherche (France), Knut and Alice Wallenberg Foundation, European Southern Observatory, Science and Technology Facilities Council (UK), European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, Ministero dell'Istruzione, dell'Università e della Ricerca, European Science Foundation, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astrofisico di Catania (OACT), Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), University of Ljubljana, Hayden M.R., Recio-Blanco A., De Laverny P., Mikolaitis S., Guiglion G., Hill V., Gilmore G., Randich S., Bayo A., Bensby T., Bergemann M., Bragaglia A., Casey A., Costado M., Feltzing S., Franciosini E., Hourihane A., Jofre P., Koposov S., Kordopatis G., Lanzafame A., Lardo C., Lewis J., Lind K., Magrini L., Monaco L., Morbidelli L., Pancino E., Sacco G., Stonkute E., Worley C.C., Zwitter T., Gilmore, Gerard [0000-0003-4632-0213], Worley, Clare [0000-0001-9310-2898], and Apollo - University of Cambridge Repository
Subjects: astro-ph.GA, Metallicity, Milky Way, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy: disk, Astronomi, astrofysik och kosmologi, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astrophysics and Cosmology, stellar content [Galaxy], Galaxy: structure, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Orbital elements, Physics, Galaxy: stellar content, 010308 nuclear & particles physics, Velocity dispersion, Astronomy and Astrophysics, kinematics and dynamics [Galaxy], Astrophysics - Astrophysics of Galaxies, Galaxy, Galaxy: kinematics and dynamics, Space and Planetary Science, Radial velocity, Stars, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), Galaxy: kinematics and dynamic, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], disk [Galaxy], structure [Galaxy]
Abstract: Context. There have been conflicting results with respect to the extent that radial migration has played in the evolution of the Galaxy. Additionally, observations of the solar neighborhood have shown evidence of a merger in the past history of the Milky Way that drives enhanced radial migration. Aims. We attempt to determine the relative fraction of stars that have undergone significant radial migration by studying the orbital properties of metal-rich ([Fe/H] > 0.1) stars within 2 kpc of the Sun. We also aim to investigate the kinematic properties, such as velocity dispersion and orbital parameters, of stellar populations near the Sun as a function of [Mg/Fe] and [Fe/H], which could show evidence of a major merger in the past history of the Milky Way. Methods. We used a sample of more than 3000 stars selected from the fourth internal data release of the Gaia-ESO Survey. We used the stellar parameters from the Gaia-ESO Survey along with proper motions from PPMXL to determine distances, kinematics, and orbital properties for these stars to analyze the chemodynamic properties of stellar populations near the Sun. Results. Analyzing the kinematics of the most metal-rich stars ([Fe/H] > 0.1), we find that more than half have small eccentricities (e< 0.2) or are on nearly circular orbits. Slightly more than 20% of the metal-rich stars have perigalacticons R> 7 kpc. We find that the highest [Mg/Fe], metal-poor populations have lower vertical and radial velocity dispersions compared to lower [Mg/Fe] populations of similar metallicity by ~10 km s. The median eccentricity increases linearly with [Mg/Fe] across all metallicities, while the perigalacticon decreases with increasing [Mg/Fe] for all metallicities. Finally, the most [Mg/Fe]-rich stars are found to have significant asymmetric drift and rotate more than 40 km s slower than stars with lower [Mg/Fe] ratios. Conclusions. While our results cannot constrain how far stars have migrated, we propose that migration processes are likely to have played an important role in the evolution of the Milky Way, with metal-rich stars migrating from the inner disk toward to solar neighborhood and past mergers potentially driving enhanced migration of older stellar populations in the disk.© ESO, 2018., The authors thank Ivan Minchev for a useful discussion and the anonymous referee for useful comments. M.R.H. and A.R.B. received financial support from ANR, reference 14-CE33-0014-01. S.F. and T.B. acknowledge support from the project grant >The New Milky Way> from the Knut and Alice Wallenberg Foundation. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell' Istruzione, dell' Universita' e della Ricerca (MIUR) in the form of the grant >Premiale VLT 2012>. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and NASA's Astrophysics Data System.
Published: 2018

19. Mapping diffuse interstellar bands in the local ISM on small scales via MUSE 3D spectroscopy

Author: Peter M. Weilbacher, Stefan Dreizler, Philipp Richter, Tim-Oliver Husser, Martin Wendt, Ana Monreal-Ibero, Lutz Wisotzki, Sebastian Kamann, Jarle Brinchmann, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut für Astrophysik [Göttingen], Georg-August-University [Göttingen], Astrophysikalisches Institut Potsdam (AIP), and Leibniz-Institut für Astrophysik Potsdam (AIP)
Subjects: Physics, Diffuse interstellar band, 010308 nuclear & particles physics, extinction, ISM: structure, Extinction (astronomy), Institut für Physik und Astronomie, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ISM: lines and bands, Space and Planetary Science, techniques: imaging spectroscopy, Globular cluster, 0103 physical sciences, globular clusters: individual: NGC 6397, Astrophysics::Solar and Stellar Astrophysics, dust, Spectroscopy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context. We map the interstellar medium (ISM) including the diffuse interstellar bands (DIBs) in absorption toward the globular cluster NGC 6397 using VLT/MUSE. Assuming the absorbers are located at the rim of the Local Bubble we trace structures on the order of mpc (milliparsec, a few thousand AU). Aims. We aimed to demonstrate the feasibility to map variations of DIBs on small scales with MUSE. The sightlines defined by binned stellar spectra are separated by only a few arcseconds and we probe the absorption within a physically connected region. Methods. This analysis utilized the fitting residuals of individual stellar spectra of NGC 6397 member stars and analyzed lines from neutral species and several DIBs in Voronoi-binned composite spectra with high signal-to-noise ratio (S/N). Results. This pilot study demonstrates the power of MUSE for mapping the local ISM on very small scales which provides a new window for ISM observations. We detect small scale variations in Na I and K I as well as in several DIBs within few arcseconds, or mpc with regard to the Local Bubble. We verify the suitability of the MUSE 3D spectrograph for such measurements and gain new insights by probing a single physical absorber with multiple sight lines.
Published: 2017

20. The Apache Point Observatory Galactic Evolution Experiment (APOGEE)

Author: Steven R. Majewski, Ricardo P. Schiavon, Peter M. Frinchaboy, Carlos Allende Prieto, Robert Barkhouser, Dmitry Bizyaev, Basil Blank, Sophia Brunner, Adam Burton, Ricardo Carrera, S. Drew Chojnowski, Kátia Cunha, Courtney Epstein, Greg Fitzgerald, Ana E. García Pérez, Fred R. Hearty, Chuck Henderson, Jon A. Holtzman, Jennifer A. Johnson, Charles R. Lam, James E. Lawler, Paul Maseman, Szabolcs Mészáros, Matthew Nelson, Duy Coung Nguyen, David L. Nidever, Marc Pinsonneault, Matthew Shetrone, Stephen Smee, Verne V. Smith, Todd Stolberg, Michael F. Skrutskie, Eric Walker, John C. Wilson, Gail Zasowski, Friedrich Anders, Sarbani Basu, Stephane Beland, Michael R. Blanton, Jo Bovy, Joel R. Brownstein, Joleen Carlberg, William Chaplin, Cristina Chiappini, Daniel J. Eisenstein, Yvonne Elsworth, Diane Feuillet, Scott W. Fleming, Jessica Galbraith-Frew, Rafael A. García, D. Aníbal García-Hernández, Bruce A. Gillespie, Léo Girardi, James E. Gunn, Sten Hasselquist, Michael R. Hayden, Saskia Hekker, Inese Ivans, Karen Kinemuchi, Mark Klaene, Suvrath Mahadevan, Savita Mathur, Benoît Mosser, Demitri Muna, Jeffrey A. Munn, Robert C. Nichol, Robert W. O’Connell, John K. Parejko, A. C. Robin, Helio Rocha-Pinto, Matthias Schultheis, Aldo M. Serenelli, Neville Shane, Victor Silva Aguirre, Jennifer S. Sobeck, Benjamin Thompson, Nicholas W. Troup, David H. Weinberg, Olga Zamora, The University of Western Australia (UWA), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), National University of Singapore (NUS), Department of Psychology, St John's University, School of Physics and Astronomy [Birmingham], University of Birmingham [Birmingham], Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), School of Physics and Astronomy, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Department of Physics and Astronomy [Aarhus], and Aarhus University [Aarhus]
Subjects: RED-GIANT STARS, abundances [galaxy], kinematics and dynamics [galaxy], EXPLORING HALO SUBSTRUCTURE, Metallicity, Milky Way, FOS: Physical sciences, CHEMICAL EVOLUTION, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, STELLAR POPULATIONS, Observatory, GLOBULAR-CLUSTERS, structure [galaxy], 0103 physical sciences, EARLY-TYPE GALAXIES, AST-1616636, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, QB, SOLAR-TYPE STARS, 010308 nuclear & particles physics, RCUK, Astronomy, Astronomy and Astrophysics, formation [galaxy], Astrophysics - Astrophysics of Galaxies, Galaxy, RESOLUTION INFRARED-SPECTROSCOPY, stellar content [galaxy], Radial velocity, Interstellar medium, Stars, Star cluster, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), evolution [galaxy], DIGITAL SKY SURVEY, MILKY-WAY, AST-1109178, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology
Abstract: The Apache Point Observatory Galactic Evolution Experiment (APOGEE), one of the programs in the Sloan Digital Sky Survey III (SDSS-III), has now completed its systematic, homogeneous spectroscopic survey sampling all major populations of the Milky Way. After a three year observing campaign on the Sloan 2.5-m Telescope, APOGEE has collected a half million high resolution (R~22,500), high S/N (>100), infrared (1.51-1.70 microns) spectra for 146,000 stars, with time series information via repeat visits to most of these stars. This paper describes the motivations for the survey and its overall design---hardware, field placement, target selection, operations---and gives an overview of these aspects as well as the data reduction, analysis and products. An index is also given to the complement of technical papers that describe various critical survey components in detail. Finally, we discuss the achieved survey performance and illustrate the variety of potential uses of the data products by way of a number of science demonstrations, which span from time series analysis of stellar spectral variations and radial velocity variations from stellar companions, to spatial maps of kinematics, metallicity and abundance patterns across the Galaxy and as a function of age, to new views of the interstellar medium, the chemistry of star clusters, and the discovery of rare stellar species. As part of SDSS-III Data Release 12, all of the APOGEE data products are now publicly available., Submitted to The Astronomical Journal: 50 pages, including 38 figures, 4 tables, and 5 appendices
Published: 2017

21. A LOFAR detection of the low mass young star T Tau at 149 MHz

Author: Adam Stewart, M. Pietka, Stephane Corbel, Tom Ray, Anna M. M. Scaife, A. Drabent, Alexander J. van der Horst, Matthias Hoeft, P. Zarka, Jean-Mathias Greißmeier, Colm P. Coughlan, Martin Bell, Rachael E. Ainsworth, Joeri van Leeuwen, Jochen Eislöffel, Ralph A. M. J. Wijers, J. W. Broderick, Sera Markoff, Dublin Institute for Advanced Studies (DIAS), Thüringer Landessternwarte Tautenburg (TLS), School of Physics and Astronomy [Southampton], University of Southampton, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Oxford Astrophysics, University of Oxford [Oxford], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ERC-2012-StG-307215 LODESTONE, European Project: 307215,EC:FP7:ERC,ERC-2012-StG_20111012,LODESTONE(2013), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Oxford, High Energy Astrophys. & Astropart. Phys (API, FNWI), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Electron density, 010504 meteorology & atmospheric sciences, Young stellar object, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 7. Clean energy, 01 natural sciences, 0103 physical sciences, individual (T Tauri) [stars], Protostar, pre-main sequence [stars], 010303 astronomy & astrophysics, stars [radio continuum], Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), protostars [stars], 0105 earth and related environmental sciences, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, LOFAR, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), thermal [radiation mechanisms], Content (measure theory), Spectral energy distribution, Low Mass
Abstract: Radio observations of young stellar objects (YSOs) enable the study of ionised plasma outflows from young protostars via their free-free radiation. Previous studies of the low-mass young system T Tau have used radio observations to model the spectrum and estimate important physical properties of the associated ionised plasma (local electron density, ionised gas content and emission measure). However, without an indication of the low-frequency turnover in the free-free spectrum, these properties remain difficult to constrain. This paper presents the detection of T Tau at 149 MHz with the Low Frequency Array (LOFAR) - the first time a YSO has been observed at such low frequencies. The recovered total flux indicates that the free-free spectrum may be turning over near 149 MHz. The spectral energy distribution is fitted and yields improved constraints on local electron density ($(7.2 \pm 2.1)\times10^{3}$ cm$^{-3}$), ionised gas mass ($(1.0 \pm 1.8)\times10^{-6}$ M$_{\odot}$) and emission measure ($(1.67 \pm 0.14)\times10^5$ pc cm$^{-6}$)., Comment: 10 pages, accepted for publication in ApJ
Published: 2017

22. The ATLAS3D project – XIX. The hot gas content of early-type galaxies: fast versus slow rotators

Author: M. Bois, Pierre-Alain Duc, Davor Krajnović, Katherine Alatalo, Pierre Yves Lablanche, Richard M. McDermid, Michele Cappellari, Sadegh Khochfar, Eric Emsellem, Lisa M. Young, Tom Oosterloo, Alison F. Crocker, Paolo Serra, Raffaella Morganti, P. T. de Zeeuw, Nicholas Scott, Anne-Marie Weijmans, Roger L. Davies, Timothy A. Davis, Thorsten Naab, Martin Bureau, Marc Sarzi, Harald Kuntschner, Leo Blitz, Frédéric Bournaud, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Department of Astronomy [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, Department of Computer and Information Science and Engineering [Gainesville] (UF|CISE), University of Florida [Gainesville] (UF), European Southern Observatory (ESO), Max-Planck-Institut für Extraterrestrische Physik (MPE), Netherlands Institute for Radio Astronomy (ASTRON), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre for Astrophysics & Supercomputing, Swinburne University of Technology [Melbourne], NASA Ames Research Center (ARC), Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, University of California [Berkeley], University of California-University of California, École normale supérieure - Paris (ENS Paris), University of Oxford [Oxford]-University of Oxford [Oxford], and Kapteyn Astronomical Institute
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), X-RAY LUMINOSITY, MULTIPARAMETRIC ANALYSIS, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, cD, STAR-FORMATION, Luminosity, X-rays: binaries, ELLIPTIC GALAXIES, 0103 physical sciences, TO-LIGHT RATIO, Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, Lenticular galaxy, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, LENTICULAR GALAXIES, [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, Star formation, Velocity dispersion, Astronomy, MASS-LOSS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, SAURON PROJECT, Galaxy, X-rays: galaxies, Stars, Supernova, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Stellar mass loss, GLOBULAR-CLUSTER SYSTEMS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: evolution, galaxies: ISM, MORPHOLOGY-DENSITY RELATION, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: For early-type galaxies, the ability to sustain a corona of hot, X-ray emitting gas could have played a key role in quenching their star-formation history. Yet, it is still unclear what drives the precise amount of hot gas around these galaxies. By combining photometric and spectroscopic measurements for the early-type galaxies observed during the Atlas3D integral-field survey with measurements of their X-ray luminosity based on X-ray data of both low and high spatial resolution we conclude that the hot-gas content of early-type galaxies can depend on their dynamical structure. Specifically, whereas slow rotators generally have X-ray halos with luminosity L_X,gas and temperature T values that are in line with what is expected if the hot-gas emission is sustained by the thermalisaton of the kinetic energy carried by the stellar-mass loss material, fast rotators tend to display L_X,gas values that fall consistently below the prediction of this model, with similar T values that do not scale with the stellar kinetic energy as observed in the case of slow rotators. Considering that fast rotators are likely to be intrinsically flatter than slow rotators, and that the few L_X,gas-deficient slow rotators also happen to be relatively flat, the observed L_X,gas deficiency in these objects would support the hypothesis whereby flatter galaxies have a harder time in retaining their hot gas. We discuss the implications that a different hot-gas content could have on the fate of both acquired and internally-produced gaseous material, considering in particular how the L_X,gas deficiency of fast rotators would make them more capable to recycle the stellar-mass loss material into new stars than slow rotators. This is consistent with the finding that molecular gas and young stars are detected only in fast rotators in the Atlas3D sample, and that fast rotators tend to dustier than slow rotators. [Abridged], 16 pages, 10 figures, accepted for publications on MNRAS. More information about our Atlas3D project see http://www-astro.physics.ox.ac.uk/atlas3d/
Published: 2013

23. 3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae★

Author: Vallery Stanishev, Wolfgang Hillebrandt, Ivo R. Seitenzahl, Friedrich K. Röpke, Stuart A. Sim, G. Blanc, Ruediger Pakmor, Ashley J. Ruiter, Markus Kromer, Nancy Elias-Rosa, M. Fink, F. Ciaraldi-Schoolmann, S. Taubenberger, The Oskar Klein Centre for Cosmoparticle Physics and Department of Physics, Stockholm University, Institut Langevin - Ondes et Images (UMR7587) (IL), Sorbonne Université (SU)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Paris (UP)-Centre National de la Recherche Scientifique (CNRS), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Heidelberger Institut für Theoretische Studien (H-ITS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Stockholm University, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Nucleosynthesis, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Ejecta, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS]Physics [physics], Physics, Astronomy, White dwarf, Astronomy and Astrophysics, Light curve, Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Deflagration, Pair-instability supernova, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 2002cx-like supernovae are a sub-class of sub-luminous Type Ia supernovae. Their light curves and spectra are characterized by distinct features that indicate strong mixing of the explosion ejecta. Pure turbulent deflagrations have been shown to produce such mixed ejecta. Here, we present hydrodynamics, nucleosynthesis and radiative transfer calculations for a 3D full-star deflagration of a Chandrasekhar-mass white dwarf. Our model is able to reproduce the characteristic observational features of SN 2005hk (a proto-typical 2002cx-like supernova), not only in the optical, but also in the near-infrared. For that purpose we present, for the first time, five near-infrared spectra of SN 2005hk from -0.2 to 26.6 days with respect to B-band maximum. Since our model burns only small parts of the initial white dwarf, it fails to completely unbind the white dwarf and leaves behind a bound remnant of ~1.03 solar masses -- consisting mainly of unburned carbon and oxygen, but also enriched by some amount of intermediate-mass and iron-group elements from the explosion products that fall back on the remnant. We discuss possibilities for detecting this bound remnant and how it might influence the late-time observables of 2002cx-like SNe., Comment: 12 pages, 8 figures, 3 tables. Accepted for publication by MNRAS
Published: 2012

24. Self-similarity in the chemical evolution of galaxies and the delay time distribution of SNe Ia

Author: Robert M. Yates, Marie Martig, Cristina Chiappini, Maria Bergemann, C. J. Walcher, Gustavo Bruzual, Ivan Minchev, Stephane Charlot, Paula Coelho, Anna Gallazzi, Leibniz-Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Extraterrestrische Physik (MPE), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Instituto de Astronomia, Geofisica et Ciencias Atmosfericas, Universidade de São Paulo (USP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Universidade de São Paulo = University of São Paulo (USP)
Subjects: Self-similarity, stars: abundances, Milky Way, FOS: Physical sciences, galaxies: elliptical and lenticular cD, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, supernovae: general, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, QD, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Galaxy: evolution, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Universality (dynamical systems), Chemical evolution, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: abundances, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Delay time
Abstract: Recent improvements in the age dating of stellar populations and single stars allow us to study the ages and abundance of stars and galaxies with unprecedented accuracy. We here compare the relation between age and \alpha-element abundances for stars in the solar neighborhood to that of local, early-type galaxies. We find both relations to be very similar. Both fall into two regimes with a flat slope for ages younger than ~9 Gyr and a steeper slope for ages older than that value. This quantitative similarity seems surprising, given the different types of galaxies and scales involved. For the sample of early-type galaxies we also show that the data are inconsistent with literature delay time distributions of either single or double Gaussian shape. The data are consistent with a power law delay time distribution. We thus confirm that the delay time distribution inferred for the Milky Way from chemical evolution arguments also must apply to massive early-type galaxies. We also offer a tentative explanation for the seeming universality of the age-[\alpha/Fe] relation as the manifestation of averaging of different stellar populations with varying chemical evolution histories., Comment: 8 pages, 3 figures, submitted to A&A, version in reply to first referee report
Published: 2016

25. THE GAIA -ESO SURVEY: METAL-RICH BANANAS IN THE BULGE

Author: G. G. Sacco, A. Hourihane, L. Morbidelli, E. Franciosini, Alejandra Recio-Blanco, Lorenzo Monaco, P. de Laverny, Gerard Gilmore, P. Francois, C. C. Worley, Martin C. Smith, Matthew Molloy, T. Costado, Nick Evans, Sergey E. Koposov, Sofia Randich, Giovanni Carraro, Karin Lind, A. A. Williams, S. Mikolaitis, Jack Lewis, Laura Magrini, Andrew R. Casey, J. Shen, Amelia Bayo, Simone Zaggia, Georges Kordopatis, Thomas Bensby, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Focas Research Institute, Dublin Institute of Technology, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Evans, Wyn [0000-0002-5981-7360], Gilmore, Gerard [0000-0003-4632-0213], Koposov, Sergey [0000-0003-2644-135X], Casey, Andrew [0000-0003-0174-0564], Worley, Clare [0000-0001-9310-2898], and Apollo - University of Cambridge Repository
Subjects: astro-ph.GA, bulge [Galaxy], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, GALACTIC BULGE, 01 natural sciences, Galaxy: bulge, galaxies: general, galaxies: kinematics and dynamics, Astronomy and Astrophysics, Space and Planetary Science, Latitude, Metal, DISK, Bulge, 0103 physical sciences, Minor axis, Astrophysics::Solar and Stellar Astrophysics, KINEMATICS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], kinematics and dynamics [Galaxies], 010308 nuclear & particles physics, GENERAL [GALAXIES], Velocity dispersion, MILKY-WAY BULGE, Giant star, SPLIT RED CLUMP, Astrophysics - Astrophysics of Galaxies, Stars, Astrophysics of Galaxies (astro-ph.GA), visual_art, visual_art.visual_art_medium, Astrophysics::Earth and Planetary Astrophysics, HIGH-VELOCITY PEAKS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We analyse the kinematics of $\sim 2000$ giant stars in the direction of the Galactic bulge, extracted from the Gaia-ESO survey in the region $-10^\circ \lesssim \ell \lesssim 10^\circ$ and $-11^\circ \lesssim b \lesssim -3^\circ$. We find distinct kinematic trends in the metal rich ($\mathrm{[M/H]}>0$) and metal poor ($\mathrm{[M/H]}, Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell’Istruzione, dell’Università e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012.” The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the European Science Foundation (ESF) through the GREAT Research Network Programme., This is the author accepted manuscript. The final version is available from IOP Publishing via http://dx.doi.org/10.3847/2041-8205/824/2/L29
Published: 2016

26. The SDSS-IV Extended Baryon Oscillation Spectroscopic Survey : overview and early data

Author: Joe Huehnerhoff, Jo Bovy, Jean-Marc Le Goff, Nicolás G. Busca, Matthew A. Bershady, Will J. Percival, Yipeng Jing, Marcio A. G. Maia, Conor Sayres, Diana Holder, Xiaohui Fan, Eric Jullo, Flavia Sobreira, Sergio Rodríguez-Torres, Vikrant Kamble, Antonio D. Montero-Dorta, Yu Liang, Andreas A. Berlind, Patrick Gaulme, Beth Reid, Stephen Bailey, Peter Nugent, Andrea Merloni, Peter M. Frinchaboy, Dmitry Bizyaev, A. C. Rosell, Gong-Bo Zhao, Tracy Naugle, Yen-Ting Lin, Vivek Mariappan, Zhongxu Zhai, Julien Guy, Hélion du Mas des Bourboux, Shirley Ho, Martin White, Éric Aubourg, Abhishek Prakash, Pasquier Noterdaeme, Yuting Wang, Audrey Oravetz, Dustin Lang, Uroš Seljak, W. N. Brandt, Demitri Muna, Patrick Petitjean, Sylvain de la Torre, M. C. Cousinou, Ian D. McGreer, Pierre Laurent, Adam D. Myers, Isabelle Paris, Andres Meza, John J. Ruan, Franco D. Albareti, Etienne Burtin, Kyle S. Dawson, Adam S. Bolton, Alina Streblyanska, Nikhil Padmanabhan, Marcos Lima, Chia-Hsun Chuang, Kaike Pan, Benjamin A. Weaver, Daniel J. Eisenstein, Branimir Sesar, Mariana Vargas-Magaña, Ashley J. Ross, Alice Pisani, Axel de la Macorra, Mark A. Klaene, Nathalie Palanque-Delabrouille, Karen Kinemuchi, Nicholas R. MacDonald, Rita Tojeiro, Nicolas Clerc, Nao Suzuki, Scott F. Anderson, Dan Long, John A. Peacock, Kirpal Nandra, Johan Comparat, D. Kirkby, Anze Slosar, Timothy A. Hutchinson, Michael Blomqvist, Donald P. Schneider, Stephanie Escoffier, Jeremy L. Tinker, Charling Tao, Irene Cruz-González, Jon Brinkmann, Michael Eracleous, Francisco-Shu Kitaura, Hu Zou, Elena Malanushenko, Yiping Shu, Anand Raichoor, W. M. Wood-Vasey, Andreu Font-Ribera, Tom Dwelly, J. Ridl, Graziano Rossi, Hee-Jong Seo, Britt Lundgren, Sarah Shandera, Brice Ménard, Luiz N. da Costa, Shadab Alam, Ricardo L. C. Ogando, Christophe Yèche, Daniel Oravetz, Matthew M. Pieri, Jean-Paul Kneib, Julian E. Bautista, Weipeng Lin, Mara Salvato, Antonis Georgakakis, Alexis Finoguenov, Hong Guo, Florian Beutler, Guangtun Zhu, Jeremy Darling, Zheng Zheng, Frances Cope, Donna Taylor, Francisco Prada, David H. Weinberg, Cheng Li, Rupert A. C. Croft, Joel R. Brownstein, Viktor Malanushenko, Paul J. Green, Jeffrey A. Newman, John K. Parejko, David J. Schlegel, Matthew D. Olmstead, Russ R. Laher, Cameron K. McBride, Cheng Zhao, Timothée Delubac, James Rich, Michael R. Blanton, Eric Armengaud, Anne Ealet, Zheng Cai, Qiufan Lin, University of St Andrews. School of Physics and Astronomy, AVL, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Research Institute of Forest Resource Information Techniques, Chinese Academy of Forestry, Centre Hospitalier Universitaire de Dijon - Hôpital François Mitterrand (CHU Dijon), McMaster University [Hamilton, Ontario], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Shanghai Astronomical Observatory [Shanghai] (SHAO), Chinese Academy of Sciences [Beijing] (CAS), Departamento de Fisica Matematica, Universidade de São Paulo = University of São Paulo (USP), Max-Planck-Institut für Astrophysik (MPA), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Universidad de Chile = University of Chile [Santiago] (UCHILE), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Department of Electrical and Computer Engineering [Minneapolis] (ECE), University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, China National Research Center of Intelligent Equipment for Agriculture [Beijing] (NRCIEA), Key Laboratory for Liquid-Solid Structural Evolution and Processing of Materials, Shandong University, Laboratoire de Chimie - UMR5182 (LC), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Universidad Autonoma de Madrid (UAM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of California [Irvine] (UCI), University of California-University of California, Département de Physique des Particules (ex SPP) (DPP), Universidade de São Paulo (USP), Universidad Santiago de Chile, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, University of Minnesota [Twin Cities], École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), UAM. Departamento de Física Teórica, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon)-Institut de Chimie du CNRS (INC), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, surveys, Tests of general relativity, 0103 physical sciences, ST/K0090X/1, QB Astronomy, Emission spectrum, observations [Cosmology], 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, QC, QB, Physics, 010308 nuclear & particles physics, Física, RCUK, Astronomy and Astrophysics, Quasar, 3rd-DAS, Redshift, Galaxy, Baryon, QC Physics, Space and Planetary Science, cosmology: observations, astro-ph.CO, Baryon acoustic oscillations, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Astrophysical Journal 151.2 (2016): 44 reproduced by permission of the AAS, In a six-year program started in 2014 July, the Extended Baryon Oscillation Spectroscopic Survey (eBOSS) will conduct novel cosmological observations using the BOSS spectrograph at Apache Point Observatory. These observations will be conducted simultaneously with the Time Domain Spectroscopic Survey (TDSS) designed for variability studies and the Spectroscopic Identification of eROSITA Sources (SPIDERS) program designed for studies of X-ray sources. In particular, eBOSS will measure with percent-level precision the distance-redshift relation with baryon acoustic oscillations (BAO) in the clustering of matter. eBOSS will use four different tracers of the underlying matter density field to vastly expand the volume covered by BOSS and map the large-scale-structures over the relatively unconstrained redshift range 0.6 < z < 2.2. Using more than 250,000 new, spectroscopically confirmed luminous red galaxies at a median redshift z = 0.72, we project that eBOSS will yield measurements of the angular diameter distance dA(z) to an accuracy of 1.2% and measurements of H(z) to 2.1% when combined with the z > 0.6 sample of BOSS galaxies. With ∼195,000 new emission line galaxy redshifts, we expect BAO measurements of dA(z) to an accuracy of 3.1% and H(z) to 4.7% at an effective redshift of z = 0.87. A sample of more than 500,000 spectroscopically confirmed quasars will provide the first BAO distance measurements over the redshift range 0.9 < z < 2.2, with expected precision of 2.8% and 4.2% on dA(z) and H(z), respectively. Finally, with 60,000 new quasars and re-observation of 60,000 BOSS quasars, we will obtain new Lyα forest measurements at redshifts z > 2.1; these new data will enhance the precision of dA(z) and H(z) at z > 2.1 by a factor of 1.44 relative to BOSS. Furthermore, eBOSS will provide improved tests of General Relativity on cosmological scales through redshift-space distortion measurements, improved tests for non-Gaussianity in the primordial density field, and new constraints on the summed mass of all neutrino species. Here, we provide an overview of the cosmological goals, spectroscopic target sample, demonstration of spectral quality from early data, and projected cosmological constraints from eBOSS, K.D. acknowledges support from the U.S. Department of Energy under Grant DE-SC000995. J.P.K. and T.D. acknowledge support from the ERC advanced grant LIDA. W.J.P. acknowledges support from the UK STFC through the consolidated grant ST/K0090X/1, and from the European Research Council through grant Darksurvey
Published: 2016

27. Wide-band, low-frequency pulse profiles of 100 radio pulsars with LOFAR

Author: J. van Leeuwen, Matthias Steinmetz, T. E. Hassall, A. Nelles, E. de Geus, M. Pilia, B. W. Stappers, Heino Falcke, H. J. A. Röttgering, Annalisa Bonafede, Oleg Smirnov, Anna V. Bilous, Satyendra Thoudam, Evan Keane, Peter G. Jonker, W. Frieswijk, Rudy Wijnands, A. Noutsos, M. Pietka, John D. Swinbank, Richard Fallows, R. J. van Weeren, M. Pandey-Pommier, Olaf Wucknitz, A. Alexov, Rebecca McFadden, E. Juette, F. Breitling, Stefan J. Wijnholds, Aris Karastergiou, Benedetta Ciardi, H. Paas, Antonia Rowlinson, Dominik J. Schwarz, Michael Kramer, A. I. F. Stewart, Y. Tang, Ashish Asgekar, K. Zagkouris, James A. Anderson, Chiara Ferrari, S. Duscha, James Miller-Jones, Andrew Lyne, Stefan Oslowski, Adam T. Deller, A. de Jong, R. C. Vermeulen, Gianni Bernardi, I. M. Avruch, M. A. Garrett, M. C. Toribio, Jochen Eislöffel, Charlotte Sobey, A. J. van der Horst, Rene P. Breton, Cyril Tasse, Marcus Brüggen, J. W. Broderick, Gerard H. Kuper, S. ter Veen, A. W. Gunst, Rob Fender, P. Zarka, D. McKay-Bukowski, Martin Bell, A. Horneffer, M. Kuniyoshi, Patrick Weltevrede, M. Serylak, A. G. Polatidis, Ralph A. M. J. Wijers, Mark J. Bentum, Christian Vocks, Jean-Mathias Grießmeier, Sera Markoff, Jason W. T. Hessels, Stephane Corbel, Laura Birzan, J. P. Hamaker, Wolfgang Reich, Michel Tagger, P. Maat, V. I. Kondratiev, George Heald, Gottfried Mann, R. Pizzo, Astronomy, Netherlands Institute for Radio Astronomy (ASTRON), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Vrije Universiteit Medical Centre (VUMC), Vrije Universiteit Amsterdam [Amsterdam] (VU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Oxford Astrophysics, University of Oxford, School of Physics and Astronomy [Southampton], University of Southampton, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Centre for Astrophysics and Supercomputing [Swinburne] (CAS), Swinburne University of Technology [Melbourne], Department of Physics [Oxford], Max-Planck-Institut für Radioastronomie (MPIFR), Universität Bielefeld = Bielefeld University, University of Cape Town, Space Telescope Science Institute (STSci), Epidémiologie et Biostatistique [Bordeaux], Université Bordeaux Segalen - Bordeaux 2-Institut de Santé Publique, d'Épidémiologie et de Développement (ISPED)-Institut National de la Santé et de la Recherche Médicale (INSERM), SRON Netherlands Institute for Space Research (SRON), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], University of Hamburg, Leibniz-Institut DSMZ-Deutsche Sammlung von Mikroorganismen und Zellkulturen GmbH / Leibniz Institute DSMZ-German Collection of Microorganisms and Cell Cultures (DSMZ), University of Edinburgh, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Structural Dynamics and Acoustics, University of Twente, Thüringer Landessternwarte Tautenburg (TLS), Institute of Mathematical and Physical Sciences, Department of Astrophysics [Oxford], Département de Géologie, Université de Montréal (UdeM), Astronomisches Institut der Ruhr-Universität Bochum, Ruhr-Universität Bochum [Bochum], Leibniz-Institut für Astrophysik Potsdam (AIP), Department of Physical Sciences, University of Oulu, University of Oulu, Curtin University [Perth], Planning and Transport Research Centre (PATREC), University of Groningen [Groningen], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Australia Telescope National Facility (ATNF), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Institute of Farm Animal Genetics (ING), Friedrich-Loeffler-Institut (FLI), SKA South Africa, Ska South Africa, Astrophysikalisches Institut Potsdam (AIP), Department of Physics [Dunedin], University of Otago [Dunedin, Nouvelle-Zélande], Princeton University, Edinburgh Research Station, Centre for Ecology and Hydrology, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astrophysics [Nijmegen], Radboud University [Nijmegen]-Radboud University [Nijmegen], Anton Pannekoek Institute for Astronomy, Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Alexander von Humboldt Foundation Agence Nationale de la Recherche ANR-09-JCJC-0001-01, ANR-09-JCJC-0001,OPALES(2009), European Project: 337062,EC:FP7:ERC,ERC-2013-StG,DRAGNET(2014), European Project: 617199,EC:FP7:ERC,ERC-2013-CoG,ALERT(2014), European Project: 224838,EC:FP7:PEOPLE,FP7-PEOPLE-2007-4-3-IRG,PULSARS WITH LOFAR(2008), ROUCHON, Nathalie, Jeunes chercheuses et jeunes chercheurs - - OPALES2009 - ANR-09-JCJC-0001 - JCJC - VALID, DRAGNET: A high-speed, wide-angle camera for catching extreme astrophysical events - DRAGNET - - EC:FP7:ERC2014-01-01 - 2018-12-31 - 337062 - VALID, ALERT - The Apertif-LOFAR Exploration of the Radio Transient Sky - ALERT - - EC:FP7:ERC2014-12-01 - 2019-11-30 - 617199 - VALID, Radio pulsars with LOFAR: a study of extreme physics laboratories. - PULSARS WITH LOFAR - - EC:FP7:PEOPLE2008-05-01 - 2012-04-30 - 224838 - VALID, High Energy Astrophys. & Astropart. Phys (API, FNWI), University of Oxford [Oxford], Radboud university [Nijmegen], Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Fakultät für Physik, Universität Bielefeld, Universität Bielefeld, University of the Western Cape, Cape Town, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), University of Twente [Netherlands], Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Radboud university [Nijmegen]-Radboud university [Nijmegen], Harvard University-Smithsonian Institution, Universiteit Leiden, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Pilia, M., Hessels, J.W.T., Stappers, B.W., Kondratiev, V.I., Kramer, M., Van Leeuwen, J., Weltevrede, P., Lyne, A.G., Zagkouris, K., Hassall, T.E., Bilous, A.V., Breton, R.P., Falcke, H., Grießmeier, J.-M., Keane, E., Karastergiou, A., Kuniyoshi, M., Noutsos, A., Osłowski, S., Serylak, M., Sobey, C., Ter Veen, S., Alexov, A., Anderson, J., Asgekar, A., Avruch, I.M., Bell, M.E., Bentum, M.J., Bernardi, G., Bîrzan, L., Bonafede, A., Breitling, F., Broderick, J.W., Brüggen, M., Ciardi, B., Corbel, S., De Geus, E., De Jong, A., Deller, A., Duscha, S., Eislöffel, J., Fallows, R.A., Fender, R., Ferrari, C., Frieswijk, W., Garrett, M.A., Gunst, A.W., Hamaker, J.P., Heald, G., Horneffer, A., Jonker, P., Juette, E., Kuper, G., Maat, P., Mann, G., Markoff, S., McFadden, R., McKay-Bukowski, D., Miller-Jones, J.C.A., Nelles, A., Paas, H., Pandey-Pommier, M., Pietka, M., Pizzo, R., Polatidis, A.G., Reich, W., Röttgering, H., Rowlinson, A., Schwarz, D., Smirnov, O., Steinmetz, M., Stewart, A., Swinbank, J.D., Tagger, M., Tang, Y., Tasse, C., Thoudam, S., Toribio, M.C., Van Der Horst, A.J., Vermeulen, R., Vocks, C., Van Weeren, R.J., Wijers, R.A.M.J., Wijnands, R., Wijnholds, S.J., Wucknitz, O., and Zarka, P.
Subjects: Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, METIS-321663, Astrophysics::Cosmology and Extragalactic Astrophysics, Low frequency, 01 natural sciences, Radio spectrum, law.invention, Telescope, Radio telescope, [SDU] Sciences of the Universe [physics], stars: neutron, Pulsar, law, pulsars: general, 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), IR-103184, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, LOFAR, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Interstellar medium, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Radio frequency, EWI-27451, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: LOFAR offers the unique capability of observing pulsars across the 10-240 MHz frequency range with a fractional bandwidth of roughly 50%. This spectral range is well-suited for studying the frequency evolution of pulse profile morphology caused by both intrinsic and extrinsic effects: such as changing emission altitude in the pulsar magnetosphere or scatter broadening by the interstellar medium, respectively. The magnitude of most of these effects increases rapidly towards low frequencies. LOFAR can thus address a number of open questions about the nature of radio pulsar emission and its propagation through the interstellar medium. We present the average pulse profiles of 100 pulsars observed in the two LOFAR frequency bands: High Band (120-167 MHz, 100 profiles) and Low Band (15-62 MHz, 26 profiles). We compare them with Westerbork Synthesis Radio Telescope (WSRT) and Lovell Telescope observations at higher frequencies (350 and1400 MHz) in order to study the profile evolution. The profiles are aligned in absolute phase by folding with a new set of timing solutions from the Lovell Telescope, which we present along with precise dispersion measures obtained with LOFAR. We find that the profile evolution with decreasing radio frequency does not follow a specific trend but, depending on the geometry of the pulsar, new components can enter into, or be hidden from, view. Nonetheless, in general our observations confirm the widening of pulsar profiles at low frequencies, as expected from radius-to-frequency mapping or birefringence theories. We offer this catalog of low-frequency pulsar profiles in a user friendly way via the EPN Database of Pulsar Profiles (http://www.epta.eu.org/epndb/)., Comment: 38 pages, 11 figures, 5 tables, A&A in press, updated with editorial corrections
Published: 2016

28. Atmospheric velocity fields in tepid main sequence stars

Author: J. Silaj, T. Officer, T. A. A. Sigut, Friedrich Kupka, S. Strasser, A. Townshend, John D. Landstreet, H. A. Ford, Armagh Observatory, College Hill, Max-Planck-Institut für Astrophysik (MPA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Department of Physics and Astronomy, University of Western Ontario
Subjects: Physics, 010308 nuclear & particles physics, Stellar atmosphere, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Effective temperature, 01 natural sciences, Spectral line, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Microturbulence, Vector field, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Main sequence, Line (formation)
Abstract: The line profiles of the stars with v sin i below a few km/s can reveal direct signatures of local velocity fields (e.g. convection) in stellar atmospheres. This effect is well established in cool main sequence stars, and has been detected and studied in three A stars. This paper reports observations of main sequence B, A and F stars with two goals: (1) to identify additional stars having sufficiently low values of v sin i to search for spectral line profile signatures of local velocity fields, and (2) to explore how the signatures of the local velocity fields in the atmosphere depend on stellar parameters such as effective temperature T_eff and peculiarity type. For stars having T_eff below about 10000 K, we always detect local atmospheric velocity fields indirectly through a non-zero microturbulence parameter, but not for hotter stars. Among the A and F stars in our sample having the sharpest lines, direct tracers of atmospheric velocity fields are found in six new stars. The velocity field signatures identified include asymmetric excess line wing absorption, deeper in the blue line wing than in the red; line profiles of strong lines that are poorly fit by computed profiles; and strong lines that are broader than they should be for the v sin i values deduced from weak lines. These effects are found in both normal and Am stars, but seem stronger in Am stars. These data still have not been satisfactorily explained by models of atmospheric convection, including numerical simulations., Acepted for publication by Astronomy and Astrophysics
Published: 2009

29. SPACE: the spectroscopic all-sky cosmic explorer

Author: A. Cimatti, M. Robberto, C. Baugh, S. V. W. Beckwith, R. Content, E. Daddi, G. De Lucia, B. Garilli, L. Guzzo, G. Kauffmann, M. Lehnert, D. Maccagni, A. Martínez-Sansigre, F. Pasian, I. N. Reid, P. Rosati, R. Salvaterra, M. Stiavelli, Y. Wang, M. Zapatero Osorio, M. Balcells, M. Bersanelli, F. Bertoldi, J. Blaizot, D. Bottini, R. Bower, A. Bulgarelli, A. Burgasser, C. Burigana, R. C. Butler, S. Casertano, B. Ciardi, M. Cirasuolo, M. Clampin, S. Cole, A. Comastri, S. Cristiani, J.-G. Cuby, F. Cuttaia, A. De Rosa, A. Diaz Sanchez, M. Di Capua, J. Dunlop, X. Fan, A. Ferrara, F. Finelli, A. Franceschini, M. Franx, P. Franzetti, C. Frenk, Jonathan P. Gardner, F. Gianotti, R. Grange, C. Gruppioni, A. Gruppuso, F. Hammer, L. Hillenbrand, A. Jacobsen, M. Jarvis, R. Kennicutt, R. Kimble, M. Kriek, J. Kurk, J.-P. Kneib, O. Le Fevre, D. Macchetto, J. MacKenty, P. Madau, M. Magliocchetti, D. Maino, N. Mandolesi, N. Masetti, R. McLure, A. Mennella, M. Meyer, M. Mignoli, B. Mobasher, E. Molinari, G. Morgante, S. Morris, L. Nicastro, E. Oliva, P. Padovani, E. Palazzi, F. Paresce, A. Perez Garrido, E. Pian, L. Popa, M. Postman, L. Pozzetti, J. Rayner, R. Rebolo, A. Renzini, H. Röttgering, E. Schinnerer, M. Scodeggio, M. Saisse, T. Shanks, A. Shapley, R. Sharples, H. Shea, J. Silk, I. Smail, P. Spanó, J. Steinacker, L. Stringhetti, A. Szalay, L. Tresse, M. Trifoglio, M. Urry, L. Valenziano, F. Villa, I. Villo Perez, F. Walter, M. Ward, R. White, S. White, E. Wright, R. Wyse, G. Zamorani, A. Zacchei, W. W. Zeilinger, F. Zerbi, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Space Telescope Science Institute (STScI), Institute for Computational Cosmology, Department of Physics, Durham University, Durham (ICC), Centre for Advanced Instrumentation, Department of Physics, Durham University (CfAI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max-Planck-Institut für Astrophysik (MPA), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Brera, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), INAF-Osservatorio Astronomico di Trieste (INAF-OATs), European Southern Observatory (ESO), Università di Milano, University of Oklahoma, Instituto de Astrofísica de Canarias (IAC), Rheinische Friedrich-Wilhelms-Universität Bonn, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Bologna), Department of Earth Atmospheric and Planetary Sciences, MIT, The Royal Observatory (ROE), Goddard Space Flight Center, NASA, Astrophysics Science Division, INAF-Osservatorio Astronomico di Bologna (OABO), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad Politecnica de Cartagena (UPCT), University of Maryland, University of Arizona, Scuola Internazionale Superiore di Studi Avanzati (SISSA), Università degli Studi di Padova = University of Padua (Unipd), University of Leiden, California Institute of Technology, Department of Astronomy (CALTECH), OpSys Project Consulting, University of Hertfordshire [Hatfield] (UH), Institute of Astronomy, University of Cambridge (IoA), Research and Scientific Support Department, ESA-ESTEC (RSSD), University of California, Santa Cruz (UCSC), Steward Observatory, University of Arizona, UC Riverside, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), University of Bucharest, Institute for Astronomy, University of Hawaii, INAF-Osservatorio Astronomico di Padova, Princeton, Ecole Polytechnique Fédérale de Lausanne (EPFL), University of Oxford, Johns Hopkins University (JHU), Yale University, University of California, Los Angeles (UCLA), University of Vienna, Cimatti A., Robberto M., Baugh C., Beckwith S. V. W., Content R., Daddi E., De Lucia G., Garilli B., Guzzo L., Kauffmann G., Lehnert M., Maccagni D., Martínez-Sansigre A., Pasian F., Reid I. N., Rosati P., Salvaterra R., Stiavelli M., Wang Y., Osorio M. Zapatero, Balcells M., Bersanelli M., Bertoldi F., Blaizot J., Bottini D., Bower R., Bulgarelli A., Burgasser A., Burigana C., Butler R. C., Casertano S., Ciardi B., Cirasuolo M., Clampin M., Cole S., Comastri A., Cristiani S., Cuby J.-G., Cuttaia F., de Rosa A., Sanchez A. Diaz, di Capua M., Dunlop J., Fan X., Ferrara A., Finelli F., Franceschini A., Franx M., Franzetti P., Frenk C., Gardner Jonathan P., Gianotti F., Grange R., Gruppioni C., Gruppuso A., Hammer F., Hillenbrand L., Jacobsen A., Jarvis M., Kennicutt R., Kimble R., Kriek M., Kurk J., Kneib J.-P., Le Fevre O., Macchetto D., MacKenty J., Madau P., Magliocchetti M., Maino D., Mandolesi N., Masetti N., McLure R., Mennella A., Meyer M., Mignoli M., Mobasher B., Molinari E., Morgante G., Morris S., Nicastro L., Oliva E., Padovani P., Palazzi E., Paresce F., Garrido A. Perez, Pian E., Popa L., Postman M., Pozzetti L., Rayner J., Rebolo R., Renzini A., Röttgering H., Schinnerer E., Scodeggio M., Saisse M., Shanks T., Shapley A., Sharples R., Shea H., Silk J., Smail I., Spanó P., Steinacker J., Stringhetti L., Szalay A., Tresse L., Trifoglio M., Urry M., Valenziano L., Villa F., Perez I. Villo, Walter F., Ward M., White R., White S., Wright E., Wyse R., Zamorani G., Zacchei A., Zeilinger W., Zerbi F., Cimatti, A., Robberto, M., Baugh, C., Beckwith, S. V. W., Content, R., Daddi, E., De, Lucia, G., Garilli, B., Guzzo, L., Kauffmann, Ferrara, Andrea, and 113, Coauthors
Subjects: Observational cosmology, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Space (mathematics), law.invention, Telescope, law, Dark energy, Spectral resolution, media_common, Physics, COSMIC cancer database, Astronomical and space-research instrumentation, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Billion years, Galaxy, Redshift, Space and Planetary Science, Sky, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We describe the scientific motivations, the mission concept and the instrumentation of SPACE, a class-M mission proposed for concept study at the first call of the ESA Cosmic-Vision 2015-2025 planning cycle. SPACE aims to produce the largest three-dimensional evolutionary map of the Universe over the past 10 billion years by taking near-IR spectra and measuring redshifts for more than half a billion galaxies at 0, Comment: 27 pages, Experimental Astronomy, in press. The SPACE team complete list is available at http://urania.bo.astro.it/cimatti/space . The article with full resolution figures is available at http://urania.bo.astro.it/cimatti/space/publications.htm
Published: 2008

30. VVDS-SWIRE

Author: S. Temporin, D. Maccagni, F. Lamareille, Duncan Farrah, Alain Mazure, C. J. Walcher, Paolo Ciliegi, Christian Marinoni, B. Garilli, V. Le Brun, O. Ilbert, D. Vergani, J. P. Picat, Fan Fang, L. Tresse, T. Contini, Angela Bongiorno, Jarle Brinchmann, E. Zucca, P. Franzetti, S. Paltani, Roberto Scaramella, R. Merighi, Stephane Arnouts, R. Pello, O. Le Fevre, Lucia Pozzetti, G. Zamorani, A. Zanichelli, Stéphane Charlot, M. Bondi, Mario Radovich, S. J. Oliver, H. J. McCracken, David L. Shupe, O. Cucciati, Carol J. Lonsdale, S. de la Torre, Yannick Mellier, D. Bottini, Bruno Marano, C. Adami, A. Pollo, I. Gavignaud, S. Bardelli, Paola Merluzzi, Luigi Guzzo, M. Bolzonella, I. Waddington, Marco Scodeggio, G. Vettolani, A. Iovino, Sylvie Foucaud, Jason Surace, B. Meneux, A. Cappi, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Brera, Department of Astronomy, Cornell University, Infrared Processing Analysis Center, California Institute of Technology (IPAC), University of Sussex, Observatoire Astronomique de l'Université de Genève, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Milano), Spitzer Science Center, California Institute of Technology (SSC), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), IRA-INAF, Bologna, INAF-Osservatorio Astronomico di Bologna (OABO), Max-Planck-Institut für Astrophysik (MPA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, University of Nottingham, Astrophysikalisches Institut Potsdam (AIP), Institute for Astronomy, University of Hawaii, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), INTEGRAL Science Data Centre, INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), and Centro de Astrofisica da Universidade do Porto (CAUP)
Subjects: Physics, Star formation, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Correlation function (astronomy), Galaxy, Redshift, Luminosity, Photometry (optics), Stars, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cluster analysis, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Aims:By combining data from the VIMOS VLT Deep Survey (VVDS) with the Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), we have built the currently largest spectroscopic sample of high redshift galaxies selected in the rest-frame near-infrared. We have obtained 2040 spectroscopic redshifts of galaxies with (m3.6)_AB < 21.5 at 3.6 mu m, and 1255 spectroscopic redshifts of galaxies with (m4.5)_AB < 21. These allow us to investigate the clustering evolution of galaxies selected via their rest-frame near-infrared luminosity in the redshift range 0.2 < z < 2.1. Methods: We use the projected two-point correlation function w_p(r_p) to study the three dimensional clustering properties of galaxies detected at 3.6 mu m and 4.5 mu m with the InfraRed Array Camera (IRAC) in the SWIRE survey with measured spectroscopic redshifts from the first epoch VVDS. We compare these properties to those of a larger sample of 16672 SWIRE galaxies for which we have accurate photometric redshifts in the same field. Results: We find that in the 3.6 mu m and 4.5 mu m flux limited samples, the apparent correlation length does not change from redshift ~2 to the present. The measured correlation lengths have a mean value of r0 ~= 3.9±0.5 h-1 Mpc for the galaxies selected at 3.6 mu m and a mean value of r0 ~= 4.4±0.5 h-1 Mpc for the galaxies selected at 4.5 mu m, across the whole redshift range explored. These values are larger than those typicaly found for I-band selected galaxies at I_AB < 24, for which r0 varies from 2.69 h-1 Mpc to 3.63 h-1 Mpc between z = 0.5 to z = 2.1. We find that the difference in correlation length between I-band and 3.6-4.5 mum selected samples decreases with increasing redshift, becoming comparable at z ~= 1.5. We interpret this as evidence that galaxies with older stellar populations and galaxies actively forming stars reside in comparably over-dense environments at epochs earlier than z ~= 1.5, supporting the recently reported flattening of the color-density relation at high redshift. The increasing difference in correlation length with cosmic time observed between rest-frame UV-optical and near-infrared selected samples could then be an indication that star formation is gradually shifting to lower density regions with decreasing redshift, while the older, passively evolving galaxies remain in the most over-dense peaks.
Published: 2007

31. Stellar science from a blue wavelength range. A possible design for the blue arm of 4MOST

Author: Hansen, C., Ludwig, H.-G., Seifert, W., Koch, A., Xu, Wei-Jiang, Caffau, E., Christlieb, N., Korn, A., Lind, K., Sbordone, L., Ruchti, G., Feltzing, S., de Jong, R., Barden, S., Schnurr, O., European Organization for Nuclear Research (CERN), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Space Physics [Uppsala], Uppsala University, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Lund Observatory, and Lund University [Lund]
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Stars: abundances, FOS: Physical sciences, Techniques: spectroscopic, Instrumentation: spectrographs, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract: From stellar spectra, a variety of physical properties of stars can be derived. In particular, the chemical composition of stellar atmospheres can be inferred from absorption line analyses. These provide key information on large scales, such as the formation of our Galaxy, down to the small-scale nucleosynthesis processes that take place in stars and supernovae. By extending the observed wavelength range toward bluer wavelengths, we optimize such studies to also include critical absorption lines in metal-poor stars, and allow for studies of heavy elements (Z>38) whose formation processes remain poorly constrained. In this context, spectrographs optimized for observing blue wavelength ranges are essential, since many absorption lines at redder wavelengths are too weak to be detected in metal-poor stars. This means that some elements cannot be studied in the visual-redder regions, and important scientific tracers and science cases are lost. The present era of large public surveys will target millions of stars. Here we describe the requirements driving the design of the forthcoming survey instrument 4MOST, a multi-object spectrograph commissioned for the ESO VISTA 4m-telescope. We focus here on high-density, wide-area survey of stars and the science that can be achieved with high-resolution stellar spectroscopy. Scientific and technical requirements that governed the design are described along with a thorough line blending analysis. For the high-resolution spectrograph, we find that a sampling of >2.5 (pixels per resolving element), spectral resolution of 18000 or higher, and a wavelength range covering 393-436 nm, is the most well-balanced solution for the instrument. A spectrograph with these characteristics will enable accurate abundance analysis (+/-0.1 dex) in the blue and allow us to confront the outlined scientific questions. (abridged), 14 pages, 8 figures, accepted for publication in AN
Published: 2015

32. The Gaia-ESO Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities

Author: Annette M. N. Ferguson, Francesco Damiani, Gerard Gilmore, Angela Bragaglia, Martin Asplund, Giovanni Carraro, Vanessa Hill, L. Morbidelli, Paula Jofre, Antonio Frasca, Elena Pancino, A. C. Lanzafame, M. T. Costado, Bengt Edvardsson, A. Hourihane, Thomas Bensby, Antonella Vallenari, T. Prusti, Andreas Korn, Nicholas A. Walton, Carmela Lardo, Lorenzo Monaco, Sofia Feltzing, Ulrike Heiter, P. de Laverny, L. Prisinzano, Emilio J. Alfaro, C. Babusiaux, E. Franciosini, Clare Worley, Hans-Walter Rix, C. Allende Prieto, S. G. Sousa, Laura Magrini, Rodolfo Smiljanic, Christophe Martayan, G. G. Sacco, Maria Bergemann, P. Francois, R. J. Jackson, R. Blomme, Alejandra Recio-Blanco, Nigel Hambly, Sofia Randich, Karin Lind, Piercarlo Bonifacio, Gianni Marconi, R. D. Jeffries, Luca Sbordone, James R. Lewis, S. Van Eck, Amelia Bayo, James Binney, I. Neguerela, Simone Zaggia, Ettore Flaccomio, Janet E. Drew, Mike Irwin, Giuseppina Micela, Sergey E. Koposov, Thomas Masseron, Jackson R.J., Jeffries R.D., Lewis J., Koposov S.E., Sacco G.G., Randich S., Gilmore G., Asplund M., Binney J., Bonifacio P., Drew J.E., Feltzing S., Ferguson A.M.N., Micela G., Neguerela I., Prusti T., Rix H.-W., Vallenari A., Alfaro E.J., Allende Prieto C., Babusiaux C., Bensby T., Blomme R., Bragaglia A., Flaccomio E., Francois P., Hambly N., Irwin M., Korn A.J., Lanzafame A.C., Pancino E., Recio-Blanco A., Smiljanic R., Van Eck S., Walton N., Bayo A., Bergemann M., Carraro G., Costado M.T., Damiani F., Edvardsson B., Franciosini E., Frasca A., Heiter U., Hill V., Hourihane A., Jofre P., Lardo C., De Laverny P., Lind K., Magrini L., Marconi G., Martayan C., Masseron T., Monaco L., Morbidelli L., Prisinzano L., Sbordone L., Sousa S.G., Worley C.C., Zaggia S., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astrofísica Estelar (AE), Keele University [Keele], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics, Astronomy and Mathematics [Hatfield], University of Hertfordshire [Hatfield] (UH), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Agence Spatiale Européenne (ESA), European Space Agency (ESA), INAF - Osservatorio Astronomico di Padova (OAPD), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Royal Observatory of Belgium [Brussels] (ROB), INAF - Osservatorio Astronomico di Bologna (OABO), Institut de Mécanique des Fluides et des Solides (IMFS), École Nationale du Génie de l'Eau et de l'Environnement de Strasbourg (ENGEES)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), University of Turin, Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Metallicity, FOS: Physical sciences, stars: kinematics and dynamics, open clusters and associations: general, Open clusters and associations: general, Stars: kinematics and dynamics, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Normal distribution, Astronomi, astrofysik och kosmologi, Observatory, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), kinematics and dynamics [stars], QC, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, QB, Astronomía y Astrofísica, [PHYS]Physics [physics], Physics, Very Large Telescope, Kinematics and dynamics, Astrometry, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Satellite, Astrophysics::Earth and Planetary Astrophysics, general [open clusters and associations], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very Large Telescope. A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (v sin i) for representative samples of Galactic stars, that will complement information obtained by the Gaia astrometry satellite. We present an analysis to empirically quantify the size and distribution of uncertainties in RV and v sin i using spectra from repeated exposures of the same stars. We show that the uncertainties vary as simple scaling functions of signal-to-noise ratio (S/N) and v sin i, that the uncertainties become larger with increasing photospheric temperature, but that the dependence on stellar gravity, metallicity and age is weak. The underlying uncertainty distributions have extended tails that are better represented by Student's t-distributions than by normal distributions. Parametrised results are provided, that enable estimates of the RV precision for almost all GES measurements, and estimates of the v sin i precision for stars in young clusters, as a function of S/N, v sin i and stellar temperature. The precision of individual high S/N GES RV measurements is 0.22-0.26 km/s, dependent on instrumental configuration., 13 pages, accepted for publication in Astronomy & Astrophysics
Published: 2015

33. Gaia -ESO Survey: Analysis of pre-main sequence stellar spectra

Author: Antonio Frasca, G. G. Sacco, Ignacio Negueruela, Hugo M. Tabernero, Andreas Korn, Martin Asplund, C. Babusiaux, Loredana Prisinzano, Francesco Damiani, Nigel Hambly, M. T. Costado, G. Carraro, Gerry Gilmore, Giuseppina Micela, Emilio J. Alfaro, Piercarlo Bonifacio, Annette M. N. Ferguson, A. Hourihane, Maria Bergemann, N. A. Walton, E. Brugaletta, Manuel Meyer, John D. Lewis, H. W. Rix, Michael G. Irwin, Vardan Adibekyan, R. Blomme, P. Francois, R. D. Jeffries, A. C. Lanzafame, Sergey E. Koposov, Lorenzo Spina, James Binney, Thomas Masseron, L. Morbidelli, D. Montes, K. Biazzo, S. G. Sousa, Antonella Vallenari, Rodolfo Smiljanic, J. M. Alcalá, Thomas Bensby, C. Allende Prieto, Sergio Messina, Luca Sbordone, Amelia Bayo, A. Bragaglia, Simone Zaggia, C. C. Worley, Janet E. Drew, Ettore Flaccomio, S. Van Eck, Paula Jofre, Laura Magrini, Bengt Edvardsson, Gianni Marconi, J. I. González Hernández, Michiel Cottaar, Rosaria Bonito, Lorenzo Monaco, Ulrike Heiter, J. F. Gameiro, Carmela Lardo, Sofia Feltzing, E. Franciosini, T. Prusti, R. J. Jackson, Vanessa Hill, Sofia Randich, Karin Lind, Ch. Martayan, E. Delgado Mena, A. Klutsch, INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), University of Turin, INAF - Osservatorio Astrofisico di Arcetri (OAA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Keele University [Keele], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics, Astronomy and Mathematics [Hatfield], University of Hertfordshire [Hatfield] (UH), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astronomico di Palermo (OAPa), Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Señal [Alicante] (DFESTS), Universidad de Alicante, Agence Spatiale Européenne (ESA), European Space Agency (ESA), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Royal Observatory of Belgium [Brussels] (ROB), INAF - Osservatorio Astronomico di Bologna (OABO), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), Uppsala University, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lanzafame A.C., Frasca A., Damiani F., Franciosini E., Cottaar M., Sousa S.G., Tabernero H.M., Klutsch A., Spina L., Biazzo K., Prisinzano L., Sacco G.G., Randich S., Brugaletta E., Delgado Mena E., Adibekyan V., Montes D., Bonito R., Gameiro J.F., Alcala J.M., Gonzalez Hernandez J.I., Jeffries R., Messina S., Meyer M., Gilmore G., Asplund M., Binney J., Bonifacio P., Drew J.E., Feltzing S., Ferguson A.M.N., Micela G., Negueruela I., Prusti T., Rix H.-W., Vallenari A., Alfaro E.J., Allende Prieto C., Babusiaux C., Bensby T., Blomme R., Bragaglia A., Flaccomio E., Francois P., Hambly N., Irwin M., Koposov S.E., Korn A.J., Smiljanic R., Van Eck S., Walton N., Bayo A., Bergemann M., Carraro G., Costado M.T., Edvardsson B., Heiter U., Hill V., Hourihane A., Jackson R.J., Jofre P., Lardo C., Lewis J., Lind K., Magrini L., Marconi G., Martayan C., Masseron T., Monaco L., Morbidelli L., Sbordone L., Worley C.C., Zaggia S., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astrofísica Estelar (AE), Lanzafame, A., Frasca, A., Damiani, F., Franciosini, E., Cottaar, M., Sousa, S., Tabernero, H., Klutsch, A., Spina, L., Biazzo, K., Prisinzano, L., Sacco, G., Randich, S., Brugaletta, E., Delgado Mena, E., Adibekyan, V., Montes, D., Bonito, R., Gameiro, J., Alcalá, J., González Hernández, J., Jeffries, R., Messina, S., Meyer, M., Gilmore, G., Asplund, M., Binney, J., Bonifacio, P., Drew, J., Feltzing, S., Ferguson, A., Micela, G., Negueruela, I., Prusti, T., Rix, H., Vallenari, A., Alfaro, E., Allende Prieto, C., Babusiaux, C., Bensby, T., Blomme, R., Bragaglia, A., Flaccomio, E., Francois, P., Hambly, N., Irwin, M., Koposov, S., Korn, A., Smiljanic, R., Van Eck, S., Walton, N., Bayo, A., Bergemann, M., Carraro, G., Costado, M., Edvardsson, B., Heiter, U., Hill, V., Hourihane, A., Jackson, R., Jofré, P., Lardo, C., Lewis, J., Lind, K., Magrini, L., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Morbidelli, L., Sbordone, L., Worley, C., and Zaggia, S.
Subjects: Accuracy and precision, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, Surveys, fundamental parameters [Stars], Astronomical spectroscopy, surveys, Angular diameter, pre-main sequence [Stars], Astrophysics::Solar and Stellar Astrophysics, Survey, data analysis [Methods], education, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astronomía y Astrofísica, Physics, education.field_of_study, general [Open clusters and associations], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Stars: fundamental parameter, Astronomy and Astrophysic, Effective temperature, open clusters and associations: general, Surface gravity, methods: data analysis, Accretion (astrophysics), Stars, Astrophysics - Solar and Stellar Astrophysics, Methods: data analysis, Open clusters and associations: general, Stars: fundamental parameters, Stars: pre-main sequence, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters, Methods: data analysi
Abstract: This paper describes the analysis of UVES and GIRAFFE spectra acquired by the Gaia-ESO Public Spectroscopic Survey in the fields of young clusters whose population includes pre-main sequence (PMS) stars. Both methods that have been extensively used in the past and new ones developed in the contest of the Gaia-ESO survey enterprise are available and used. The internal precision of these quantities is estimated by inter-comparing the results obtained by such different methods, while the accuracy is estimated by comparison with independent external data, like effective temperature and surface gravity derived from angular diameter measurements, on a sample of benchmarks stars. Specific strategies are implemented to deal with fast rotation, accretion signatures, chromospheric activity, and veiling. The analysis carried out on spectra acquired in young clusters' fields during the first 18 months of observations, up to June 2013, is presented in preparation of the first release of advanced data products. Stellar parameters obtained with the higher resolution and larger wavelength coverage from UVES are reproduced with comparable accuracy and precision using the smaller wavelength range and lower resolution of the GIRAFFE setup adopted for young stars, which allows us to provide with confidence stellar parameters for the much larger GIRAFFE sample. Precisions are estimated to be $\approx$ 120 K r.m.s. in Teff, $\approx$0.3 dex r.m.s. in logg, and $\approx$0.15 dex r.m.s. in [Fe/H], for both the UVES and GIRAFFE setups., 22 pages, 18 figures, accepted for publication on A&A
Published: 2015

34. The ATLAS^(3D) project – XXIX. The new look of early-type galaxies and surrounding fields disclosed by extremely deep optical images

Author: Tom Oosterloo, Eric Emsellem, Frédéric Bournaud, Roger L. Davies, Harald Kuntschner, Leo Blitz, Jean-Charles Cuillandre, Sadegh Khochfar, Alison F. Crocker, Michele Cappellari, Thorsten Naab, Emin Karabal, Katherine Alatalo, Davor Krajnović, P. T. de Zeeuw, Martin Bureau, Marc Sarzi, Timothy A. Davis, Léo Michel-Dansac, Lisa M. Young, Nicholas Scott, Raffaella Morganti, Sanjaya Paudel, Richard M. McDermid, Pierre-Alain Duc, Paolo Serra, Anne-Marie Weijmans, Département de Physique Nucléaire (ex SPhN) (DPHN), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire de Paris, Université Paris sciences et lettres (PSL), European Southern Observatory (ESO), Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Infrared Processing Analysis Center, California Institute of Technology (IPAC), Department of Astronomy, University of California, Ritter Astrophysical Observatory, University of Toledo, Toledo, Observatoire de Lyon, University of Edinburgh, Astrophysikalisches Institut Potsdam (AIP), Department of Physics and Astronomy, Macquarie University, Netherlands Institute for Radio Astronomy (ASTRON), Max-Planck-Institut für Astrophysik (MPA), University of Hertfordshire [Hatfield] (UH), Sydney Institute for Astronomy (SIfA), School of Physics and Astronomy, University of St Andrews, Physics Department, New Mexico Institute of Mining and Technology, University of St Andrews. School of Physics and Astronomy, and Kapteyn Astronomical Institute
Subjects: FOS: Physical sciences, interactions [Galaxies], Astrophysics, Star count, Astrophysics::Cosmology and Extragalactic Astrophysics, elliptical and lenticular, cD [Galaxies], 01 natural sciences, law.invention, cD, Telescope, techniques: photometric, law, 0103 physical sciences, galaxies: interactions, QB Astronomy, Surface brightness, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Dwarf galaxy, Luminous infrared galaxy, Physics, 010308 nuclear & particles physics, Star formation, photometry [Galaxies], photometric [Techniques], Astronomy, Local Group, Astronomy and Astrophysics, 3rd-DAS, Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: photometry, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: stellar content, stellar content [Galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Galactic archeology based on star counts is instrumental to reconstruct the past mass assembly of Local Group galaxies. The development of new observing techniques and data-reduction, coupled with the use of sensitive large field of view cameras, now allows us to pursue this technique in more distant galaxies exploiting their diffuse low surface brightness (LSB) light. As part of the Atlas3D project, we have obtained with the MegaCam camera at the Canada-France Hawaii Telescope extremely deep, multi--band, images of nearby early-type galaxies. We present here a catalog of 92 galaxies from the Atlas3D sample, that are located in low to medium density environments. The observing strategy and data reduction pipeline, that achieve a gain of several magnitudes in the limiting surface brightness with respect to classical imaging surveys, are presented. The size and depth of the survey is compared to other recent deep imaging projects. The paper highlights the capability of LSB--optimized surveys at detecting new prominent structures that change the apparent morphology of galaxies. The intrinsic limitations of deep imaging observations are also discussed, among those, the contamination of the stellar halos of galaxies by extended ghost reflections, and the cirrus emission from Galactic dust. The detection and systematic census of fine structures that trace the present and past mass assembly of ETGs is one of the prime goals of the project. We provide specific examples of each type of observed structures -- tidal tails, stellar streams and shells --, and explain how they were identified and classified. We give an overview of the initial results. The detailed statistical analysis will be presented in future papers., Comment: MNRAS in press, On-line version of the catalog of galaxies with available deep images and figures (including navigation tools) are available from http://irfu.cea.fr/Projets/matlas/public/Atlas3D/atlas3d-pXXIX.html
Published: 2015

35. Combined CO and dust scaling relations of depletion time and molecular gas fractions with cosmic time, specific star-formation rate, and stellar mass

Author: Linda J. Tacconi, Fabian Walter, Jonathan Freundlich, Peter Timothy Cox, A. Burkert, P. Salomé, N. M. Förster Schreiber, Amelie Saintonge, Alberto Bolatto, Katarina Kovac, R. Neri, S. J. Lilly, Marcella Carollo, Reinhard Genzel, Stijn Wuyts, Magdalena Lippa, Javier Graciá-Carpio, Benjamin Magnelli, F. Bournaud, T. Naab, Chiara Feruglio, S. Berta, T. Contini, Luis Colina, Michael C. Cooper, Dieter Lutz, Ben Weiner, Frederic Boone, Alvio Renzini, Francoise Combes, Stéphanie Juneau, Jérémie Boissier, Axel Weiss, Amiel Sternberg, Nicolas Bouché, Santiago García-Burillo, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Max-Planck-Institut für Extraterrestrische Physik (MPE), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), OAN, Madrid, Observatorio Astronomico Nacional, Madrid, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Biologie et écologie tropicale et méditerranéenne (BETM), Université de Perpignan Via Domitia (UPVD)-École pratique des hautes études (EPHE)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universitätssternwarte der Ludwig-Maximiliansuniversität, Ludwig-Maximiliansuniversität, Department of Physics, Durham University, Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), AUTRES, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], Max-Planck-Institut für Astronomie (MPIA), Steward observatory, University of Arizona, Max-Planck-Institut für Extraterrestriche Physik (MPE), University College of London [London] (UCL), Rheinische Friedrich-Wilhelms-Universität Bonn, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Galaxies et cosmologie, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Department of Astronomy, University of Maryland, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy, Department of Physics, ETH Zürich, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Molecular and Infrared Astrophysics, Consejo Superior de Investigaciones Científicas (DAMIR/CSIC), Department of Physics and Astronomy, University of California, Atacama Large Millimeter Array (ALMA), Max-Planck-Institut für Astrophysik (MPA), INAF-Osservatorio Astronomico di Padova, Tel Aviv University (TAU), Steward Observatory, University of Arizona, Max-Planck-Institut für Radioastronomie (MPIfR), École normale supérieure - Paris (ENS Paris), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Biologie et écologie tropicale et méditerranéenne [2007-2010] (BETM), Université de Perpignan Via Domitia (UPVD)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Stellar mass, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Atomic, Physical Chemistry, Flattening, high-redshift [Galaxies], Particle and Plasma Physics, galaxies [Infrared], Astrophysics::Solar and Stellar Astrophysics, Nuclear, Scaling, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Range (particle radiation), Star formation, Gas depletion, kinematics and dynamics [Galaxies], Galaxies: high-redshift, Galaxies: kinematics and dynamics, Galaxies: evolution, Molecular, Astronomy and Astrophysics, Infrared: galaxies, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract: 25 pags.; 15 figs.; 5 tabs., © 2015. The American Astronomical Society. All rights reserved. We combine molecular gas masses inferred from CO emission in 500 star-forming galaxies (SFGs) between z = 0 and 3, from the IRAM-COLDGASS, PHIBSS1/2, and other surveys, with gas masses derived from Herschel far-IR dust measurements in 512 galaxy stacks over the same stellar mass/redshift range. We constrain the scaling relations of molecular gas depletion timescale (tdepl) and gas to stellar mass ratio (Mmol gas/M∗) of SFGs near the star formation >main-sequence> with redshift, specific star-formation rate (sSFR), and stellar mass (M∗). The CO- and dust-based scaling relations agree remarkably well. This suggests that the CO → H2 mass conversion factor varies little within ±0.6 dex of the main sequence (sSFR(ms, z, M∗)), and less than 0.3 dex throughout this redshift range. This study builds on and strengthens the results of earlier work. We find that tdepl scales as (1 + z)-0.3 × (sSFR/sSFR(ms, z, M∗))-0.5, with little dependence on M∗. The resulting steep redshift dependence of Mmol gas/M∗≈ (1 + z)3 mirrors that of the sSFR and probably reflects the gas supply rate. The decreasing gas fractions at high M∗are driven by the flattening of the SFR-M∗relation. Throughout the probed redshift range a combination of an increasing gas fraction and a decreasing depletion timescale causes a larger sSFR at constant M∗. As a result, galaxy integrated samples of the Mmol gas-SFR rate relation exhibit a super-linear slope, which increases with the range of sSFR. With these new relations it is now possible to determine Mmol gas with an accuracy of ±0.1 dex in relative terms, and ±0.2 dex including systematic uncertainties.
Published: 2015

36. Avoiding progenitor bias: The structural and mass evolution of Brightest Group and Cluster Galaxies in Hierarchical models since z~1

Author: Vincent Bouillot, Ravi K. Sheth, Simona Mei, Lauriane Delaye, Rossella Licitra, Begoña Ascaso, Marc Huertas-Company, Stewart Buchan, Alessandro Rettura, Anand Raichoor, Jorge Moreno, Mariangela Bernardi, Francesco Shankar, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Cosmologie: Origine et Structures, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Observatoire de Paris, Université Paris sciences et lettres (PSL), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, cosmology: theory, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Effective radius, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Halo, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The mass and structural evolution of massive galaxies is one of the hottest topics in galaxy formation. This is because it may reveal invaluable insights into the still debated evolutionary processes governing the growth and assembly of spheroids. However, direct comparison between models and observations is usually prevented by the so-called "progenitor bias", i.e., new galaxies entering the observational selection at later epochs, thus eluding a precise study of how pre-existing galaxies actually evolve in size. To limit this effect, we here gather data on high-redshift brightest group and cluster galaxies, evolve their (mean) host halo masses down to z=0 along their main progenitors, and assign as their "descendants" local SDSS central galaxies matched in host halo mass. At face value, the comparison between high redshift and local data suggests a noticeable increase in stellar mass of a factor of >2 since z~1, and of >2.5 in mean effective radius. We then compare the inferred stellar mass and size growth with those predicted by hierarchical models for central galaxies, selected at high redshifts to closely match the halo and stellar mass bins as in the data. Only hierarchical models characterized by very limited satellite stellar stripping and parabolic orbits are capable of broadly reproducing the stellar mass and size increase of a factor ~2-4 observed in cluster galaxies since z ~1. The predicted, average (major) merger rate since z~1 is in good agreement with the latest observational estimates., 9 pages, 5 figures. ApJ, in press. Additional (minor) editing included in text and figure captions
Published: 2015
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37. Spectrophotometric properties of galaxies at intermediate redshifts (z ~ 0.2–1.0)

Author: F. Lamareille, T. Contini, Jean-Francois Le Borgne, Stéphane Charlot, Jarle Brinchmann, Johan Richard, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto, and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, Metallicity, FOS: Physical sciences, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Stellar classification, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), galaxies: fundamental parameters, Astronomy and Astrophysics, Galaxy, Universe, Redshift, Space and Planetary Science, galaxies: abundances, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Data reduction
Abstract: We present the gas-phase oxygen abundance (O/H) for a sample of 131 star-forming galaxies at intermediate redshifts ($0.2, Comment: 19 pages. Accepted for publication on A&A; reference added; bug corrected: flux scaled by (1+z)
Published: 2006

38. The Ultraviolet Luminosity Function of GALEX Galaxies at Photometric Redshifts between 0.07 and 0.25

Author: B. F. Madore, Tom A. Barlow, Stéphane Charlot, Luciana Bianchi, Susan G. Neff, Young-Wook Lee, Peter G. Friedman, Ted K. Wyder, O. H. W. Siegmund, Patrick N. Jelinsky, Alexander S. Szalay, Roger F. Malina, R. M. Rich, T. Small, Y. I. Byun, Patrick Morrissey, Barry Y. Welsh, Marie Treyer, Jose Donas, Karl Forster, Stephane Arnouts, David Schiminovich, Timothy M. Heckman, Tamás Budavári, Mark Seibert, D. C. Martin, B. Milliard, Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, California Institute of Technology (CALTECH), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Center for Astrophysical Sciences [Baltimore], Center for Space Astrophysics [Seoul], Yonsei University, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center (GSFC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of California [Berkeley], and University of California-University of California
Subjects: media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, medicine.disease_cause, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Photometry (optics), 0103 physical sciences, medicine, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Luminosity function (astronomy), Physics, galaxies: evolution galaxies: luminosity function, 010308 nuclear & particles physics, Astrophysics (astro-ph), Late type, mass functiongalaxies: photometrysurveysultraviolet: galaxies, Astronomy and Astrophysics, Galaxy, Redshift, Space and Planetary Science, Sky, Ultraviolet
Abstract: We present measurements of the UV galaxy luminosity function and the evolution of luminosity density from GALEX observations matched to the Sloan Digital Sky Survey (SDSS). We analyze galaxies in the Medium Imaging Survey overlapping the SDSS DR1 with a total coverage of 44 deg^2. Using the combined GALEX+SDSS photometry, we compute photometric redshifts and study the LF in three redshift shells between z=0.07 and 0.25. The Schechter function fits indicate that the faint-end slope alpha is consistent with -1.1 at all redshifts but the characteristic UV luminosity M* brightens by 0.2 mag from z=0.07 to 0.25. In the lowest redshift bin, early and late type galaxies are studied separately and we confirm that red galaxies tend to be brighter and have a shallower slope alpha than blue ones. The derived luminosity densities are consistent with other GALEX results based on a local spectroscopic sample from 2dF and the evolution follows the trend reported by deeper studies., This paper will be published as part of the Galaxy Evolution Explorer (GALEX) Astrophysical Journal Letters Special Issue. Links to the full set of papers will be available at http://www.galex.caltech.edu/PUBLICATIONS/ after November 22, 2004
Published: 2005

39. Spectroscopy of clusters in the ESO Distant Cluster Survey (EDisCS)

Author: Alfonso Aragón-Salamanca, Bo Milvang-Jensen, R. Pello, C. Halliday, Luc Simard, Bianca M. Poggianti, G. De Lucia, Roberto P. Saglia, G. Rudnick, Simon D. M. White, P. Jablonka, S. Poirier, Julianne J. Dalcanton, D. Clowe, Dennis Zaritsky, INAF-Osservatorio Astronomico di Padova, Max-Planck-Institut für Extraterrestriche Physik (MPE), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, University of Nottingham, Max-Planck-Institut für Astrophysik (MPA), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), National Research Council of Canada (NRC), Rheinische Friedrich-Wilhelms-Universität Bonn, Department of Astronomy [Seattle], University of Washington [Seattle], and Steward Observatory, University of Arizona
Subjects: Physics, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Space and Planetary Science, Cluster (physics), Galaxy formation and evolution, Substructure, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Spectroscopy, Astrophysics::Galaxy Astrophysics, Data reduction
Abstract: International audience; We present spectroscopic observations of galaxies in 4 clusters at z = 0.7-0.8 and in one cluster at z ˜ 0.5 obtained with the FORS2 spectrograph on the VLT as part of the ESO Distant Cluster Survey (EDisCS), a photometric and spectroscopic survey of 20 intermediate to high redshift clusters. We describe our target selection, mask design, observation and data reduction procedures, using these first 5 clusters to demonstrate how our strategies maximise the number of cluster members for which we obtain spectroscopy. We present catalogues containing positions, I-band magnitudes and spectroscopic redshifts for galaxies in the fields of our 5 clusters. These contain 236 cluster members, with the number of members per cluster ranging from 30 to 67. Our spectroscopic success rate, i.e. the fraction of spectroscopic targets which are cluster members, averages 50% and ranges from 30% to 75%. We use a robust biweight estimator to measure cluster velocity dispersions from our spectroscopic redshift samples. We also make a first assessment of substructure within our clusters. The velocity dispersions range from 400 to 1100 km s-1. Some of the redshift distributions are significantly non-Gaussian and we find evidence for significant substructure in two clusters, one at z ˜ 0.79 and the other at z ˜ 0.54. Both have velocity dispersions exceeding 1000 km s-1 but are clearly not fully virialised; their velocity dispersions may thus be a poor indicator of their masses. The properties of these first 5 EDisCS clusters span a wide range in redshift, velocity dispersion, richness and substructure, but are representative of the sample as a whole. Spectroscopy for the full dataset will allow a comprehensive study of galaxy evolution as a function of cluster environment and redshift.
Published: 2004

40. The ATLAS3D project – XXVII. Cold gas and the colours and ages of early-type galaxies

Author: Roger L. Davies, Thorsten Naab, P. T. de Zeeuw, Martin Bureau, Marc Sarzi, Tom Oosterloo, Eric Emsellem, Sadegh Khochfar, M. Bois, Raffaella Morganti, Alison F. Crocker, Davor Krajnović, Katherine Alatalo, Michele Cappellari, Lisa M. Young, Paolo Serra, Nicholas Scott, Pierre-Alain Duc, Harald Kuntschner, E. Bayet, Leo Blitz, Timothy A. Davis, Richard M. McDermid, Frédéric Bournaud, Anne-Marie Weijmans, CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Department of Astronomy [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, European Southern Observatory (ESO), Max-Planck-Institut für Extraterrestrische Physik (MPE), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Netherlands Institute for Radio Astronomy (ASTRON), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, University of St Andrews. School of Physics and Astronomy, Kapteyn Astronomical Institute, University of California [Berkeley], University of California-University of California, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and University of Oxford [Oxford]-University of Oxford [Oxford]
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, structure [Galaxies], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, elliptical and lenticular, cD [Galaxies], 01 natural sciences, glaxies [Radio lines], cD, Peculiar galaxy, Galaxy group, ISM [Galaxies], 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, galaxies: elliptical and lenticular, Disc, 010303 astronomy & astrophysics, Lenticular galaxy, evolution [galaxies], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, QB, radio lines: galaxies, Luminous infrared galaxy, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, evolution [cD-galaxies], Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, galaxies [radio lines], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, galaxies: structure, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], elliptical and lenticular [galaxies], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a study of the cold gas contents of the Atlas3D early-type galaxies, in the context of their optical colours, near-UV colours, and H�� absorption line strengths. Early-type (elliptical and lenticular) galaxies are not as gas-poor as previously thought, and at least 40% of local early-type galaxies are now known to contain molecular and/or atomic gas. This cold gas offers the opportunity to study recent galaxy evolution through the processes of cold gas acquisition, consumption (star formation), and removal. Molecular and atomic gas detection rates range from 10% to 34% in red sequence early-type galaxies, depending on how the red sequence is defined, and from 50% to 70% in blue early-type galaxies. Notably, massive red sequence early-type galaxies (stellar masses > 5e10 Msun, derived from dynamical models) are found to have HI masses up to M(HI)/Mstar ~ 0.06 and H_2 masses up to M(H$_2$)/Mstar ~ 0.01. Some 20% of all massive early-type galaxies may have retained atomic and/or molecular gas through their transition to the red sequence. However, kinematic and metallicity signatures of external gas accretion (either from satellite galaxies or the intergalactic medium) are also common, particularly at stellar masses, 20 pages. Accepted for publication in MNRAS
Published: 2014

41. The ATLAS3D project - XXV: Two-dimensional kinematic analysis of simulated galaxies and the cosmological origin of fast and slow rotators

Author: Katherine Alatalo, Lisa M. Young, Timothy A. Davis, Peter H. Johansson, Davor Krajnović, Eric Emsellem, Nicholas Scott, Frédéric Bournaud, Michaela Hirschmann, Alison F. Crocker, E. Bayet, Michele Cappellari, Richard M. McDermid, G. van de Ven, Thorsten Naab, M. Bois, Leo Blitz, Sadegh Khochfar, Martin Bureau, Marc Sarzi, Pierre-Alain Duc, Roger L. Davies, Anne-Marie Weijmans, Raffaella Morganti, Ludwig Oser, P. T. de Zeeuw, Paolo Serra, Tom Oosterloo, Harald Kuntschner, University of St Andrews. School of Physics and Astronomy, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford [Oxford]-University of Oxford [Oxford], NASA Herschel Science Center, NASA-California Institute of Technology (CALTECH), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Columbia Astrophysics Laboratory (CAL), Columbia University [New York], Department of Earth Sciences [Oxford], University of Oxford [Oxford], CSA, Canadian Space Agency (CSA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Netherlands Institute for Radio Astronomy (ASTRON), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), University of St Andrews [Scotland], École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Oxford-University of Oxford, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH)-California Institute of Technology (CALTECH), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Oxford, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), and Kapteyn Astronomical Institute
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Rotation, Disc galaxy, cD, Peculiar galaxy, galaxies: formation, QB Astronomy, galaxies: elliptical and lenticular, galaxies: kinematics and dynamics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, formation [Stars], QC, QB, Physics, [PHYS]Physics [physics], Star formation, Astronomy, Velocity dispersion, Astronomy and Astrophysics, Galaxy, kinematics and dynamics [ISM], QC Physics, Space and Planetary Science, galaxies: structure, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], clouds [ISM], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a detailed two-dimensional stellar dynamical analysis of a sample of 44 cosmological hydrodynamical simulations of individual central galaxies and their satellites. Kinematic maps of the stellar line-of-sight velocity, velocity dispersion, and higher-order Gauss-Hermite moments $h_3$ and $h_4$ are constructed for each central galaxy and for the most massive satellites. The amount of rotation is quantified using the $\lambda_{\mathrm{R}}$-parameter. The velocity, velocity dispersion, $h_3$, and $h_4$ fields of the simulated galaxies show a diversity similar to observed kinematic maps of early-type galaxies in the ATLAS$^{\rm{3D}}$ survey. This includes fast (regular), slow, and misaligned rotation, hot spheroids with embedded cold disk components as well as galaxies with counter-rotating cores or central depressions in the velocity dispersion. We link the present day kinematic properties to the individual cosmological formation histories of the galaxies. In general, major galaxy mergers have a significant influence on the rotation properties resulting in both a spin-down as well as a spin-up of the merger remnant. Lower mass galaxies with significant in-situ formation of stars, or with additional gas-rich major mergers - resulting in a spin-up - in their formation history, form elongated fast rotators with a clear anti-correlation of $h_3$ and $v/\sigma$. An additional formation path for fast rotators includes gas poor major mergers leading to a spin-up of the remnants. This formation path does not result in anti-correlated $h_3$ and $v/\sigma$. The galaxies most consistent with the rare class of non-rotating round early-type galaxies grow by gas-poor minor mergers alone. In general, more massive galaxies have less in-situ star formation since $z \sim 2$, rotate slower and have older stellar populations. (shortened), Comment: Accepted for publication in MNRAS
Published: 2014

42. The Atlas3D project - XXIV. The intrinsic shape distribution of early-type galaxies

Author: Nicholas Scott, Katherine Alatalo, Timothy A. Davis, Sadegh Khochfar, M. Bois, Eric Emsellem, P. T. de Zeeuw, Pierre-Alain Duc, Raffaella Morganti, Anne-Marie Weijmans, Roger L. Davies, Harald Kuntschner, Michele Cappellari, Alison F. Crocker, Tom Oosterloo, Gijsbert Verdoes Kleijn, Davor Krajnović, Lisa M. Young, Thorsten Naab, Richard M. McDermid, Martin Bureau, Marc Sarzi, Paolo Serra, Leo Blitz, Frédéric Bournaud, P.-Y. Lablanche, Kapteyn Astronomical Institute, University of St Andrews. School of Physics and Astronomy, Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, European Southern Observatory (ESO), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, Max-Planck-Institut für Extraterrestrische Physik (MPE), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Netherlands Institute for Radio Astronomy (ASTRON), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), University of California [Berkeley], University of California-University of California, École normale supérieure - Paris (ENS Paris), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and University of Oxford [Oxford]-University of Oxford [Oxford]
Subjects: Gaussian, structure [Galaxies], Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, elliptical and lenticular, cD [Galaxies], Standard deviation, Flattening, law.invention, cD, symbols.namesake, law, QB Astronomy, galaxies: elliptical and lenticular, 10. No inequality, education, ComputingMilieux_MISCELLANEOUS, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, [PHYS]Physics [physics], education.field_of_study, Spiral galaxy, Newtonian telescope, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, symbols, galaxies: structure, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BDC
Abstract: We use the Atlas3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q=0.25 and standard deviation sigma_q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and sigma_q =0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrisations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial., 19 pages, 19 figures. Accepted for publication in MNRAS
Published: 2014

43. ACTIVE GALACTIC NUCLEI EMISSION LINE DIAGNOSTICS AND THE MASS-METALLICITY RELATION UP TO REDSHIFT z ∼ 2: THE IMPACT OF SELECTION EFFECTS AND EVOLUTION

Author: Raphael Gobat, Ingrid Jean-Baptiste, Emanuele Daddi, Emeric Le Floc'h, Jarle Brinchmann, C. Schreiber, M. D. Lehnert, Pierre-Alain Duc, Stéphane Charlot, Mark Dickinson, Frédéric Bournaud, Jonathan R. Trump, Stéphanie Juneau, Maurilio Pannella, David Elbaz, C. Pacifici, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), University of Connecticut (UCONN), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, [PHYS]Physics [physics], education.field_of_study, Active galactic nucleus, 010308 nuclear & particles physics, Metallicity, Population, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Stars, Space and Planetary Science, 0103 physical sciences, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Line (formation)
Abstract: Emission line diagnostic diagrams probing the ionization sources in galaxies, such as the Baldwin-Phillips-Terlevich (BPT) diagram, have been used extensively to distinguish active galactic nuclei (AGN) from purely star-forming galaxies. However, they remain poorly understood at higher redshifts. We shed light on this issue with an empirical approach based on a z ~ 0 reference sample built from ~300,000 Sloan Digital Sky Survey galaxies, from which we mimic selection effects due to typical emission line detection limits at higher redshift. We combine this low-redshift reference sample with a simple prescription for luminosity evolution of the global galaxy population to predict the loci of high-redshift galaxies on the BPT and Mass-Excitation (MEx) diagnostic diagrams. The predicted bivariate distributions agree remarkably well with direct observations of galaxies out to z ~ 1.5, including the observed stellar mass-metallicity (MZ) relation evolution. As a result, we infer that high-redshift star-forming galaxies are consistent with having normal interstellar medium (ISM) properties out to z ~ 1.5, after accounting for selection effects and line luminosity evolution. Namely, their optical line ratios and gas-phase metallicities are comparable to that of low-redshift galaxies with equivalent emission-line luminosities. In contrast, AGN narrow-line regions may show a shift toward lower metallicities at higher redshift. While a physical evolution of the ISM conditions is not ruled out for purely star-forming galaxies and may be more important starting at z 2, we find that reliably quantifying this evolution is hindered by selections effects. The recipes provided here may serve as a basis for future studies toward this goal. Code to predict the loci of galaxies on the BPT and MEx diagnostic diagrams and the MZ relation as a function of emission line luminosity limits is made publicly available.
Published: 2014

44. TESTING THE ASTEROSEISMIC MASS SCALE USING METAL-POOR STARS CHARACTERIZED WITH APOGEE AND KEPLER

Author: Savita Mathur, Peter M. Frinchaboy, Fred R. Hearty, Benoit Mosser, Courtney R. Epstein, Keivan G. Stassun, Aldo Serenelli, Paul Harding, Victor Silva Aguirre, Dennis Stello, Jamie Tayar, Timothy R. Bedding, Timothy C. Beers, Ricardo P. Schiavon, Sarbani Basu, Inese I. Ivans, Marc H. Pinsonneault, Daniel Huber, Ralph Schönrich, Rafael A. García, Dmitry Bizyaev, Steven R. Majewski, Yvonne Elsworth, Matthew Shetrone, William J. Chaplin, Gail Zasowski, David L. Nidever, Donald P. Schneider, Jennifer A. Johnson, Saskia Hekker, Ana G. Pérez, Jennifer Sobeck, School of Physics and Astronomy [Birmingham], University of Birmingham [Birmingham], J. A. Baker Institute, Cornell University [New York], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, National University of Singapore (NUS), Sydney Institute for Astronomy (SIfA), The University of Sydney, Department of Psychology, St John's University, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional de Costa Rica, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Pennsylvania State University (Penn State), Penn State System, Vanderbilt University [Nashville], Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: media_common.quotation_subject, fundamental parameters [stars], FOS: Physical sciences, Astrophysics, asteroseismology, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, Asteroseismology, Spitzer Space Telescope, halo [Galaxy], Astrophysics::Solar and Stellar Astrophysics, Scaling, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Physics, [PHYS]Physics [physics], Astronomy and Astrophysics, Radius, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Sky, Magnitude (astronomy), Halo, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Fundamental stellar properties, such as mass, radius, and age, can be inferred using asteroseismology. Cool stars with convective envelopes have turbulent motions that can stochastically drive and damp pulsations. The properties of the oscillation frequency power spectrum can be tied to mass and radius through solar-scaled asteroseismic relations. Stellar properties derived using these scaling relations need verification over a range of metallicities. Because the age and mass of halo stars are well-constrained by astrophysical priors, they provide an independent, empirical check on asteroseismic mass estimates in the low-metallicity regime. We identify nine metal-poor red giants (including six stars that are kinematically associated with the halo) from a sample observed by both the Kepler space telescope and the Sloan Digital Sky Survey-III APOGEE spectroscopic survey. We compare masses inferred using asteroseismology to those expected for halo and thick-disk stars. Although our sample is small, standard scaling relations, combined with asteroseismic parameters from the APOKASC Catalog, produce masses that are systematically higher (=0.17+/-0.05 Msun) than astrophysical expectations. The magnitude of the mass discrepancy is reduced by known theoretical corrections to the measured large frequency separation scaling relationship. Using alternative methods for measuring asteroseismic parameters induces systematic shifts at the 0.04 Msun level. We also compare published asteroseismic analyses with scaling relationship masses to examine the impact of using the frequency of maximum power as a constraint. Upcoming APOKASC observations will provide a larger sample of ~100 metal-poor stars, important for detailed asteroseismic characterization of Galactic stellar populations., Comment: 4 figures; 1 table. Accepted to ApJL
Published: 2014

45. NGC 1266 AS A LOCAL CANDIDATE FOR RAPID CESSATION OF STAR FORMATION

Author: Katherine Alatalo, Kristina Nyland, Genevieve Graves, Susana Deustua, Kristen Shapiro Griffin, Pierre-Alain Duc, Michele Cappellari, Richard M. McDermid, Timothy A. Davis, Alison F. Crocker, Lisa M. Young, Philip Chang, Nicholas Scott, Sabrina L. Cales, Estelle Bayet, Leo Blitz, Maxime Bois, Frédéric Bournaud, Martin Bureau, Roger L. Davies, P. T. de Zeeuw, Eric Emsellem, Sadegh Khochfar, Davor Krajnović, Harald Kuntschner, Raffaella Morganti, Thorsten Naab, Tom Oosterloo, Marc Sarzi, Paolo Serra, Anne-Marie Weijmans, Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford [Oxford]-University of Oxford [Oxford], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), European Southern Observatory (ESO), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Netherlands Institute for Radio Astronomy (ASTRON), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Oxford-University of Oxford, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Astronomy, and University of St Andrews. School of Physics and Astronomy
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), active [Galaxies], Stellar population, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, galaxies: individual: NGC 1266, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Disc, Spectroscopy, education, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, individual: NGC 1266 [Galaxies], QB, Line (formation), Physics, [PHYS]Physics [physics], education.field_of_study, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, evolution [Galaxies], Galaxy, QC Physics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present new Spectrographic Areal Unit for Research on Optical Nebulae (SAURON) integral-field spectroscopy and Swift Ultraviolet Optical Telescope (UVOT) observations of molecular outflow host galaxy NGC 1266 that indicate NGC 1266 has experienced a rapid cessation of star formation. Both the SAURON maps of stellar population age and the Swift UVOT observations demonstrate the presence of young ($< 1$ Gyr) stellar populations within the central 1 kpc, while existing Combined Array for Research in Millimeter-wave Astronomy (CARMA) CO(1--0) maps indicate that the sites of current star formation are constrained to the inner few hundred parsecs of the galaxy only. The optical spectrum of NGC 1266 from Moustakas & Kennicutt (2006) reveal a characteristic post-starburst (K+A) stellar population and Davis et al. (2012) confirm that ionized gas emission in the system originate from a shock. Galaxies with K+A spectra and shock-like ionized gas line ratios may comprise an important, overlooked segment of the post-starburst population, containing exactly those objects in which the AGN is actively expelling the star-forming material. While AGN activity is not the likely driver of the post-starburst event that occurred 500 Myr ago, the faint spiral structure seen in the Hubble Space Telescope (HST) Wide-field Camera 3 (WFC3) Y-, J- and H-band imaging seems to point to the possibility of gravitational torques being the culprit. If the molecular gas were driven into the center at the same time as the larger scale galaxy disk underwent quenching, the AGN might be able to sustain the presence of molecular gas for $\gtrsim 1$ Gyr by cyclically injecting turbulent kinetic energy into the dense molecular gas via a radio jet, inhibiting star formation., 11 pages, 7 figures, accepted by the Astrophysical Journal
Published: 2014

46. THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS

Author: David L. Nidever, Travis S. Metcalfe, D. A. García-Hernández, Jennifer A. Johnson, Rafael A. García, Donald P. Schneider, Carlos Allende Prieto, Daniel Huber, Saskia Hekker, Steven Bloemen, Andrea Miglio, Fred R. Hearty, Marc H. Pinsonneault, Courtney R. Epstein, Ronald L. Gilliland, Thomas Kallinger, Gail Zasowski, Jon Holtzman, Demitri Muna, Dmitry Bizyaev, Verne V. Smith, Savita Mathur, Peter M. Frinchaboy, Sarbani Basu, Paul Harding, Olga Zamora, William J. Chaplin, Matthew Shetrone, Sz. Meszaros, Aldo Serenelli, Jamie Tayar, Steven R. Majewski, Ana G. Pérez, Inese I. Ivans, Léo Girardi, Benoit Mosser, Paul G. Beck, Deokkeun An, Dennis Stello, Timothy C. Beers, Victor Silva Aguirre, Jo Bovy, Yvonne Elsworth, Katia Cunha, Joris De Ridder, Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), School of Physics and Astronomy, University of Birmingham [Birmingham], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], Department of Psychology, St John's University, J. A. Baker Institute, Cornell University [New York], Research institute of Computer Vision and Robotics [Girona] (VICOROB), Universitat de Girona (UdG), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max-Planck-Institut für Astrophysik (MPA), National University of Singapore (NUS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Sydney Institute for Astronomy (SIfA), The University of Sydney, Département des Sciences et Gestion de l'Environnement/Océanologie [Liège], Université de Liège, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pennsylvania State University (Penn State), Penn State System, Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Max-Planck-Institut für Sonnensystemforschung (MPS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: RED-GIANT STARS, NGC 6791, oscillations (including pulsations) [stars], Metallicity, Astronomy, fundamental parameters [stars], PHOTOMETRIC SYSTEM, Extinction (astronomy), FOS: Physical sciences, MILKY-WAY DISK, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Asteroseismology, Kepler Input Catalog, surveys, Observatory, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], STELLAR EVOLUTION CODE, GALACTIC CHEMICAL EVOLUTION, Astronomy and Astrophysics, Observable, Radius, Effective temperature, abundances [stars], FUNDAMENTAL PROPERTIES, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, OPEN CLUSTERS, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SOLAR-LIKE OSCILLATIONS, MAIN-SEQUENCE STARS, catalogs
Abstract: We present the first APOKASC catalog of spectroscopic and asteroseismic properties of 1916 red giants observed in the Kepler fields. The spectroscopic parameters provided from the Apache Point Observatory Galactic Evolution Experiment project are complemented with asteroseismic surface gravities, masses, radii, and mean densities determined by members of the Kepler Asteroseismology Science Consortium. We assess both random and systematic sources of error and include a discussion of sample selection for giants in the Kepler fields. Total uncertainties in the main catalog properties are of order 80 K in Teff , 0.06 dex in [M/H], 0.014 dex in log g, and 12% and 5% in mass and radius, respectively; these reflect a combination of systematic and random errors. Asteroseismic surface gravities are substantially more precise and accurate than spectroscopic ones, and we find good agreement between their mean values and the calibrated spectroscopic surface gravities. There are, however, systematic underlying trends with Teff and log g. Our effective temperature scale is between 0-200 K cooler than that expected from the Infrared Flux Method, depending on the adopted extinction map, which provides evidence for a lower value on average than that inferred for the Kepler Input Catalog (KIC). We find a reasonable correspondence between the photometric KIC and spectroscopic APOKASC metallicity scales, with increased dispersion in KIC metallicities as the absolute metal abundance decreases, and offsets in Teff and log g consistent with those derived in the literature. We present mean fitting relations between APOKASC and KIC observables and discuss future prospects, strengths, and limitations of the catalog data., Comment: 49 pages. ApJSupp, in press. Full machine-readable ascii files available under ancillary data. Categories: Kepler targets, asteroseismology, large spectroscopic surveys
Published: 2014

47. The ATLAS3D Project - XXVIII. Dynamically-driven star formation suppression in early-type galaxies

Author: Eric Emsellem, Frédéric Bournaud, Sadegh Khochfar, Alison F. Crocker, Katherine Alatalo, Davor Krajnović, Leo Blitz, Lisa M. Young, Roger L. Davies, Harald Kuntschner, Michele Cappellari, M. Bois, Richard M. McDermid, Thorsten Naab, Martin Bureau, Marc Sarzi, Anne-Marie Weijmans, Pierre-Alain Duc, Nicholas Scott, E. Bayet, Timothy A. Davis, P. T. de Zeeuw, Tom Oosterloo, Raffaella Morganti, Paolo Serra, University of St Andrews. School of Physics and Astronomy, Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford [Oxford]-University of Oxford [Oxford], Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, European Southern Observatory (ESO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Max-Planck-Institut für Extraterrestrische Physik (MPE), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Netherlands Institute for Radio Astronomy (ASTRON), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, Kapteyn Astronomical Institute, University of Oxford-University of Oxford, University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, elliptical and lenticular, cD [Galaxies], Peculiar galaxy, cD, ISM [Galaxies], Galaxy formation and evolution, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, galaxies: elliptical and lenticular, Lenticular galaxy, ComputingMilieux_MISCELLANEOUS, molecules [ISM], QC, Astrophysics::Galaxy Astrophysics, QB, [PHYS]Physics [physics], Physics, Luminous infrared galaxy, Spiral galaxy, mass-loss [Stars], Star formation, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, ISM: molecules, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], stars: mass-loss, galaxies: ISM
Abstract: We present measurements of the star formation rate (SFR) in the early-type galaxies (ETGs) of the ATLAS3D sample, based on Wide-field Infrared Survey Explorer (WISE) 22um and Galaxy Evolution Explorer (GALEX) far-ultraviolet emission. We combine these with gas masses estimated from 12CO and HI data in order to investigate the star formation efficiency (SFE) in a larger sample of ETGs than previously available. We first recalibrate (based on WISE data) the relation between old stellar populations (traced at Ks-band) and 22um luminosity, allowing us to remove the contribution of 22um emission from circumstellar dust. We then go on to investigate the position of ETGs on the Kennicutt-Schmidt (KS) relation. Molecular gas-rich ETGs have comparable star formation surface densities to normal spiral galaxy centres, but they lie systematically offset from the KS relation, having lower star formation efficiencies by a factor of ~2.5 (in agreement with other authors). This effect is driven by galaxies where a substantial fraction of the molecular material is in the rising part of the rotation curve, and shear is high. We show here for the first time that although the number of stars formed per unit gas mass per unit time is lower in ETGs, it seems that the amount of stars formed per free-fall time is approximately constant. The scatter around this dynamical relation still correlates with galaxy properties such as the shape of the potential in the inner regions. This leads us to suggest that dynamical properties (such as shear or the global stability of the gas) may be important second parameters that regulate star formation and cause much of the scatter around star-formation relations., Comment: 16 (+4) pages, 10 figures, accepted for publication in MNRAS
Published: 2014
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48. The APOGEE red-clump catalog: Precise distances, velocities, and high-resolution elemental abundances over a large area of the Milky Way's disk

Author: David L. Nidever, Hans-Walter Rix, Audrey Simmons, Marc H. Pinsonneault, Dmitry Bizyaev, Donald P. Schneider, Rafael A. García, L. Koesterke, Jennifer A. Johnson, John C. Wilson, Gail Zasowski, Peter M. Frinchaboy, Saskia Hekker, William J. Chaplin, Verne V. Smith, Léo Girardi, Robert W. O'Connell, Katia Cunha, Sarbani Basu, Keivan G. Stassun, Aldo Serenelli, Steven R. Majewski, Olga Zamora, D. A. García-Hernández, Jon A. Holtzman, Thomas Kallinger, Matthew Shetrone, Annie C. Robin, Kaike Pan, Carlos Allende Prieto, Szabolcs Mészáros, Benoit Mosser, Ana G. Pérez, Brett H. Andrews, Daniel Oravetz, Fred R. Hearty, David H. Weinberg, Michael F. Skrutskie, Dennis Stello, Thaíse S. Rodrigues, Ricardo P. Schiavon, Mathias Schultheis, Courtney R. Epstein, Adam Burton, Michael R. Hayden, S. Drew Chojnowski, Timothy C. Beers, Karen Kinemuchi, Yvonne Elsworth, Victor Silva Aguirre, Jo Bovy, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, J. A. Baker Institute, Cornell University [New York], Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], National University of Singapore (NUS), Department of Psychology, St John's University, School of Physics and Astronomy, University of Birmingham [Birmingham], Research institute of Computer Vision and Robotics [Girona] (VICOROB), Universitat de Girona (UdG), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pennsylvania State University (Penn State), Penn State System, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Max-Planck-Institut für Astrophysik (MPA), Vanderbilt University [Nashville], World Bank, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Proper motion, Metallicity, Milky Way, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Asteroseismology, Galaxy: disk, Bulge, 0103 physical sciences, distances [stars], stellar content [Galaxy], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Red clump, Galaxy: structure, stars: general, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, [PHYS]Physics [physics], Galaxy: stellar content, 010308 nuclear & particles physics, general [stars], Astrophysics::Instrumentation and Methods for Astrophysics, abundances [Galaxy], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), stars: distances, Galaxy: abundances, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], disk [Galaxy], structure [Galaxy]
Abstract: International audience; The Sloan Digital Sky Survey III's Apache Point Observatory Galactic Evolution Experiment (APOGEE) is a high-resolution near-infrared spectroscopic survey covering all of the major components of the Galaxy, including the dust-obscured regions of the inner Milky Way disk and bulge. Here we present a sample of 10,341 likely red-clump stars (RC) from the first two years of APOGEE operations, selected based on their position in color–metallicity–surface-gravity–effective-temperature space using a new method calibrated using stellar evolution models and high-quality asteroseismology data. The narrowness of the RC locus in color–metallicity–luminosity space allows us to assign distances to the stars with an accuracy of 5%–10%. The sample extends to typical distances of about 3 kpc from the Sun, with some stars out to 8 kpc, and spans a volume of approximately 100 kpc3 over 5 kpc ≲ R ≲ 14 kpc, |Z| ≲ 2 kpc, and −15° ≲ Galactocentric azimuth ≲ 30°. The APOGEE red-clump (APOGEE-RC) catalog contains photometry from the Two Micron All Sky Survey, reddening estimates, distances, line-of-sight velocities, stellar parameters and elemental abundances determined from the high-resolution APOGEE spectra, and matches to major proper motion catalogs. We determine the survey selection function for this data set and discuss how the RC selection samples the underlying stellar populations. We use this sample to limit any azimuthal variations in the median metallicity within the ≈45° azimuthal region covered by the current sample to be ⩽0.02 dex, which is more than an order of magnitude smaller than the radial metallicity gradient. This result constrains coherent non-axisymmetric flows within a few kiloparsecs from the Sun.
Published: 2014

49. The ATLAS3D project – XVIII. CARMA CO imaging survey of early-type galaxies

Author: Leo Blitz, Thorsten Naab, Frédéric Bournaud, Katherine Alatalo, Sadegh Khochfar, Lisa M. Young, Paolo Serra, Martin Bureau, Marc Sarzi, Raffaella Morganti, Michele Cappellari, P. T. de Zeeuw, Timothy A. Davis, M. Bois, Nicholas Scott, Davor Krajnović, Eric Emsellem, Harald Kuntschner, E. Bayet, Roger L. Davies, Alison F. Crocker, Pierre Yves Lablanche, Richard M. McDermid, Pierre-Alain Duc, Anne-Marie Weijmans, Tom Oosterloo, Department of Astronomy [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Department of Computer and Information Science and Engineering [Gainesville] (UF|CISE), University of Florida [Gainesville] (UF), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, Dept of physics and astrophysics, University College of London [London] (UCL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, European Southern Observatory (ESO), Max-Planck-Institut für Extraterrestrische Physik (MPE), Netherlands Institute for Radio Astronomy (ASTRON), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Centre for Astrophysics & Supercomputing, Swinburne University of Technology [Melbourne], NASA Ames Research Center (ARC), Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, University of California [Berkeley], University of California-University of California, University of Oxford [Oxford]-University of Oxford [Oxford], École normale supérieure - Paris (ENS Paris), and Kapteyn Astronomical Institute
Subjects: MAGNITUDE RELATION, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, BAR DIAGNOSTICS, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, cD, STAR-FORMATION, surveys, ELLIPTIC GALAXIES, 0103 physical sciences, NEARBY GALAXIES, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, LOPSIDED SPIRAL GALAXIES, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Spiral galaxy, 010308 nuclear & particles physics, Star formation, Astronomy, Astronomy and Astrophysics, VIRGO CLUSTER, Virgo Cluster, ISM: molecules, MOLECULAR GAS, Galaxy, NEUTRAL HYDROGEN, Interstellar medium, Space and Planetary Science, galaxies: star formation, Millimeter, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, INTERSTELLAR MATTER, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the Combined Array for Research in Millimeter Astronomy (CARMA) ATLAS3D molecular gas imaging survey, a systematic study of the distribution and kinematics of molecular gas in CO-rich early-type galaxies. Our full sample of 40 galaxies (30 newly mapped and 10 taken from the literature) is complete to a 12CO(1-0) integrated flux of 18.5 Jy km/s, and it represents the largest, best-studied sample of its type to date. A comparison of the CO distribution of each galaxy to the g-r color image (representing dust) shows that the molecular gas and dust distributions are in good agreement and trace the same underlying interstellar medium. The galaxies exhibit a variety of CO morphologies, including discs (50%), rings (15%), bars+rings (10%), spiral arms (5%), and mildly (12.5%) and strongly (7.5%) disrupted morphologies. There appear to be weak trends between galaxy mass and CO morphology, whereby the most massive galaxies in the sample tend to have molecular gas in a disc morphology. We derive a lower limit to the total accreted molecular gas mass across the sample of 2.48x10^10 Msuns, or approximately 8.3x10^8 Msuns per minor merger within the sample, consistent with minor merger stellar mass ratios., Comment: 52 pages, 5 figures (+ 33 appendix figures), MNRAS, accepted
Published: 2013

50. The ATLAS(3D) project: XXII. Low-efficiency star formation in early-type galaxies: hydrodynamic models and observations

Author: Harald Kuntschner, Katherine Alatalo, Frédéric Bournaud, Pierre-Alain Duc, Avishai Dekel, M. Bois, P. T. de Zeeuw, Anne-Marie Weijmans, Raffaella Morganti, Timothy A. Davis, Eric Emsellem, Nicholas Scott, Kristen Shapiro Griffin, Leo Blitz, Paolo Serra, Lisa M. Young, Tom Oosterloo, Alison F. Crocker, Roger L. Davies, Richard M. McDermid, Thorsten Naab, Romain Teyssier, Martin Bureau, Marc Sarzi, Jesús Falcón-Barroso, Michele Cappellari, J. M. Gabor, Sadegh Khochfar, Davor Krajnović, Marie Martig, Kapteyn Astronomical Institute, Centre for Astrophysics and Supercomputing, Swinburne University of Technology [Melbourne], Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, European Southern Observatory (ESO), CEA/DSM Centre de Saclay (CEA/DSM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, Department of Computer and Information Science and Engineering [Gainesville] (UF|CISE), University of Florida [Gainesville] (UF), Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), Max-Planck-Institut für Extraterrestrische Physik (MPE), Netherlands Institute for Radio Astronomy (ASTRON), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Centre for Astrophysics & Supercomputing, NASA Ames Research Center (ARC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Dunlap Institute for Astronomy and Astrophysics [Toronto], University of Toronto, University of California [Berkeley], University of California-University of California, École normale supérieure - Paris (ENS Paris), University of Oxford [Oxford]-University of Oxford [Oxford], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), INITIAL MASS FUNCTION, IRAM LEGACY SURVEY, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, 01 natural sciences, Peculiar galaxy, cD, CO-TO-H-2 CONVERSION FACTOR, Bulge, ELLIPTIC GALAXIES, MOLECULAR INTERSTELLAR-MEDIUM, 0103 physical sciences, TO-LIGHT RATIO, Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, Disc, galaxies: elliptical and lenticular, 010303 astronomy & astrophysics, Lenticular galaxy, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, Luminous infrared galaxy, [PHYS]Physics [physics], 010308 nuclear & particles physics, Star formation, Astronomy, Astronomy and Astrophysics, Space and Planetary Science, galaxies: star formation, Elliptical galaxy, MULTI-GAUSSIAN EXPANSION, Astrophysics::Earth and Planetary Astrophysics, HIGH-REDSHIFT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the global efficiency of star formation in high resolution hydrodynamical simulations of gas discs embedded in isolated early-type and spiral galaxies. Despite using a universal local law to form stars in the simulations, we find that the early-type galaxies are offset from the spirals on the large-scale Kennicutt relation, and form stars 2 to 5 times less efficiently. This offset is in agreement with previous results on morphological quenching: gas discs are more stable against star formation when embedded in early-type galaxies due to the lower disc self-gravity and increased shear. As a result, these gas discs do not fragment into dense clumps and do not reach as high densities as in the spiral galaxies. Even if some molecular gas is present, the fraction of very dense gas (above 10^4 cm-3) is significantly reduced, which explains the overall lower star formation efficiency. We also analyse a sample of local early-type and spiral galaxies, measuring their CO and HI surface densities and their star formation rates as determined by their non-stellar 8um emission. As predicted by the simulations, we find that the early-type galaxies are offset from the Kennicutt relation compared to the spirals, with a twice lower efficiency. Finally, we validate our approach by performing a direct comparison between models and observations. We run a simulation designed to mimic the stellar and gaseous properties of NGC524, a lenticular galaxy, and find a gas disc structure and global star formation rate in good agreement with the observations. Morphological quenching thus seems to be a robust mechanism, and is also consistent with other observations of a reduced star formation efficiency in early-type galaxies in the COLD GASS survey. This lower efficiency of star formation is not enough to explain the formation of the whole Red Sequence, but can contribute to the reddening of some galaxies., Comment: 15 pages, 8 figures, accepted for publication in MNRAS
Published: 2013

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