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Cited by 179Galaxies: Formation, Evolution, PhenomenaAstrophysics and Star Formation StudiesStellar, planetary, and galactic studies

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THE HERSCHEL EXPLOITATION OF LOCAL GALAXY ANDROMEDA (HELGA). II. DUST AND GAS IN ANDROMEDA

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Smith, M. W. L., Eales, S. A., Gomez, H. L., Roman-Duval, J., Fritz, J., Braun, R., Baes, M., Bendo, G. J., Blommaert, J. A. D. L., Boquien, M., Boselli, A., Clements, D. L., Cooray, A. R., Cortese, L., de Looze, I., Ford, G. P., Gear, W. K., Gentile, G., Gordon, K. D., Kirk, J., Lebouteiller, V., Madden, S., Mentuch, E., O’Halloran, B., Page, M. J., Schulz, B., Spinoglio, L., Verstappen, J., Wilson, C. D., Thilker, D. A.·2012·The Astrophysical Journal
DOI 10.1088/0004-637x/756/1/40
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Abstract

We present an analysis of the dust and gas in Andromeda, using Herschel images sampling the entire far-infrared peak. We fit a modified-blackbody model to ∼4000 quasi-independent pixels with spatial resolution of ∼140 pc and find that a variable dust-emissivity index (β) is required to fit the data. We find no significant long-wavelength excess above this model, suggesting there is no cold dust component. We show that the gas-to-dust ratio varies radially, increasing from ∼20 in the center to ∼70 in the star-forming ring at 10 kpc, consistent with the metallicity gradient. In the 10 kpc ring the average β is ∼1.9, in good agreement with values determined for the Milky Way (MW). However, in contrast to the MW, we find significant radial variations in β, which increases from 1.9 at 10 kpc to ∼2.5 at a radius of 3.1 kpc and then decreases to 1.7 in the center. The dust temperature is fairly constant in the 10 kpc ring (ranging from 17 to 20 K), but increases strongly in the bulge to ∼30 K. Within 3.1 kpc we find the dust temperature is highly correlated with the 3.6 μm flux, suggesting the general stellar population in the bulge is the dominant source of dust heating there. At larger radii, there is a weak correlation between the star formation rate and dust temperature. We find no evidence for "dark gas" in M31 in contrast to recent results for the MW. Finally, we obtained an estimate of the CO X-factor by minimizing the dispersion in the gas-to-dust ratio, obtaining a value of (1.9 ± 0.4) × 10 20 cm −2 [K km s −1 ] −1 .

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Metadata

Authors
Smith, M. W. L., Eales, S. A., Gomez, H. L., Roman-Duval, J., Fritz, J., Braun, R., Baes, M., Bendo, G. J., Blommaert, J. A. D. L., Boquien, M., Boselli, A., Clements, D. L., Cooray, A. R., Cortese, L., de Looze, I., Ford, G. P., Gear, W. K., Gentile, G., Gordon, K. D., Kirk, J., Lebouteiller, V., Madden, S., Mentuch, E., O’Halloran, B., Page, M. J., Schulz, B., Spinoglio, L., Verstappen, J., Wilson, C. D., & Thilker, D. A.
Affiliations
  • Cardiff University (GB)
  • Space Telescope Science Institute (US)
  • Ghent University (BE)
  • Commonwealth Scientific and Industrial Research Organisation (AU)
  • University of Manchester (GB)
  • KU Leuven (BE)
  • Centre National de la Recherche Scientifique (FR)
  • Imperial College London (GB)
  • University of California, Irvine (US)
  • European Southern Observatory (DE)
  • Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR)
  • The University of Texas at Austin (US)
  • University College London (GB)
  • California Institute of Technology (US)
  • National Institute for Astrophysics (IT)
  • McMaster University (CA)
  • Johns Hopkins University (US)
Corresponding author
  • Smith, M. W. L.
  • Gear, W. K.
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2012-08-13
Volume
756
Issue
1
Pages
40
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/756/1/40
OpenAlex
W2021546478
Cited by
179
References
0
Citations by year
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FWCI
12.61
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • CaltechAUTHORS (California Institute of Technology) (submittedVersion)
  • UWA Profiles and Research Repository (UWA) (submittedVersion)
  • HAL (submittedVersion)
  • Ghent University Academic Bibliography (Ghent University) (submittedVersion)
  • UCL Discovery (University College London) (submittedVersion)
  • Research Explorer (The University of Manchester) (submittedVersion)
  • Texas ScholarWorks (Texas Digital Library) (submittedVersion, other-oa)
  • arXiv (Cornell University)
  • Texas Digital Library (University of Texas)
Funders
  • National Aeronautics and Space Administration
  • California Institute of Technology
  • University of Lethbridge
  • UK Space Agency
  • Imperial College London
  • European Commission (229517)
  • University of Sussex
  • Cardiff University
  • Centre National d’Etudes Spatiales
  • Fonds Wetenschappelijk Onderzoek
  • Università degli Studi di Padova (2007-2013)
  • KU Leuven
  • Centre National de la Recherche Scientifique
  • Bundesministerium für Verkehr, Innovation und Technologie
  • Vlaamse regering
  • Max-Planck-Institut für Astronomie
  • Science and Technology Facilities Council (ST/J001449/1, FP7/2007-2013, ST/J001562/1, ST/I005765/1, ST/G004633/1, ST/H001530/1, ST/H00260X/1)
  • National Astronomical Observatories, Chinese Academy of Sciences
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Keywords
M31, interstellar dust, interstellar gas, modified blackbody, dust emissivity index, dust-to-gas ratio, dust temperature, star-forming ring, Galactic bulge, dark gas, metallicity gradients

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