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1. Origins Space Telescope: trades and decisions leading to the baseline mission concept

Author

David Leisawitz, David C. Redding, John Steeves, Greg Feller, Martina C. Wiedner, Charles R. Lawrence, Jonathan W. Arenberg, James Bauer, Deborah Padgett, Johannes Staguhn, Jonathan J. Fortney, Thomas P. Greene, Alison Nordt, Gerard L. Rafanelli, Paul A. Lightsey, Matthew East, Edward Amatucci, Asantha Cooray, Bret G. Drake, Damon Bradley, Ray Bell, Klaus M. Pontoppidan, Jonas Zmuidzinas, Kate Y. L. Su, J. Booth, Kevin B. Stevenson, Edwin A. Bergin, Cara Battersby, Dominic Benford, John C. Mather, Larry Dewell, Samuel H. Moseley, Lee Armus, Zachary A. Granger, Angel Flores, C. Sandin, Edward L. Wright, Joaquin Vieira, George H. Rieke, Gary J. Melnick, Kartik Sheth, Tiffany Kataria, Charles M. Bradford, John S. Knight, James A. Corsetti, Ruth Carter, Desika Narayanan, Michael J. DiPirro, Karin Sandstrom, Lynn N. Allen, Sean Carey, Lawrence M. Sokolsky, David Yanatsis, Joseph M. Howard, Alexandra Pope, Kimberly Ennico, Stefanie N. Milam, Cassandra Webster, Craig W. McMurtry, Anita Sengupta, Margaret Meixner, Thomas L. Roellig, Itsuki Sakon, C. Wu, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)

Subjects
Computer science, Space (commercial competition), 01 natural sciences, 7. Clean energy, law.invention, 010309 optics, Telescope, Spitzer Space Telescope, law, 0103 physical sciences, Architecture, Baseline (configuration management), 010303 astronomy & astrophysics, Instrumentation, Scientific instrument, [PHYS]Physics [physics], Planetary habitability, Mechanical Engineering, James Webb Space Telescope, Astronomy and Astrophysics, Electronic, Optical and Magnetic Materials, 13. Climate action, Space and Planetary Science, Control and Systems Engineering, Systems engineering, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the universe today? How do habitable planets form? How common are life-bearing worlds? We describe how Origins was designed to answer these alluring questions. We discuss the key decisions taken by the Origins mission concept study team, the rationale for those choices, and how they led through an exploratory design process to the Origins baseline mission concept. To understand the concept solution space, we studied two distinct mission concepts and descoped the second concept, aiming to maximize science per dollar and hit a self-imposed cost target. We report on the study approach and describe the concept evolution. The resulting baseline design includes a 5.9-m diameter telescope cryocooled to 4.5 K and equipped with three scientific instruments. The chosen architecture is similar to that of the Spitzer Space Telescope and requires very few deployments after launch. The cryo-thermal system design leverages James Webb Space Telescope technology and experience.

Published
2021
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2. The Life Cycle of Dust

Author

Sarah Sadavoy, Mikako Matsuura, Lee Armus, Cara Battersby, Caitlin Casey, Christopher Clark, Asantha Cooray, Karine Demyk, Neal Evans, Karl Gordon, Frédéric Galliano, Maryvonne Gerin, Benne Holwerda, Nia Imara, Doug Johnstone, Alvaro Labiano, David Leisawitz, Wanggi Lim, Leslie Looney, Margaret Meixner, Eric Murphy, Roberta Paladini, Julia Roman-Duval, Karin Sandstrom, John-David Smith, Ian Stephens, Nathalie Ysard, University of Manchester [Manchester], Cornell University [New York], California Institute of Technology (CALTECH), Centre d'étude spatiale des rayonnements (CESR), 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, CSIRO Entomology, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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), École normale supérieure - Paris (ENS-PSL), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cornell University, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), and Galliano, Frédéric

Subjects
[PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR.GA] Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

Dust offers a unique probe of the interstellar medium (ISM) across multiple size, density, and temperature scales. Dust is detected in outflows of evolved stars, star-forming molecular clouds, planet-forming disks, and even in galaxies at the dawn of the Universe. These grains also have a profound effect on various astrophysical phenomena from thermal balance and extinction in galaxies to the building blocks for planets, and changes in dust grain properties will affect all of these phenomena. A full understanding of dust in all of its forms and stages requires a multi-disciplinary investigation of the dust life cycle. Such an investigation can be achieved with a statistical study of dust properties across stellar evolution, star and planet formation, and redshift. Current and future instrumentation will enable this investigation through fast and sensitive observations in dust continuum, polarization, and spectroscopy from near-infrared to millimeter wavelengths., Science white paper submitted to the Astro2020 Decadal Survey

Published
2019

3. SPICA —A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Author

M. Kawada, B. Larsson, D. Arrazola, Brian Jackson, C.M. Bradford, Lee Armus, K. Shinozaki, Hiroshi Shibai, Francisca Kemper, N. Isobe, I. Funaki, R. Huisman, M. Giard, L. Duband, Shiang-Yu Wang, P. Khosropanah, Shinki Oyabu, P. P. Kooijman, R. Shipman, Daisuke Ishihara, I. Charles, L. Rodriguez, V. Reveret, S. Withington, Frank Helmich, Kotaro Kohno, Willem Jellema, Pieter Dieleman, M. Audard, T. Wada, B. Vandenbussche, D. van Loon, A. Di Giorgio, Peter Roelfsema, David A. Naylor, I. Sakon, H. Ogawa, G. de Lange, Franz Kerschbaum, J. Kwon, R. Hijmering, W. M. Laauwen, J. van der Kuur, Jaap Evers, Francisco Najarro, Inga Kamp, Takashi Onaka, Albrecht Poglitsch, T. Yamada, L. M. González Fernández, H. Jacobs, S. C. Madden, Hidehiro Kaneda, Yasuo Doi, Jian-Rong Gao, C. K. Wafelbakker, H. van Weers, M. Eggens, I. Yamamura, L. Spinoglio, H. Matsuhara, Oliver Krause, T. Suzuki, Takao Nakagawa, Matthew Joseph Griffin, F. F. S. van der Tak, H. Sugita, Michael D. Audley, Y. Sato, J. Torres Redondo, 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), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], Institut Nanosciences et Cryogénie (INAC), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Massachusetts Institute of Technology (MIT), inconnu, Inconnu, 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), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), School of Physics and Astronomy [Cardiff], Cardiff University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], AUTRES, National Institute for Subatomic Physics [Amsterdam] (NIKHEF), 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), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics, Nara Women's University, Department of Environmental and Materials Engineering, Nagoya Institute, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), Antarctic Research a European Network for Astrophysics (ARENA), Nanomaterials Research Institute, foreign laboratories (FL), CERN [Genève], SRON Netherlands Institute for Space Research (SRON), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), NASA Goddard Space Flight Center (GSFC), Astronomy, Université de Genève = University of Geneva (UNIGE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), 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), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)

Subjects
infrared: galaxies, infrared: general, infrared: planetary systems, instrumentation: photometers, instrumentation: spectrographs, space vehicles: instruments, Astrophysics - Instrumentation and Methods for Astrophysics, instruments [space vehicles], Direct assessment, Infrared, media_common.quotation_subject, Infrared wavelength, FOS: Physical sciences, Spica, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Space (mathematics), 01 natural sciences, galaxies [infrared], infrared: galaxies, Spitzer Space Telescope, 0103 physical sciences, photometers [instrumentation], space vehicles: instruments, 010306 general physics, infrared: planetary systems, planetary systems [infrared], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, general [infrared], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, instrumentation: spectrographs, MISSION, Luminous infrared galaxy, Physics, Science & Technology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Universe, instrumentation: photometers, SPITZER, Space and Planetary Science, Physical Sciences, Astrophysics::Earth and Planetary Astrophysics, infrared: general, Astrophysics - Instrumentation and Methods for Astrophysics, spectrographs [instrumentation]
Abstract

著者人数: 70名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 芝井, 広; 船木, 一幸; 磯部, 直樹; 川田, 光伸; 權, 靜美; 松原, 英雄; 中川, 貴雄; 小川, 博之; 佐藤, 洋一; 篠崎, 慶亮; 杉田, 寛之; 和田, 武彦; 山田, 亨; 山村, 一誠), Number of authors: 70(Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Shibai, Hiroshi; Funaki, Ikkoh; Isobe, Naoki; Kawada, Mitsunobu; Kwon, Jungmi; Matsuhara, Hideo; Nakagawa, Takao; Ogawa, Hiroyuki; Sato, Yoichi; Shinozaki, Keisuke; Sugita, Hiroyuki; Wada, Takehiko; Yamada, Toru; Yamamura, Issei), 資料番号: SA1180106000

Published
2018
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4. Probing highly obscured, self-absorbed galaxy nuclei with vibrationally excited HCN

Author

Roberto Neri, Carsten Henkel, Francoise Combes, Thomas R. Greve, Gary A. Fuller, P. van der Werf, Francesco Costagliola, Eduardo González-Alfonso, Susanne Aalto, Sergio Martín, Eckhard Sturm, José Cernicharo, Lee Armus, Santiago García-Burillo, S. Muhle, Aaron S. Evans, M. Spaans, K. Sakamoto, Sebastien Muller, S. Viti, Chalmers University of Technology [Göteborg], Centre de Recherches du Service de Santé des Armées (CRSSA), Service de Santé des Armées, Universidad de Alcalá - University of Alcalá (UAH), General Electric Medical Systems [Buc] (GE Healthcare), General Electric Medical Systems, Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Institut für Physik (Institut für Physik), Universität Potsdam, Astronomy, Observatorio Astronomico Nacional, Madrid, Universiteit Leiden, École normale supérieure - Paris (ENS-PSL), Collège de France - Chaire Galaxies et cosmologie, Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and University of Potsdam = Universität Potsdam

Subjects
Continuum absorption, Active galactic nucleus, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, High resolution, FOS: Physical sciences, Self-absorbed, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, ISM [Galaxies], molecules [ISM], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, Luminous infrared galaxy, [PHYS]Physics [physics], Supermassive black hole, Astronomy, Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, ISM: molecules, Space and Planetary Science, nuclei [Galaxies], Excited state, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: nuclei, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

We present high resolution (0."4) IRAM PdBI and ALMA mm and submm observations of the (ultra) luminous infrared galaxies ((U)LIRGs) IRAS17208-0014, Arp220, IC860 and Zw049.057 that reveal intense line emission from vibrationally excited ($��_2$=1) J=3-2 and 4-3 HCN. The emission is emerging from buried, compact (r$$5\times 10^{13}$ L$_{\odot}$ kpc$^{-2}$. These nuclei are likely powered by accreting supermassive black holes (SMBHs) and/or hot (>200 K) extreme starbursts. Vibrational, $��_2$=1, lines of HCN are excited by intense 14 micron mid-infrared emission and are excellent probes of the dynamics, masses, and physical conditions of (U)LIRG nuclei when H$_2$ column densities exceed $10^{24}$ cm$^{-2}$. It is clear that these lines open up a new interesting avenue to gain access to the most obscured AGNs and starbursts. Vibrationally excited HCN acts as a proxy for the absorbed mid-infrared emission from the embedded nuclei, which allows for reconstruction of the intrinsic, hotter dust SED. In contrast, we show strong evidence that the ground vibrational state ($��$=0), J=3-2 and 4-3 rotational lines of HCN and HCO$^+$ fail to probe the highly enshrouded, compact nuclear regions owing to strong self- and continuum absorption. The HCN and HCO$^+$ line profiles are double-peaked because of the absorption and show evidence of non-circular motions - possibly in the form of in- or outflows. Detections of vibrationally excited HCN in external galaxies are so far limited to ULIRGs and early-type spiral LIRGs, and we discuss possible causes for this. We tentatively suggest that the peak of vibrationally excited HCN emission is connected to a rapid stage of nuclear growth, before the phase of strong feedback., 13 pages, 7 figures, accepted for publication in Astronomy and Astrophysics

Published
2015
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5. Spatially resolved Spitzer-IRS spectral maps of the superwind in M82

Author

J. D. Smith, Charles G. Hoopes, Patrick L. Shopbell, Fabian Walter, P. Beirao, Lee Armus, Kartik Sheth, David Hollenbach, Jason Surace, F. Boulanger, Charles W. Engelbracht, Pierre Guillard, Timothy M. Heckman, Matthew D. Lehnert, Bruce T. Draine, 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), Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), Spitzer Science Center, California Institute of Technology, Pasadena, California Institute of Technology (CALTECH), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), AUTRES, Steward Observatory, University of Arizona, École normale supérieure - Paris (ENS Paris), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Population, FOS: Physical sciences, Flux, Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, Emission spectrum, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Line (formation), Luminous infrared galaxy, Physics, [PHYS]Physics [physics], education.field_of_study, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Outflow, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We have mapped the superwind/halo region of the nearby starburst galaxy M82 in the mid-infrared with $Spitzer-IRS$. The spectral regions covered include the H$_2 S(1)-S(3)$, [NeII], [NeIII] emission lines and PAH features. We estimate the total warm H$_2$ mass and the kinetic energy of the outflowing warm molecular gas to be between $M_{warm}\sim5-17\times10^6$ M$_{\odot}$ and $E_{K}\sim6-20\times10^{53}$ erg. Using the ratios of the 6.2, 7.7 and 11.3 micron PAH features in the IRS spectra, we are able to estimate the average size and ionization state of the small grains in the superwind. There are large variations in the PAH flux ratios throughout the outflow. The 11.3/7.7 and the 6.2/7.7 PAH ratios both vary by more than a factor of five across the wind region. The Northern part of the wind has a significant population of PAH's with smaller 6.2/7.7 ratios than either the starburst disk or the Southern wind, indicating that on average, PAH emitters are larger and more ionized. The warm molecular gas to PAH flux ratios (H$_2/PAH$) are enhanced in the outflow by factors of 10-100 as compared to the starburst disk. This enhancement in the H$_2/PAH$ ratio does not seem to follow the ionization of the atomic gas (as measured with the [NeIII]/[NeII] line flux ratio) in the outflow. This suggests that much of the warm H$_2$ in the outflow is excited by shocks. The observed H$_2$ line intensities can be reproduced with low velocity shocks ($v < 40$ km s$^{-1}$) driven into moderately dense molecular gas ($10^2, Comment: 19 pages and 12 figures; accepted in MNRAS

Published
2015
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6. Erratum: 'Accretion-Inhibited Star formation in the Warm Molecular Disk of the Green-valley Elliptical Galaxy NGC 3226?' (2014, ApJ, 797, 117)

Author

Lee Armus, Theodoros Bitsakis, Ute Lisenfeld, Carole Mundell, Katherine Alatalo, Mark Lacy, P. N. Appleton, P. M. Ogle, Vassilis Charmandaris, Pierre-Alain Duc, NASA Herschel Science Center, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH)-California Institute of Technology (CALTECH), Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), National Radio Astronomy Observatory, Charlottesville (NRAO), Spitzer Science Center, California Institute of Technology (SSC), Crete Center for Theoretical Physics, Department of Physics, Observatoire de Paris, Université Paris sciences et lettres (PSL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Universidad de Granada = University of Granada (UGR), and Infrared Processing Analysis Center, California Institute of Technology (IPAC)

Subjects
Physics, Space and Planetary Science, Star formation, Observatory, Elliptical galaxy, Astronomy, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Infrared Processing and Analysis Center, Accretion (astrophysics)
Abstract

P-A. Duc, U. Lisenfeld, and P. Ogle 1 NASA Herschel Science Center, Infrared Processing and Analysis Center, Caltech, 770S Wilson Av., Pasadena, CA 91125; apple@ipac.caltech.edu 2 Astrophysics Research Institute, John Moores University, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK 3 Instituto de Astronomia, National Autonomous University of Mexico, P. O. 70-264, 04510 D. F., Mexico 4 NRAO, Charlottesville 5 Spitzer NASA Herschel Science Center, 1200 E. California Blvd., Caltech, Pasadena, CA 91125 6 Department of Physics, University of Crete, GR-71003, Heraklion, Greece 7 Institute for Astronomy, Astrophysics, Space Applications & Remote Sensing, National Observatory of Athens, GR-15236, Penteli, Greece 8 Chercheur Associe, Observatoire de Paris, F-75014, Paris, France 9 Service d’Astrophysique, Laboratoire AIM, CEA-Saclay, Orme des Merisiers, Bat 709, 91191 Gif sur Yvette, France 10 Dept. Fisica Teorica y del Cosmos, University of Granada, Edifica Mecenas, Granada, Spain 11 NASA Extragalactic Database, IPAC, Caltech, 1200 E. California Blvd, Caltech, Pasadena, CA 91125

Published
2015
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7. MID-INFRARED PROPERTIES OF LUMINOUS INFRARED GALAXIES. II. PROBING THE DUST AND GAS PHYSICS OF THE GOALS SAMPLE

Author

Tanio Díaz-Santos, Jeffrey A. Rich, Henrik Spoon, S. Stierwalt, Jennifer L. Marshall, Hanae Inami, Justin Howell, Aaron S. Evans, Lee Armus, Vassilis Charmandaris, S. Haan, Eric J. Murphy, Andreea Petric, K. Iwasawa, D. C. Kim, Observatoire de Paris, Université Paris sciences et lettres (PSL), Universidad Diego Portales [Santiago] (UDP), Universidad Autonoma de Madrid (UAM), Aberystwyth University, Istituto Nazionale di Astrofisica (INAF), Nano Powder Metallurgy Group, Korea Institute of Machinery and Materials, 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Universidad Autónoma de Madrid (UAM), 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)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Luminous infrared galaxy, [PHYS]Physics [physics], Active galactic nucleus, 010308 nuclear & particles physics, Star formation, Infrared, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Photodissociation region, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Luminosity, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract

The Great Observatories All-Sky LIRG Survey (GOALS) is a comprehensive, multiwavelength study of luminous infrared galaxies (LIRGs) in the local universe. Here we present the results of a multi-component, spectral decomposition analysis of the low resolution mid-IR Spitzer IRS spectra from 5-38um of 244 LIRG nuclei. The detailed fits and high quality spectra allow for characterization of the individual PAH features, warm molecular hydrogen emission, and optical depths for silicate dust grains and water ices. We find that starbursting LIRGs, which make up the majority of GOALS, are very consistent in their MIR properties (i.e. tau_9.7um, tau_ice, neon line and PAH feature ratios). However, as their PAH EQW decreases, usually an indicator of an increasingly dominant AGN, LIRGs cover a larger spread in these MIR parameters. The contribution from PAHs to the total L(IR) in LIRGs varies from 2-29% and LIRGs prior to their first encounter show higher L(PAH)/L(IR) ratios on average. We observe a correlation between the strength of the starburst (IR8) and the PAH fraction at 8um but not with the 7.7 to 11.3 PAH ratio, suggesting the fractional PDR emission, and not the overall grain properties, is associated with the rise in IR8 for galaxies off the starburst main sequence. We detect crystalline silicate features in 6% of the sample but only in the most obscured sources (s_9.7um < -1.24). Ice absorption features are observed in 11% (56%) of GOALS LIRGs (ULIRGs). Most GOALS LIRGs have L(H2)/L(PAH) ratios elevated above those observed for normal star-forming galaxies and exhibit a trend for increasing L(H2)/L(PAH) ratio with increasing L(H2). While star formation appears to be the dominant process responsible for exciting the H2 in most of the GOALS galaxies, a subset of LIRGs (10%) show excess H2 emission that is inconsistent with PDR models and may be excited by shocks or AGN-induced outflows., 21 pages with 20 figures plus 2 tables

Published
2014
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8. WARM MOLECULAR GAS IN LUMINOUS INFRARED GALAXIES

Author

Lee Armus, Joseph M. Mazzarella, P. N. Appleton, Vassilis Charmandaris, Hanae Inami, Justin Howell, Aaron S. Evans, Andreea Petric, P. van der Werf, Kate Gudrun Isaak, C. K. Xu, Yinghe Zhao, Kazushi Iwasawa, Yu Gao, David B. Sanders, S. D. Lord, Jamie Leech, Jason Surace, Bernhard Schulz, Nanyao Lu, Tanio Díaz-Santos, University of Regina (UR), Sichuan University [Chengdu] (SCU), School of Physics and Astronomy [Cardiff], Cardiff University, Observatoire de Paris, Université Paris sciences et lettres (PSL), Universidad Diego Portales [Santiago] (UDP), iROc Technologies (IROC TECHNOLOGIES), Cadence Connection-EDA Consortium-FSA-Cubic Micro, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), AUTRES, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), and Universiteit Leiden

Subjects
Physics, Luminous infrared galaxy, [PHYS]Physics [physics], Active galactic nucleus, Infrared, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Spectral line, Luminosity, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS, Line (formation)
Abstract

We present our initial results on the CO rotational spectral line energy distribution (SLED) of the $J$ to $J$$-$1 transitions from $J=4$ up to $13$ from Herschel SPIRE spectroscopic observations of 65 luminous infrared galaxies (LIRGs) in the Great Observatories All-Sky LIRG Survey (GOALS). The observed SLEDs change on average from one peaking at $J \le 4$ to a broad distribution peaking around $J \sim\,$6$-$7 as the IRAS 60-to-100 um color, $C(60/100)$, increases. However, the ratios of a CO line luminosity to the total infrared luminosity, $L_{\rm IR}$, show the smallest variation for $J$ around 6 or 7. This suggests that, for most LIRGs, ongoing star formation (SF) is also responsible for a warm gas component that emits CO lines primarily in the mid-$J$ regime ($5 \lesssim J \lesssim 10$). As a result, the logarithmic ratios of the CO line luminosity summed over CO (5$-$4), (6$-$5), (7$-$6), (8$-$7) and (10$-$9) transitions to $L_{\rm IR}$, $\log R_{\rm midCO}$, remain largely independent of $C(60/100)$, and show a mean value of $-4.13$ ($\equiv \log R^{\rm SF}_{\rm midCO}$) and a sample standard deviation of only 0.10 for the SF-dominated galaxies. Including additional galaxies from the literature, we show, albeit with small number of cases, the possibility that galaxies, which bear powerful interstellar shocks unrelated to the current SF, and galaxies, in which an energetic active galactic nucleus contributes significantly to the bolometric luminosity, have their $R_{\rm midCO}$ higher and lower than $R^{\rm SF}_{\rm midCO}$, respectively., Comment: Accepted for publication in the ApJ Letters; 5 pages, 4 figures

Published
2014
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9. The build-up of nuclear stellar cusps in extreme starburst galaxies and major mergers

Author

Jason Melbourne, Eric J. Murphy, Joseph M. Mazzarella, Justin Howell, Carrie Bridge, T. Vavilkin, Jason Surace, Vassilis Charmandaris, D. C. Kim, Lee Armus, Andreea Petric, Robert Braun, S. Stierwalt, Tanio Díaz-Santos, Aaron S. Evans, S. Haan, Hanae Inami, D. B. Sanders, AUTRES, IESL, Observatoire de Paris, Université Paris sciences et lettres (PSL), iROc Technologies (IROC TECHNOLOGIES), Cadence Connection-EDA Consortium-FSA-Cubic Micro, Universidad Diego Portales [Santiago] (UDP), Nano Powder Metallurgy Group, Korea Institute of Machinery and Materials, inconnu temporaire UPEMLV, Inconnu, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Nir light, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Luminous infrared galaxy, Cusp (singularity), Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Radius, Galaxy, Space and Planetary Science, Magnitude (astronomy), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Nuclear stellar cusps are defined as central excess light component in the stellar light profiles of galaxies and are suggested to be stellar relics of intense compact starbursts in the central ~100-500 pc region of gas-rich major mergers. Here we probe the build-up of nuclear cusps during the actual starburst phase for a complete sample of Luminous Infrared Galaxy systems (85 LIRGs, with 11.4, Comment: 30 pages, 15 figures, Accepted for publication in MNRAS

Published
2013
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10. Spitzer IRS Spectral Mapping of the Toomre Sequence: Spatial Variations of PAH, Gas, and Dust Properties in nearby Major Mergers

Author

J. D. Smith, Aaron S. Evans, M. S. Yun, Seppo Laine, S. Haan, Lee Armus, Francois Schweizer, John E. Hibbard, Eric J. Murphy, Thomas H. Jarrett, Jason Surace, Tanio Díaz-Santos, P. Beirao, Vassilis Charmandaris, Sabrina Stierwalt, Bernhard R. Brandl, Spitzer Science Center, California Institute of Technology (SSC), Department of Physics and Institute of Theoretical and Computational Physics, 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), Ritter Astrophysical Observatory, University of Toledo, Toledo, Observatories of the Carnegie Institution of Washington, Leiden Observatory, National Radio Astronomy Observatory, Charlottesville (NRAO), Department of Astronomy, University of Massachusetts, and Infrared Processing Analysis Center, California Institute of Technology (IPAC)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star formation, Infrared, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Power law, Galaxy, Flux (metallurgy), Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Line (formation), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have mapped the key mid-IR diagnostics in eight major merger systems of the Toomre Sequence (NGC4676, NGC7592, NGC6621, NGC2623, NGC6240, NGC520, NGC3921, and NGC7252) using the Spitzer Infrared Spectrograph (IRS). With these maps, we explore the variation of the ionized-gas, PAH, and warm-gas (H_2) properties across the sequence and within the galaxies. While the global PAH interband strength and ionized gas flux ratios ([Ne III]/[Ne II]) are similar to those of normal star forming galaxies, the distribution of the spatially resolved PAH and fine structure line flux ratios is significant different from one system to the other. Rather than a constant H_2/PAH flux ratio, we find that the relation between the H_2 and PAH fluxes is characterized by a power law with a roughly constant exponent (0.61+/-0.05) over all merger components and spatial scales. While following the same power law on local scales, three galaxies have a factor of ten larger integrated (i.e. global) H_2/PAH flux ratio than the rest of the sample, even larger than what it is in most nearby AGNs. These findings suggest a common dominant excitation mechanism for H_2 emission over a large range of global H_2/PAH flux ratios in major mergers. Early merger systems show a different distribution between the cold (CO J=1-0) and warm (H_2) molecular gas component, which is likely due to the merger interaction. Strong evidence for buried star formation in the overlap region of the merging galaxies is found in two merger systems (NGC6621 and NGC7592) as seen in the PAH, [Ne II], [Ne III], and warm gas line emission, but with no apparent corresponding CO (J=1-0) emission. Our findings also demonstrate that the variations of the physical conditions within a merger are much larger than any systematic trends along the Toomre Sequence., Comment: 35 pages, accepted for publication in ApJS

Published
2011
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11. A SPITZER HIGH-RESOLUTION MID-INFRARED SPECTRAL ATLAS OF STARBURST GALAXIES

Author

Lei Hao, Henrik Spoon, James R. Houck, Yanling Wu, Duncan Farrah, Vassilis Charmandaris, Vianney Lebouteiller, Jeronimo Bernard-Salas, Bernhard R. Brandl, Daniel W. Weedman, Gregory C. Sloan, Lee Armus, Daniel Devost, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astronomy Centre, University of Sussex, Departments of Medicine, Pharmacology and Therapeutics, McGill University = Université McGill [Montréal, Canada], School of Science, China University of Petroleum, Qingdao, China University of Petroleum, Hydrosystèmes et Bioprocédés (UR HBAN), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), 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), 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), McGill University, Hydrosystèmes et bioprocédés (UR HBAN), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), École normale supérieure - Paris (ENS-PSL), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], FOS: Physical sciences, Polycyclic aromatic hydrocarbon, chemistry.chemical_element, Astrophysics, 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Neon, 0103 physical sciences, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Line (formation), chemistry.chemical_classification, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], chemistry, Space and Planetary Science, Spectral atlas, Excitation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present an atlas of Spitzer/IRS high resolution (R~600) 10-37um spectra for 24 well known starburst galaxies. The spectra are dominated by fine-structure lines, molecular hydrogen lines, and emission bands of polycyclic aromatic hydrocarbons. Six out of the eight objects with a known AGN component show emission of the high excitation [NeV] line. This line is also seen in one other object (NGC4194) with, a priori, no known AGN component. In addition to strong polycyclic aromatic hydrocarbon emission features in this wavelength range (11.3, 12.7, 16.4um), the spectra reveal other weak hydrocarbon features at 10.6, 13.5, 14.2um, and a previously unreported emission feature at 10.75um. An unidentified absorption feature at 13.7um is detected in many of the starbursts. We use the fine-structure lines to derive the abundance of neon and sulfur for 14 objects where the HI 7-6 line is detected. We further use the molecular hydrogen lines to sample the properties of the warm molecular gas. Several basic diagrams characterizing the properties of the sample are also shown. We have combined the spectra of all the pure starburst objects to create a high S/N template, which is available to the community., 25 pages (emulate apj), 6 tables, 14 figures, Accepted for publication in ApJS

Published
2009
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12. High-Velocity Neon Line Emission From the ULIRG IRAS F00183-7111: Revealing the Optically Obscured Base of a Nuclear Outflow

Author

Jeronimo Bernard-Salas, Brian R. Kent, Duncan Farrah, Vassilis Charmandaris, Henrik Spoon, Jason Marshall, Lee Armus, Department of Astronomy, Cornell University, Spitzer Science Center, California Institute of Technology (SSC), Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Crete Center for Theoretical Physics, Department of Physics, 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), and National Radio Astronomy Observatory, Charlottesville (NRAO)

Subjects
Physics, Infrared, Extinction (astronomy), Astrophysics (astro-ph), chemistry.chemical_element, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, Galaxy, Blueshift, Wavelength, Neon, chemistry, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Line (formation)
Abstract

We report the first mid-IR detection of highly disturbed ionized gas in the ultraluminous infrared galaxy IRAS F00183-7111. The gas, traced by the 12.81um [NeII] and 15.56um [NeIII] lines, spans a velocity range of-3500 to 3000 km/s with respect to systemic velocity. Optical and near-IR spectroscopic studies show no evidence for similarly high velocity gas components in forbidden lines at shorter wavelengths. We interpret this as the result of strong extinction (Av=10-50) on the high-velocity gas, which identifies the base of the outflow traced in 5007A [OIII] as a plausible origin. Unusual excitation conditions are implied by a comparison of the mid-infrared low-excitation neon line emission and the PAH emission for a sample of 56 ULIRGs. For IRAS F00183, the neon/PAH ratio is 8 times higher than the average ratio. Similar mid-infrared kinematic and excitation characteristics are found for only 2 other ULIRGs in our sample: IRAS 12127-1412NE and IRAS 13451+1232. Both sources have an elevated neon/PAH ratio and exhibit pronounced blue wings in their 15.56um [NeIII] line profiles. IRAS 13451 even shows a strongly blue shifted and broad 14.32um [NeV] line. While for IRAS 13451 the observed [NeIII]/[NeII] and [NeV]/[NeII] line ratios indicate exposure of the blue shifted gas to direct radiation from the AGN, for IRAS F00183 and 12127 the neon line ratios are consistent with an origin in fast shocks in a high-density environment, and with an evolutionary scenario in which strongly blue shifted [Ne II] and [Ne III] emission trace the (partial) disruption of the obscuring medium around a buried AGN. The detection of strongly blue shifted [Ne V] emission in IRAS 13451 would then indicate this process to be much further advanced in this ULIRG than in IRAS F00183 and 12127, where this line is undetected., 13 pages, 10 figures, accepted for publication in the Astrophysical Journal

Published
2009
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13. PAH Emission from Ultraluminous Infrared Galaxies

Author

Jason Marshall, Bernhard R. Brandl, B. T. Soifer, James R. Houck, Harry I. Teplitz, Daniel Devost, Sarah J.U. Higdon, Jeronimo Bernard-Salas, Vandana Desai, Lee Armus, Patrick Ogle, Henrik Spoon, Duncan Farrah, Vassilis Charmandaris, Division of Physics, Mathematics and Astronomy, California Institute of Technology, Spitzer Science Center, California Institute of Technology (SSC), Department of Astronomy, Cornell University, Crete Center for Theoretical Physics, Department of Physics, 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), Leiden Observatory, and Department of Physics, Georgia Southern University

Subjects
Physics, Luminous infrared galaxy, Infrared, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Silicate, Redshift, chemistry.chemical_compound, chemistry, Spitzer Space Telescope, Space and Planetary Science, Spectral slope, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Spectrograph, Astrophysics::Galaxy Astrophysics, Order of magnitude
Abstract

We explore the relationships between the Polycyclic Aromatic Hydrocarbon (PAH) feature strengths, mid-infrared continuum luminosities, far-infrared spectral slopes, optical spectroscopic classifications, and silicate optical depths within a sample of 107 ULIRGs observed with the Infrared Spectrograph on the Spitzer Space Telescope. The detected 6.2 micron PAH equivalent widths (EQWs) in the sample span more than two orders of magnitude (0.006-0.8 micron), and ULIRGs with HII-like optical spectra or steep far-infrared spectral slopes (S_{25} / S_{60} < 0.2) typically have 6.2 micron PAH EQWs that are half that of lower-luminosity starbursts. A significant fraction (~40-60%) of HII-like, LINER-like, and cold ULIRGs have very weak PAH EQWs. Many of these ULIRGs also have large (tau_{9.7} > 2.3) silicate optical depths. The far-infrared spectral slope is strongly correlated with PAH EQW, but not with silicate optical depth. In addition, the PAH EQW decreases with increasing rest-frame 24 micron luminosity. We argue that this trend results primarily from dilution of the PAH EQW by continuum emission from dust heated by a compact central source, probably an AGN. High luminosity, high-redshift sources studied with Spitzer appear to have a much larger range in PAH EQW than seen in local ULIRGs, which is consistent with extremely luminous starburst systems being absent at low redshift, but present at early epochs., 15 pages, 9 Figures; Accepted for publication in ApJ

Published
2007
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14. Observations of Ultraluminous Infrared Galaxies with the Infrared Spectrograph on the Spitzer Space Telescope. II. The IRAS Bright Galaxy Sample

Author

B. T. Soifer, Henrik Spoon, Jason Marshall, Vandana Desai, James R. Houck, Yanling Wu, Terry Herter, Gregory C. Sloan, Lee Armus, Bernhard R. Brandl, Sarah J.U. Higdon, Harry I. Teplitz, Lei Hao, Jeronimo Bernard-Salas, Daniel Devost, Vassilis Charmandaris, Henry, Florence, Spitzer Science Center, California Institute of Technology (SSC), Crete Center for Theoretical Physics, Department of Physics, 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), Department of Astronomy, Cornell University, Division of Physics, Mathematics and Astronomy, California Institute of Technology, and Leiden University

Subjects
Luminous infrared galaxy, Physics, Infrared, Molecular cloud, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Spectral line, Luminosity, Spitzer Space Telescope, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Line (formation)
Abstract

We present spectra taken with the Infrared Spectrograph on Spitzer covering the 5-38 micron region of the ten Ultraluminous Infrared Galaxies (ULIRGs) found in the IRAS Bright Galaxy Sample. Among the BGS ULIRGs, we find a factor of 50 spread in the rest-frame mid to far-infrared spectral slope. The 9.7 micron silicate optical depths range from less than 0.4 more than 4.2, implying line of sight extinctions of A(V) ~ 8 - 78 mag. There is evidence for water ice and hydrocarbon absorption and C2H2 and HCN absorption features in four and possibly six of the 10 BGS ULIRGs, indicating shielded molecular clouds and a warm, dense ISM. We have detected [NeV] emission in three of the ten BGS ULIRGs, at flux levels of 5-18E-14 erg/cm^2/sec and [NeV] 14.3/[NeII] 12.8 line flux ratios of 0.12-0.85. The remaining BGS ULIRGs have limits on their [NeV]/[NeII] line flux ratios which range from less than 0.15 to less than 0.01. Among the BGS ULIRGs, the AGN fractions implied by either the [NeV]/[NeII] or [OIV]/[NeII] line flux ratios (or their upper limits) are significantly lower than implied by the MIR slope or EQW of the 6.2 micron PAH feature. Fitting the SEDs, we see evidence for hot (T > 300K) dust in five of the BGS ULIRGs, with the fraction of hot dust to total dust luminosity ranging from ~1-23%, before correcting for extinction. When integrated over the IRAC-8, IRS blue peakup, and MIPS-24 filter bandpasses, the IRS spectra imply very blue colors for some ULIRGs at z ~ 1.3. This is most extreme for sources with significant amounts of warm dust and deep silicate absorption., accepted for publication in the Astrophysical Journal

Published
2007

15. Silicate Emission in the Spitzer IRS Spectrum of FSC 10214+4724

Author

Yanling Wu, Charles R. Lawrence, Jason Marshall, Sarah J.U. Higdon, B. T. Soifer, Terry Herter, Harry I. Teplitz, J. R. Houck, Lee Armus, Mark Lacy, Peter Eisenhardt, Vassilis Charmandaris, Lei Hao, Henrik Spoon, Spitzer Science Center, California Institute of Technology (SSC), Department of Astronomy, Cornell University, 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), and Jet Propulsion Laboratory, California Institute of Technology (JPL)

Subjects
Physics, Infrared, Astrophysics (astro-ph), Continuum (design consultancy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Luminosity, Spitzer Space Telescope, Space and Planetary Science, Spectral energy distribution, Emission spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width
Abstract

We present the first MIR spectrum of the z=2.2856 ultraluminous, infrared galaxy FSC 10214+4724, obtained with the Infrared Spectrograph onboard the Spitzer Space Telescope. The spectrum spans a rest wavelength range of 2.3-11.5 microns, covering a number of key diagnostic emission and absorption features. The most prominent feature in the IRS spectrum is the silicate emission at rest-frame 10 microns. We also detect an unresolved emission line at a rest wavelength of 7.65 microns which we identify with [NeVI], and a slightly resolved feature at 5.6 microns identified as a blend of [Mg VII] and [Mg V]. There are no strong PAH emission features in the FSC 10214+4724 spectrum. We place a limit of 0.1 micron on the equivalent width of 6.2 micron PAH emission but see no evidence of a corresponding 7.7 micron feature. Semi-empirical fits to the spectral energy distribution suggest about 45% of the bolometric luminosity arises from cold 50 K dust, half arises from warm (190 K) dust, and the remainder, 5%, originates from hot (640 K) dust. The hot dust is required to fit the blue end of the steep MIR spectrum. The combination of a red continuum, strong silicate emission, little or no PAH emission, and no silicate absorption, makes FSC 10214+4724 unlike most other ULIRGs or AGN observed thus far with IRS. These apparently contradictory properties may be explained by an AGN which is highly magnified by the lens, masking a (dominant) overlying starburst with unusually weak PAH emission., Comment: Accepted for publication in ApJL

Published
2006
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16. First Mid-Infrared Spectrum of a Faint High-z Galaxy: Observations of CFRS 14.1157 with the Infrared Spectrograph on the Spitzer Space Telescope

Author

Lee Armus, Vassilis Charmandaris, James L. Higdon, Daniel W. Weedman, James R. Houck, Bernhard R. Brandl, Terry Herter, B. T. Soifer, Sarah J.U. Higdon, Lei Hao, Henry, Florence, Department of Astronomy, Cornell University, 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), Spitzer Science Center, California Institute of Technology (SSC), and Leiden University

Subjects
Physics, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Spectrum (functional analysis), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Spectral line, Redshift, Spitzer Space Telescope, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Absorption (electromagnetic radiation), [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract

The unprecedented sensitivity of the Infrared Spectrograph on the Spitzer Space Telescope allows for the first time the measurement of mid-infrared spectra from 14 to 38 microns of faint high-z galaxies. This unique capability is demonstrated with observations of sources having 16 micron fluxes of 3.6 mJy (CFRS 14.1157) and 0.35 mJy (CFRS 14.9025). A spectral-fitting technique is illustrated which determines the redshift by fitting emission and absorption features characteristic of nearby galaxies to the spectrum of an unknown source. For CFRS 14.1157, the measured redshift is z = 1.00+/-0.20 in agreement with the published result of z = 1.15. The spectrum is dominated by emission from an AGN, similar to the nucleus of NGC 1068, rather than a typical starburst with strong PAH emission like M82. Such spectra will be crucial in characterizing the nature of newly discovered distant galaxies, which are too faint for optical follow-up., Accepted in ApJ Sup. Spitzer Special Issue, 4 pages, 5 figures

Published
2004

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