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Your search keyword '"Department of Astrophysics [Nagoya]"' showing total 9 results
Start Over Author "Department of Astrophysics [Nagoya]" Topic astrophysics::cosmology and extragalactic astrophysics
9 results on '"Department of Astrophysics [Nagoya]"'

1. 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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2. 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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3. 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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4. 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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5. 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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6. 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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7. 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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8. 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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9. 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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