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1. Burton's Curse: The Impact of Bulk Flows on the Galactic Longitude-Velocity Diagram and the Illusion of a Continuous Perseus Arm

Author

J. E. G. Peek, Kirill Tchernyshyov, Marc-Antoine Miville-Deschenes, 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.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

In this work we demonstrate that the Perseus Arm is not a continuous structure of molecular gas in the second quadrant. We first show that the observed, distanced-resolved velocity structure of the Galaxy in the outer disk is capable of creating illusory spiral arms, as was first proposed by Burton (1971). Second, we measure the distances to a collection of CO clouds at velocities consistent with the Perseus arm with $135^\circ < l < 160^\circ$. We find these distances using 3D dust maps from Green et al. (2019). We determine that these molecular cloud do not preferentially lie at the distance of a purported Perseus arm, but rather extend over 3 kpc in distance, with some evidence for a closer, high pitch angle structure between 1 and 1.5 kpc away. Finally, we demonstrate that velocity perturbations of the amplitude found near the Perseus arm can wreak havoc on our interpretation of the longitude-velocity diagram for more than half of the Milky Way disk., 14 pages, 7 figures. Accepted to the Astrophysical Journal

Published
2021
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2. Which Molecular Cloud Structures Are Bound?

Author

Marc-Antoine Miville-Deschenes, Mark H. Heyer, Neal J. Evans, Manuel Merello, Quang Nguyen-Luong, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université Paris Cité (UPCité)

Subjects
Physics, Molecular cloud, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Molecular clouds, Star-forming regions, Astrophysics::Galaxy Astrophysics
Abstract

We analyze surveys of molecular cloud structures defined by tracers ranging from CO $J = 1-0$ through $^{13}$CO $J = 1-0$ to dust emission together with NH$_3$ data. The mean value of the virial parameter and the fraction of mass in bound structures depends on the method used to identify structures. Generally, the virial parameter decreases and the fraction of mass in bound structures increases with the effective density of the tracer, the surface density and mass of the structures, and the distance from the center of a galaxy. For the most complete surveys of structures in the Galaxy defined by CO $J = 1-0$, the fraction of mass that is in bound structures is 0.19. For catalogs of other galaxies based on CO $J = 2-1$, the fraction is 0.35. These results offer substantial alleviation of the fundamental problem of slow star formation. If only clouds found to be bound are counted and they are assumed to collapse in a free-fall time at their mean cloud density, the sum over all clouds in a complete survey of the Galaxy yields a predicted star formation rate of 46 solar masses per year, a factor of 6.5 less than if all clouds are bound., Comment: 26 pages, 14 figures, accepted to ApJ

Published
2021
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3. C18O, 13CO, and 12CO abundances and excitation temperatures in the Orion B molecular cloud

Author

Emeric Bron, Marc-Antoine Miville-Deschenes, Pierre Gratier, Jérôme Pety, Jan H. Orkisz, Nicolas Peretto, Maxime Vono, Evelyne Roueff, Antoine Roueff, Albrecht Sievers, Javier R. Goicoechea, Jacques Le Bourlot, Victor de Souza Magalhaes, Jouni Kainulainen, Annie Hughes, Franck Petit, Viviana V. Guzmán, Maryvonne Gerin, Harvey S. Liszt, François Levrier, Antoine Marchal, Jocelyn Chanussot, David Languignon, Sébastien Bardeau, M. Gaudel, Pierre Chainais, Centre National de la Recherche Scientifique (France), Max Planck Society, Instituto Geográfico Nacional (España), European Space Agency, Centre National D'Etudes Spatiales (France), Agencia Estatal de Investigación (España), PhyTI (PhyTI), Institut FRESNEL (FRESNEL), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), FORMATION STELLAIRE 2020, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Instituto de Física Fundamental [Madrid] (IFF), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Signal et Communications (IRIT-SC), Institut de recherche en informatique de Toulouse (IRIT), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Toulouse Mind & Brain Institut (TMBI), Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), GIPSA - Signal Images Physique (GIPSA-SIGMAPHY), GIPSA Pôle Sciences des Données (GIPSA-PSD), Grenoble Images Parole Signal Automatique (GIPSA-lab), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA)-Grenoble Images Parole Signal Automatique (GIPSA-lab), Université Grenoble Alpes (UGA), Centre de Recherche en Informatique, Signal et Automatique de Lille - UMR 9189 (CRIStAL), Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Pontificia Universidad Católica de Chile (UC), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), National Radio Astronomy Observatory [Charlottesville] (NRAO), National Radio Astronomy Observatory (NRAO), Canadian Institute for Theoretical Astrophysics (CITA), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Cardiff University, ANR-19-P3IA-0003,MIAI,MIAI @ Grenoble Alpes(2019), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Onsala Space Observatory, Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Ecole Centrale de Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse 1 Capitole (UT1), 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), Université de Lille-Ecole Centrale de Lille-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
statistical [Methods], Astrophysics, 7. Clean energy, 01 natural sciences, Molecular physics, ISM: clouds, Spectral line, Methods: data analysis, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Isotopologue, [INFO]Computer Science [cs], data analysis [Methods], 010303 astronomy & astrophysics, molecules [ISM], Astrophysics::Galaxy Astrophysics, Methods: statistical, Line (formation), Physics, 010308 nuclear & particles physics, Molecular cloud, Estimator, Velocity dispersion, Astronomy and Astrophysics, ISM: molecules, 3. Good health, 13. Climate action, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], clouds [ISM], Excitation
Abstract

27 pags., 23 figs., 3 tabs., Context. CO isotopologue transitions are routinely observed in molecular clouds for the purpose of probing the column density of the gas and the elemental ratios of carbon and oxygen, in addition to tracing the kinematics of the environment. Aims. Our study is aimed at estimating the abundances, excitation temperatures, velocity field, and velocity dispersions of the three main CO isotopologues towards a subset of the Orion B molecular cloud, which includes IC 434, NGC 2023, and the Horsehead pillar. Methods. We used the Cramer Rao bound (CRB) technique to analyze and estimate the precision of the physical parameters in the framework of local-thermodynamic-equilibrium (LTE) excitation and radiative transfer with added white Gaussian noise. We propose a maximum likelihood estimator to infer the physical conditions from the 1-0 and 2-1 transitions of CO isotopologues. Simulations show that this estimator is unbiased and proves efficient for a common range of excitation temperatures and column densities (Tex > 6 K, N > 1014-1015 cm-2). Results. Contrary to general assumptions, the various CO isotopologues have distinct excitation temperatures and the line intensity ratios between different isotopologues do not accurately reflect the column density ratios. We find mean fractional abundances that are consistent with previous determinations towards other molecular clouds. However, significant local deviations are inferred, not only in regions exposed to the UV radiation field, but also in shielded regions. These deviations result from the competition between selective photodissociation, chemical fractionation, and depletion on grain surfaces. We observe that the velocity dispersion of the C18O emission is 10% smaller than that of 13CO. The substantial gain resulting from the simultaneous analysis of two different rotational transitions of the same species is rigorously quantified. Conclusions. The CRB technique is a promising avenue for analyzing the estimation of physical parameters from the fit of spectral lines. Future works will generalize its application to non-LTE excitation and radiative transfer methods., This work is based on observations carried out under project numbers 019-13, 022-14, 145-14, 122-15, 018-16, and finally the large program number 124-16 with the IRAM 30m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). This research also used data from the Herschel Gould Belt survey (HGBS) project (http:// gouldbelt-herschel.cea.fr). The HGBS is a Herschel Key Programme jointly carried out by SPIRE Specialist Astronomy Group 3 (SAG 3), scientists of several institutes in the PACS Consortium (CEA Saclay, INAF-IFSI Rome and INAF-Arcetri, KU Leuven, MPIA Heidelberg), and scientists of the Herschel Science Center (HSC). We thank CIAS for their hospitality during the many workshops devoted to the ORION-B project. This project has received financial support from the CNRS through the MITI interdisciplinary programs. This work was supported in part by the Programme National “Physique et Chimie du Milieu Interstellaire” (PCMI) of CNRS/INSU with INC/INP, co-funded by CEA and CNES. JRG thanks Spanish MICI for funding support under grant AYA2017- 85111-P. Finally, we thank the anonymous referee for helpful comments on the manuscript.

Published
2020
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4. Galactic interstellar filaments as probed by LOFAR and Planck

Author

Katia Ferrière, François Levrier, Vishambhar Pandey, Andrea Bracco, Marc-Antoine Miville-Deschenes, Vibor Jelić, Luitje Koopmans, Robin Kooistra, M. I. R. Alves, Juan D. Soler, Tuhin Ghosh, F. Boulanger, L. Montier, Saleem Zaroubi, Michiel A. Brentjens, de Antonius Bruyn, Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Peuplements végétaux et bioagresseurs en milieu tropical (UMR PVBMT), Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad)-Institut de Recherche pour le Développement (IRD)-Institut National de la Recherche Agronomique (INRA)-Université de La Réunion (UR), 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), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Netherlands Institute for Radio Astronomy (ASTRON), 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), 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), UMR Peuplement Végétaux et Bioagresseurs en Milieu Tropical (UMR PVBMT - INRA), Institut National de la Recherche Agronomique (INRA), Istituto Nazionale di Fisica Nucleare [Milano] (INFN), Université Toulouse III - Paul Sabatier (UT3), 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), 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), Astronomy, 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), 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), École normale supérieure - Paris (ENS-PSL), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))

Subjects
media_common.quotation_subject, ISM: structure, radio continuum: general, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, symbols.namesake, law, 0103 physical sciences, Planck, Faraday cage, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, media_common, ISM: general, Physics, [PHYS]Physics [physics], Line-of-sight, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Quasar, Astronomy and Astrophysics, LOFAR, Polarization (waves), Astrophysics - Astrophysics of Galaxies, techniques, interferometric, ISM, general, magnetic fields, structure, radio continuum, submillimetre, Magnetic field, submillimetre: ISM, Space and Planetary Science, Sky, techniques: interferometric, Astrophysics of Galaxies (astro-ph.GA), symbols, ISM: magnetic fields, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Recent Low Frequency Array (LOFAR) observations at 115-175 MHz of a field at medium Galactic latitudes (centered at the bright quasar 3C196) have shown striking filamentary structures in polarization that extend over more than 4 degrees across the sky. In addition, the Planck satellite has released full sky maps of the dust emission in polarization at 353GHz. The LOFAR data resolve Faraday structures along the line of sight, whereas the Planck dust polarization maps probe the orientation of the sky projected magnetic field component. Hence, no apparent correlation between the two is expected. Here we report a surprising, yet clear, correlation between the filamentary structures, detected with LOFAR, and the magnetic field orientation, probed by the Planck satellite. This finding points to a common, yet unclear, physical origin of the two measurements in this specific area in the sky. A number of follow-up multi- frequency studies are proposed to shed light on this unexpected finding., Comment: 6 pages, 4 figures, accepted for publication in MNRAS Letters

Published
2015
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5. Mapping a Lower Limit on the Mass Fraction of the Cold Neutral Medium Using Fourier-transformed H i 21 cm Emission Line Spectra: Application to the DRAO Deep Field from DHIGLS and the HI4PI Survey

Author

Antoine Marchal, Peter G. Martin, Marc-Antoine Miville-Deschênes, Naomi M. McClure-Griffiths, Callum Lynn, Andrea Bracco, and Luka Vujeva

Subjects
Interstellar medium, Cold neutral medium, Neutral hydrogen clouds, Fast Fourier transform, Astrophysics, QB460-466
Abstract

We develop a new method for spatially mapping a lower limit on the mass fraction of the cold neutral medium by analyzing the amplitude structure of ${\hat{T}}_{b}({k}_{v})$ , the Fourier transform of T _b ( v ), the spectrum of the brightness temperature of the H i 21 cm line emission with respect to the radial velocity v . This advances a broader effort exploiting 21 cm emission line data alone (without absorption line data, τ ) to extract integrated properties of the multiphase structure of the H i gas and to map each phase separately. Using toy models, we illustrate the origin of interference patterns seen in ${\hat{T}}_{b}({k}_{v})$ . Building on this, a lower limit on the cold gas mass fraction is obtained from the amplitude of ${\hat{T}}_{b}$ at high k _v . Tested on a numerical simulation of thermally bi-stable turbulence, the lower limit from this method has a strong linear correlation with the “true” cold gas mass fraction from the simulation for a relatively low cold gas mass fraction. At a higher mass fraction, our lower limit is lower than the “true” value, because of a combination of interference and opacity effects. Comparison with absorption surveys shows a similar behavior, with a departure from linear correlation at N _H I ≳ 3–5 × 10 ^20 cm ^−2 . Application to the DRAO Deep Field from DHIGLS reveals a complex network of cold filaments in the Spider, an important structural property of the thermal condensation of the H i gas. Application to the HI4PI survey in the velocity range −90 < v < 90 km s ^−1 produces a full sky map of a lower limit on the mass fraction of the cold neutral medium at 16.′2 resolution. Our new method has the ability to extract a lower limit on the cold gas mass fraction for massive amounts of emission line data alone with low computing time and memory, pointing the way to new approaches suitable for the new generation of radio interferometers.

Published
2024
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6. Multiwavelength observations of cirrus clouds in the North Celestial Loop: the transition from atomic to molecular gas

Author

Peter G. Martin, T. L. Landecker, A. R. Taylor, Jeroen Stil, Douglas J. Marshall, Roland Kothes, L. Barriault, Edith Falgarone, Marc-Antoine Miville-Deschenes, Mark H. Heyer, Douglas Scott, Gilles Joncas, F. Boulanger, Christopher M. Brunt, K. Blagrave, and T. Foster

Subjects
Physics, Loop (topology), Ursa Major, Space and Planetary Science, Observatory, TRACER, Astronomy, Astronomy and Astrophysics, Cirrus, Astrophysics, Excitation, Spectral line, Latitude
Abstract

Two potential sites of H 2 formation have been discovered in diffuse gas at high Galactic latitude through examining the far-infrared (FIR) H I ratio and looking for an excess over that expected from an atomic medium. We call these the Spider and Ursa Major fields. New 12 CO and 13 CO Five College Radio Astronomical Observatory observations are presented for both regions (53 936 spectra in the Spider and 23 517 spectra in Ursa Major). Although there is a correlation between FIR excess and CO emission, we find that the FIR excess peaks do not coincide with the 12 CO emission peaks, indicating that CO might be a poor tracer of H 2 in diffuse regions. This implies (i) that the density is too small to allow CO excitation, (ii) that the CO self-shielding is insufficient or (iii) local variations of the dust properties. The 12 CO observations are compared with H I observation from the Dominion Radio Astrophysical Observatory. We decompose the 10 000 H I profiles of the Spider and the 20 302 H I profiles of Ursa Major into Gaussian components. We always find at most two narrow components and one broad component. CO always seems to appear where two H I velocity components merge or where there is a H I velocity-shear.

Published
2010
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7. Automatic Detection of Expanding H<scp>i</scp>Shells in the Canadian Galactic Plane Survey Data

Author

Gilles Joncas, Marc Parizeau, Anik Daigle, and Marc-Antoine Miville-Deschenes

Subjects
Physics, Channel (digital image), Pixel, Artificial neural network, 010308 nuclear & particles physics, business.industry, Detector, Perseus Arm, Shell (structure), Astronomy and Astrophysics, Scale (descriptive set theory), Pattern recognition, Astrophysics, 01 natural sciences, Identification (information), Space and Planetary Science, 0103 physical sciences, Artificial intelligence, business, 010303 astronomy & astrophysics
Abstract

The identification of expanding HI shells is difficult because of their variable morphological characteristics. The detection of HI bubbles on a global scale therefore never has been attempted. In this paper, an automatic detector for expanding HI shells is presented. The detection is based on the more stable dynamical characteristics of expanding shells and is performed in two stages. The first one is the recognition of the dynamical signature of an expanding bubble in the velocity spectra, based on the classification of an artificial neural network. The pixels associated with these recognized spectra are identified on each velocity channel. The second stage consists in looking for concentrations of those pixels that were firstly pointed out, and to decide if they are potential detections by morphological and 21-cm emission variation considerations. Two test bubbles are correctly detected and a potentially new case of shell that is visually very convincing is discovered. About 0.6% of the surveyed pixels are identified as part of a bubble. These may be false detections, but still constitute regions of space with high probability of finding an expanding shell. The subsequent search field is thus significantly reduced. We intend to conduct in the near future a large scale HI shells detection over the Perseus Arm using our detector.

Published
2007
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8. On the structure of the turbulent interstellar atomic hydrogen

Author

Edouard Audit, Patrick Hennebelle, Marc-Antoine Miville-Deschenes, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'astrophysique spatiale (IAS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)

Subjects
Physics, Line-of-sight, Computer simulation, Hydrogen, Turbulence, Molecular cloud, chemistry.chemical_element, Astronomy and Astrophysics, Astrophysics, Instability, Spectral line, Interstellar medium, chemistry, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; Aims:It is necessary to understand the dynamics of atomic gas to use complex modeling and to carry out detailed comparisons between theoretical models and observations. Methods: In a companion paper, we present high resolution bidimensional numerical simulations of the interstellar atomic hydrogen. Here, we further characterize these simulations and we compare our results with various observations. Results: We give statistics of the column density and velocity along the line of sight and show that they compare favorably with observations of high-latitude lines of sight. We compute synthetic HI spectra and qualitatively discuss the information that could be inferred if these spectra were observed. Finally, we extract CNM clouds and study their physical properties finding strong similarities with real clouds. In particular, we find that the clouds follow Larson-type relations, i.e. M ∝ L^gamma, where gamma ~= 1.7 (we propose a theory which predicts gamma ~= 2.5 in 3D) and &surd;{< delta v^2> } ∝ L0.4. We also find that the distribution, N(N), of the column density, N, of the CNM structures formed in the simulation follows N(N) ∝ N-1.2 which is marginally compatible with the observational result obtained by Heiles & Troland ([CITE], ApJ, 624, 773). From the mass-size relation and the mass spectrum, we derive an exponent for the column density distribution close to the value obtained in the numerical simulation. Conclusions: .We conclude that the simulations reproduce various observational features reasonably well. An important implication suggested by our results is that the "turbulence" within the cold interstellar atomic gas is mainly the result of individual long living cloudlet (confined by an external warm medium) motions rather than supersonic turbulence within nearly isothermal clouds. Another important aspect is that the CNM structures produced in the simulation present various physical characteristics that are similar to the characteristics of the molecular clouds. This raises the question as to whether the physical properties of the molecular clouds are determined at a very early stage, before the gas becomes molecular.

Published
2007
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9. Dust variations in the diffuse interstellar medium: constraints on Milky Way dust from Planck-HFI observations

Author

M. Koehler, Marc-Antoine Miville-Deschenes, Anthony P. Jones, Lapo Fanciullo, Nathalie Ysard, A. Abergel, Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Met Office Hadley Centre for Climate Change (MOHC), and United Kingdom Met Office [Exeter]

Subjects
Milky Way, FOS: Physical sciences, chemistry.chemical_element, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Mantle (geology), evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, ISM: general, Physics, extinction, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Amorphous solid, Interstellar medium, Amorphous carbon, chemistry, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Particle-size distribution, submillimeter: ISM, Astrophysics::Earth and Planetary Astrophysics, dust, Carbon, Intensity (heat transfer)
Abstract

The Planck-HFI all-sky survey from 353 to 857GHz combined with the 100 microns IRAS show that the dust properties vary in the diffuse ISM at high Galactic latitude (1e19, Comment: Accepted for publication in A&A (abstract modified to fit arxiv standards) Corrected version of the paper on the 30th of March 2015 (missing lines in Figs. 6a and 6c)

Published
2015
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10. On the Use of Fractional Brownian Motion Simulations to Determine the Three‐dimensional Statistical Properties of Interstellar Gas

Author

Marc-Antoine Miville-Deschenes, François Levrier, and E. Falgarone

Subjects
Physics, Transverse plane, Spectral index, Fractional Brownian motion, Scale (ratio), Space and Planetary Science, Spectral density, Centroid, Astronomy and Astrophysics, Vector field, Astrophysics, Computational physics, Line (formation)
Abstract

Based on fractional Brownian motion (fBm) simulations of 3D gas density and velocity fields, we present a study of the statistical properties of spectro-imagery observations (channel maps, integrated emission, and line centroid velocity) in the case of an optically thin medium at various temperatures. The power spectral index gamma_W of the integrated emission is identified with that of the 3D density field (gamma_n) provided the medium's depth is at least of the order of the largest transverse scale in the image, and the power spectrum of the centroid velocity map is found to have the same index gamma_C as that of the velocity field (gamma_v). Further tests with non-fBm density and velocity fields show that this last result holds, and is not modified either by the effects of density-velocity correlations. A comparison is made with the theoretical predictions of Lazarian & Pogosyan (2000).

Published
2003
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12. [Untitled]

Author

Alain Abergel, H. Aussel, Marc-Antoine Miville-Deschenes, Michel Perault, F. X. Désert, and Marc Sauvage

Subjects
Physics, Data processing, Silicon, business.industry, Infrared, Detector, chemistry.chemical_element, Flux, Astronomy and Astrophysics, Photometry (optics), Optics, chemistry, Space and Planetary Science, Transient (oscillation), business, Communication channel
Abstract

The detector of the long wavelength channel of the ISOCAMcamera on-board the Infrared Space Observatory is a Galliumdoped Silicon photo-conductor hybridized by Indium bump. Itpresents systematic memory effects of the response which canbias the photometry by a factor of typically 40%. The main features of the response after flux variations are discussed. A simple empirical model actually used to correct systematically the data with a photometric accuracy of 5–10% is detailed.

Published
2000
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13. Probing the origin of the microwave anomalous foreground ( Corrigendum )

Author

Marc-Antoine Miville-Deschenes, Laurent Verstraete, Nathalie Ysard, 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), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11)

Subjects
Physics, 010308 nuclear & particles physics, extinction, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Space and Planetary Science, Extinction (optical mineralogy), [SDU]Sciences of the Universe [physics], 0103 physical sciences, dust, 010303 astronomy & astrophysics, addenda, Microwave, ComputingMilieux_MISCELLANEOUS, errata, ISM: general
Abstract

The Letter “Probing the origin of the microwave anomalous foreground” was published in A&A 509, L1 (2010). This corrigendum corrects the legend of Fig. 5, where the linestyles (dotted and dashed) were inverted (Fig. 1). Consequently, the results presented in Sect. 7.4 and Fig. 17 in Hoang et al. (2011) are in good agreement with the results of Ysard et al. (2010), regarding both the peak frequencies of the spectra and their relative intensities.

Published
2012
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14. An accurate measurement of the anisotropies and mean level of the Cosmic Infrared Background at 100 and 160 um

Author

Peter G. Martin, Aurélie Pénin, K. Blagrave, Julien Grain, Marc-Antoine Miville-Deschenes, Nicolas Ponthieu, Guilaine Lagache, Felix J. Lockman, and Alberto Noriega-Crepo

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, Astrophysics::High Energy Astrophysical Phenomena, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Space and Planetary Science, Cosmic infrared background, Galaxy formation and evolution, Millimeter, Cirrus, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The measurement of the anisotropies in the cosmic infrared background (CIB) is a powerful mean of studying the evolution of galaxies and large-scale structures. These anisotropies have been measured by a number of experiments, from the far-infrared to the millimeter. One of the main impediments to an accurate measurement on large scales is the contamination of the foreground signal by Galactic dust emission. Our goal is to show that we can remove the Galactic cirrus contamination using HI data, and thus accurately measure the clustering of starburst galaxies in the CIB. We use observations of the ELAIS N1 field at far-infrared (100 and 160{\mu}m) and radio (21 cm) wavelengths. We compute the correlation between dust emission, traced by far-infrared observations, and HI gas traced by 21cm observations, and derive dust emissivities that enable us to subtract the cirrus emission from the far-infrared maps. We then derive the power spectrum of the CIB anisotropies, as well as its mean level at 100{\mu}m and 160{\mu}m. We also combine the HI data and Spitzer total power mode absolute measurements to determine the CIB mean level at 160{\mu}m. We find B160=0.77\pm0.04\pm0.12MJy/sr,where the first error is statistical and the second systematic. Combining this measurement with the B100/B160 color of the correlated anisotropies, we also derive the CIB mean at 100 {\mu}m, B100=0.24\pm0.08\pm0.04 MJy/sr. This measurement is in line with values obtained with recent models of infrared galaxy evolution and Herschel/PACS data, but is much smaller than the previous DIRBE measurements. The use of high-angular resolution Hi data is mandatory to accurately differentiate the cirrus from the CIB emission. The 100 {\mu}m IRAS map (and thus the map developed by Schlegel and collaborators) in such extragalactic fields is highly contaminated by the CIB anisotropies and hence cannot be used as a Galactic cirrus tracer., Comment: 13 pages, 14 figures, published in A&A, the abstract has been reduced

Published
2011
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15. Planck pre-launch status: HFI ground calibration

Author

L. Montier, Y. Giraud-Héraud, C. Mercier, C. Rosset, D. Yvon, Michel Lefebvre, J. P. Torre, Etienne Pointecouteau, Andrew E. Lange, J.-J. Fourmond, V. Hervier, P. Eng, D. Broszkiewicz, M. Charra, C. Nicolas, L. Guglielmi, G. Guyot, J.-L. Beney, O. Perdereau, K. Dassas, F. Piacentini, M. Piat, A. Chardin, C. Evesque, B. Leriche, Bruno Maffei, M. Veneziani, Peter A. R. Ade, F. Couchot, F. Pajot, R. V. Sudiwala, P. Duret, S. François, C. Marty, Sophie Henrot-Versille, J. Charra, Thierry Maciaszek, R. Pons, J. Haissinski, I. Ristorcelli, J.-M. Lamarre, A. Mahendran, W. C. Jones, Jean-Loup Puget, C. Rioux, W. A. Holmes, D. Vallée, Giorgio Savini, A. Catalano, Matthieu Tristram, Stéphane Plaszczynski, P. de Marcillac, C. Carabétian, Philippe Camus, B. Mansoux, N. Ponthieu, F. Noviello, M. Giard, B. P. Crill, P. Lami, J. C. Renault, Marc-Antoine Miville-Deschenes, Claude Leroy, J. F. Macías-Pérez, A. Coulais, Silvia Masi, E. Bréelle, F.-X. Désert, P. de Bernardis, J. Daubin, D. Rambaud, J.-M. Delouis, C. Renault, R. Cizeron, 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), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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), Cryogénie (NEEL - Cryo), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire 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), Centre d'étude spatiale des rayonnements (CESR), 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), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, PLANCK, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), Cryogénie (Cryo), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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, 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, Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Cryo - Cryogénie, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université 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), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)

Subjects
cosmic microwave background, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, 0103 physical sciences, Calibration, space vehicles: instruments, Planck, 010303 astronomy & astrophysics, space vehicles : instruments, QB, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, submillimeter: general, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], On board, Cardinal point, Space and Planetary Science, symbols, Vacuum chamber
Abstract

Context. The Planck satellite was successfully launched on May 14th 2009. We have completed the pre-launch calibration measurements of the High Frequency Instrument (HFI) on board Planck and their processing.\ud \ud Aims. We present the results ot the pre-launch calibration of HFI in which we have multiple objectives. First, we determine instrumental parameters that cannot be measured in-flight and predict parameters that can. Second, we take the opportunity to operate and understand the instrument under a wide range of anticipated operating conditions. Finally, we estimate the performance of the instrument built.\ud \ud Methods. We obtained our pre-launch calibration results by characterising the component and subsystems, then by calibrating the focal plane at IAS (Orsay) in the Saturne simulator, and later from the tests at the satellite level carried out in the CSL (Liège) cryogenic vacuum chamber. We developed models to estimate the instrument pre-launch parameters when no measurement could be performed.\ud \ud Results. We reliably measure the Planck-HFI instrument characteristics and behaviour, and determine the flight nominal setting of all parameters. The expected in-flight performance exceeds the requirements and is close or superior to the goal specifications.

Published
2010
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16. Physical properties of the Sh2-104 HII region as seen by Herschel

Author

B. M. Swinyard, K. Blagrave, G. Lagache, H. Moseley, Edward Polehampton, P. A. R. Ade, François Orieux, D. Pinheiro Gonçalvez, T. Lin, Trevor Fulton, Frédérique Motte, David A. Naylor, Jean-Paul Baluteau, L. D. Anderson, Martin Cohen, Mathieu Compiegne, Derek Ward-Thompson, C. Joblin, S. C. Madden, Sergio Molinari, Marc-Antoine Miville-Deschenes, C. A. Beichman, G. Davis, Sylvain Bontemps, H. Arab, Locke D. Spencer, J.-P. Bernard, Pierre Cox, Cecile Gry, Mark Halpern, E. Habart, Sunil Sidher, Gibion Makiwa, Maohai Huang, K. Okumura, Jason M. Kirk, Emmanuel Dartois, D. Russeil, Paolo Saraceno, S. C. Jones, Alain Abergel, F. Boulanger, Pierrick Martin, Glenn J. White, Ph. André, J. A. Rodón, R. J. Emery, Thomas Rodet, Annie Zavagno, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Department of Ecology and Evolutionary Biology [Princeton], Princeton University, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, Cardiff 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), CITA, University of Toronto, Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), School of Physics and Astronomy [Cardiff], STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN), 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, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)

Subjects
H II region, FOS: Physical sciences, Context (language use), Astrophysics, Photodissociation region, 01 natural sciences, Spectral line, Photometry (optics), H ii regions, 0103 physical sciences, Isotopologue, 010306 general physics, 010303 astronomy & astrophysics, Physics, infrared: ISM, stars: formation, extinction, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ISM: individual objects: Sh2-104, Spectral density, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), dust, ISM: bubbles
Abstract

Context: Sh2-104 is a Galactic H ii region with a bubble morphology, detected at optical and radio wavelengths. It is considered the first observational confirmation of the collect-and-collapse model of triggered star-formation. Aims: We aim to analyze the dust and gas properties of the Sh2-104 region to better constrain its effect on local future generations of stars. In addition, we investigate the relationship between the dust emissivity index {\beta} and the dust temperature, T_dust. Methods: Using Herschel PACS and SPIRE images at 100, 160, 250, 350 and 500 {\mu}m we determine T_dust and {\beta} throughout Sh2-104, fitting the spectral energy distributions (SEDs) obtained from aperture photometry. With the SPIRE Fourier transform spectrometer (FTS) we obtained spectra at different positions in the Sh2-104 region. We detect J-ladders of CO and 13CO, with which we derive the gas temperature and column density. We also detect proxies of ionizing flux as the [NII] 3P1-3P0 and [CI] 3P2-3P1 transitions. Results: We find an average value of {\beta} ~ 1.5 throughout Sh2-104, as well as a T dust difference between the photodissociation region (PDR, ~ 25 K) and the interior (~ 40 K) of the bubble. We recover the anti-correlation between {\beta} and dust temperature reported numerous times in the literature. The relative isotopologue abundances of CO appear to be enhanced above the standard ISM values, but the obtained value is very preliminary and is still affected by large uncertainties., Comment: Accepted by A&A, to be published on the Herschel A&A Special Issue. 5 pages, 5 figures.

Published
2010
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17. Herschel-SPIRE spectroscopy of the DR21 molecular cloud core

Author

Jean-Paul Baluteau, J. A. Rodón, D. Pinheiro Gocalvez, K. Okumura, C. Joblin, Mathieu Compiegne, Derek Ward-Thompson, Matthew Joseph Griffin, Peter A. R. Ade, H. Moseley, Thomas Rodet, G. Lagache, Annie Zavagno, Emmanuel Dartois, Trevor Fulton, Martin Cohen, D. Russeil, Sergio Molinari, P. Saraceno, F. Boulanger, B. M. Swinyard, Sarah Leeks, R. J. Emery, Edward Polehampton, David A. Naylor, Marc-Antoine Miville-Deschenes, B. G. Gom, T. L. Lim, Peter G. Martin, Locke D. Spencer, K. Blagrave, J.-P. Bernard, E. Habart, Sunil Sidher, Glenn J. White, Peter Timothy Cox, Ph. André, G. Davis, Cecile Gry, Frédérique Motte, Gibion Makiwa, Alain Abergel, H. Arab, Maohai Huang, S. C. Jones, S. C. Madden, L. D. Anderson, Nicola Schneider, Jason M. Kirk, Sylvain Bontemps, STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), 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), 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'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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, Laboratoire d'Informatique de Nantes Atlantique (LINA), Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Department of Ecology and Evolutionary Biology [Princeton], Princeton University, School of Physics and Astronomy [Cardiff], Cardiff University, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), Agroscope Reckenholz - Tänikon (ART), Agroscope, Centre for Ecology and Hydrology (CEH), Natural Environment Research Council (NERC), Laboratoire de Probabilités et Modèles Aléatoires (LPMA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), CITA, University of Toronto, Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université 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), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), 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), and Agroscope Reckenholz-Tänikon Research Station ART

Subjects
Physics, Spectrometer, 010308 nuclear & particles physics, Filling factor, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, FOS: Physical sciences, Astronomy and Astrophysics, Rotational temperature, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Spectral line, Trace gas, 13. Climate action, Space and Planetary Science, Excited state, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Spectroscopy, 010303 astronomy & astrophysics
Abstract

We present far-infrared spectra and maps of the DR21 molecular cloud core between 196 and 671 microns, using the Herschel-SPIRE spectrometer. Nineteen molecular lines originating from CO, 13CO, HCO+ and H2O, plus lines of [N II] and [CI] were recorded, including several transitions not previously detected. The CO lines are excited in warm gas with Tkin ~ 125 K and nH2 ~ 7 x 10^4 cm-3, CO column density N(CO) ~ 3.5 x 10^18 cm^-2 and a filling factor of ~ 12%, and appear to trace gas associated with an outflow. The rotational temperature analysis incorporating observations from ground-based telescopes reveals an additional lower excitation CO compoment which has a temperature ~ 78 K and N(CO) ~ 4.5 x 10^21 cm^-2. Astronomy & Astrophysics HERSCHEL special Issue, in press., 5 pages, 6 figures

Published
2010
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18. SPIRE spectroscopy of the prototypical Orion Bar photodissociation region

Author

J. A. Rodón, J.-P. Baluteau, Cecile Gry, Marvin L. Cohen, Peter A. R. Ade, Gibion Makiwa, Sunil Sidher, K. Okumura, Marc-Antoine Miville-Deschenes, Annie Zavagno, Alain Abergel, Sylvain Bontemps, S. C. Jones, Trevor Fulton, D. Pinheiro Gonçalves, Sergio Molinari, R. J. Emery, J.-P. Bernard, Guilaine Lagache, H. Moseley, H. Arab, C. Joblin, D. Russeil, F. Boulanger, T. L. Lim, Peter Timothy Cox, B. M. Swinyard, David A. Naylor, Maohai Huang, Peter G. Martin, K. Blagrave, Emmanuel Dartois, Paolo Saraceno, G. Davis, Emilie Habart, S. C. Madden, Mathieu Compiegne, Derek Ward-Thompson, Locke D. Spencer, Glenn J. White, Ph. André, Frédérique Motte, Edward Polehampton, Jason M. Kirk, L. D. Anderson, 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 d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Department of Ecology and Evolutionary Biology [Princeton], Princeton University, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), School of Physics and Astronomy, Cardiff University, Laboratoire de Probabilités et Modèles Aléatoires (LPMA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), CITA, University of Toronto, Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, School of Physics and Astronomy [Cardiff], Engineering Department, University of Cambridge [UK] (CAM), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), 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), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, and Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN)

Subjects
Astrophysics, Photodissociation region, 7. Clean energy, 01 natural sciences, 0103 physical sciences, evolution, Isotopologue, Emission spectrum, 010306 general physics, Spectroscopy, 010303 astronomy & astrophysics, Optical depth, QB, ISM: general, Physics, infrared: ISM, Spectrometer, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Astronomy, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ISM: molecules, ISM: lines and bands, Spire, 13. Climate action, Space and Planetary Science, submillimeter: ISM
Abstract

International audience; Aims: We present observations of the Orion Bar photodissociation region (PDR) obtained with the SPIRE instrument on-board Herschel. Methods: We obtained SPIRE Fourier-transform spectrometer (FTS) sparse sampled maps of the Orion bar. Results: The FTS wavelength coverage and sensitivity allow us to detect a wealth of rotational lines of CO (and its isotopologues), fine structure lines of C and N+, and emission lines from radicals and molecules such as CH+, CH, H2O or H2S. For species detected from the ground, our estimates of the column densities agree with previously published values. The comparison between 12CO and 13CO maps shows particularly the effects of optical depth and excitation in the molecular cloud. The distribution of the 12CO and 13CO lines with upper energy levels indicates the presence of warm (~100-150 K) CO. This warm CO component is a significant fraction of the total molecular gas, confirming previous ground based studies. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

Published
2010
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19. Herschel-SPIRE spectroscopy of G29.96-0.02: fitting the full SED

Author

H. Moseley, Trevor Fulton, Mathieu Compiegne, Derek Ward-Thompson, Emmanuel Dartois, Gibion Makiwa, Edward Polehampton, D. Russeil, J.-P. Bernard, Tanya Lim, Sergio Molinari, Peter A. R. Ade, B. M. Swinyard, Cecile Gry, Alain Abergel, C. Joblin, L. D. Anderson, Maohai Huang, K. Blagrave, Jean-Paul Baluteau, Pierre Cox, Sunil Sidher, Frédérique Motte, S. C. Madden, F. Boulanger, G. Davis, David A. Naylor, Marc-Antoine Miville-Deschenes, H. Arab, Peter G. Martin, G. Lagache, S. C. Jones, Sylvain Bontemps, E. Habart, K. Okumura, Locke D. Spencer, Jason M. Kirk, Annie Zavagno, Glenn J. White, Ph. André, R. J. Emery, Martin Cohen, P. Saraceno, J. A. Rodón, D. Pinheiro Gocalvez, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Centre d'étude spatiale des rayonnements (CESR), 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), School of Physics and Astronomy [Cardiff], Cardiff University, Engineering Department, University of Cambridge [UK] (CAM), 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), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Department of Ecology and Evolutionary Biology [Princeton], Princeton University, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), Laboratoire de Probabilités et Modèles Aléatoires (LPMA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), CITA, University of Toronto, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Consiglio Nazionale delle Ricerche (CNR), 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 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, Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN), and Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Physics, 010504 meteorology & atmospheric sciences, Spectrometer, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 7. Clean energy, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Spectral line, Luminosity, Wavelength, Spire, Spitzer Space Telescope, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Emissivity, Spectroscopy, 010303 astronomy & astrophysics, QB, 0105 earth and related environmental sciences
Abstract

We use the SPIRE Fourier-Transform Spectrometer (FTS) on-board the ESA Herschel Space Telescope to analyse the submillimetre spectrum of the Ultra-compact HII region G29.96-0.02. Spectral lines from species including 13CO, CO, [CI], and [NII] are detected. A sparse map of the [NII] emission shows at least one other HII region neighbouring the clump containing the UCHII. The FTS spectra are combined with ISO SWS and LWS spectra and fluxes from the literature to present a detailed spectrum of the source spanning three orders of magnitude in wavelength. The quality of the spectrum longwards of 100 {\mu}m allows us to fit a single temperature greybody with temperature 80.3\pm0.6K and dust emissivity index 1.73\pm0.02, an accuracy rarely obtained with previous instruments. We estimate a mass of 1500 Msol for the clump containing the HII region. The clump's bolometeric luminosity of 4 x 10^6 Lsol is comparable to, or slightly greater than, the known O-star powering the UCHII region., Comment: 5 pages including affiliations, 4 figures, accepted by A&A

Published
2010
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20. PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper

Author

Philippe, A, Baccigalupi, C, Anthony, B, Domingos, B, Barreiro, B, James, B, Bartolo, N, Stefano Battistelli, E, Battye, R, Bendo, G, Benoit, A, Bernard, J, Bersanelli, M, Bethermin, M, Pawel, B, Bonaldi, A, Francois, B, Jan, B, Martin, B, Burigana, C, Cai, Z, Philippe, C, Casas, F, Casasola, V, Guillaume, C, Anthony, C, Jens, C, Chon, G, Colafrancesco, S, Comis, B, Cuttaia, F, D'Alessandro, G, Da Silva, A, Davis, R, Avillez Miguel, D, Bernardis, P, De Bernardis, P, De Petris, M, De Rosa, A, De Zotti, G, Jacques, D, Desert, F, Dickinson, C, Maria Diego, J, Dunkley, J, Ensslin, T, Errard, J, Falgarone, E, Ferreira, P, Ferriere, K, Finelli, F, Andrew, F, Fosalba, P, Gary, F, Galli, S, Ken, G, Juan, G, Ghribi, A, Martin, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Keith, G, Gruppuso, A, Alex, H, Hamilton, J, Haverkorn, M, Hernandez-Monteagudo, C, Herranz, D, Mark, J, Andrew, J, Khatri, R, Martin, K, Lamagna, L, Lattanzi, M, Leahy, P, Julien, L, Liguori, M, Liuzzo, E, Marcos, L, Juan, M, Maffei, B, Maino, D, Mangilli, A, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Melchiorri, A, Melin, J, Mennella, A, Mignano, A, Miville-Deschenes, M, Monfardini, A, Anthony, M, Pavel, N, Nati, F, Natoli, P, Negrello, M, Noviello, F, O'Sullivan, C, Paci, F, Pagano, L, Paladino, R, Nathalie, P, Paoletti, D, Peiris, H, Perrotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Polenta, G, Pollo, A, Nicolas, P, Mathieu, R, Ricciardi, S, Roman, M, Rosset, C, Rubino-Martin, J, Salatino, M, Schillaci, A, Paul, S, Silk, J, Starobinsky, A, Stompor, R, Rashid, S, Tartari, A, Terenzi, L, Toffolatti, L, Tomasi, M, Neil, T, Tristram, M, Trombetti, T, Tucci, M, Van De Weijgaert, R, Van Tent, B, Verde, L, Vielva, P, Ben, W, Watson, R, Stafford, W, André Philippe, Carlo Baccigalupi, Banday Anthony, Barbosa Domingos, Belen Barreiro, Bartlett James, Nicola Bartolo, Elia Stefano Battistelli, Richard Battye, George Bendo, Alain Benoit, Jean-Philippe Bernard, Marco Bersanelli, Matthieu Bethermin, Bielewicz Pawel, Anna Bonaldi, Bouchet Francois, Boulanger Francois, Brand Jan, Bucher Martin, Carlo Burigana, Zhen-Yi Cai, Camus Philippe, Francisco Casas, Viviana Casasola, Castex Guillaume, Challinor Anthony, Chluba Jens, Gayoung Chon, Sergio Colafrancesco, Barbara Comis, Francesco Cuttaia, Giuseppe D'Alessandro, Antonio Da Silva, Richard Davis, D.E. Avillez Miguel, Paolo D.E. Bernardis, Paolo De Bernardis, Marco De Petris, Adriano De Rosa, Gianfranco De Zotti, Delabrouille Jacques, Francois-Xavier Desert, Clive Dickinson, Jose Maria Diego, Joanna Dunkley, Torsten Ensslin, Josquin Errard, Edith Falgarone, Pedro Ferreira, Katia Ferriere, Fabio Finelli, Fletcher Andrew, Pablo Fosalba, Fuller Gary, Silvia Galli, Ganga Ken, García-Bellido Juan, Adnan Ghribi, Giard Martin, Yannick Giraud-Heraud, Joaquin Gonzalez-Nuevo, Grainge Keith, Alessandro Gruppuso, Hall Alex, Jean-Christophe Hamilton, Marijke Haverkorn, Carlos Hernandez-Monteagudo, Diego Herranz, Jackson Mark, Jaffe Andrew, Rishi Khatri, Kunz Martin, Luca Lamagna, Massimiliano Lattanzi, Paddy Leahy, Lesgourgues Julien, Michele Liguori, Elisabetta Liuzzo, Lopez-Caniego Marcos, Macias-Perez Juan, Bruno Maffei, Davide Maino, Anna Mangilli, Enrique Martinez-Gonzalez, Carlos J.A.P. Martins, Silvia Masi, Marcella Massardi, Sabino Matarrese, Alessandro Melchiorri, Jean-Baptiste Melin, Aniello Mennella, Arturo Mignano, Marc-Antoine Miville-Deschenes, Alessandro Monfardini, Murphy Anthony, Naselsky Pavel, Federico Nati, Paolo Natoli, Mattia Negrello, Fabio Noviello, Créidhe O'Sullivan, Francesco Paci, Luca Pagano, Rosita Paladino, Palanque-Delabrouille Nathalie, Daniela Paoletti, Hiranya Peiris, Francesca Perrotta, Francesco Piacentini, Michel Piat, Lucio Piccirillo, Giampaolo Pisano, Gianluca Polenta, Agnieszka Pollo, Ponthieu Nicolas, Remazeilles Mathieu, Sara Ricciardi, Matthieu Roman, Cyrille Rosset, Jose-Alberto Rubino-Martin, Maria Salatino, Alessandro Schillaci, Shellard Paul, Joseph Silk, Alexei Starobinsky, Radek Stompor, Sunyaev Rashid, Andrea Tartari, Luca Terenzi, Luigi Toffolatti, Maurizio Tomasi, Trappe Neil, Matthieu Tristram, Tiziana Trombetti, Marco Tucci, Rien Van De Weijgaert, Bartjan Van Tent, Licia Verde, Patricio Vielva, Wandelt Ben, Robert Watson, Withington Stafford, Philippe, A, Baccigalupi, C, Anthony, B, Domingos, B, Barreiro, B, James, B, Bartolo, N, Stefano Battistelli, E, Battye, R, Bendo, G, Benoit, A, Bernard, J, Bersanelli, M, Bethermin, M, Pawel, B, Bonaldi, A, Francois, B, Jan, B, Martin, B, Burigana, C, Cai, Z, Philippe, C, Casas, F, Casasola, V, Guillaume, C, Anthony, C, Jens, C, Chon, G, Colafrancesco, S, Comis, B, Cuttaia, F, D'Alessandro, G, Da Silva, A, Davis, R, Avillez Miguel, D, Bernardis, P, De Bernardis, P, De Petris, M, De Rosa, A, De Zotti, G, Jacques, D, Desert, F, Dickinson, C, Maria Diego, J, Dunkley, J, Ensslin, T, Errard, J, Falgarone, E, Ferreira, P, Ferriere, K, Finelli, F, Andrew, F, Fosalba, P, Gary, F, Galli, S, Ken, G, Juan, G, Ghribi, A, Martin, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Keith, G, Gruppuso, A, Alex, H, Hamilton, J, Haverkorn, M, Hernandez-Monteagudo, C, Herranz, D, Mark, J, Andrew, J, Khatri, R, Martin, K, Lamagna, L, Lattanzi, M, Leahy, P, Julien, L, Liguori, M, Liuzzo, E, Marcos, L, Juan, M, Maffei, B, Maino, D, Mangilli, A, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Melchiorri, A, Melin, J, Mennella, A, Mignano, A, Miville-Deschenes, M, Monfardini, A, Anthony, M, Pavel, N, Nati, F, Natoli, P, Negrello, M, Noviello, F, O'Sullivan, C, Paci, F, Pagano, L, Paladino, R, Nathalie, P, Paoletti, D, Peiris, H, Perrotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Polenta, G, Pollo, A, Nicolas, P, Mathieu, R, Ricciardi, S, Roman, M, Rosset, C, Rubino-Martin, J, Salatino, M, Schillaci, A, Paul, S, Silk, J, Starobinsky, A, Stompor, R, Rashid, S, Tartari, A, Terenzi, L, Toffolatti, L, Tomasi, M, Neil, T, Tristram, M, Trombetti, T, Tucci, M, Van De Weijgaert, R, Van Tent, B, Verde, L, Vielva, P, Ben, W, Watson, R, Stafford, W, André Philippe, Carlo Baccigalupi, Banday Anthony, Barbosa Domingos, Belen Barreiro, Bartlett James, Nicola Bartolo, Elia Stefano Battistelli, Richard Battye, George Bendo, Alain Benoit, Jean-Philippe Bernard, Marco Bersanelli, Matthieu Bethermin, Bielewicz Pawel, Anna Bonaldi, Bouchet Francois, Boulanger Francois, Brand Jan, Bucher Martin, Carlo Burigana, Zhen-Yi Cai, Camus Philippe, Francisco Casas, Viviana Casasola, Castex Guillaume, Challinor Anthony, Chluba Jens, Gayoung Chon, Sergio Colafrancesco, Barbara Comis, Francesco Cuttaia, Giuseppe D'Alessandro, Antonio Da Silva, Richard Davis, D.E. Avillez Miguel, Paolo D.E. Bernardis, Paolo De Bernardis, Marco De Petris, Adriano De Rosa, Gianfranco De Zotti, Delabrouille Jacques, Francois-Xavier Desert, Clive Dickinson, Jose Maria Diego, Joanna Dunkley, Torsten Ensslin, Josquin Errard, Edith Falgarone, Pedro Ferreira, Katia Ferriere, Fabio Finelli, Fletcher Andrew, Pablo Fosalba, Fuller Gary, Silvia Galli, Ganga Ken, García-Bellido Juan, Adnan Ghribi, Giard Martin, Yannick Giraud-Heraud, Joaquin Gonzalez-Nuevo, Grainge Keith, Alessandro Gruppuso, Hall Alex, Jean-Christophe Hamilton, Marijke Haverkorn, Carlos Hernandez-Monteagudo, Diego Herranz, Jackson Mark, Jaffe Andrew, Rishi Khatri, Kunz Martin, Luca Lamagna, Massimiliano Lattanzi, Paddy Leahy, Lesgourgues Julien, Michele Liguori, Elisabetta Liuzzo, Lopez-Caniego Marcos, Macias-Perez Juan, Bruno Maffei, Davide Maino, Anna Mangilli, Enrique Martinez-Gonzalez, Carlos J.A.P. Martins, Silvia Masi, Marcella Massardi, Sabino Matarrese, Alessandro Melchiorri, Jean-Baptiste Melin, Aniello Mennella, Arturo Mignano, Marc-Antoine Miville-Deschenes, Alessandro Monfardini, Murphy Anthony, Naselsky Pavel, Federico Nati, Paolo Natoli, Mattia Negrello, Fabio Noviello, Créidhe O'Sullivan, Francesco Paci, Luca Pagano, Rosita Paladino, Palanque-Delabrouille Nathalie, Daniela Paoletti, Hiranya Peiris, Francesca Perrotta, Francesco Piacentini, Michel Piat, Lucio Piccirillo, Giampaolo Pisano, Gianluca Polenta, Agnieszka Pollo, Ponthieu Nicolas, Remazeilles Mathieu, Sara Ricciardi, Matthieu Roman, Cyrille Rosset, Jose-Alberto Rubino-Martin, Maria Salatino, Alessandro Schillaci, Shellard Paul, Joseph Silk, Alexei Starobinsky, Radek Stompor, Sunyaev Rashid, Andrea Tartari, Luca Terenzi, Luigi Toffolatti, Maurizio Tomasi, Trappe Neil, Matthieu Tristram, Tiziana Trombetti, Marco Tucci, Rien Van De Weijgaert, Bartjan Van Tent, Licia Verde, Patricio Vielva, Wandelt Ben, Robert Watson, and Withington Stafford

Abstract

PRISM (Polarized Radiation Imaging and Spectroscopy Mission) was proposed to ESA in May 2013 as a large-class mission for investigating within the framework of the ESA Cosmic Vision program a set of important scientific questions that require high resolution, high sensitivity, full-sky observations of the sky emission at wavelengths ranging from millimeter-wave to the far-infrared. PRISM's main objective is to explore the distant universe, probing cosmic history from very early times until now as well as the structures, distribution of matter, and velocity flows throughout our Hubble volume. PRISM will survey the full sky in a large number of frequency bands in both intensity and polarization and will measure the absolute spectrum of sky emission more than three orders of magnitude better than COBE FIRAS. The data obtained will allow us to precisely measure the absolute sky brightness and polarization of all the components of the sky emission in the observed frequency range, separating the primordial and extragalactic components cleanly from the galactic and zodiacal light emissions. The aim of this Extended White Paper is to provide a more detailed overview of the highlights of the new science that will be made possible by PRISM, which include: (1) the ultimate galaxy cluster survey using the Sunyaev-Zeldovich (SZ) effect, detecting approximately 10 6 clusters extending to large redshift, including a characterization of the gas temperature of the brightest ones (through the relativistic corrections to the classic SZ template) as well as a peculiar velocity survey using the kinetic SZ effect that comprises our entire Hubble volume; (2) a detailed characterization of the properties and evolution of dusty galaxies, where the most of the star formation in the universe took place, the faintest population of which constitute the diffuse CIB (Cosmic Infrared Background); (3) a characterization of the B modes from primordial gravity waves generated during inflation and fro

Published
2014

21. MIPSGAL: A Survey of the Inner Galactic Plane at 24 and 70 μm

Author

William B. Latter, T. A. Kuchar, G. B. Berriman, Marc-Antoine Miville-Deschenes, D. R. Mizuno, Alberto Noriega-Crespo, Leonardo Testi, Nicolas Flagey, Remy Indebetouw, Babar Ali, Nicolas Billot, Francine R. Marleau, J. Ingalls, E. L. Ryan, Kathleen Kraemer, Roberta Paladini, Deborah Padgett, F. Boulanger, R. F. Shipman, Sergio Molinari, Eli Bressert, Peter G. Martin, Daniela Pinheiro Gonçalves, Sean Carey, S. Shenoy, Luisa Rebull, and S. D. Price

Subjects
SPECTRAL IRRADIANCE CALIBRATION, APERTURE-SUBMILLIMETER-TELESCOPE, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, H-II REGIONS, Spitzer Space Telescope, INFRARED-DARK CLOUDS, Infrared dark cloud, Disc, SMALL-MAGELLANIC-CLOUD, Supernova remnant, TRIGGERED STAR-FORMATION, Astrophysics::Galaxy Astrophysics, Cosmic dust, SPITZER-SPACE-TELESCOPE, Physics, Ecliptic, Astronomy, Astronomy and Astrophysics, Galactic plane, YOUNG STELLAR OBJECTS, Space and Planetary Science, Asteroid, SUPERNOVA REMNANT, MULTIBAND IMAGING PHOTOMETER, Astrophysics::Earth and Planetary Astrophysics
Abstract

MIPSGAL is a 278 deg(2) survey of the inner Galactic plane using the Multiband Infrared Photometer for Spitzer aboard the Spitzer Space Telescope. The survey field was imaged in two passbands, 24 and 70 mu m with resolutions of 6 '' and 18 '', respectively. The survey was designed to provide a uniform, well-calibrated and well-characterized data set for general inquiry of the inner Galactic plane and as a longer-wavelength complement to the shorter-wavelength Spitzer survey of the Galactic plane: Galactic Plane Infrared Mapping Survey Extraordinaire. The primary science drivers of the current survey are to identify all high-mass (M > 5 M-circle dot) protostars in the inner Galactic disk and to probe the distribution, energetics, and properties of interstellar dust in the Galactic disk. The observations were planned to minimize data artifacts due to image latents at 24 mu m and to provide full coverage at 70 mu m. Observations at ecliptic latitudes within 15 of the ecliptic plane were taken at multiple epochs to help reject asteroids. The data for the survey were collected in three epochs, 2005 September-October, 2006 April, and 2006 October with all of the data available to the public. The estimated point-source sensitivities of the survey are 2 and 75 mJy (3 sigma) at 24 and 70 mu m, respectively. Additional data processing was needed to mitigate image artifacts due to bright sources at 24 mu m and detector responsivity variations at 70 mu m due to the large dynamic range of the Galactic plane. Enhanced data products including artifact-mitigated mosaics and point-source catalogs are being produced with the 24 mu m mosaics already publicly available from the NASA/IPAC Infrared Science Archive. Some preliminary results using the enhanced data products are described.

Published
2009

22. BLAST05: Power Spectra of Bright Galactic Cirrus at Submillimeter Wavelengths

Author

Jacob Klein, Philip Daniel Mauskopf, James J. Bock, Peter G. Martin, A. Roy, Peter Charles Hargrave, David H. Hughes, Donald V. Wiebe, Mark Halpern, Matthew D. P. Truch, Christopher Semisch, Mark J. Devlin, Simon Dicker, Calvin B. Netterfield, Douglas Scott, Gaelen Marsden, Enzo Pascale, Luca Olmi, Gregory S. Tucker, Carole Tucker, Marco P. Viero, Marie Rex, Marc-Antoine Miville-Deschenes, Edward L. Chapin, Joshua O. Gundersen, Guillaume Patanchon, Matthew Joseph Griffin, Peter A. R. Ade, Department of Astronomy and Astrophysics, University of Toronto, 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), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Physics Department, University of Puerto Rico, 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
Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Observable, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Spectral line, Wavelength, Amplitude, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Spectral energy distribution, Cirrus, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Noise (radio), Astrophysics::Galaxy Astrophysics
Abstract

We report multi-wavelength power spectra of diffuse Galactic dust emission from BLAST observations at 250, 350, and 500 microns in Galactic Plane fields in Cygnus X and Aquila. These submillimeter power spectra statistically quantify the self-similar structure observable over a broad range of scales and can be used to assess the cirrus noise which limits the detection of faint point sources. The advent of submillimeter surveys with the Herschel Space Observatory makes the wavelength dependence a matter of interest. We show that the observed relative amplitudes of the power spectra can be related through a spectral energy distribution (SED). Fitting a simple modified black body to this SED, we find the dust temperature in Cygnus X to be 19.9 +/- 1.3 K and in the Aquila region 16.9 +/- 0.7 K. Our empirical estimates provide important new insight into the substantial cirrus noise that will be encountered in forthcoming observations., Comment: Submitted to the Astrophysical Journal. Maps and other data are available at http://blastexperiment.info/

Published
2009
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23. Cirrus as a probe for the galactic bubble bath

Author

Marc-Antoine Miville-Deschenes, F. Boulanger, and William T. Reach

Subjects
Interstellar medium, Physics, Local Bubble, Bubble bath, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Cirrus, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, Physics::Atmospheric and Oceanic Physics, Astrophysics::Galaxy Astrophysics, Latitude
Abstract

Galactic filaments called cirrus are used here to study the froth structure of the interstellar medium. Using the Leiden/Dwingeloo HI survey we observe that a significant fraction of intermediate latitude cirrus are distant clouds (R Gal

Published
2008
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24. The Cool Interstellar Medium

Author

Alain Abergel, Laurent Verstraete, Christine Joblin, René J. Laureijs, and Marc-Antoine Miville-Deschenes

Subjects
Physics, Electron density, Astrochemistry, Interstellar ice, Interstellar cloud, Infrared spectroscopy, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, Interstellar medium, Photometry (optics), Planetary science, 13. Climate action, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Infrared spectroscopy and photometry with ISO covering most of the emission range of the interstellar medium has led to important progress in the understanding of the physics and chemistry of the gas, the nature and evolution of the dust grains and also the coupling between the gas and the grains. We review here the ISO results on the cool and low-excitation regions of the interstellar medium, where T gas≲ 500 K, nH ∼ 100–105 cm−3 and the electron density is a few 10−4.

Published
2006
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25. First detection of dust emission in a High-Velocity Cloud

Author

William T. Reach, Marc-Antoine Miville-Deschenes, F. Boulanger, and A. Noreiga-Crespo

Subjects
Physics, Filling factor, Metallicity, Milky Way, Astrophysics (astro-ph), Green Bank Telescope, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Interstellar medium, High-velocity cloud, Spitzer Space Telescope, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

By comparing sensitive Spitzer Space Telescope (SST) infrared and Green Bank Telescope 21 cm observations, we are able to report the first detection of dust emission in Complex C, the largest High Velocity Cloud in the sky. Dust in the region of Complex C studied here has a colder temperature ($T=10.7^{+0.9}_{-0.8}$ K - 1$\sigma$) than the local interstellar medium ($T=17.5$ K), in accordance with its great distance from the Galactic plane. Based on the metallicity measurements and assuming diffuse Galactic interstellar medium dust properties and dust/metals ratio, this detection could imply gas column densities more than 5 times higher than observed in HI. We suggest that the dust emission detected here comes from small molecular clumps, spatially correlated with the HI but with a low surface filling factor. Our findings imply that the HVCs' mass would be much larger than inferred from HI observations and that most of the gas falling on the Milky Way would be in cold and dense clumps rather than in a diffuse phase., Comment: Accepted for publication in the Astrophysical Journal Letter, 5 pages, 4 figures

Published
2005

26. IRIS: A new generation of IRAS maps

Author

Guilaine Lagache, Marc-Antoine Miville-Deschenes, Canadian Institute for Theoretical Astrophysics (CITA), 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11)

Subjects
Brightness, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, symbols.namesake, Observational cosmology, 0103 physical sciences, Planck, astronomical data bases: miscellaneous, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Zodiacal light, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Interstellar medium, Space and Planetary Science, symbols, Satellite, Infrared cirrus, infrared: general- surveys
Abstract

The Infrared Astronomical Satellite (IRAS) had a tremendous impact on many areas of modern astrophysics. In particular it revealed the ubiquity of infrared cirrus that are a spectacular manifestation of the interstellar medium complexity but also an important foreground for observational cosmology. With the forthcoming Planck satellite there is a need for all-sky complementary data sets with arcminute resolution that can bring informations on specific foreground emissions that contaminate the Cosmic Microwave Background radiation. With its 4 arcmin resolution matching perfectly the high-frequency bands of Planck, IRAS is a natural data set to study the variations of dust properties at all scales. But the latest version of the images delivered by the IRAS team (the ISSA plates) suffer from calibration, zero level and striping problems that can preclude its use, especially at 12 and 25 micron. In this paper we present how we proceeded to solve each of these problems and enhance significantly the general quality of the ISSA plates in the four bands (12, 25, 60 and 100 micron). This new generation of IRAS images, called IRIS, benefits from a better zodiacal light subtraction, from a calibration and zero level compatible with DIRBE, and from a better destriping. At 100 micron the IRIS product is also a significant improvement from the Schlegel et al. (1998) maps. IRIS keeps the full ISSA resolution, it includes well calibrated point sources and the diffuse emission calibration at scales smaller than 1 degree was corrected for the variation of the IRAS detector responsivity with scale and brightness. The uncertainty on the IRIS calibration and zero level are dominated by the uncertainty on the DIRBE calibration and on the accuracy of the zodiacal light model., 16 pages, 17 figures, accepted for publication in ApJ (Suppl). Higher resolution version available at http://www.cita.utoronto.ca/~mamd/IRIS/IrisTechnical.html

Published
2004
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27. Power spectrum of the cosmic infrared background at 60 and 100 microns with IRAS

Author

Marc-Antoine Miville-Deschenes, J.-L. Puget, G. Lagache, Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), 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), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, COSMIC cancer database, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Astrophysics (astro-ph), Spectral density, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, 13. Climate action, Space and Planetary Science, Cosmic infrared background, 0103 physical sciences, Cirrus, 010303 astronomy & astrophysics, Noise (radio), Luminosity function, 0105 earth and related environmental sciences
Abstract

Based on a power spectrum analysis of the IRAS ISSA maps, we present the first detection of the Cosmic far-Infrared Background (CIB) fluctuations at 60 and 100 microns. The power spectrum of 12 low cirrus emission regions is characterized by a power excess at spatial frequencies higher than k~0.02 arcmin^{-1}. Most of this excess is due to noise and to nearby point sources with a flux stronger than 1 Jy. But we show that when these contributions are carefully removed, there is still a power excess that is the signature of the CIB fluctuations. The power spectrum of the CIB at 60 and 100 microns is compatible with a Poissonian distribution, at spatial frequencies between 0.025 and 0.2 arcmin^{-1}. The fluctuation level is ~1.6x10^3 Jy^2/sr and ~5.8x10^3 Jy^2/sr at 60 and 100 microns respectively. The levels of the fluctuations are used in a larger framework, with other observationnal data, to constrain the evolution of IR galaxies (Lagache et al. 2002). The detections reported here, coupled with the level of the fluctuations at 170 microns, give strong constraints on the evolution of the IR luminosity function. The combined results at 60, 100 and 170 microns for the CIB and its fluctuations allows, on the CIB at 60 microns, to put a firm upper limit of 0.27 MJy/sr and to give an estimate of 0.18 MJy/sr., Comment: 11 pages, 8 figures, Astronomy and Astrophysics in press

Published
2002
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28. Erratum: 'Structure and Colors of Diffuse Emission in the Spitzer Galactic First Look Survey' (ApJS, 154, 281 [2004])

Author

W. J. Glaccum, S. Stolovy, James G. Ingalls, Stefanie Wachter, Marc-Antoine Miville-Deschenes, Jennifer L. Karr, Sergio Fajardo-Acosta, Sean Carey, J. O'Linger, John Stauffer, George Helou, Alberto Noriega-Crespo, Jeonghee Rho, Martin Burgdorf, Deborah Padgett, William T. Reach, D. W. Hoard, F. Boulanger, and L. M. Rebull

Subjects
Physics, Mean square, Space and Planetary Science, Structure (category theory), Vertical axis, Astronomy and Astrophysics, Astrophysics, Surface brightness, Spectral line
Abstract

We have discovered an error in the scaling of our IRAC 8 m and MIPS 70 m data, which affected the caption for Figure 1 and the vertical axis scales for Figure 2. The original units in the images displayed in Figure 1 were MJy sr 1 for 8 m and Jy arcsec 2 for MIPS 24 and 70 m. We incorrectly multiplied our IRAC data by 0.0425 (the conversion from Jy arcsec 2 to MJy sr ), but neglected to multiply our MIPS 70 m data by that factor. (MIPS 24 m data were scaled correctly.) Thus, contrary to the caption of Figure 1, the gray levels for panels (a) and (b) actually range from 6.7 to 7.8 MJy sr , and the gray levels for panels (e) and ( f ) actually range from 0.85 to 20.8MJy sr . The power spectra in Figure 2 should have been normalized such that the integral over the spectrum equals the mean square image surface brightness. In the original paper, however, the IRAC power spectrumwas incorrectly multiplied by (0.0425), whereas theMIPS 70 m spectrum should have been multiplied by this factor but was not. We correct this in a revised version of Figure 2 included here. We thank Rick Arendt for calling our attention to this error.

Published
2006
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29. The evolution of very small dust particles in molecular clouds observed with ISOCAM

Author

M. M. Casali, P. Persi, Francois Boulanger, Jean-Loup Puget, Pascal André, Alain Abergel, Michel Perault, C. J. Cesarsky, J. P. Bernard, L. Nordh, Thierry Montmerle, A. A. Kaas, D. Cesarsky, M. Huldtgren, Marc-Antoine Miville-Deschenes, Sylvain Bontemps, F. Sibille, Edith Falgarone, G. Olofsson, and Anthony P. Jones

Subjects
Physics, Infrared, Spatial structure, Molecular cloud, Dust particles, General Engineering, Astronomy, Astronomy and Astrophysics, Astrophysics, Radiation, Wavelength, Space and Planetary Science, Low density, Small particles
Abstract

We present ISOCAM observations (5-18 μm) of illuminated surfaces of molecular clouds. The emission properties of the transiently heated small particles, which dominate the emission observed by ISOCAM, are analysed in relation with the spatial structure of the material. Striking spatial variations of the infrared colour (5-8.5 μm/12-18 μm) are detected. Spectroscopic observations show that they are due to variations of the intensity of the aromatic features (especially at 7.7 μm) relatively to the continuum emission increasing towards long wavelengths. Compared to the intensity of the continuum emission, the intensity of the aromatic features are significantly fainter at the illuminated surfaces of dense structures than in low density regions surrounding these dense structures. This effect could be the signature of photo-chemical evolution, size segregation due to grain dynamics in uni-directional radiation fields, or abundance variations of very small particles.

Published
2002
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31. Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way

Author

J. A. Rodón, K. Ganga, M. Pomarès, Friedrich Wyrowski, Mika Juvela, F. Piacentini, Melvin Hoare, William T. Reach, Stefano Pezzuto, A. Roy, Jean-Paul Baluteau, Marc-Antoine Miville-Deschenes, Russell H. Taylor, Pierre Royer, Alessio Traficante, Peter Schilke, D. Paradis, Glenn J. White, Cara Battersby, Alberto Noriega-Crespo, Harriet Parsons, M. Veneziani, Dimitrios Stamatellos, Vincent Minier, Lorenzo Piazzo, Guy S. Stringfellow, Michael G. Burton, L. K. Morgan, Frederic Schuller, F. Faustini, P. Saraceno, S. D. Lord, Jason Glenn, E. Sturm, Michael D. Smith, G. Joncas, A. M. di Giorgio, D. Polychroni, L. Montier, D. J. Marshall, N. Billot, José Cernicharo, F. Boulanger, M. T. Beltrán, Paul Martin, Matthew Joseph Griffin, B. Swinyard, Guilaine Lagache, Serena Viti, Mathieu Compiegne, Derek Ward-Thompson, P. de Bernardis, Frédérique Motte, B. Sibthorpe, Sukanya Chakrabarti, Nicolas Flagey, Christopher M. Brunt, Maggie A. Thompson, Qizhou Zhang, J.-P. Bernard, Annie Zavagno, Jean-François Robitaille, L. Spinoglio, Marc Sauvage, D. Russeil, Paolo Natoli, A. Abergel, Babar Ali, Davide Elia, D. Ikhenaode, Gary A. Fuller, C. Joblin, G. de Gasperis, Eugenio Schisano, Pedro García-Lario, Jin-Zeng Li, Isabelle Ristorcelli, Sergio Molinari, Luca Calzoletti, M. R. Pestalozzi, Nicolas Peretto, Thomas P. Robitaille, Mikako Matsuura, Riccardo Cesaroni, Rene Plume, Jan Brand, Paul F. Goldsmith, Leonardo Testi, Joseph C. Mottram, H. W. Yorke, Cristina Popescu, Martin Cohen, M. Benedettini, M. J. Barlow, Antonio Chrysostomou, Paola Caselli, Luca Olmi, Maohai Huang, Massimo Marengo, R. Paladini, Fabrizio Massi, L. A. Wilcock, Grazia Umana, Francesco Strafella, Toby J. T. Moore, Benjamin L. Schulz, R. Vavrek, T. Mueller, John Bally, J. A. D. L. Blommaert, L. D. Anderson, C. Waelkens, T. L. Lim, Richard J. Tuffs, Sean Carey, Yasuo Fukui, J. Neves, Nicola Schneider, Jason M. Kirk, Silvia Masi, Pascal André, Howard A. Smith, Luca Valenziano, Sylvain Bontemps, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique 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), CITA, University of Toronto, European Southern Observatory (ESO), 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), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratory of Comparative Carcinogenesis (LABORATORY OF COMPARATIVE CARCINOGENESIS), National Cancer Institute [Bethesda] (NCI-NIH), National Institutes of Health [Bethesda] (NIH)-National Institutes of Health [Bethesda] (NIH), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), 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), FORMATION STELLAIRE 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, 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), ISO Data Centre (ESA - Espagne), Agence Spatiale Européenne = European Space Agency (ESA), Herschel Science Centre (ESA Espagne), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Universiti Brunei Darussalam, Biology Department, Universitii Brunei Darussalam, Università degli Studi di Roma Tor Vergata [Roma], University of Manchester [Manchester], 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), Tenovus Centre for Cancer Research, Welsh School of Pharmacy, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Inter University Accelerator Centre, Aruna Asaf Ali Marg, LEOSPHERE France, LEOSPHERE, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Atmospheric Sciences Division [Hampton], NASA Langley Research Center [Hampton] (LaRC), School of Physics and Astronomy [Cardiff], Cardiff University, Shanghai Inst Opt & Fine Mech, Key Lab Mat Sci & Technol High Power Lasers, Molinari, S., Swinyard, B., Bally, J., Barlow, M., Bernard, J. P., Martin, P., Moore, T., Noriega Crespo, A., Plume, R., Testi, L., Zavagno, A., Abergel, A., Ali, B., Anderson, L., Andre, P., Baluteau, J. P., Battersby, C., Beltrán, M. T., Benedettini, M., Billot, N., Blommaert, J., Bontemps, S., Boulanger, F., Brand, J., Brunt, C., Burton, M., Calzoletti, L., Carey, S., Caselli, P., Cesaroni, R., Cernicharo, J., Chakrabarti, S., Chrysostomou, A., Cohen, M., Compiegne, M., de Bernardis, P., de Gasperis, G., di Giorgio, A. M., Elia, Davide Quintino, Faustini, F., Flagey, N., Fukui, Y., Fuller, G. A., Ganga, K., Garcia Lario, P., Glenn, J., Goldsmith, P. F., Griffin, M., Hoare, M., Huang, M., Ikhenaode, D., Joblin, C., Joncas, G., Juvela, M., Kirk, J. M., Lagache, G., Li, J. Z., Lim, T. L., Lord, S. D., Marengo, M., Marshall, D. J., Masi, S., Massi, F., Matsuura, M., Minier, V., Miville Deschênes, M. A., Montier, L. A., Morgan, L., Motte, F., Mottram, J. C., Müller, T. G., Natoli, P., Neves, J., Olmi, L., Paladini, R., Paradis, D., Parsons, H., Peretto, N., Pestalozzi, M., Pezzuto, S., Piacentini, F., Piazzo, L., Polychroni, D., Pomarès, M., Popescu, C. C., Reach, W. T., Ristorcelli, I., Robitaille, J. F., Robitaille, T., Rodón, J. A., Roy, A., Royer, P., Russeil, D., Saraceno, P., Sauvage, M., Schilke, P., Schisano, E., Schneider, N., Schuller, F., Schulz, B., Sibthorpe, B., Smith, H. A., Smith, M. D., Spinoglio, L., Stamatellos, D., Strafella, Francesco, Stringfellow, G. S., Sturm, E., Taylor, R., Thompson, M. A., Traficante, A., Tuffs, R. J., Umana, G., Valenziano, L., Vavrek, R., Veneziani, M., Viti, S., Waelkens, C., Ward Thompson, D., White, G., Wilcock, L. A., Wyrowski, F., Yorke, H. W., Zhang, Q., Consiglio Nazionale delle Ricerche (CNR), 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, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), 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), European Space Agency (ESA), Dipartimento di Fisica, Universita` di Roma Tor Vergata, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-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), 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), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), 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)-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), Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), ITA, USA, GBR, FRA, DEU, and ESP

Subjects
010504 meteorology & atmospheric sciences, Field (physics), Milky Way, stars: formation, ISM: structure, ISM: clouds, Galaxy: general, FOS: Physical sciences, ism: structure, ism: clouds, galaxy: general, Astrophysics, 01 natural sciences, Protein filament, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Protostar, Infrared dark cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Galactic plane, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Core (optical fiber), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Magnetohydrodynamics
Abstract

We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key-project that will map the inner Galactic Plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2{\deg} x 2{\deg} tiles approximately centered at l=30{\deg} and l=59{\deg}. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call 'cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around A_V of about 1 is exceeded for the regions in the l=59{\deg} field; a A_V value between 5 and 10 is found for the l=30{\deg} field, likely due to the relatively larger distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm-2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows., Comment: A&A, accepted

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32. Planck 2015 results. II. Low Frequency Instrument data processing

Author

E. Martínez-González, F. Couchot, Hannu Kurki-Suonio, M. Piat, T. Riller, P. A. R. Ade, W. A. Holmes, B. Racine, S. Mottet, Peregrine McGehee, J.-F. Sygnet, F. Cuttaia, D. L. Clements, N. Ponthieu, L. Sanselme, J. J. Bock, X. Dupac, A. Curto, Simon Prunet, Jérôme Bobin, A. Chamballu, R. Kneissl, R. Keskitalo, Steven Gratton, K. Ganga, P. Bielewicz, G. Rocha, William T. Reach, O. Doré, J.-L. Puget, D. L. Harrison, Jean-François Cardoso, L. Perotto, Jose M. Diego, Lloyd Knox, E. P. S. Shellard, R. Paladini, O. Herent, W. Hovest, E. Pointecouteau, P. B. Lilje, R. J. Laureijs, J. A. Tauber, R. B. Barreiro, Michele Liguori, J. Borrill, A. Benoit-Lévy, Fernando Atrio-Barandela, K. M. Górski, M. Tristram, J. Delabrouille, F. Piacentini, L. Vibert, M. Giard, F. Noviello, D. Hanson, Aurelien A. Fraisse, R. J. Davis, G. Hurier, A. Gregorio, George Helou, François R. Bouchet, Calvin B. Netterfield, B. P. Crill, Charles R. Lawrence, G. Patanchon, J. F. Macías-Pérez, G. Roudier, Fabio Finelli, D. Pietrobon, Carol Anne Oxborrow, A. Zonca, D. Yvon, Bruno Maffei, F. Paci, Lung-Yih Chiang, Silvia Masi, S. D. M. White, F. Pajot, R. D. Davies, M. Le Jeune, A. de Rosa, H. C. Chiang, Sophie Henrot-Versille, L. P. L. Colombo, Michael P. Hobson, Peter Meinhold, K. Benabed, F. Perrotta, Dmitry Novikov, M. Frailis, Daniele Tavagnacco, Carlo Baccigalupi, F.-X. Désert, Alessandro Melchiorri, Julien Lesgourgues, Mika Juvela, E. Hivon, Xin Chen, J. R. Bond, Dipak Munshi, François Orieux, George Efstathiou, J.-M. Lamarre, Alessandro Gruppuso, Nicola Vittorio, M. Arnaud, J. González-Nuevo, A. Zacchei, T. Poutanen, C. Armitage-Caplan, G. W. Pratt, B. Rusholme, Michael Rowan-Robinson, Andrew H. Jaffe, Fabio Pasian, F. Villa, J.-P. Bernard, Gianluca Morgante, G. Umana, Sabino Matarrese, Marc-Antoine Miville-Deschenes, L. Montier, Locke D. Spencer, Philip Lubin, A. Moneti, Luca Valenziano, S. Mitra, J. Knoche, Allan Hornstrup, Michele Maris, Federico Nati, Z. Hou, Torsten A. Enßlin, M. Ashdown, Anthony Lasenby, H. K. Eriksen, M. Tomasi, D. Paoletti, G. Lagache, S. Osborne, R. V. Sudiwala, E. Keihänen, Jean-Luc Starck, S. R. Hildebrandt, D. J. Marshall, Luca Terenzi, C. Combet, V. Stolyarov, C. J. MacTavish, P. R. Christensen, Marco Bersanelli, B. D. Wandelt, Rafael Rebolo, A. Coulais, T. R. Jaffe, D. Herranz, M. Kunz, P. Natoli, Martin Reinecke, E. Battaner, Carlo Burigana, L. Mendes, Pavel D. Naselsky, F. Boulanger, L. Danese, P. de Bernardis, Stéphane Plaszczynski, Mathieu Remazeilles, I. Ristorcelli, G. de Zotti, Giovanna Giardino, Clive Dickinson, M. Douspis, D. Sutton, J. Aumont, J. Valiviita, C. North, A. Sauvé, Aurélien Benoit, Lawrence A. Wade, S. Ricciardi, B. Van Tent, A. J. Banday, F. Sureau, Nazzareno Mandolesi, J.-M. Delouis, C. Rosset, Jon E. Gudmundsson, L. Pagano, Hans Ulrik Nørgaard-Nielsen, R. Stompor, D. Girard, F. Matthai, Jörg P. Rachen, C. Renault, A.-S. Suur-Uski, D. Santos, M. Bucher, M. Migliaccio, R. Leonardi, Olivier Forni, F. K. Hansen, M. Tucci, Stéphane Colombi, M. Bridges, E. Franceschi, P. Vielva, S. Galeotta, Pierrick Martin, Elena Pierpaoli, Y. Giraud-Héraud, Pasquale Mazzotta, H. Dole, Theodore Kisner, Claude Leroy, I. D. Novikov, G. Prézeau, M. López-Caniego, R.-R. Chary, L. Popa, Daniel J. Mortlock, C. Hernández-Monteagudo, Kevin M. Huffenberger, Jo Dunkley, G. Polenta, M. Linden-Vørnle, Sarah E. Church, J. W. Bowyer, W. C. Jones, A. Mennella, Nabila Aghanim, O. Perdereau, S. Donzelli, Giorgio Savini, A. Catalano, S. Techene, Ade, P. A. R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Battaglia, PAOLA MARIA, Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. F., Castex, G., Catalano, A., Chamballu, A., Christensen, P. R., Colombi, S., Colombo, L. P. L., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Dole, H., Donzelli, Simona, Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschet, C., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D. L., Henrot Versillé, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Juvela, M., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., Lindholm, V., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Mcgehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Novikov, D., Novikov, I., Oppermann, N., Paci, F., Pagano, L., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Romelli, Erik, Rosset, C., Rossetti, M., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., Wilkinson, A., Yvon, D., Zacchei, A, Zonca, A., Ade, P, Aghanim, N, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, A, Barreiro, R, Bartolo, N, Basak, S, Battaglia, P, Battaner, E, Benabed, K, Benoît, A, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bock, J, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Bucher, M, Burigana, C, Butler, R, Calabrese, E, Cardoso, J, Castex, G, Catalano, A, Chamballu, A, Christensen, P, Colombi, S, Colombo, L, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, T, Eriksen, H, Fergusson, J, Finelli, F, Forni, O, Frailis, M, Franceschet, C, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Giard, M, Giraud Héraud, Y, Gjerløw, E, González Nuevo, J, Górski, K, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, F, Hanson, D, Harrison, D, Henrot Versillé, S, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Hurier, G, Jaffe, A, Jaffe, T, Juvela, M, Keihänen, E, Keskitalo, R, Kiiveri, K, Kisner, T, Knoche, J, Krachmalnicoff, N, Kunz, M, Kurki Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Leahy, J, Leonardi, R, Lesgourgues, J, Levrier, F, Liguori, M, Lilje, P, Linden Vørnle, M, Lindholm, V, López Caniego, M, Lubin, P, Macías Pérez, J, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, P, Martínez González, E, Masi, S, Matarrese, S, Mazzotta, P, Mcgehee, P, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Montier, L, Morgante, G, Morisset, N, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Nørgaard Nielsen, H, Novikov, D, Novikov, I, Oppermann, N, Paci, F, Pagano, L, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Pearson, T, Peel, M, Perdereau, O, Perotto, L, Perrotta, F, Pettorino, V, Piacentini, F, Pierpaoli, E, Pietrobon, D, Pointecouteau, E, Polenta, G, Pratt, G, Prézeau, G, Prunet, S, Puget, J, Rachen, J, Rebolo, R, Reinecke, M, Remazeilles, M, Renzi, A, Rocha, G, Romelli, E, Rosset, C, Rossetti, M, Roudier, G, Rubiño Martín, J, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Scott, D, Seiffert, M, Shellard, E, Spencer, L, Stolyarov, V, Sutton, D, Suur Uski, A, Sygnet, J, Tauber, J, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Türler, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vassallo, T, Vielva, P, Villa, F, Wade, L, Wandelt, B, Watson, R, Wehus, I, Wilkinson, A, Yvon, D, Zonca, A, Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-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 )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Planck, Hélium : du fondamental aux applications (NEEL - HELFA), 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), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Space vehicles: instruments – Methods:data analysis – cosmic microwave background, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Cosmic microwave background, FOS: Physical sciences, Space vehicles: instrument, Cosmic background radiation, 01 natural sciences, NO, instruments [Space vehicles], Optics, Settore FIS/05 - Astronomia e Astrofisica, Methods: data analysis, 0103 physical sciences, instrument [Space vehicles], Calibration, Space vehicles: instruments, Astronomy and Astrophysics, Space and Planetary Science, Angular resolution, data analysis [Methods], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB, Physics, 010308 nuclear & particles physics, business.industry, Instrument Data, Detector, Spectral density, Ranging, Astronomy and Astrophysic, data analysi [Methods], business, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Methods: data analysi, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

CSIC, Consejo Superior de Investigaciones Científicas; ERC, European Research Council; MINECO, Ministerio de Economía y Competitividad; MPG, Max-Planck-Gesellschaft; NASA, National Aeronautics and Space Administration; etc., Ade, P.A.R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A.J., Barreiro, R.B., Bartolo, N., Basak, S., Battaglia, P., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Bucher, M., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.-F., Castex, G., Catalano, A., Chamballu, A., Christensen, P.R., Colombi, S., Colombo, L.P.L., Crill, B.P., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J.M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschet, C., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K.M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F.K., Hanson, D., Harrison, D.L., Henrot-Versillé, S., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Juvela, M., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T.S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leahy, J.P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Lubin, P.M., Macías-Pérez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P.G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., McGehee, P., Meinhold, P.R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Moss, A., Munshi, D., Murphy, J.A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C.B., Nørgaard-Nielsen, H.U., Novikov, D., Novikov, I., Oppermann, N., Paci, F., Pagano, L., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T.J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G.W., Prézeau, G., Prunet, S., Puget, J.-L., Rachen, J.P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Romelli, E., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J.A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M.D., Shellard, E.P.S., Spencer, L.D., Stolyarov, V., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Watson, R., Wehus, I.K., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A.

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33. Evolution of interstellar dust with Herschel. First results in the photodissociation regions of NGC 7023

Author

Marc-Antoine Miville-Deschenes, H. Moseley, H. Arab, F. Boulanger, Pierrick Martin, Pierre Cox, Marc Sauvage, Annie Zavagno, E. Habart, Ph. André, Cecile Gry, Marvin L. Cohen, C. Joblin, Frédérique Motte, Paolo Saraceno, Jason M. Kirk, Trevor Fulton, L. D. Anderson, David A. Naylor, R. J. Emery, Guilaine Lagache, T. L. Lim, J.-P. Baluteau, Sunil Sidher, Mathieu Compiegne, Derek Ward-Thompson, Emmanuel Dartois, B. M. Swinyard, S. C. Jones, J. A. Rodón, Edward Polehampton, G. J. White, Alain Abergel, K. Blagrave, D. Russeil, Sylvain Bontemps, Locke D. Spencer, S. C. Madden, J.-P. Bernard, Peter A. R. Ade, Gibion Makiwa, K. Okumura, D. Pinheiro Gonçalves, Sergio Molinari, Maohai Huang, G. Davis, 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), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), 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), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Department of Ecology and Evolutionary Biology [Princeton], Princeton University, National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), 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), CITA, University of Toronto, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), 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 de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, School of Physics and Astronomy [Cardiff], Cardiff University, Engineering Department, University of Cambridge [UK] (CAM), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN), 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, Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Consiglio Nazionale delle Ricerche (CNR), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Laboratoire de Probabilités et Modèles Aléatoires (LPMA), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Extinction (astronomy), Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, photon-dominated region (PDR), 0103 physical sciences, evolution, Emissivity, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Cosmic dust, Physics, 010308 nuclear & particles physics, Star formation, extinction, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 13. Climate action, Space and Planetary Science, Circumstellar dust, submillimeter: ISM, Astrophysics::Earth and Planetary Astrophysics, dust
Abstract

International audience; Context. In photodissociation regions (PDRs), the physical conditions and the excitation evolve on short spatial scales as a function of depth within the cloud, providing a unique opportunity to study how the dust and gas populations evolve with the excitation and physical conditions. The mapping of the PDRs in NGC 7023 performed during the science demonstration phase of Herschel is part of the “Evolution of interstellar dust” key program. The goal of this project is to build a coherent database on interstellar dust emission from diffuse clouds to the sites of star formation. Aims: We study the far-infrared/submillimeter emission of the PDRs and their fainter surrounding regions. We combine the Herschel and Spitzer maps to derive at each position the full emission spectrum of all dust components, which we compare to dust and radiative transfer models in order to learn about the spatial variations in both the excitation conditions and the dust properties. Methods: We adjust the emission spectra derived from PACS and SPIRE maps using modified black bodies to derive the temperature and the emissivity index β of the dust in thermal equilibrium with the radiation field. We present a first modeling of the NGC 7023-E PDR with standard dust properties and abundances. Results: At the peak positions, a value of β equal to 2 is compatible with the data. The detected spectra and the spatial structures are strongly influenced by radiative transfer effects. We are able to reproduce the spectra at the peak positions deduced from Herschel maps and emitted by dust particles at thermal equilibrium, and also the evolution of the spatial structures observed from the near infrared to the submillimeter. On the other hand, the emission of the stochastically heated smaller particles is overestimated by a factor ~2. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

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