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Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample

Draine, B. T. and Dale, D. A. and Bendo, G. and Gordon, K. D. and Smith, J. D. T. and Armus, L. and Engelbracht, C. W. and Helou, G. and Kennicutt, R. C., Jr. and Li, A. and Roussel, H. and Walter, F. and Calzetti, D. and Moustakas, J. and Murphy, E. J. and Rieke, G. H. and Bot, C. and Hollenbach, D. J. and Sheth, K. and Teplitz, H. I. (2007) Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample. Astrophysical Journal, 663 (2). pp. 866-894. ISSN 0004-637X. doi:10.1086/518306. https://resolver.caltech.edu/CaltechAUTHORS:20100218-131653499

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Abstract

Physical dust models are presented for 65 galaxies in SINGS that are strongly detected in the four IRAC bands and three MIPS bands. For each galaxy we estimate (1) the total dust mass, (2) the fraction of the dust mass contributed by PAHs, and (3) the intensity of the starlight heating the dust grains. We find that spiral galaxies have dust properties resembling the dust in the local region of the Milky Way, with similar dust-to-gas ratio and similar PAH abundance. The observed SEDs, including galaxies with SCUBA photometry, can be reproduced by dust models that do not require "cold" (T ≾ 10 K) dust. The dust-to-gas ratio is observed to be dependent on metallicity. In the interstellar media of galaxies with A_O ≡ 12 + log_(10)(O/H) > 8.1, grains contain a substantial fraction of interstellar Mg, Si, and Fe. Galaxies with A_O < 8.1 and extended H I envelopes in some cases appear to have global dust-to-gas ratios that are low for their measured oxygen abundance, but the dust-to-gas ratio in the regions where infrared emission is detected generally appears to be consistent with a substantial fraction of interstellar Mg, Si, and Fe being contained in dust. The PAH index q_(PAH), the fraction of the dust mass in the form of PAHs, correlates with metallicity. The nine galaxies in our sample with A_O < 8.1 have a median q_(PAH) = 1.0%, whereas galaxies with A_O > 8.1 have a median q_(PAH) = 3.55%. The derived dust masses favor a value X_(CO) ≈ 4 × 10^(20) cm^(-2) (K km s^(-1))^(-1) for the CO-to-H_2 conversion factor. Except for some starbursting systems (Mrk 33, Tol 89, NGC 3049), dust in the diffuse ISM dominates the IR power.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/518306 DOIArticle
http://www.iop.org/EJ/abstract/0004-637X/663/2/866/PublisherArticle
ORCID:
AuthorORCID
Draine, B. T.0000-0002-0846-936X
Dale, D. A.0000-0002-5782-9093
Smith, J. D. T.0000-0003-1545-5078
Armus, L.0000-0003-3498-2973
Helou, G.0000-0003-3367-3415
Kennicutt, R. C., Jr.0000-0001-5448-1821
Walter, F.0000-0003-4793-7880
Calzetti, D.0000-0002-5189-8004
Murphy, E. J.0000-0001-7089-7325
Rieke, G. H.0000-0003-2303-6519
Sheth, K.0000-0002-5496-4118
Teplitz, H. I.0000-0002-7064-5424
Additional Information:© 2007 The American Astronomical Society. Received 2007 January 16; accepted 2007 March 5. We thank S. Madden and the anonymous referee for helpful comments. Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through the Jet Propulsion Laboratory under NASA contract 1407. B. T. D. was supported in part by NSF grant AST 04-06883. B. T. D. is grateful to R. H. Lupton for availability of the SM graphics program.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA1407
NSFAST 04-06883
Subject Keywords:dust; extinction; galaxies : abundances; galaxies : general; galaxies : ISM; infrared : galaxies; ISM : general
Issue or Number:2
DOI:10.1086/518306
Record Number:CaltechAUTHORS:20100218-131653499
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20100218-131653499
Official Citation:Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample B. T. Draine, D. A. Dale, G. Bendo, K. D. Gordon, J. D. T. Smith, L. Armus, C. W. Engelbracht, G. Helou, R. C. Kennicutt, Jr., A. Li, H. Roussel, F. Walter, D. Calzetti, J. Moustakas, E. J. Murphy, G. H. Rieke, C. Bot, D. J. Hollenbach, K. Sheth, and H. I. Teplitz 2007 ApJ 663 866-894 doi: 10.1086/518306
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17523
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:19 Feb 2010 17:43
Last Modified:08 Nov 2021 23:36

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