Cool dust heating and temperature mixing in nearby star-forming galaxies

被引：52
作者：
Hunt, L. K. [1 ]
Draine, B. T. [2 ]
Bianchi, S. [1 ]
Gordon, K. D. [3 ,4 ]
Aniano, G. [2 ,5 ]
Calzetti, D. [6 ]
Dale, D. A. [7 ]
Helou, G. [8 ]
Hinz, J. L. [9 ]
Kennicutt, R. C. [10 ]
Roussel, H. [11 ]
Wilson, C. D. [12 ]
Bolatto, A. [13 ]
Boquien, M. [10 ,14 ]
Croxall, K. V. [15 ]
Galametz, M. [16 ]
Gil de Paz, A. [17 ]
Koda, J. [18 ]
Munoz-Mateos, J. C. [19 ]
Sandstrom, K. M. [9 ,20 ]
Sauvage, M. [21 ]
Vigroux, L. [22 ]
Zibetti, S. [1 ]
机构：
[1] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy
[2] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA
[3] Space Telescope Sci Inst, Baltimore, MD 21218 USA
[4] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium
[5] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR 8617, F-91405 Orsay, France
[6] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA
[7] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA
[8] CALTECH, IPAC, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA
[9] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA
[10] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[11] Univ Paris 06, Inst Astrophys Paris, Univ Sorbonne, CNRS,UMR 7095, F-75014 Paris, France
[12] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada
[13] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
[14] Univ Maryland, Lab Millimeter Wave Astron, College Pk, MD 20742 USA
[15] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA
[16] European So Observ, D-85748 Garching, Germany
[17] Univ Complutense Madrid, Dept Astrofis, E-28040 Madrid, Spain
[18] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA
[19] European So Observ, Santiago 19, Chile
[20] Max Planck Inst Astron, D-69117 Heidelberg, Germany
[21] CEA, Lab AIM, Orme Merisiers, Irfu,SAp, F-91191 Gif Sur Yvette, France
[22] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France
来源：
ASTRONOMY & ASTROPHYSICS | 2015年 / 576卷
基金：
美国国家科学基金会;
关键词：
galaxies: ISM; dust; extinction; galaxies: star formation; HERSCHEL REFERENCE SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; SUBMILLIMETER EXCESS EMISSION; SMALL-MAGELLANIC-CLOUD; 60; MU-M; SPIRAL GALAXIES; DWARF GALAXIES; COLD DUST; INFRARED-EMISSION; INTERSTELLAR DUST;
D O I：
10.1051/0004-6361/201424734
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Physical conditions of the interstellar medium in galaxies are closely linked to the ambient radiation field and the heating of dust grains. In order to characterize dust properties in galaxies over a wide range of physical conditions, we present here the radial surface brightness profiles of the entire sample of 61 galaxies from Key Insights into Nearby Galaxies: Far-Infrared Survey with Herschel (KINGFISH). The main goal of our work is the characterization of the grain emissivities, dust temperatures, and interstellar radiation fields (ISRFs) responsible for heating the dust. We first fit the radial profiles with exponential functions in order to compare stellar and cool-dust disk scalelengths, as measured by 3.6 mu m and 250 mu m surface brightnesses. Our results show that the stellar and dust scalelengths are comparable, with a mean ratio of 1.04, although several galaxies show dust-to-stellar scalelength ratios of 1.5 or more. We then fit the far-infrared spectral energy distribution (SED) in each annular region with single-temperature modified blackbodies using both variable (MBBV) and fixed (MBBF) emissivity indices beta, as well as with physically motivated dust models. The KINGFISH profiles are well suited to examining trends of dust temperature T-dust and beta because they span a factor of similar to 200 in the ISRF intensity heating the bulk of the dust mass, U-min. Results from fitting the profile SEDs suggest that, on average, T-dust, dust optical depth tau(dust), and U-min decrease with radius. The emissivity index beta also decreases with radius in some galaxies, but in others is increasing, or rising in the inner regions and falling in the outer ones. Despite the fixed grain emissivity (average beta similar to 2.1) of the physically-motivated models, they are well able to accommodate flat spectral slopes with beta less than or similar to 1. An analysis of the wavelength variations of dust emissivities in both the data and the models shows that flatter slopes (beta less than or similar to 1.5) are associated with cooler temperatures, contrary to what would be expected from the usual T-dust-beta degeneracy. This trend is related to variations in U-min since beta and U-min are very closely linked over the entire range in U-min sampled by the KINGFISH galaxies: low U-min is associated with flat beta less than or similar to 1. Both these results strongly suggest that the low apparent beta values (flat slopes) in MBBV fits are caused by temperature mixing along the line of sight, rather than by intrinsic variations in grain properties. Finally, a comparison of dust models and the data show a slight similar to 10% excess at 500 mu m for low metallicity (12 + log (O/H) less than or similar to 8) and low far-infrared surface brightness (Sigma(500)).
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页数：23
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