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4. THE DISTANCE TO M104

Author

Kennicutt, Robert [Institute for Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA (United Kingdom)]

Published
2016
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5. Gaia Data Release 3: Analysis of the Gaia BP/RP spectra using the General Stellar Parameterizer from Photometry

Author

Andrae, R., Fouesneau, M., Sordo, R., Bailer-Jones, C. A. L., Dharmawardena, T. E., Rybizki, J., De Angeli, F., Lindstrøm, H. E. P., Marshall, D. J., Drimmel, R., Korn, A. J., Soubiran, C., Brouillet, N., Casamiquela, L., Rix, H. -W., Aramburu, A. Abreu, Álvarez, M. A., Bakker, J., Bellas-Velidis, I., Bijaoui, A., Brugaletta, E., Burlacu, A., Carballo, R., Chaoul, L., Chiavassa, A., Contursi, G., Cooper, W. J., Creevey, O. L., Dafonte, C., Dapergolas, A., de Laverny, P., Delchambre, L., Demouchy, C., Edvardsson, B., Frémat, Y., Garabato, D., García-Lario, P., García-Torres, M., Gavel, A., Gomez, A., González-Santamaría, I., Hatzidimitriou, D., Heiter, U., Piccolo, A. Jean-Antoine, Kontizas, M., Kordopatis, G., Lanzafame, A. C., Lebreton, Y., Licata, E. L., Livanou, E., Lobel, A., Lorca, A., Romeo, A. Magdaleno, Manteiga, M., Marocco, F., Mary, N., Nicolas, C., Ordenovic, C., Pailler, F., Palicio, P. A., Pallas-Quintela, L., Panem, C., Pichon, B., Poggio, E., Recio-Blanco, A., Riclet, F., Robin, C., Santoveña, R., Sarro, L. M., Schultheis, M. S., Segol, M., Silvelo, A., Slezak, I., Smart, R. L., Süveges, M., Thévenin, F., Elipe, G. Torralba, Ulla, A., Utrilla, E., Vallenari, A., van Dillen, E., Zhao, H., Zorec, J., Max Planck Institute for Astronomy (MPIA), Max-Planck Institute for Astronomy, Konigstuhl 17, D-69117, Heidelberg, Germany, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Astronomie (MPIA), Institute of Astronomy, University of Cambridge (IoA), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), 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 Nazionale di Astrofisica, Torino, Italy, Department of Astronomy and Space Physics [Uppsala], Uppsala University, Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), M2A 2018, Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), UNIVERSITY OF HULL IECS GBR, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Conservation Ecology, Groningen Institute for Evolutionary Life Sciences (GELIFES), University of Groningen, Groningen, The Netherlands, National Observatory of Athens (NOA), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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), 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), Institut de Physique de Rennes (IPR), and Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)

Subjects
stars: fundamental parameters -methods: data analysis, Astrophysics - Solar and Stellar Astrophysics, surveys, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, statistical, Solar and Stellar Astrophysics (astro-ph.SR), catalogs, stars: fundamental parameters -methods: data analysis statistical surveys catalogs
Abstract

We present the General Stellar Parameterizer from Photometry (GSP-Phot), which is part of the astrophysical parameters inference system (Apsis). GSP-Phot is designed to produce a homogeneous catalogue of parameters for hundreds of millions of single non-variable stars based on their astrometry, photometry, and low-resolution BP/RP spectra. These parameters are effective temperature, surface gravity, metallicity, absolute $M_G$ magnitude, radius, distance, and extinction for each star. GSP-Phot uses a Bayesian forward-modelling approach to simultaneously fit the BP/RP spectrum, parallax, and apparent $G$ magnitude. A major design feature of GSP-Phot is the use of the apparent flux levels of BP/RP spectra to derive, in combination with isochrone models, tight observational constraints on radii and distances. We carefully validate the uncertainty estimates by exploiting repeat Gaia observations of the same source. The data release includes GSP-Phot results for 471 million sources with $G20$), mostly within 2kpc. Metallicity estimates exhibit substantial biases compared to literature values and are only useful at a qualitative level. However, we provide an empirical calibration of our metallicity estimates that largely removes these biases. Extinctions $A_0$ and $A_{\rm BP}$ show typical differences from reference values of 0.07-0.09 mag. MCMC samples of the parameters are also available for 95% of the sources. GSP-Phot provides a homogeneous catalogue of stellar parameters, distances, and extinctions that can be used for various purposes, such as sample selections (OB stars, red giants, solar analogues etc.)., 23 pages, 19 figures

Published
2022
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6. Gaia Data Release 3: Astrophysical parameters inference system (Apsis) I -- methods and content overview

Author

Creevey, O. L., Sordo, R., Pailler, F., Frémat, Y., Heiter, U., Thévenin, F., Andrae, R., Fouesneau, M., Lobel, A., Bailer-Jones, C. A. L., Garabato, D., Bellas-Velidis, I., Brugaletta, E., Lorca, A., Ordenovic, C., Palicio, P. A., Sarro, L. M., Delchambre, L., Drimmel, R., Rybizki, J., Elipe, G. Torralba, Korn, A. J., Recio-Blanco, A., Schultheis, M. S., de Angeli, F., Montegriffo, P., Aramburu, A. Abreu, Accart, S., Álvarez, M. A., Bakker, J., Brouillet, N., Burlacu, A., Carballo, R., Casamiquela, L., Chiavassa, A., Contursi, G., Cooper, W. J., Dafonte, C., Dapergolas, A., de Laverny, P., Dharmawardena, T. E., Edvardsson, B., Le Fustec, Y., García-Lario, P., García-Torres, M., Gomez, A., González-Santamaría, I., Hatzidimitriou, D., Jean-Antoine Piccolo, A., Kontizas, M., Kordopatis, G., Lanzafame, A. C., Lebreton, Y., Licata, E. L., Lindstrøm, H. E. P., Livanou, E., Magdaleno Romeo, A., Manteiga, M., Marocco, F., Marshall, D. J., Mary, N., Nicolas, C., Pallas-Quintela, L., Panem, C., Pichon, B., Poggio, E., Riclet, F., Robin, C., Santoveña, R., Silvelo, A., Slezak, I., Smart, R. L., Soubiran, C., Süveges, M., Ulla, A., Utrilla, E., Vallenari, A., Zhao, H., Zorec, J., Barrado, D., Bijaoui, A., Bouret, J.-C., Blomme, R., Brott, I., Cassisi, S., Kochukhov, O., Martayan, C., Shulyak, D., Silvester, J., 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), Centre National d'Études Spatiales [Toulouse] (CNES), Royal Observatory of Belgium [Brussels] (ROB), Uppsala University, Max Planck Institute for Astronomy (MPIA), Max-Planck Institute for Astronomy, Konigstuhl 17, D-69117, Heidelberg, Germany, Universidade da Coruña, National Observatory of Athens (NOA), INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional de Educación a Distancia (UNED), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, INAF - Osservatorio Astrofisico di Torino (OATo), 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), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Institute of Astronomy, University of Cambridge (IoA), INAF - Osservatorio Astronomico di Bologna (OABO), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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), Institut de recherche en astrophysique et planétologie (IRAP), 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), Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
Galaxy: stellar content, FOS: Physical sciences, galaxies: fundamental parameters, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), stars: fundamental parameters, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), catalogs, Solar and Stellar Astrophysics (astro-ph.SR), ISM: general
Abstract

Gaia Data Release 3 contains a wealth of new data products for the community. Astrophysical parameters are a major component of this release. They were produced by the Astrophysical parameters inference system (Apsis) within the Gaia Data Processing and Analysis Consortium. The aim of this paper is to describe the overall content of the astrophysical parameters in Gaia Data Release 3 and how they were produced. In Apsis we use the mean BP/RP and mean RVS spectra along with astrometry and photometry, and we derive the following parameters: source classification and probabilities for 1.6 billion objects, interstellar medium characterisation and distances for up to 470 million sources, including a 2D total Galactic extinction map, 6 million redshifts of quasar candidates and 1.4 million redshifts of galaxy candidates, along with an analysis of 50 million outlier sources through an unsupervised classification. The astrophysical parameters also include many stellar spectroscopic and evolutionary parameters for up to 470 million sources. These comprise Teff, logg, and m_h (470 million using BP/RP, 6 million using RVS), radius (470 million), mass (140 million), age (120 million), chemical abundances (up to 5 million), diffuse interstellar band analysis (0.5 million), activity indices (2 million), H-alpha equivalent widths (200 million), and further classification of spectral types (220 million) and emission-line stars (50 thousand). This catalogue is the most extensive homogeneous database of astrophysical parameters to date, and it is based uniquely on Gaia data., Comment: 35 pages (incl 7 pages references, appendix, affiliations, acknowledgements), 29 figures, A&A, accepted

Published
2022
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7. A Case for Electron-Astrophysics

Author

Satoshi Kasahara, Julia E. Stawarz, Thierry Dudok de Wit, Daniel Told, Yuri V. Khotyaintsev, Christopher S. Reynolds, Stepan Stverak, Bennett A. Maruca, David Burgess, Milan Maksimovic, Jiansen He, Owen Roberts, Joachim Saur, Robert T. Wicks, Benoit Lavraud, Shinji Saito, Olga Alexandrova, Luca Franci, Sergio Servidio, Ferdinand Plaschke, Katja Klein, Raffaella D'Amicis, Pierre Henri, Chadi S. Salem, Christopher H. K. Chen, Johan De Keyser, Daniel Verscharen, Fouad Sahraoui, Roberto Bruno, Stefaan Poedts, Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), 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), 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), Laboratoire de Physique des Plasmas (LPP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-École polytechnique (X)-Sorbonne Universités-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), University of New Hampshire (UNH), University of Northumbria at Newcastle [United Kingdom], 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), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Queen Mary University of London (QMUL), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), School of Earth and Space Sciences [Beijing], Peking University [Beijing], 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)-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), The University of Tokyo (UTokyo), Institutet för Rymdfysik, University of Arizona, 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), 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), Bartol Research Institute, University of Delaware [Newark], Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Centre for Mathematical Plasma-Astrophysics [Leuven] (CmPA), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Maria Curie-Sklodowska University (UMCS), Institute of Astronomy, University of Cambridge, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), National Institute of Information and Communications Technology [Tokyo, Japan] (NICT), University of California [Berkeley], University of California, Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, Università della Calabria [Arcavacata di Rende] (Unical), Department of Physics [Imperial College London], Imperial College London, Czech Academy of Sciences [Prague] (CAS), Max Planck Institute for Plasma physics (IPP-MPG), Max-Planck-Gesellschaft, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), 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), Verscharen, Daniel [0000-0002-0497-1096], and Apollo - University of Cambridge Repository

Subjects
Field (physics), F300, FOS: Physical sciences, Electrons, F500, Electron, 7. Clean energy, 01 natural sciences, F900, Physics - Space Physics, Voyage 2050, Physics::Plasma Physics, 0103 physical sciences, Thermal, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Plasma, space missions, Dissipation, plasma astrophysics, Physics - Plasma Physics, Space Physics (physics.space-ph), [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], Computational physics, Magnetic field, Plasma Physics (physics.plasm-ph), space plasma, Solar wind, Astrophysics - Solar and Stellar Astrophysics, solar wind, Space and Planetary Science, Physics::Space Physics, Astrophysical plasma, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

A grand-challenge problem at the forefront of physics is to understand how energy is transported and transformed in plasmas. This fundamental research priority encapsulates the conversion of plasma-flow and electromagnetic energies into particle energy, either as heat or some other form of energisation. The smallest characteristic scales, at which electron dynamics determines the plasma behaviour, are the next frontier in space and astrophysical plasma research. The analysis of astrophysical processes at these scales lies at the heart of the field of electron-astrophysics. Electron scales are the ultimate bottleneck for dissipation of plasma turbulence, which is a fundamental process not understood in the electron-kinetic regime. Since electrons are the most numerous and most mobile plasma species in fully ionised plasmas and are strongly guided by the magnetic field, their thermal properties couple very efficiently to global plasma dynamics and thermodynamics., Comment: White Paper for the Voyage 2050 Long-Term Plan in the ESA Science Programme; 27 pages

Published
2022
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34. The Pristine Inner Galaxy Survey (PIGS) II: Uncovering the most metal-poor populations in the inner Milky Way

Author

Geraint F. Lewis, Jeffrey D. Simpson, Nicolas F. Martin, Zhen Wan, David Aguado, Kim A. Venn, Daniel B. Zucker, Anke Arentsen, Carlos Allende Prieto, Lyudmila Mashonkina, Rubén Sánchez-Janssen, Jonay I. González Hernández, Else Starkenburg, J. E. O'Connell, Julio F. Navarro, K. Youakim, Roger E. Cohen, Guillaume F. Thomas, Doug Geisler, Raymond G. Carlberg, Mathias Schultheis, Vanessa Hill, Leibniz Institute for Astrophysics Potsdam (AIP), 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), Institute of Astronomy, University of Cambridge, Universidad de La Laguna [Tenerife - SP] (ULL), Joseph Louis LAGRANGE (LAGRANGE), Centre National de la Recherche Scientifique (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)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), University of British Columbia (UBC), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Leibniz-Institut für Astrophysik Potsdam (AIP), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Macquarie University, Instituto de Astrofisica de Canarias (IAC), Departamento de Astrofísica [La laguna], 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), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Russian Academy of Sciences [Moscow] (RAS), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), Sydney Institute for Astronomy (SIfA), The University of Sydney, School of Physics [UNSW Sydney] (UNSW), University of New South Wales [Sydney] (UNSW), Space Telescope Science Institute (STSci), Departamento de Astronomía [Concepción], Universidad de Concepción - University of Concepcion [Chile], Instituto de Investigación Multidisciplinario en Ciencia y Tecnología, Universidad de La Serena (USERENA), Departamento de Física y Astronomía [La Serena], Astronomy, and Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France.

Subjects
Metallicity, Milky Way, FOS: Physical sciences, Astrophysics, 01 natural sciences, Galaxy: bulge, Photometry (optics), techniques: photometric, Bulge, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Physics, Galaxy: stellar content, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Cosmic distance ladder, Astronomy and Astrophysics, stars: Population II, Horizontal branch, Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], stars: fundamental parameters, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic
Abstract

Metal-poor stars are important tools for tracing the early history of the Milky Way, and for learning about the first generations of stars. Simulations suggest that the oldest metal-poor stars are to be found in the inner Galaxy. Typical bulge surveys, however, lack low metallicity ([Fe/H] < -1.0) stars because the inner Galaxy is predominantly metal-rich. The aim of the Pristine Inner Galaxy Survey (PIGS) is to study the metal-poor and very metal-poor (VMP, [Fe/H] < -2.0) stars in this region. In PIGS, metal-poor targets for spectroscopic follow-up are selected from metallicity-sensitive CaHK photometry from the CFHT. This work presents the ~250 deg^2 photometric survey as well as intermediate-resolution spectroscopic follow-up observations for ~8000 stars using AAOmega on the AAT. The spectra are analysed using two independent tools: ULySS with an empirical spectral library, and FERRE with a library of synthetic spectra. The comparison between the two methods enables a robust determination of the stellar parameters and their uncertainties. We present a sample of 1300 VMP stars -- the largest sample of VMP stars in the inner Galaxy to date. Additionally, our spectroscopic dataset includes ~1700 horizontal branch stars, which are useful metal-poor standard candles. We furthermore show that PIGS photometry selects VMP stars with unprecedented efficiency: 86%/80% (lower/higher extinction) of the best candidates satisfy [Fe/H] < -2.0, as do 80%/63% of a larger, less strictly selected sample. We discuss future applications of this unique dataset that will further our understanding of the chemical and dynamical evolution of the innermost regions of our Galaxy., accepted for publication in MNRAS, 17 pages, 9 figures

Published
2020
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35. The Pristine survey – IX. CFHT ESPaDOnS spectroscopic analysis of 115 bright metal-poor candidate stars

Author

Carmela Lardo, Christopher Sneden, Nicolas F. Martin, Else Starkenburg, Federico Sestito, Julio F. Navarro, Rubén Sánchez Janssen, Jonay I. Gonzalez-Hernandez, Collin Kielty, Pascale Jablonka, Anke Arentsen, K. Youakim, Raymond G. Carlberg, Lyudmilla Mashonkina, Piercarlo Bonifacio, Kim A. Venn, Vanessa Hill, G. F. Thomas, Elisabetta Caffau, David Aguado, Khyati Malhan, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), 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), Leibniz Institute for Astrophysics Potsdam (AIP), 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)-Centre National de la Recherche Scientifique (CNRS), 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), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Russian Academy of Sciences [Moscow] (RAS), Department of Astronomy [Austin], University of Texas at Austin [Austin], National Research Council Herzberg Astronomy and Astrophysics, Instituto de Astrofisica de Canarias (IAC), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, The Oskar Klein Centre for Cosmoparticle Physics and Department of Physics, Stockholm University, Venn K.A., Kielty C.L., Sestito F., Starkenburg E., Martin N., Aguado D.S., Arentsen A., Bonifacio P., Caffau E., Hill V., Jablonka P., Lardo C., Mashonkina L., Navarro J.F., Sneden C., Thomas G., Youakim K., Gonzalez-Hernandez J.I., Janssen R.S., Carlberg R., Malhan K., University of British Columbia (UBC), Institute of Astronomy, University of Cambridge, 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)-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)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), and Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France.

Subjects
Star, stars: abundances, Milky Way, stars: kinematics and dynamics, 1st stars, Stellar content -Galaxy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, fe, lte line formation, hamburg/eso survey, Abundance, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, milky-way, Astrophysics::Galaxy Astrophysics, Population II, Physics, stellar halo, [PHYS]Physics [physics], Galaxy: stellar content, galactic bar, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galactic Center, Astronomy and Astrophysics, stars: Population II, Kinematics and dynamic, model atmospheres, Galaxy, Stars, Narrow band, Hamburg/ESO Survey, 13. Climate action, Space and Planetary Science, Galaxy: abundances, chemical-composition, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxy: kinematics and dynamics
Abstract

A chemo-dynamical analysis of 115 metal-poor candidate stars selected from the narrow-band Pristine photometric survey is presented based on CFHT high-resolution ESPaDOnS spectroscopy. We have discovered 28 new bright (V < 15) stars with [Fe/H] < −2.5 and 5 with [Fe/H] < −3.0 for success rates of 40 (28/70) and 19 per cent (5/27), respectively. A detailed model atmosphere analysis is carried out for the 28 new metal-poor stars. Stellar parameters were determined from SDSS photometric colours, Gaia DR2 parallaxes, MESA/MIST stellar isochrones, and the initial Pristine survey metallicities, following a Bayesian inference method. Chemical abundances are determined for 10 elements (Na, Mg, Ca, Sc, Ti, Cr, Fe, Ni, Y, and Ba). Most stars show chemical abundance patterns that are similar to the normal metal-poor stars in the Galactic halo; however, we also report the discoveries of a new r-process-rich star, a new CEMP-s candidate with [Y/Ba] > 0, and a metal-poor star with very low [Mg/Fe]. The kinematics and orbits for all of the highly probable metal-poor candidates are determined by combining our precision radial velocities with Gaia DR2 proper motions. Some stars show unusual kinematics for their chemistries, including planar orbits, unbound orbits, and highly elliptical orbits that plunge deeply into the Galactic bulge (Rperi < 0.5 kpc); also, eight stars have orbital energies and actions consistent with the Gaia-Enceladus accretion event. This paper contributes to our understanding of the complex chemo-dynamics of the metal-poor Galaxy, and increases the number of known bright metal-poor stars available for detailed nucleosynthetic studies.

Published
2020
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44. The Pristine survey X: a large population of low-metallicity stars permeates the Galactic disk

Author

Pedro A. Palicio, Thomas G. Wilson, Jonay I. González Hernández, R. Lucchesi, Kim A. Venn, Nicolas F. Martin, Nicolas Longeard, Kristopher Youakim, G. Kordopatis, Yeisson Osorio, Eline Tolstoy, David Aguado, Lee Patrick, Rodrigo A. Ibata, Anke Arentsen, Raymond G. Carlberg, Guillame Thomas, Spencer Bialek, Julio F. Navarro, Federico Sestito, Pascale Jablonka, Rafael Garcia-Dias, Khyati Malhan, Vanessa Hill, Rubén Sánchez-Janssen, Else Starkenburg, Pierre North, Luis Peralta de Arriba, Collin Kielty, 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), Leibniz Institute for Astrophysics Potsdam (AIP), University of British Columbia (UBC), Institute of Astronomy, University of Cambridge, 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), University of St Andrews. School of Physics and Astronomy, and Astronomy

Subjects
History, galaxy: evolution, Chemical evolution, Astrophysics, 01 natural sciences, galaxy: halo, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, ComputingMilieux_MISCELLANEOUS, Physics, education.field_of_study, espadons, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], galaxy: abundances, Signatures, Thick, oldest, Espadons, Oldest, formation [Galaxy], Astrophysics - Solar and Stellar Astrophysics, thick, signatures, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], history, Astrophysics::Earth and Planetary Astrophysics, Halos, Milky Way, Metallicity, Population, 1st stars, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Milky-way, evolution [Galaxy], Galactic halo, galaxy: formation, 0103 physical sciences, Galaxy formation and evolution, halo [Galaxy], halos, education, Solar and Stellar Astrophysics (astro-ph.SR), milky-way, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], abundances [Galaxy], Astronomy and Astrophysics, DAS, kinematics and dynamics [Galaxy], Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Stars, disc [Galaxy], QC Physics, galaxy: disc, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxy: kinematics and dynamics, galaxy, chemical evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The orbits of the least chemically enriched stars open a window on the formation of our Galaxy when it was still in its infancy. The common picture is that these low-metallicity stars are distributed as an isotropic, pressure-supported component since these stars were either accreted from the early building blocks of the assembling Milky Way, or were later brought by the accretion of faint dwarf galaxies. Combining the metallicities and radial velocities from the Pristine and LAMOST surveys and Gaia DR2 parallaxes and proper motions for an unprecedented large and unbiased sample of very metal-poor stars at $[Fe/H]\leq-2.5$ we show that this picture is incomplete. This sample shows strong statistical evidence (at the $5.0\sigma$ level) of asymmetry in their kinematics, favouring prograde motion. Moreover, we find that $31\%$ of the stars that currently reside in the disk do not venture outside of the disk plane throughout their orbit. The discovery of this population implies that a significant fraction of stars with iron abundances $[Fe/H]\leq-2.5$ formed within or concurrently with the Milky Way disk and that the history of the disk was quiet enough to allow them to retain their disk-like orbital properties., Comment: Submitted to MNRAS letter, 5 pages with 1 figure. Appendices A and B with 3 figures

Published
2019
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45. The Pristine Dwarf-Galaxy survey - II. In-depth observational study of the faint Milky Way satellite Sagittarius II

Author

Pascale Jablonka, Nicolas Longeard, Dougal Mackey, Jonay I. González Hernández, Anke Arentsen, Julio F. Navarro, Nicolas F. Martin, Rubén Sánchez-Janssen, Else Starkenburg, Benjamin P M Laevens, Michelle L. M. Collins, R. Michael Rich, Rodrigo A. Ibata, David Aguado, 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), Leibniz Institute for Astrophysics Potsdam (AIP), Institute of Astronomy, University of Cambridge, Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), 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
Absolute magnitude, na-o anticorrelation, catalog, Stellar population, globular-cluster, Metallicity, Milky Way, population, FOS: Physical sciences, Astrophysics, telescope, 01 natural sciences, local group, evolution, 0103 physical sciences, Binary star, 010303 astronomy & astrophysics, companion, ComputingMilieux_MISCELLANEOUS, Dwarf galaxy, Physics, 010308 nuclear & particles physics, horizontal branches, Local Group, Velocity dispersion, Astronomy and Astrophysics, galaxies: dwarf, Astrophysics - Astrophysics of Galaxies, dark-matter, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], discovery
Abstract

We present an extensive study of the Sagittarius II (Sgr II) stellar system using MegaCam g and i photometry, narrow-band, metallicity-sensitive calcium H&K doublet photometry and Keck II/DEIMOS multiobject spectroscopy. We derive and refine the Sgr II structural and stellar properties inferred at the time of its discovery. The colour–magnitude diagram implies Sgr II is old (12.0 ± 0.5 Gyr) and metal poor. The CaHK photometry confirms the metal-poor nature of the satellite ([Fe/H] CaHK = −2.32 ± 0.04 dex) and suggests that Sgr II hosts more than one single stellar population ($\sigma _\mathrm{[FeH]}^\mathrm{CaHK} = 0.11^{+0.05}_{-0.03}$ dex). Using the Ca infrared triplet measured from our highest signal-to-noise spectra, we confirm the metallicity and dispersion inferred from the Pristine photometric metallicities ([Fe/H]spectro = −2.23 ± 0.05 dex, $\sigma _\mathrm{[Fe/H]}^\mathrm{spectro} = 0.10 ^{+0.06}_{-0.04}$ dex). The velocity dispersion of the system is found to be $\sigma _{v} = 2.7^{+1.3}_{-1.0} {\rm \, km \,\, s^{-1}}$ after excluding two potential binary stars. Sgr II’s metallicity and absolute magnitude (MV = −5.7 ± 0.1 mag) place the system on the luminosity–metallicity relation of the Milky Way dwarf galaxies despite its small size. The low but resolved metallicity and velocity dispersions paint the picture of a slightly dark-matter-dominated satellite ($M/L = 23.0^{+32.8}_{-23.0}$ M⊙ L$^{-1}_{\odot }$). Furthermore, using the Gaia Data Release 2, we constrain the orbit of the satellite and find an apocentre of $118.4 ^{+28.4}_{-23.7} {\rm \, kpc}$ and a pericentre of $54.8 ^{+3.3}_{-6.1} {\rm \, kpc}$. The orbit of Sgr II is consistent with the trailing arm of the Sgr stream and indicates that it is possibly a satellite of the Sgr dSph that was tidally stripped from the dwarf’s influence.

Published
2019
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46. SOLIS IV. Hydrocarbons in the OMC-2 FIR4 Region, a Probe of Energetic Particle Irradiation of the Region

Author

Patrice Theulé, Claudio Codella, Paola Caselli, Francesco Fontani, Nadia Balucani, Cecilia Ceccarelli, S. Manigand, A. Jaber Al-Edhari, Cécile Favre, Felipe O. Alves, Mihkel Kama, E. Bianchi, Emmanuel Caux, Ian R. Sims, Jaime E. Pineda, François Dulieu, Claudine Kahane, R. Neri, Ana López-Sepulcre, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 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]), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), IT University of Copenhagen, University of Cambridge [UK] (CAM), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Università degli Studi di Perugia (UNIPG), 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), LERMA Cergy (LERMA), 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)-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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Physique des interactions ioniques et moléculaires (PIIM), Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), French space agency CNES, Italian Ministry of Education, Universities and Research, project SIR [RBSI14ZRHR], European Research Council (ERC), projects PALs [320620], DOC [741002], French program Physique et Chimie du Milieu Interstellaire (PCMI) - Conseil National de la Recherche Scientifique (CNRS), Centre National d'Etudes Spatiales (CNES), Italian Ministero dell'Istruzione, Universita e Ricerca through the grant Progetti Premiali -iALMA [CUP C52I13000140001], European Project: 320620,EC:FP7:ERC,ERC-2012-ADG_20120216,PALS(2013), IT University of Copenhagen (ITU), Università degli Studi di Perugia = University of Perugia (UNIPG), 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 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)-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), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), 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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Centre for Star and Planet Formation, Institute of Astronomy, University of Cambridge (IoA), Max-Planck-Institut für Extraterrestrische Physik (MPE), University of AL-Muthanna, College of Science, Physics Department, AL-Muthanna, Iraq, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-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), Molécules dans l'Univers, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA (UMR_8112)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)

Subjects
010504 meteorology & atmospheric sciences, radio lines ISM, FOS: Physical sciences, Particle irradiation, ISM: clouds, 01 natural sciences, Molecular physics, ISM: abundances, ISM molecules, ISM: molecules, radio lines: ISM, Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, ISM abundances, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Astrophysics - Astrophysics of Galaxies, ISM clouds, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We report new interferometric images of cyclopropenylidene, c-C$_3$H$_2$, towards the young protocluster OMC-2 FIR\,4. The observations were performed at 82 and 85 GHz with the NOrthern Extended Millimeter Array (NOEMA) as part of the project Seeds Of Life In Space (SOLIS). In addition, IRAM-30m data observations were used to investigate the physical structure of OMC-2 FIR\,4. We find that the c-C$_3$H$_2$ gas emits from the same region where previous SOLIS observations showed bright HC$_5$N emission. From a non-LTE analysis of the IRAM-30m data, the c-C$_3$H$_2$ gas has an average temperature of $\sim$40K, a H$_2$ density of $\sim$3$\times$10$^{5}$~cm$^{-3}$, and a c-C$_3$H$_2$ abundance relative to H$_2$ of ($7\pm1$)$\times$10$^{-12}$. In addition, the NOEMA observations provide no sign of significant c-C$_3$H$_2$ excitation temperature gradients across the region (about 3-4 beams), with T$_{ex}$ in the range 8$\pm$3 up to 16$\pm$7K. We thus infer that our observations are inconsistent with a physical interaction of the OMC-2 FIR\,4 envelope with the outflow arising from OMC-2 FIR\,3, as claimed by previous studies. The comparison of the measured c-C$_3$H$_2$ abundance with the predictions from an astrochemical PDR model indicates that OMC-2 FIR\,4 is irradiated by a FUV field $\sim$1000 times larger than the interstellar one, and by a flux of ionising particles $\sim$4000 times larger than the canonical value of $1\times10^{-17}$~s$^{-1}$ from the Galaxy cosmic rays, which is consistent with our previous HC$_5$N observations. This provides an important and independent confirmation of other studies that one or more sources inside the OMC-2 FIR\,4 region emit energetic ($\geq10$~MeV) particles., Accepted for publication in ApJ - 14 pages, 10 figures, 4 tables

Published
2018
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47. New constraints on the disk characteristics and companion candidates around T Chamaeleontis with VLT/SPHERE

Author

Th. Henning, E. Sissa, R. van Boekel, André Müller, Silvano Desidera, C. Perrot, Anne-Marie Lagrange, Anne-Lise Maire, Sebastian Daemgen, Johan Olofsson, Alice Zurlo, Gael Chauvin, Antonio Garufi, Beth Biller, Ch. Ginski, R. G. van Holstein, Dino Mesa, Arthur Vigan, R. G. Gratton, Maud Langlois, Tomas Stolker, M. Cudel, Myriam Benisty, Francois Menard, Judit Szulágyi, M. Kasper, J. de Boer, Carsten Dominik, Francois Wildi, Markus Janson, Anthony Cheetham, Christophe Pinte, Quentin Kral, M. Feldt, Anthony Boccaletti, A. Pohl, Mickael Bonnefoy, 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'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), ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), Max-Planck-Institut für Astronomie (MPIA), INAF-Osservatorio Astronomico di Padova, 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), Leiden Observatory, Departamento de Física y Astronomía, Universidad de Valparaiso, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institute for Astronomy, Department of Physics, ETH Zürich, Astronomical Institute Anton Pannekoek, University of Amsterdam, Institute of Astronomy, University of Cambridge (IoA), Nucleo de Astronomia, Facultad de Ingenieria, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile, Observatoire astronomique de l'Universite de Geneve, 51 ch. des Maillettes, 1290, Versoix, Switzerland, European Southern Observatory (ESO), and Low Energy Astrophysics (API, FNWI)

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, 010309 optics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Coordination network, Astrophysics::Solar and Stellar Astrophysics, Christian ministry, European commission, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The transition disk around the T Tauri star T Cha possesses a large gap, making it a prime target for high-resolution imaging in the context of planet formation. We aim to find signs of disk evolutionary processes by studying the disk geometry and the dust grain properties at its surface, and to search for companion candidates. We analyze a set of VLT/SPHERE data at near-infrared and optical wavelengths. We performed polarimetric imaging of T Cha with IRDIS (1.6 $\mu$m) and ZIMPOL (0.5-0.9 $\mu$m), and obtained intensity images from IRDIS dual-band imaging with simultaneous spectro-imaging with IFS (0.9-1.3 $\mu$m). The disk around T Cha is detected in all observing modes and its outer disk is resolved in scattered light with unprecedented angular resolution and signal-to-noise. The images reveal a highly inclined disk with a noticeable east-west brightness asymmetry. The significant amount of non-azimuthal polarization signal in the $U_{\phi}$ images, with a $U_{\phi}$/$Q_{\phi}$ peak-to-peak value of 14%, is in accordance with theoretical studies on multiple scattering. Our optimal axisymmetric radiative transfer model considers two coplanar inner and outer disks, separated by a gap of 0.28" (~30au) in size. We derive a disk inclination of ~69 deg and PA of ~114 deg. In order to self-consistently reproduce the intensity and polarimetric images, the dust grains, responsible for the scattered light, need to be dominated by sizes of around ten microns. A point source is detected at an angular distance of 3.5" from the central star. It is, however, found not to be co-moving. We confirm that the dominant source of emission is forward scattered light from the near edge of the outer disk. Our point source analysis rules out the presence of a companion heavier than ~8.5 $M_{\mathrm{jup}}$ between 0.1" and 0.3". The detection limit decreases to ~2 $M_{\mathrm{jup}}$ for 0.3" to 4.0"., Comment: 17 pages, 14 figures, accepted for publication in A&A. Revised version after language editing

Published
2017
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48. 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
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49. Cold gas in the Perseus cluster core: excitation of molecular gas in filaments

Author

Francoise Combes, R. M. Johnstone, P. Salomé, Alastair C. Edge, Yves Revaz, Andrew C. Fabian, Nina A. Hatch, Institut de RadioAstronomie Millimétrique (IRAM), 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), 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), Ecole Polytechnique Fédérale de Lausanne (EPFL), Department of Physics, University of Durham, South Road, Leiden Observatory, and Institute of Astronomy, University of Cambridge (IoA)

Subjects
galaxies : cooling flows, Ngc 1275, Tidal Dwarf Galaxies, FOS: Physical sciences, galaxies : elliptical and lenticular, cD, Astrophysics, Cooling-Flow Clusters, IRAM 30m telescope, law.invention, Emission, Protein filament, Telescope, law, Cluster (physics), Region, galaxies : individual : NGC 1275, Emission spectrum, Line (formation), Physics, Ngc-1275, galaxies : intergalactic medium, Astrophysics (astro-ph), Astronomy and Astrophysics, HERA, Galaxy, Space and Planetary Science, High-Velocity System, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hydrogen
Abstract

We have recently detected CO lines in the well-known filaments around NGC 1275, the galaxy at the centre of the Perseus cluster of galaxies. These previous observations, with the HERA multi-beam array at the IRAM 30m telescope enabled us to make a large map of the CO(2-1) line and to see hints of molecular gas far away from the cluster centre. To confirm the presence of CO emission lines in the outer filaments and to study the CO(2-1)/CO(1-0) line ratio, we observed seven regions of interest again with the 30m telescope in both CO(1-0) and CO(2-1). The regions we observed were: the eastern filament, the horseshoe, the northern filament and a southern extension, all selected from Halpha emission line mapping. Molecular gas is detected in all the observed regions. This result confirms the large extent of the cold molecular gas filaments. We discuss the CO(2-1)/CO(1-0) ratios in the filaments. The eastern filament has optically thick gas, whereas further away, the line ratio increases close to values expected for a warmer optically thin medium. We also show CO(1-0) and CO(2-1) lines in 9 regions closer to the centre. The kinematics of the CO is studied here in more detail and confirms that it follows the motions of the warm H_2 gas found in the near-infrared. Finally, we searched for dense gas tracers around 3C84 and claim here the first detection of HCN(3-2)., Comment: 10 pages, 6 figures, A&A in press

Published
2008
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50. Hα kinematics of the Spitzer Infrared Nearby Galaxies Survey – II

Author

A. Boselli, L. Chemin, Oscar F. Hernández, Chantal Balkowski, M.-M. de Denus-Baillargeon, Philippe Amram, Claude Carignan, Isabelle Dicaire, Kambiz Fathi, Olivier Daigle, Robert C. Kennicutt, Laboratoire d'Astrophysique Expérimentale (LAE), Observatoire du Mont Mégantic, 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), 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), Institut FRESNEL (FRESNEL), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Canarias (IAC), and Institute of Astronomy, University of Cambridge (IoA)

Subjects
Luminous infrared galaxy, Physics, 010308 nuclear & particles physics, Galactic Center, Dark matter, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Kinematics, Astrophysics, 01 natural sciences, Radial velocity, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Spitzer Infrared Nearby Galaxies Survey, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy rotation curve
Abstract

International audience; This is the second part of an Halpha kinematics follow-up survey of the Spitzer Infrared Nearby Galaxies Survey (SINGS) sample. The aim of this paper is to shed new light on the role of baryons and their kinematics and on the dark/luminous matter relation in the star-forming regions of galaxies, in relation with studies at other wavelengths. The data for 37 galaxies are presented. The observations were made using Fabry-Perot interferometry with the photon-counting camera FaNTOmM on four different telescopes, namely the Canada-France-Hawaii 3.6-m, the ESO La Silla 3.6-m, the William Herschel 4.2-m and the Observatoire du mont Mégantic 1.6-m telescopes. The velocity fields are computed using custom IDL routines designed for an optimal use of the data. The kinematical parameters and rotation curves are derived using the GIPSY software. It is shown that non-circular motions associated with galactic bars affect the kinematical parameters fitting and the velocity gradient of the rotation curves. This leads to incorrect determinations of the baryonic and dark matter distributions in the mass models derived from those rotation curves.

Published
2008
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