The dust and gas properties of M83

Autor: Roussel, H., Baes, M., Boquien, M., Boselli, A., Clements, D. L., Cooray, A., Davies, J. I., Eales, S. A., Madden, S., Page, M. J., Spinoglio, L., Foyle, K., Wilson, C. D., Mentuch, E., Bendo, G., Dariush, A., Parkin, T., Pohlen, M., Sauvage, M., Smith, M. W. L.
Přispěvatelé: Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universiteit Gent = Ghent University [Belgium] (UGENT), 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), AUTRES, California Institute of Technology (CALTECH), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California-University of California, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), McMaster University [Hamilton, Ontario], University of Manchester [Manchester], School of Physics and Astronomy [Cardiff], Cardiff University, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universiteit Gent = Ghent University (UGENT), 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), University of California (UC)-University of California (UC), Science and Technology Facilities Council (STFC), Universiteit Gent [Ghent]
Jazyk: angličtina
Rok vydání: 2012
Předmět:
Zdroj: Monthly Notices of the Royal Astronomical Society
Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P-Oxford Open Option A, 2012, 421 (4), pp.2917--2929. ⟨10.1111/j.1365-2966.2012.20520.x⟩
Monthly Notices of the Royal Astronomical Society, 2012, 421 (4), pp.2917--2929. ⟨10.1111/j.1365-2966.2012.20520.x⟩
ISSN: 0035-8711
1365-2966
Popis: International audience; We examine the dust and gas properties of the nearby, barred galaxy M83, which is part of the Very Nearby Galaxy Survey. Using images from the Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging REceiver (SPIRE) instruments of Herschel, we examine the dust temperature and dust mass surface density distribution. We find that the nuclear, bar and spiral arm regions exhibit higher dust temperatures and masses compared to interarm regions. However, the distributions of dust temperature and mass are not spatially coincident. Assuming a trailing spiral structure, the dust temperature peaks in the spiral arms lie ahead of the dust surface density peaks. The dust mass surface density correlates well with the distribution of molecular gas as traced by CO (J= 3?2) images (James Clerk Maxwell Telescope) and the star formation rate as traced by Ha with a correction for obscured star formation using 24-mu m emission. Using H i images from The H i Nearby Galaxy Survey (THINGS) to trace the atomic gas component, we make total gas mass surface density maps and calculate the gas-to-dust ratio. We find a mean gas-to-dust ratio of 84 +/- 4 with higher values in the inner region assuming a constant CO-to-H2 conversion factor. We also examine the gas-to-dust ratio using CO-to-H2 conversion factor that varies with metallicity.
Databáze: OpenAIRE
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