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13. VizieR Online Data Catalog: Distance of HiGAL sources (Mege+, 2021)

Author

Mège, P., Russeil, D., Zavagno, Annie, Elia, D., Molinari, S., Brunt, C.~m., Butora, R., Cambresy, L., Di, Giorgio A.~m., Fenouillet, T., Fukui, Y., Lambert, J.~c., Makai, Z., Merello, M., Meunier, J.~c., Molinaro, M., Moreau, C., Pezzuto, S., Poulin, Y., Schisano, E., Schuller, F., 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 Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), 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), Department of Astrophysics [Nagoya], Nagoya University, West Virginia University [Morgantown], Departamento de Astronomia (DAS), INAF - Osservatorio Astronomico di Trieste (OAT), Environnement, Ville, Société (EVS), École normale supérieure de Lyon (ENS de Lyon)-École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Université Lumière - Lyon 2 (UL2)-Université Jean Moulin - Lyon 3 (UJML), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-École Nationale des Travaux Publics de l'État (ENTPE)-École nationale supérieure d'architecture de Lyon (ENSAL)-Centre National de la Recherche Scientifique (CNRS), and Max-Planck-Institut für Radioastronomie (MPIFR)

Subjects
Milky Way, Radial velocities, [SDU]Sciences of the Universe [physics], Molecular clouds, Stars: distances
Abstract

Velocity and Distance of HiGAL sources. \\\\(2 data files).

Published
2020

14. Herschel spectroscopy of Massive Young Stellar Objects in the Magellanic Clouds

Author

D. Cormier, J. Th. van Loon, C.-H. R. Chen, Remy Indebetouw, Vianney Lebouteiller, Margaret Meixner, Joana M. Oliveira, L. R. Carlson, M. Sewilo, S. C. Madden, Min-Young Lee, Miroslav Filipovic, Yasuo Fukui, Benjamin A. Sargent, Laboratório de Neurobiologia II - IBCCF / UFRJ [Rio de Janeiro], Instituto de Biofísica Carlos Chagas Filho [Rio de Janeiro] (IBCCF / UFRJ), Universidade Federal do Rio de Janeiro (UFRJ)-Universidade Federal do Rio de Janeiro (UFRJ), 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), Department of Astrophysics [Nagoya], Nagoya University, Laboratório de Neurobiologia II - UFRJ [Universidade de Rio de Janeiro - Brésil], Universidade Federal do Rio de Janeiro [Rio de Janeiro] (UFRJ), 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
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Young stellar object, Metallicity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, clouds, Astrophysics::Cosmology and Extragalactic Astrophysics, Photodissociation region, 7. Clean energy, 01 natural sciences, ISM: clouds, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Magellanic Clouds, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Physics, stars: formation, Spectrometer, stars: protostars, 010308 nuclear & particles physics, Astronomy and Astrophysics, Photoelectric effect, Astrophysics - Astrophysics of Galaxies, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We present Herschel Space Observatory Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver Fourier Transform Spectrometer (SPIRE FTS) spectroscopy of a sample of twenty massive Young Stellar Objects (YSOs) in the Large and Small Magellanic Clouds (LMC and SMC). We analyse the brightest far infrared (far-IR) emission lines, that diagnose the conditions of the heated gas in the YSO envelope and pinpoint their physical origin.We compare the properties of massive Magellanic and Galactic YSOs.We find that [OI] and [CII] emission, that originates from the photodissociation region associated with the YSOs, is enhanced with respect to the dust continuum in the Magellanic sample. Furthermore the photoelectric heating efficiency is systematically higher for Magellanic YSOs, consistent with reduced grain charge in low metallicity environments. The observed CO emission is likely due to multiple shock components. The gas temperatures, derived from the analysis of CO rotational diagrams, are similar to Galactic estimates. This suggests a common origin to the observed CO excitation, from low-luminosity to massive YSOs, both in the Galaxy and the Magellanic Clouds. Bright far-IR line emission provides a mechanism to cool the YSO environment. We find that, even though [OI], CO and [CII] are the main line coolants, there is an indication that CO becomes less important at low metallicity, especially for the SMC sources. This is consistent with a reduction in CO abundance in environments where the dust is warmer due to reduced ultraviolet-shielding. Weak H$_2$O and OH emission is detected, consistent with a modest role in the energy balance of wider massive YSO environments., 38 pages; accepted for publication by MNRAS; full integrated version; journal version will include appendices on-line only

Published
2019
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15. Correlation of gas dynamics and dust in the evolved filament G82.65-02.00

Author

L. V. Toth, Toshikazu Onishi, V.-M. Pelkonen, Tomomi Shimoikura, A. Rivera-Ingraham, Mika Saajasto, J. Malinen, L. Montier, O. Fehér, Kazuhito Dobashi, J.-Ph. Bernard, I. Ristorcelli, Mika Juvela, D. J. Marshall, J. Montillaud, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, 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), 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), foreign laboratories (FL), CERN [Genève], Centre d'étude spatiale des rayonnements (CESR), Department of Astrophysics [Nagoya], Nagoya University, University of Helsinki-University of Helsinki, 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), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, and Department of Physics

Subjects
Milky Way, ISM: structure, FOS: Physical sciences, Astrophysics, 01 natural sciences, ISM: clouds, Spectral line, STAR-FORMATION, SHOCKS, Protein filament, NEBULA, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, ISM: kinematics and dynamics, Nebula, HERSCHEL, 010308 nuclear & particles physics, Star formation, extinction, Molecular cloud, Astronomy and Astrophysics, Virial mass, YOUNG STELLAR OBJECTS, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), EVOLUTION, ISM: lines and bands, Space and Planetary Science, OUTFLOWS, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR CLOUDS, MILKY-WAY, dust, extinction, dust, EMISSION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The combination of line and continuum observations can provide vital insights to the formation and fragmentation of filaments and the initial conditions for star formation. We have carried out line observations to map the kinematics of an evolved, actively star forming filament G82.65-2.00. The filament was first The combination of line and continuum observations can provide vital insights to the formation and fragmentation of filaments and the initial conditions for star formation. We have carried out line observations to map the kinematics of an evolved, actively star forming filament G82.65-2.00. The filament was first identified from the Planck data as a region of particularly cold dust emission and was mapped at 100-500 $\mu$m as a part of Herschel key program Galactic Cold Cores. The observations reveal several velocity components in the field, with strongest line emission concentrated to velocity range $\sim [3,5]$ km $\rm s^{-1}$. The column density of molecular hydrogen along the filament varies from 1.0 to 2.3 $\times 10^{22}$ $\rm cm^{2}$. We have examined six cold clumps from the central part of the filament. The clumps have masses in the range $10 - 20$ $M_{\odot}$ ($\sim70M_{\odot}$ in total) and are close to or above the virial mass. Furthermore, the main filament is heavily fragmented and most of the the substructures have a mass lower than or close to the virial mass, suggesting that the filament is dispersing as a whole. Position-velocity maps of $\rm ^{12}CO$ and $\rm ^{13}CO$ lines indicate that at least one of the striations is kinematically connected to two of the clumps, potentially indicating mass accretion from the striation onto the main filament. We tentatively estimate the accretion rate to be $\dot{M}$ = $2.23 \times 10^{-6}$ $ M_{\odot} / \rm year$., Comment: Accepted for publication in A&A

Published
2017
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16. Observations of M31 and M33 with the Fermi Large Area Telescope: A Galactic Center Excess in Andromeda?

Author

Jiancheng Wang, Diego F. Torres, Marco Ajello, S. Cutini, Jürgen Knödlseder, L. Latronico, F. Loparco, Ronaldo Bellazzini, R. A. Cameron, S. Rainò, J. F. Ormes, I. A. Grenier, E. Cavazzuti, David H. Green, Gloria Spandre, Jingcheng Li, G. Barbiellini, Andrea Albert, P. Spinelli, R. Buehler, P. Bruel, G. La Mura, Eric Charles, Xian Hou, Nicola Omodei, Kazuhiko Hayashi, Peter F. Michelson, Marcello Giroletti, M. N. Mazziotta, N. Di Lalla, Luca Baldini, Francesco Longo, Jean Ballet, M. Caragiulo, F. Gargano, Giacomo Principe, Claudia Cecchi, D. Malyshev, Sylvain Guiriec, Carmelo Sgrò, Riccardo Rando, Frederic Piron, E. J. Siskind, D. Simone, David Paneque, P. Martin, E. Orlando, M. Razzano, R. Bonino, Filippo D'Ammando, Johan Bregeon, K. Tanaka, A. Chekhtman, C. Favuzzi, Yasunobu Uchiyama, Nestor Mirabal, Elliott D. Bloom, P. Fusco, Matthew Wood, Warit Mitthumsiri, M. Kuss, M. Di Mauro, Matteo Negro, A. Morselli, Francesco Giordano, Stefan Funk, P. Lubrano, F. Spada, R. Caputo, Igor V. Moskalenko, Stefan Larsson, Gabrijela Zaharijas, Olaf Reimer, Melissa Pesce-Rollins, Tsunefumi Mizuno, S. W. Digel, G. Chiaro, R. Desiante, Ming Zhou, Miguel A. Sánchez-Conde, K. S. Wood, T. Ohsugi, Eleonora Troja, T. J. Brandt, L. Di Venere, E. Nuss, Gudlaugur Johannesson, M. E. Monzani, Lucas Guillemot, M. Ackermann, S. Maldera, F. Costanza, T. Kamae, L. Tibaldo, Nicola Giglietto, Elisabetta Bissaldi, Massimo Persic, P. A. Caraveo, T. Glanzman, Denis Bastieri, S. Ciprini, F. de Palma, Eugenio Bottacini, Alberto Manfreda, Albert K. H. Kong, T. A. Porter, Ackermann, M., Ajello, M., Albert, A., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bellazzini, R., Bissaldi, E., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bregeon, J., Bruel, P., Buehler, R., Cameron, R. A., Caputo, R., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Cecchi, C., Charles, E., Chekhtman, A., Chiaro, G., Ciprini, S., Costanza, F., Cutini, S., D'Ammando, F., De Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Favuzzi, C., Funk, S., Fusco, P., Gargano, F., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Green, D., Grenier, I. A., Guillemot, L., Guiriec, S., Hayashi, K., Hou, X., Jóhannesson, G., Kamae, T., Knödlseder, J., Kong, A. K. H., Kuss, M., Mura, G. La, Larsson, S., Latronico, L., Li, J., Longo, Francesco, Loparco, F., Lubrano, P., Maldera, S., Malyshev, D., Manfreda, A., Martin, P., Mazziotta, M. N., Michelson, P. F., Mirabal, N., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Persic, M., Pesce Rollins, M., Piron, F., Porter, T. A., Principe, G., Rainò, S., Rando, R., Razzano, M., Reimer, O., Sánchez Conde, M., Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Tanaka, K., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Wang, J. C., Wood, K. S., Wood, M., Zaharijas, G., Zhou, M., Deutsches Elektronen-Synchrotron [Hamburg] (DESY), Department of Physics and Astronomy [Clemson], Clemson University, Los Alamos National Laboratory (LANL), Istituto Nazionale di Fisica Nucleare [Pisa] (INFN), Istituto Nazionale di Fisica Nucleare (INFN), 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), Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare, sezione di Bari (INFN, sezione di Bari), Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (INFN, Sezione di Torino), NASA Goddard Space Flight Center (GSFC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, Santa Cruz Institute for Particle Physics (SCIPP), University of California [Santa Cruz] (UCSC), University of California-University of California, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Agenzia Spaziale Italiana (ASI) Science Data Center, Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN, Sezione di Perugia), George Mason University [Fairfax], Universita degli Studi di Padova, Istituto di Radioastronomia [Bologna] (IRA), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Department of Astrophysics [Nagoya], Nagoya University, Yunnan Observatories, Chinese Academy of Sciences, Science Institute, University of Iceland, University of Iceland [Reykjavik], Tokyo University of Science [Tokyo], 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), National Tsing Hua University [Hsinchu] (NTHU), DIEE, University of Cagliari, Royal Institute of Technology [Stockholm] (KTH ), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Mahidol University [Bangkok], Hiroshima University, Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tor Vergata (INFN, Sezione di Roma Tor Vergata), Department of Physics and Astronomy [Denver], University of Denver, Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, Leopold-Franzens Universitat Innsbruck, Stockholm University, NYCB Real-Time Computing Inc., Lattingtown, NYCB Real-Time Computing Inc. [Lattingtown], Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Rikkyo University [Tokyo], Università degli Studi di Udine - University of Udine [Italie], ITA, 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Università degli Studi di Padova = University of Padua (Unipd), 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 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), Universität Innsbruck [Innsbruck], Ackermann M, Ajello M, Albert A, Baldini L, Ballet J, Barbiellini G, Bastieri D, Bellazzini R, Bissaldi E, Bloom E D, Bonino R, Bottacini E, Brandt T J, Bregeon J, Bruel P, Buehler R, Cameron R A, Caputo R, Caragiulo M, Caraveo P A, Cavazzuti E, Cecchi C, Charles E, Chekhtman A, Chiaro G, Ciprini S, Costanza F, Cutini S, DAmmando F, de Palma F, Desiante R, Digel S W, Di Lalla N, Di Mauro M, Di Venere L, Favuzzi C, Funk S, Fusco P, Gargano F, Giglietto N, Giordano F, Giroletti M, Glanzman T, Green D, Grenier I A, Guillemot L, Guiriec S, Hayashi K, Hou X, Jóhannesson G, Kamae T, Knödlseder J, Kong A K H, Kuss M, La Mura G, Larsson S, Latronico L, Li J, Longo F, Loparco F, Lubrano P, Maldera S, Malyshev D, Manfreda A, Martin P, Mazziotta M N, Michelson P F, Mirabal N, Mitthumsiri W, Mizuno T, Monzani M E, Morselli A, Moskalenko I V, Negro M, Nuss E, Ohsugi T, Omodei N, Orlando E, Ormes J F, Paneque D, Persic M, Pesce-Rollins M, Piron F, Porter T A, Principe G, Rainò S, Rando R, Razzano M, Reimer O, Sánchez-Conde M, Sgrò C, Simone D, Siskind E J, Spada F, Spandre G, Spinelli P, Tanaka K, Tibaldo L, Torres D F, Troja E, Uchiyama Y, Wang J C, Wood K S, Wood M, Zaharijas G, Zhou M, National Institute for Nuclear Physics (INFN), Stanford University [Stanford], 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), Helmholtz-Gemeinschaft, Istituto di Radioastronomia INAF, 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), Department of Astrophysics, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)

Subjects
Andromeda Galaxy, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], cosmic rays, gamma rays: galaxies, Local Group, Astronomy and Astrophysics, Space and Planetary Science, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Galaxy formation and evolution, galaxie [gamma rays], Interacting galaxy, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, cosmic ray, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysic, Galaxy, Dwarf spheroidal galaxy, cosmic rays – gamma rays: galaxies – Local Group, Globular cluster, Elliptical galaxy, ddc:520, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Fermi LAT has opened the way for comparative studies of cosmic rays (CRs) and high-energy objects in the Milky Way (MW) and in other, external, star-forming galaxies. Using 2 yr of observations with the Fermi LAT, local Group galaxy M31 was detected as a marginally extended gamma-ray source, while only an upper limit (UL) has been derived for the other nearby galaxy M33. We revisited the gamma-ray emission in the direction of M31 and M33 using more than 7 yr of LAT Pass 8 data in the energy range 0.1-100 GeV, presenting detailed morphological and spectral analyses. M33 remains undetected and we computed an UL for it. This revised UL remains consistent with the observed correlation between gamma-ray luminosity and star-formation rate tracers and implies an average CR density in M33 that is at most half of that of the MW. M31 is detected with a significance of nearly 10 sigma and to be extended with 4 sigma. Its spectrum is consistent with a power law. The spatial distribution of the emission is consistent with a uniform disk with a radius of 0.4 deg and no offset from the center of M31, but nonuniform intensity distributions cannot be excluded. The flux from M31 appears confined to the inner regions of the galaxy and does not fill the disk or extend far from it. The gamma-ray signal is not correlated with regions rich in gas or star-formation activity suggesting that the emission is not interstellar in origin, unless the energetic particles radiating in gamma rays do not originate in recent star formation. Alternative and nonexclusive interpretations are that the emission results from a population of millisecond pulsars dispersed in the bulge and disk of M31 by disrupted globular clusters or from the decay or annihilation of dark matter particles, similar to what has been proposed to account for the so-called Galactic Center excess found in Fermi-LAT observations of the MW., Comment: 14 pages, 7 figures, 4 tables

Published
2017
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17. Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud

Author

Lee, M.-Y., Madden, S. C., Lebouteiller, Vianney, Gusdorf, A., Godard, B., Wu, R., Galametz, M., Cormier, D., Le Petit, F., Roueff, E., Bron, E., Carlson, L., Chevance, M., Fukui, Y., Galliano, F., Hony, S., Hughes, A., Indebetouw, R., Israel, F. P., Kawamura, A., Le Bourlot, J., Lesaffre, Pierre, Meixner, M., Muller, E., Nayak, O., Onishi, T., Roman-Duval, J., Sewiło, M., 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), 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), 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), University of Cambridge [UK] (CAM), Department of Astrophysics [Nagoya], Nagoya University, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institute of Environmental Systems (SUIKO), Kyushu University, 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), 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), Kyushu University [Fukuoka], and École normale supérieure - Paris (ENS Paris)

Subjects
infrared: ISM, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Magellanic Clouds, ISM: molecules, galaxies: ISM
Abstract

International audience; We present Herschel SPIRE Fourier Transform Spectrometer (FTS) observations of N159W, an active star-forming region in the Large Magellanic Cloud (LMC). In our observations, a number of far-infrared cooling lines, including carbon monoxide (CO) J = 4 → 3 to J = 12 → 11, [CI] 609 μm and 370 μm, and [NII] 205 μm, are clearly detected. With an aim of investigating the physical conditions and excitation processes of molecular gas, we first construct CO spectral line energy distributions (SLEDs) on 10 pc scales by combining the FTS CO transitions with ground-based low-J CO data and analyze the observed CO SLEDs using non-LTE (local thermodynamic equilibrium) radiative transfer models. We find that the CO-traced molecular gas in N159W is warm (kinetic temperature of 153-754 K) and moderately dense (H2 number density of (1.1-4.5) × 103 cm-3). To assess the impact of the energetic processes in the interstellar medium on the physical conditions of the CO-emitting gas, we then compare the observed CO line intensities with the models of photodissociation regions (PDRs) and shocks. We first constrain the properties of PDRs by modeling Herschel observations of [OI] 145 μm, [CII] 158 μm, and [CI] 370 μm fine-structure lines and find that the constrained PDR components emit very weak CO emission. X-rays and cosmic-rays are also found to provide a negligible contribution to theCO emission, essentially ruling out ionizing sources (ultraviolet photons, X-rays, and cosmic-rays) as the dominant heating source for CO in N159W. On the other hand, mechanical heating by low-velocity C-type shocks with 10 km s-1 appears sufficient enough to reproduce the observed warm CO. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.The final reduced Herschel data (FITS files) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/596/A85

Published
2016
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18. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues First data release for the inner Milky Way:+68 degrees \textgreater= l \textgreater=-70 degrees

Author

MOLINARI, S., SCHISANO, E., ELIA, D., PESTALOZZI, M., TRAFICANTE, A., PEZZUTO, S., SWINYARD, B. M., NORIEGA-CRESPO, A., BALLY, J., MOORE, T. J. T., PLUME, R., ZAVAGNO, Annie, GIORGIO, A. M., LIU, S. J., PILBRATT, G. L., MOTTRAM, J. C., RUSSEIL, D., PIAZZO, L., VENEZIANI, M., BENEDETTINI, M., CALZOLETTI, L., FAUSTINI, F., NATOLI, P., PIACENTINI, F., MERELLO, M., PALMESE, A., DEL GRANDE, R., POLYCHRONI, D., RYG, K. L. J., POLENTA, G., BARLOW, M. J., BERNARD, J. -P., MARTIN, P. G., TESTI, L., ALI, B., ANDRÉ, P., BELTRAN, M. T., BILLOT, N., CAREY, S., CESARONI, R., COMPIÈGNE, M., EDEN, D., FUKUI, Y., GARCIA-LARIO, P., HOARE, M. G., HUANG, M., JONCAS, G., LIM, T. L., LORD, . D., MARTINAVARRO-ARMENGOL, S., MOTTE, F., PALADINI, R., PARADIS, D., PERETTO, N., ROBITAILLE, T., SCHILKE, P., SCHNEIDER, N., SCHULZ, B., SIBTHORPE, B., STRAFELLA, F., THOMPSON, M. A., UMANA, G., WARD-THOMPSON, D., WYROWSKI, F., INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Faculty of Informatics [Lugano], Università della Svizzera italiana = University of Italian Switzerland (USI), Space Telescope Science Institute (STSci), Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Department of Physics and Astronomy [Calgary], University of Calgary, 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), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), 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), 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), 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), École Nationale Supérieure d’Agronomie [Alger] (ENSA), 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), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Department of Astrophysics [Nagoya], Nagoya University, ISO Data Centre (ESA - Espagne), Herschel Science Centre (ESA Espagne), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), 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, Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, University Hospital of Cologne [Cologne], FORMATION STELLAIRE 2016, 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 de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), AUTRES, Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Max-Planck-Institut für Radioastronomie (MPIFR), 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), European Space Agency (ESA), 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), 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), 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), Universität zu Köln, Università della Svizzera italiana (USI), 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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Aims. We present the first public release of high-quality data products (DR1) from Hi-GAL, the Herschel infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic plane surveys from the near-IR to the radio and covers five wavebands at 70, 160, 250, 350 and 500 mu m, encompassing the peak of the spectral energy distribution of cold dust for 8 less than or similar to T less than or similar to 50 K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68 degrees greater than or similar to l greater than or similar to -70 degrees in a vertical bar b vertical bar \textless= 1 degrees latitude strip. Methods. Photometric maps have been produced with the ROMAGAL pipeline, which optimally capitalizes on the excellent sensitivity and stability of the bolometer arrays of the Herschel PACS and SPIRE photometric cameras. It delivers images of exquisite quality and dynamical range, absolutely calibrated with Planck and IRAS, and recovers extended emission at all wavelengths and all spatial scales, from the point-spread function to the size of an entire 2 degrees x 2 degrees “tile” that is the unit observing block of the survey. The compact source catalogues were generated with the CuTEx algorithm, which was specifically developed to optimise source detection and extraction in the extreme conditions of intense and spatially varying background that are found in the Galactic plane in the thermal infrared. Results. Hi-GAL DR1 images are cirrus noise limited and reach the 1 sigma-rms predicted by the Herschel Time Estimators for parallel-mode observations at 60 `' s(-1) scanning speed in relatively low cirrus emission regions. Hi-GAL DR1 images will be accessible through a dedicated web-based image cutout service. The DR1 Compact Source Catalogues are delivered as single-band photometric lists containing, in addition to source position, peak, and integrated flux and source sizes, a variety of parameters useful to assess the quality and reliability of the extracted sources. Caveats and hints to help in this assessment are provided. Flux completeness limits in all bands are determined from extensive synthetic source experiments and greatly depend on the specific line of sight along the Galactic plane because the background strongly varies as a function of Galactic longitude. Hi-GAL DR1 catalogues contain 123210, 308509, 280685, 160972, and 85460 compact sources in the five bands.

Published
2016
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19. The dust properties and physical conditions of the interstellar medium in the LMC massive star-forming complex N11

Author

J.M. Oliviera, Sacha Hony, Annie Hughes, S. C. Madden, C. Bot, Alberto D. Bolatto, Vianney Lebouteiller, Maud Galametz, Julia Roman-Duval, Diane Cormier, D. Paradis, Min-Young Lee, Toshikazu Onishi, Monica Rubio, Frank P. Israel, Yasuo Fukui, Akiko Kawamura, Margaret Meixner, Frédéric Galliano, Marta Sewilo, M. Albrecht, Eric W. Pellegrini, University of Cambridge [UK] (CAM), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Leibniz-Institut für Kristallzüchtung, 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, 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 Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, 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), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Météo-France [Paris], Météo France, Institut Laue-Langevin (ILL), ILL, Department of Astrophysics [Nagoya], Nagoya University, Institute of Environmental Systems (SUIKO), Kyushu University [Fukuoka], 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), Universiteit Leiden, Météo-France, and Kyushu University

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Magellanic Clouds, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Cosmic dust, Line (formation), ISM: general, Physics, infrared: ISM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Spectral density, Astronomy and Astrophysics, galaxies: dwarf, Intergalactic dust, Mass ratio, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, submillimetre: ISM, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM
Abstract

We combine Spitzer and Herschel data of the star-forming region N11 in the Large Magellanic Cloud to produce detailed maps of the dust properties in the complex and study their variations with the ISM conditions. We also compare APEX/LABOCA 870um observations with our model predictions in order to decompose the 870um emission into dust and non-dust (free-free emission and CO(3-2) line) contributions. We find that in N11, the 870um can be fully accounted for by these 3 components. The dust surface density map of N11 is combined with HI and CO observations to study local variations in the gas-to-dust mass ratios. Our analysis leads to values lower than those expected from the LMC low-metallicity as well as to a decrease of the gas-to-dust mass ratio with the dust surface density. We explore potential hypotheses that could explain the low observed gas-to-dust mass ratios (variations in the XCO factor, presence of CO-dark gas or of optically thick HI or variations in the dust abundance in the dense regions). We finally decompose the local SEDs using a Principal Component Analysis (i.e. with no a priori assumption on the dust composition in the complex). Our results lead to a promising decomposition of the local SEDs in various dust components (hot, warm, cold) coherent with that expected for the region. Further analysis on a larger sample of galaxies will follow in order to understand how unique this decomposition is or how it evolves from one environment to another., 24 pages, 16 figures, accepted for publication in MNRAS

Published
2015
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20. Erratum: 'The Herschel Inventory of the Agents of Galaxy Evolution (Heritage) in the Magellanic Clouds, a Herschel Open Time Key Program' (2013, AJ, 146, 62)

Author

Alberto D. Bolatto, Karl D. Gordon, Sundar Srinivasan, Linda J. Smith, Marc Sauvage, P. Chanial, Barbara A. Whitney, Remy Indebetouw, Frank P. Israel, K. Okumura, Martha L. Boyer, Tracy L. Beck, E. Montiel, Francisca Kemper, Mikako Matsuura, C. Bot, Pasquale Panuzzo, L. R. Carlson, Ramin A. Skibba, J. Seale, Brian Babler, Alexander G. G. M. Tielens, S. Hony, Yasuo Fukui, C.-H. R. Chen, Diane Cormier, Joseph L. Hora, Thomas P. Robitaille, Masaaki Otsuka, J.-P. Bernard, Sungeun Kim, Vianney Lebouteiller, Marta Sewilo, Annie Hughes, Chad Engelbracht, Karl Misselt, Toshikazu Onishi, Erik Muller, B. A. Sargent, Julia Roman-Duval, William T. Reach, Geoffrey C. Clayton, D. Paradis, Joana M. Oliveira, Maud Galametz, E. Kwon, Margaret Meixner, Monica Rubio, Frédéric Galliano, Aigen Li, Akiko Kawamura, Albrecht Poglitsch, S. C. Madden, Knox S. Long, J. Th. van Loon, 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), 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), Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, 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), Department of Astrophysics [Nagoya], Nagoya University, University of Cambridge [UK] (CAM), University of Virginia, Leiden Observatory [Leiden], Universiteit Leiden, Institute of Environmental Systems (SUIKO), Kyushu University, 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 Physics and Astronomy [UCL London], University College of London [London] (UCL), Météo-France, Max-Planck-Institut für Extraterrestrische Physik (MPE), inconnu, Inconnu, 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 Virginia [Charlottesville], Universiteit Leiden [Leiden], Kyushu University [Fukuoka], Météo-France [Paris], Météo France, and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Subtraction, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Table (information), 01 natural sciences, Galaxy, Spire, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Galaxy formation and evolution, Calibration, Cirrus, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

We provide a corrected Table 4 that lists the total galaxy fluxes for the HERTIAGE bands and corresponding Figure 19 which plots these fluxes in comparison to prior measurements These corrected fluxes differ by up to 41% to what we reported in the original paper. These revised fluxes utilize a more appropriate subtraction of the Milky Way Foreground Cirrus emission which contaminates especially the PACS 100 and 160 micron bands. The subtraction process uses the HI 21 cm emission to develop a model for the MW cirrus dust emission. In addition, the better subtraction process corrected for an over subtraction of the background in the SPIRE images of the SMC that occurred during the original data processing. The need for these better foreground subtractions was realized while working on an analysis of the dust masses and gas-to-dust ratios in the LMC and SMC reported by Gordon et al. (2014) and Roman-Duval et al. (2014). After the subtraction has been done, the fluxes were derived by simply summing up all the pixels in the image. The errors we quote for the fluxes reflect the absolute flux calibration errors for extended sources which are approx.10% for PACS and approx. 8% for SPIRE. In the revised Figure 19, we confirm that these corrected global fluxes remain within the range of prior global measurements for both the LMC and SMC. Indeed, the shape of the corrected spectral energy distributions appears better aligned with prior measurements.

Published
2015
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21. Dust from Comet 209P/LINEAR during its 2014 Return: Parent Body of a New Meteor Shower, the May Camelopardalids

Author

Ishiguro, M, Kuroda, D, Hanayama, H, Takahashi, J, Hasegawa, S, Sarugaku, Y, Watanabe, M, Imai, M, Goda, S, Akitaya, H, Takagi, Y, Morihana, K, Honda, S, Arai, A, Sekiguchi, K, Oasa, Y, Saito, Yoshihiko, Morokuma, T, Murata, K, Nogami, D, Nagayama, T, Yanagisawa, K, Yoshida, M, Ohta, K, Kawai, Nobuyuki, Miyaji, T, Fukushima, H, Watanabe, J.-i., Opitom, C, Jehin, E, Gillon, M, Vaubaillon, J.~J., Department of Physics and Astronomy and Center for Theoretical Physics, Seoul National University, Seoul National University [Seoul], Okayama Astrophysical Observatory ( OAO ), National Astronomical Observatory of Japan ( NAOJ ), Ishigakijima Astronomical Observatory, Nishi-Harima Astronomical Observatory, Center for Astronomy, Institute of Space and Astronautical Science ( ISAS ), Department of Cosmosciences, Hokkaido University, Hiroshima Astrophysical Science Center, Hiroshima University, Japan, Faculty of Education, Saitama University, Department of Physics [Tokyo], Tokyo Institure of Technology, Institute of Astronomy, Graduate School of Science, The University of Tokyo, Department of Astrophysics, Nagoya University, Department of astronomy, Kyoto University, Graduate School of Science and Engineering, Kagoshima University, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [Seoul], Seoul National University [Seoul] (SNU), Center for Theoretical Physics [Seoul], Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Okayama Astrophysical Observatory (OAO), National Astronomical Observatory of Japan (NAOJ), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Hokkaido University [Sapporo, Japan], Hiroshima University, The University of Tokyo (UTokyo), Department of Astrophysics [Nagoya], Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Terminal velocity, Meteoroid, Comet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Escape velocity, comets: individual: 209P/LINEAR, 01 natural sciences, comets: individual (209P/LINEAR), Jupiter, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Comet nucleus, 0103 physical sciences, interplanetary medium, Meteor shower, 010303 astronomy & astrophysics, [ SDU ] Sciences of the Universe [physics], Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences, Cosmic dust
Abstract

著者人数: 32名, Accepted: 2014-12-11, 資料番号: SA1005017000

Published
2015
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22. SPLASH: the Southern Parkes Large-Area Survey in Hydroxyl – first science from the pilot region

Author

Cormac Purcell, Courtney Jones, Andrew Walsh, John M. Dickey, Yasuo Fukui, Maria Cunningham, José-Luis Gómez, Paul Jones, Simon Ellingsen, Shari Breen, Naomi McClure-Griffiths, Steven J. Gibson, Ettore Carretti, Vicki Lowe, Takahiro Hayakawa, Akira Mizuno, Patrick Hennebelle, J. A. Green, Hiroshi Imai, Joanne Dawson, N. Lo, James Caswell, V. Krishnan, Microbiology Department, St. Jame's Hospital, Swinburne University of Technology (Hawthorn campus), University of New South Wales [Sydney] (UNSW), School of Mathematics and Physics, University of Tasmania [Hobart, Australia] (UTAS), 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), Unidad de Glaciología y Recursos Hídricos, 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), Observatoire de Paris - Site de Paris (OP), 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), Department of Materials Science and Engineering, Nagoya Institute of Technology, Department of Astrophysics [Nagoya], Nagoya University, Institute for Space-Earth Environmental Research [Nagoya] (ISEE), 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
Physics, [PHYS]Physics [physics], education.field_of_study, Splash, Molecular cloud, Population, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Excitation temperature, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, law.invention, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Maser, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract

SPLASH (the Southern Parkes Large-Area Survey in Hydroxyl) is a sensitive, unbiased and fully-sampled survey of the Southern Galactic Plane and Galactic Centre in all four ground-state transitions of the hydroxyl (OH) radical. The survey provides a deep census of 1612-, 1665-, 1667- and 1720-MHz OH absorption and emission from the Galactic ISM, and is also an unbiased search for maser sources in these transitions. We present here first results from the SPLASH pilot region, which covers Galactic longitudes 334 to 344 degrees and latitudes of -2 to +2 degrees. Diffuse OH is widely detected in all four transitions, with optical depths that are always small (averaged over the Parkes beam), and with departures from LTE common even in the 1665- and 1667-MHz main lines. To a 3$\sigma$ sensitivity of 30 mK, we find no evidence of OH envelopes extending beyond the CO-bright regions of molecular cloud complexes, and conclude that the similarity of the OH excitation temperature and the level of the continuum background is at least partly responsible for this. We detect masers and maser candidates in all four transitions, approximately 50 per cent of which are new detections. This implies that SPLASH will produce a substantial increase in the known population of ground-state OH masers in the Southern Galactic Plane., Comment: 20 pages, 9 figures, accepted for publication in MNRAS

Published
2014
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23. THE HERSCHEL INVENTORY OF THE AGENTS OF GALAXY EVOLUTION IN THE MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM

Author

Sungeun Kim, Pasquale Panuzzo, Martha L. Boyer, Barbara A. Whitney, William T. Reach, Geoffrey C. Clayton, Chad Engelbracht, E. Montiel, Francisca Kemper, Tracy L. Beck, Thomas P. Robitaille, Alberto D. Bolatto, Marc Sauvage, J.-P. Bernard, Sundar Srinivasan, Albrecht Poglitsch, C. Bot, D. Paradis, K. Okumura, Toshikazu Onishi, S. C. Madden, Joana M. Oliveira, B. A. Sargent, Karl Misselt, Frédéric Galliano, Maud Galametz, L. R. Carlson, Ramin A. Skibba, Monica Rubio, Marta Sewilo, Julia Roman-Duval, C.-H. R. Chen, Margaret Meixner, Aigen Li, Alexander G. G. M. Tielens, Erik Muller, Annie Hughes, Masaaki Otsuka, E. Kwon, Akiko Kawamura, Vianney Lebouteiller, J. Seale, Mikako Matsuura, Brian Babler, Yasuo Fukui, Diane Cormier, Joseph L. Hora, Knox S. Long, J. Th. van Loon, Sacha Hony, Karl D. Gordon, Linda J. Smith, P. Chanial, Remy Indebetouw, Frank P. Israel, 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), Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Matrice extracellulaire et dynamique cellulaire - UMR 7369 (MEDyC), SFR CAP Santé (Champagne-Ardenne Picardie Santé), Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-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, 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), University of California [Los Angeles] (UCLA), University of California, Laboratoire de Génie Civil et Génie Mécanique (LGCGM), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA), Department of Astrophysics [Nagoya], Nagoya University, University of Cambridge [UK] (CAM), Institute of Environmental Systems (SUIKO), Kyushu University [Fukuoka], Institute of Oceanology [China], Earth Consultants International, Department of Physics and Astronomy [UCL London], University College of London [London] (UCL), CQ-VR, Universidade de Trás-os-Montes e Alto Douro, Météo-France [Paris], Météo France, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Centre de recherche de l'hôpital Sainte Justine, CHU Sainte Justine [Montréal], inconnu, Inconnu, 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), 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), 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), University of California (UC), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Kyushu University, Météo-France, Centre de recherche du CHU Sainte-Justine / Research Center of the Sainte-Justine University Hospital [Montreal, Canada], Université de Montréal (UdeM)-CHU Sainte Justine [Montréal], 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), and 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)

Subjects
Luminous infrared galaxy, Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010308 nuclear & particles physics, Young stellar object, Extinction (astronomy), Astronomy, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Interstellar medium, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, 0103 physical sciences, Small Magellanic Cloud, Large Magellanic Cloud, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Cosmic dust, QB
Abstract

We present an overview of the HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) in the Magellanic Clouds project, which is a Herschel Space Observatory open time key program. We mapped the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) at 100, 160, 250, 350, and 500 μm with the Spectral and Photometric Imaging Receiver (SPIRE) and Photodetector Array Camera and Spectrometer (PACS) instruments on board Herschel using the SPIRE/PACS parallel mode. The overriding science goal of HERITAGE is to study the life cycle of matter as traced by dust in the LMC and SMC. The far-infrared and submillimeter emission is an effective tracer of the interstellar medium (ISM) dust, the most deeply embedded young stellar objects (YSOs), and the dust ejected by the most massive stars. We describe in detail the data processing, particularly for the PACS data, which required some custom steps because of the large angular extent of a single observational unit and overall the large amount of data to be processed as an ensemble. We report total global fluxes for the LMC and SMC and demonstrate their agreement with measurements by prior missions. The HERITAGE maps of the LMC and SMC are dominated by the ISM dust emission and bear most resemblance to the tracers of ISM gas rather than the stellar content of the galaxies. We describe the point source extraction processing and the criteria used to establish a catalog for each waveband for the HERITAGE program. The 250 μm band is the most sensitive and the source catalogs for this band have ~25,000 objects for the LMC and ~5500 objects for the SMC. These data enable studies of ISM dust properties, submillimeter excess dust emission, dust-to-gas ratio, Class 0 YSO candidates, dusty massive evolved stars, supernova remnants (including SN1987A), H II regions, and dust evolution in the LMC and SMC. All images and catalogs are delivered to the Herschel Science Center as part of the community support aspects of the project. These HERITAGE images and catalogs provide an excellent basis for future research and follow up with other facilities.

Published
2013
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24. The thermal dust emission in the N158-N159-N160 (LMC) star forming complex mapped by Spitzer, Herschel and LABOCA

Author

Marc Sauvage, Monica Rubio, Maud Galametz, S. C. Madden, Aigen Li, Diane Cormier, Frank P. Israel, M. Albrecht, Frédéric Galliano, Akiko Kawamura, Sacha Hony, J. Seale, E. Montiel, Marta Sewilo, P. Panuzzo, Yasuo Fukui, C. Bot, Vianney Lebouteiller, Julia Roman-Duval, Chad Engelbracht, M. Meixner, Karl Misselt, K. Okumura, J. Th. van Loon, University of Cambridge [UK] (CAM), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Leibniz-Institut für Kristallzüchtung, 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), Steward Observatory, University of Arizona, Department of Astrophysics [Nagoya], Nagoya University, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institute of Environmental Systems (SUIKO), Kyushu University [Fukuoka], Institute of Oceanology [China], 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), Universiteit Leiden, and Kyushu University

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spitzer Space Telescope, 0103 physical sciences, Emissivity, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Molecular cloud, Astronomy, Astronomy and Astrophysics, Mass ratio, Astrophysics - Astrophysics of Galaxies, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a study of the infrared/submm emission of the LMC star forming complex N158-N159-N160. Combining observations from the Spitzer Space Telescope (3.6-70um), the Herschel Space Observatory (100-500um) and LABOCA (870um) allows us to work at the best angular resolution available now for an extragalactic source. We observe a remarkably good correlation between SPIRE and LABOCA emission and resolve the low surface brightnesses emission. We use the Spitzer and Herschel data to perform a resolved Spectral Energy Distribution (SED) modelling of the complex. Using MBB, we derive a global emissivity index beta_c of 1.47. If beta cold is fixed to 1.5, we find an average temperature of 27K. We also apply the Galliano et al. (2011) modelling technique (and amorphous carbon to model carbon dust) to derive maps of the star formation rate, the mean starlight intensity, the fraction of PAHs or the dust mass surface density of the region. We observe that the PAH fraction strongly decreases in the HII regions. This decrease coincides with peaks in the mean radiation field intensity map. The dust surface densities follow the FIR distribution, with a total dust mass of 2.1x10^4 Msolar (2.8 times less than when using graphite grains) in the resolved elements we model. We find a non-negligible amount of dust in the molecular cloud N159 South (showing no massive SF). We also investigate the drivers of the Herschel/PACS and SPIRE submm colours as well as the variations in the gas-to-dust mass ratio (G/D) and the XCO conversion factor in the region N159. We finally model individual regions to analyse variations in the SED shape across the complex and the 870um emission in more details. No measurable submm excess emission at 870um seems to be detected in these regions., Comment: Accepted for publication in MNRAS; 23 pages, 11 figures, 2 tables

Published
2013
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25. Modeling the gamma-ray emission produced by runaway cosmic rays in the environment of RX J1713.7-3946

Author

Hiroaki Yamamoto, Toshikazu Onishi, David I. Jones, Kazufumi Torii, Akiko Kawamura, Gavin Rowell, Felix Aharonian, Sabrina Casanova, Hidetoshi Sano, Yasuo Fukui, Stefano Gabici, Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Dublin Institute for Advanced Studies (DIAS), Department of Astrophysics [Nagoya], Nagoya University, APC - Astrophysique des Hautes Energies (APC - AHE), 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)-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)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), School of Chemistry and Physics, University of Adelaide, Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), 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 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), 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)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), and Gabici, Stefano

Subjects
ISM: cosmic rays, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma rays: theory, ISM: clouds, 01 natural sciences, 7. Clean energy, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], 13. Climate action, Space and Planetary Science, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants
Abstract

Diffusive shock acceleration in supernova remnants is the most widely invoked paradigm to explain the Galactic cosmic ray spectrum. Cosmic rays escaping supernova remnants diffuse in the interstellar medium and collide with the ambient atomic and molecular gas. From such collisions gamma-rays are created, which can possibly provide the first evidence of a parent population of runaway cosmic rays. We present model predictions for the GeV to TeV gamma-ray emission produced by the collisions of runaway cosmic rays with the gas in the environment surrounding the shell-type supernova remnant RX J1713.7-3946. The spectral and spatial distributions of the emission, which depend upon the source age, the source injection history, the diffusion regime and the distribution of the ambient gas, as mapped by the LAB and NANTEN surveys, are studied in detail. In particular, we find for the region surrounding RX J1713-3946, that depending on the energy one is observing at, one may observe startlingly different spectra or may not detect any enhanced emission with respect to the diffuse emission contributed by background cosmic rays. This result has important implications for current and future gamma-ray experiments., Comment: version published on PASJ

Published
2010
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26. AKARI and BLAST Observations of the Cassiopeia A Supernova Remnant and Surrounding Interstellar Medium

Author

Ho-Gyu Lee, Mark J. Devlin, Peter Charles Hargrave, Joshua O. Gundersen, Carole Tucker, Hidehiro Kaneda, Marco P. Viero, James J. Bock, Luca Olmi, Jeff Klein, Bon-Chul Koo, Calvin B. Netterfield, David H. Hughes, Peter G. Martin, Marie Rex, Douglas Scott, Dae-Sik Moon, Philip Daniel Mauskopf, Matthew Joseph Griffin, Peter A. R. Ade, Bruce Sibthorpe, Enzo Pascale, Woong-Seob Jeong, Christopher Semisch, Mark Halpern, Guillaume Patanchon, Gregory S. Tucker, G. Marsden, Donald V. Wiebe, Edward L. Chapin, Matthew D. P. Truch, Simon Dicker, A. Roy, UK Astronomy Technology Centre, Royal Observatory Edinburgh (UKATC), Cardiff University, Jet Propulsion Laboratory, California Institute of Technology (JPL), Department of Physics and Astronomy, University of British Columbia, Department of Physics and Astronomy, University of Pennsylvania, Department of Physics, University of Miami, Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE), Korea Astronomy and Space Science Institute (KASI), Department of Astrophysics, Nagoya University, Department of Physics and Astronomy, Seoul National University, Canadian Institute for Theoretical Astrophysics, McLennan Physical Laboratories, University of Toronto (CITA), Department of Astronomy and Astrophysics, University of Toronto, Istituto di Radioastronomia, Firenze, 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), and Department of Physics, Brown University

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Population, Extinction (astronomy), Early universe, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: supernova remnants, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Supernova remnant, education, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, education.field_of_study, Redshift, Interstellar medium, Cassiopeia A, Supernova, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract

We use new large area far infrared maps ranging from 65 - 500 microns obtained with the AKARI and the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) missions to characterize the dust emission toward the Cassiopeia A supernova remnant (SNR). Using the AKARI high resolution data we find a new "tepid" dust grain population at a temperature of ~35K and with an estimated mass of 0.06 solar masses. This component is confined to the central area of the SNR and may represent newly-formed dust in the unshocked supernova ejecta. While the mass of tepid dust that we measure is insufficient by itself to account for the dust observed at high redshift, it does constitute an additional dust population to contribute to those previously reported. We fit our maps at 65, 90, 140, 250, 350, and 500 microns to obtain maps of the column density and temperature of "cold" dust (near 16 K) distributed throughout the region. The large column density of cold dust associated with clouds seen in molecular emission extends continuously from the surrounding interstellar medium to project on the SNR, where the foreground component of the clouds is also detectable through optical, X-ray, and molecular extinction. At the resolution available here, there is no morphological signature to isolate any cold dust associated only with the SNR from this confusing interstellar emission. Our fit also recovers the previously detected "hot" dust in the remnant, with characteristic temperature 100 K., Accepted for publication in the Astrophysical Journal. Maps and related data are available at http://blastexperiment.info/

Published
2009
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27. Molecular line mapping of the giant molecular cloud associated with RCW 106 – II. Column density and dynamical state of the clumps

Author

Arthur Vigan, Yasuo Fukui, K. L. Thomas, Steven N. Longmore, Maria Cunningham, Tony Wong, Paul A. Jones, D. Brisbin, Indra Bains, Michael G. Burton, Carsten Kramer, Nadia Lo, Bhaswati Mookerjea, E. F. Ladd, Akiko Kawamura, Swinburne University of Technology (Hawthorn campus), Bucknell University, University of New South Wales [Sydney] (UNSW), 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), KOSMA, I. Physikalisches Institut, Universität zu Köln = University of Cologne, Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Department of Astrophysics [Nagoya], Nagoya University, Institute of Environmental Systems (SUIKO), Kyushu University, 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), Universität zu Köln, and Kyushu University [Fukuoka]

Subjects
stars, ISM: structure, Binding energy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ISM: clouds, Virial theorem, Luminosity, Gravitation, clouds -ISM, 0103 physical sciences, Optical depth (astrophysics), structure, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, formation -ISM, stars: formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Molecular cloud, Astrophysics (astro-ph), molecules -ISM, Astronomy and Astrophysics, Galactic plane, ISM: molecules, Space and Planetary Science, Mass spectrum
Abstract

We present a fully sampled C^{18}O (1-0) map towards the southern giant molecular cloud (GMC) associated with the HII region RCW 106, and use it in combination with previous ^{13}CO (1-0) mapping to estimate the gas column density as a function of position and velocity. We find localized regions of significant ^{13}CO optical depth in the northern part of the cloud, with several of the high-opacity clouds in this region likely associated with a limb-brightened shell around the HII region G333.6-0.2. Optical depth corrections broaden the distribution of column densities in the cloud, yielding a log-normal distribution as predicted by simulations of turbulence. Decomposing the ^{13}CO and C^{18}O data cubes into clumps, we find relatively weak correlations between size and linewidth, and a more sensitive dependence of luminosity on size than would be predicted by a constant average column density. The clump mass spectrum has a slope near -1.7, consistent with previous studies. The most massive clumps appear to have gravitational binding energies well in excess of virial equilibrium; we discuss possible explanations, which include magnetic support and neglect of time-varying surface terms in the virial theorem. Unlike molecular clouds as a whole, the clumps within the RCW 106 GMC, while elongated, appear to show random orientations with respect to the Galactic plane., Comment: 17 pages, to appear in MNRAS

Published
2008
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28. The two Titan stellar occultations of 14 November 2003

Author

M. Kidger, H. Lüdemann, B. Thomé, F. Bode, Daisuke Baba, C. Martinez, François Colas, C. Tegtmeier, D. Fiel, Jean Lecacheux, Takahiro Nagayama, M. Kretlow, P. Schoenau, T. Payet, Françoise Roques, S. Renner, Brian Fraser, Ian S. Glass, M. Rapaport, H. J. Bode, D. Neubauer, M. Hernandez, P. Meintjies, J. P. Teng, Robert R. Howell, C. Turk, S. Lacour, W. Beisker, F. Hund, C. Etienne, O. Naranjo, Bruno Sicardy, Tetsuya Nagata, Thomas Widemann, A. Bellucci, Terry J. Jones, Francesca Ferri, K.-L. Bath, E. Frappa, S. Itting-Enke, J. Lüdemann, A. Jansen, Agnes Fienga, Emmanuel Lellouch, A. Tegtmeier, G. Hesler, J. L. Ortiz, S. Pau, P. Rosenzweig, A. Peyrot, M. Vignand, C. DeWitt, 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, Ingénieurs, Techniciens et Administratifs, Pôle Planétologie du LESIA, 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 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 Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), International Occultation Timing Association, European Section (IOTA/ES), Centro Interdipartimentale di Studi e Attività Spaziali 'Giuseppe Colombo', Università di Padova (CISAS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Instituto Superior de Ciencias Astronómicas, South African Astronomical Observatory (SAAO), Department of Astrophysics, Nagoya University, Windhoek, Hakos Guestfarm, Astronomical Society of Southern Africa, Boyden Observatory, University of the Free State, Association des Utilisateurs de Détecteurs Electroniques (AUDE), Association des Utilisateurs de Détecteurs Electroniques, Lycée Stanislas, Paris, Astronef-Planétarium de Saint-Etienne, Observatoire astronomique des Makes, Association Réunionnaise pour l'Etude du Ciel Austral (ARECA), Wyoming InfraRed Observatory, Department of Physics and Astronomy, Instituto de Astrofísica de Canarias (IAC), Instituto de Astrofisica de Andalucia, CSIC (IAA), Universidad de Los Andes, Facultad de Ciencias, Departamento de Física, Grupo de Astrofísica Teórica, Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Atmospheric Science, Haze, Equator, Soil Science, Aquatic Science, Oceanography, Atmospheric sciences, Latitude, symbols.namesake, Altitude, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Southern Hemisphere, Stratosphere, Earth-Surface Processes, Water Science and Technology, Ecology, Paleontology, Forestry, Light curve, Geophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], symbols, Titan (rocket family), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology
Abstract

[1] We report the observation of two stellar occultations by Titan on 14 November 2003, using stations in the Indian Ocean, southern Africa, Spain, and northern and southern Americas. These occultations probed altitudes between ∼550 and 250 km (∼1 to 250 μbar) in Titan's upper stratosphere. The light curves reveal a sharp inversion layer near 515 ± 6 km altitude (1.5 μbar pressure level), where the temperature increases by 15 K in only 6 km. This layer is close to an inversion layer observed fourteen months later by the Huygens HASI instrument during the entry of the probe in Titan's atmosphere on 14 January 2005 [Fulchignoni et al., 2005]. Central flashes observed during the first occultation provide constraints on the zonal wind regime at 250 km, with a strong northern jet (∼200 m s -1 ) around the latitude 55°N, wind velocities of ∼150 m s -1 near the equator, and progressively weaker winds as more southern latitudes are probed. The haze distribution around Titan's limb at 250 km altitude is close to that predicted by the Global Circulation Model of Rannou et al. (2004) in the southern hemisphere, but a clearing north of 40°N is necessary to explain our data. This contrasts with Rannou et al.'s (2004) model, which predicts a very thick polar hood over Titan's northern polar regions. Simultaneous observations of the flashes at various wavelengths provide a dependence of τ ∝ λ -q , with q = 1.8 ± 0.5 between 0.51 and 2.2 μm for the tangential optical depth of the hazes at 250 km altitude.

Published
2006
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29. Imbricate architecture of the upper Paleozoic to Jurassic oceanic Cache Creek Terrane, central British Columbia

Author

Lambertus C. Struik, Henriette Lapierre, Hiroyoshi Sano, Michael J. Orchard, Marc Tardy, P. Schiarizza, Fabrice Cordey, D. G. MacIntyre, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Department of Astrophysics [Nagoya], Nagoya University, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Basalt, 010504 meteorology & atmospheric sciences, Paleozoic, Permian, Geochemistry, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 010502 geochemistry & geophysics, Ophiolite, 01 natural sciences, Conglomerate, Paleontology, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, Sedimentary rock, Siltstone, Geology, 0105 earth and related environmental sciences, Terrane
Abstract

International audience; Upper Paleozoic to Lower Jurassic oceanic rocks of the Cache Creek Terrane near Fort St. James, in central British Columbia, form a stack of thrust sheets cut by steeply dipping strike-slip faults. Paleontologically dated upper Paleozoic strata include bioclastic shallow-water limestone and ribbon chert. Isotopically dated Permian rocks consist of tonalite sills and stocks and rhyolite flows intercalated with basalt flows. Paleontologically dated lower Mesozoic rocks include greywacke, sandstone, siltstone, argillite, ribbon chert, conglomerate, limestone, and basalt tuff. Trembleur Ultramafite unit of the Cache Creek Complex, in places part of an ophiolite suite, forms thrust sheets and klippen that overlie lower Mesozoic sedimentary rocks. Sedimentological, lithochemical, paleontological, petrological, and textural comparisons with other areas and established models demonstrate that Cache Creek Terrane is an accretionary complex, a structurally stacked assemblage of rocks that originated in diverse and disparate oceanic paleoenvironments. These environments include spreading ridge, oceanic plateau, atoll, trench fill, and possibly arc. Internal imbrication of the terrane is as young as Early Jurassic, as determined from fossil evidence, and the minimum age of obduction of the thrust stack westward onto Stikine Terrane is Middle Jurassic, as determined from dating of a crosscutting pluton. Triassic blueschist and eclogite of Cache Creek Terrane are interpreted to have been primarily uplifted to upper crustal levels during Triassic subduction. Cache Creek Terrane, as a remnant of that subduction process, and caught in the collision between Stikine and Quesnel terranes, marks the position of a lithosphere-scale suture zone, the Pinchi Suture.; Les roches océaniques du terrane de Cache Creek (Paléozoïque supérieur à Jurassique inférieur), près de Fort St. James, au centre de la Colombie-Britannique forment un empilement de nappes de charriage recoupé par des failles de décrochement à pendage abrupt. Les strates du Paléozoïque supérieur, datées par la paléontologie, comprennent des calcaires bioclastiques d'eau peu profonde et des cherts rubanés. Les roches du Permien, datées par analyse isotopique, comprennent des filons-couches et des petits intrusifs de tonalite ainsi que des écoulements de rhyolite intercalés avec des écoulements de basaltes. Les roches du Mésozoïque inférieur, datées par la paléontologie, comprennent des grauwackes, des grès, des microgrès, des argilites, des cherts rubanés, des conglomérats, des calcaires et des tufs basaltiques. L'unité ultramafique Trembleur du complexe de Cache Creek, qui à certains endroits fait partie d'une suite ophiolitique, forme des nappes de charriage et des klippes qui reposent sur les roches sédimentaires du Mésozoïque inférieur. Des comparaisons sédimentologiques, lithochimiques, paléontologiques, pétrologiques et texturales avec d'autres régions et avec des modèles établis démontrent que le terrane de Cache Creek est un complexe formé par accrétion, un assemblage de roches empilées structurellement qui proviennent de paléoenvironnements divers et disparates. Ces environnements océaniques comprennent des crêtes qui s'écartent, des plateaux océaniques, des atolls, des remplissages de fosses et possiblement des arcs. Une imbrication interne du terrane s'est effectuée aussi tôt que le Jurassique précoce, tel qu'il a été déterminé par des évidences de fossiles, et l'âge minimum pour l'obduction de l'empilement de charriage vers l'ouest sur le terrane de Stikine serait du Jurassique moyen, tel que déterminé par la datation d'un pluton qui le recoupe. Le schiste bleu et l'éclogite du terrane de Cache Creek (du Trias) sont interprétés comme ayant été principalement soulevés à des niveaux supérieurs de la croûte au cours de la subduction au Trias. Le terrane de Cache Creek, en tant que lambeau de ce processus de subduction pris dans la collision entre les terranes de Stikine et Quesnel, marque la position d’une zone de suture à l’échelle de la lithosphère, soit la suture Pinchi.

Published
2001
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30. Biostratigraphic and biogeographic constraints on the Carboniferous to Jurassic Cache Creek Terrane in central British Columbia

Author

H. J. Taylor, E. W. Bamber, Fabrice Cordey, Lambertus C. Struik, Bernard Mamet, Hiroyoshi Sano, L. Rui, Michael J. Orchard, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Department of Astrophysics [Nagoya], Nagoya University, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010506 paleontology, Radiolaria [radiolarians], Permian, Early Triassic, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Foraminifera, Jurassic, 010502 geochemistry & geophysics, 01 natural sciences, Paleontology, Carboniferous, Conodonta, 14. Life underwater, Anthozoa [Sea anemones], 0105 earth and related environmental sciences, Terrane, geography, geography.geographical_feature_category, biology, Canada, British Columbia, Ladinian, 15. Life on land, biology.organism_classification, Triassic, Craton, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, Sedimentary rock, Conodont, Geology
Abstract

International audience; Conodonts, radiolarians, foraminiferids, and corals provide constraints on the geology and tectonics of the Nechako region. They also support the notion that the Cache Creek Terrane is allochthonous with respect to the North American craton. The 177 conodont collections, assigned to 20 faunas, range in age from Bashkirian (Late Carboniferous) to Norian (Late Triassic); 70 radiolarian collections representing 12 zones range from Gzhelian (Late Carboniferous) to Toarcian (Early Jurassic); 335 collections assigned to 11 fusulinacean assemblages (with associated foram-algal associations) range from Bashkirian to Wordian (Middle Permian); and two coral faunas are of Bashkirian and Wordian age. The fossils document a long but sporadic history of sedimentary events within the Cache Creek Complex that included two major carbonate buildups in the Late Carboniferous (Pope limestone) and Middle Permian (Copley limestone), punctuated by intervening Early Permian deepening; basaltic eruptions during the mid Carboniferous and mid Permian; the onset of oceanic chert sedimentation close to the Carboniferous–Permian boundary and its persistence through the Late Triassic (Sowchea succession); latest Permian and Early Triassic mixed clastics and volcanics (Kloch Lake succession); Middle and Late Triassic reworking of carbonates (Whitefish limestone), including cavity fill in older limestones (Necoslie breccia), and fine-grained clastic sedimentation extending into the Early Jurassic (Tezzeron succession). Tethyan, eastern Pacific, and (or) low-latitude biogeographic attributes of the faunas are noted in the Gzhelian (fusulines), Artinskian (conodonts, fusulines), Wordian (fusulines, corals, conodonts), and Ladinian (conodonts, radiolarians). The Cache Creek Terrane lay far to the west of the North American continent during these times.; Les conodontes, radiolaires, foraminiféridés et les coraux améliorent les données géologiques et tectoniques de la région de Nechako. Ils appuient aussi la notion que le terrane de Cache Creek est allochtone par rapport au craton nord-américain. Cent soixante-dix-sept collections de conodontes, assignés à 20 faunes, ont des âges allant du Bashkirien (Carbonifère tardif) au Norien (Trias tardif); 70 collections de radiolaires représentant 12 zones vont du Gzelien (Carbonifère tardif) au Toarcien (Jurassique précoce); 335 collections assignées à 11 assemblages de fusulinides (avec des associations foraminifères-algues associées) vont du Bashkirien au Wordien (Permien moyen) et deux faunes coralliennes sont du Bashkirien et du Wordien. Les fossiles enregistrent un historique long mais sporadique d'événements sédimentaires à l'intérieur du complexe de Cache Creek qui comprend deux grandes formation carbonatées au Carbonifère tardif (calcaire Pope) et au Permien moyen (calcaire Copley) ponctuées par un nouvel approfondissement au Permien précoce; des éruptions basaltiques au cours du Carbonifère moyen et du Permien moyen; le déclenchement de la sédimentation océanique de chert près de la limite Carbonifère-Permien et sa persistance à travers le Trias tardif (séquence de Sowchea); des mélanges de clastiques et de volcaniques au Permien terminal et au Trias précoce (séquence de Kloch Lake); le remaniement des carbonates (calcaire de Whitefish) au Trias moyen et tardif, comprenant le remplissage de cavités dans des calcaires plus âgés (brèche de Necoslie) et une sédimentation clastique à grains fins se poursuivant jusqu'au Jurassique précoce (séquence de Tezzeron). Des attributs biogéographiques du genre téthysien, de l'est du Pacifique et (ou) de basse latitude, sont notés dans les faunes du Gzelien (Fusulines) de l'Artinskien (conodontes, fusulines), du Wordien (fusulines, coraux, conodontes) et du Ladinien (conodontes, radiolaires). Le terrane de Cache Creek était potentillement très éloigné à l'ouest du continent nord-américain durant ces époques.

Published
2001
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31. Molecular loops in the galactic center: evidence for magnetic flotation.

Author

Fukui Y, Yamamoto H, Fujishita M, Kudo N, Torii K, Nozawa S, Takahashi K, Matsumoto R, Machida M, Kawamura A, Yonekura Y, Mizuno N, Onishi T, and Mizuno A

Abstract

The central few hundred parsecs of the Milky Way host a massive black hole and exhibit very violent gas motion and high temperatures in molecular gas. The origin of these properties has been a mystery for the past four decades. Wide-field imaging of the (12)CO (rotational quantum number J = 1 to 0) 2.6-millimeter spectrum has revealed huge loops of dense molecular gas with strong velocity dispersions in the galactic center. We present a magnetic flotation model to explain that the formation of the loops is due to magnetic buoyancy caused by the Parker instability. The model has the potential to offer a coherent explanation for the origin of the violent motion and extensive heating of the molecular gas in the galactic center.

Published
2006
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32. Laboratory detection of a new interstellar free radical CH2CN(2B1).

Author

Saito S, Yamamoto S, Irvine WM, Ziurys LM, Suzuki H, Ohishi M, and Kaifu N

Subjects
Astronomical Phenomena, Astronomy, Chemical Phenomena, Chemistry, Microwaves, Models, Molecular, Spectrum Analysis, Acetonitriles analysis, Extraterrestrial Environment, Free Radicals analysis, Hydrocarbons analysis
Abstract

An asymmetric-top free radical CH2CN, which as a 2B1 ground state, was detected for the first time by laboratory microwave spectroscopy. The radical was produced in a free-space absorption cell by a DC glow discharge in pure CH3CN gas. About 60 fine-structure components were observed for the N = 11-10 to 14-13 a-type rotational transitions in the frequency region of 220-260 GHz, and many hyperfine resolved components for the N = 4-3 and 5-4 transitions in the 80 and 100 GHz regions, respectively. The molecular constants, including the rotational constants, centrifugal distortion constants, and spin-rotation coupling constants with centrifugal distortion correction terms were determined from the fine-structure resolved transitions, and the hyperfine coupling constants due to the hydrogen and nitrogen nuclei were obtained from the low-N transitions. As a result we assigned U100602 and U80484 from Sgr B2, and U40240 and U20120 from TMC-1, to the N = 5-4, 4-3, 2-1, and 1-0 transitions with K-1 = 0 of the CH2CN radical.

Published
1988
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