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Untangling the Nature of Spatial Variations of Cold Dust Properties in Star Forming Galaxies

Untangling the Nature of Spatial Variations of Cold Dust Properties in Star Forming Galaxies

Kirkpatrick, Allison, Calzetti, Daniela, Kennicutt, Robert, Galametz, Maud, Gordon, Karl, Groves, Brent, Hunt, Leslie, Dale, Daniel, Hinz, Joannah, & Tabatabaei, Fatemeh
2014, The Astrophysical Journal, 789, 130

We investigate the far-infrared (IR) dust emission for 20 local star forming galaxies from the Key Insights on Nearby Galaxies: A Far-IR Survey with Herschel (KINGFISH) sample. We model the far-IR/submillimeter spectral energy distribution (SED) using images from Spitzer Space Telescope and Herschel Space Observatory. We calculate the cold dust temperature (Tc ) and emissivity (ЮВ) on a pixel by pixel basis (where each pixel ranges from 0.1 to 3 kpc2) using a two-temperature modified blackbody fitting routine. Our fitting method allows us to investigate the resolved nature of temperature and emissivity variations by modeling from the galaxy centers to the outskirts (physical scales of ~15-50 kpc, depending on the size of the galaxy). We fit each SED in two ways: (1) fit Tc and ЮВ simultaneously, (2) hold ЮВ constant and fit Tc . We compare Tc and ЮВ with star formation rates (calculated from L HЮБ and L 24 ЮМm), the luminosity of the old stellar population (traced through L 3.6 ЮМm), and the dust mass surface density (traced by 500 ЮМm luminosity, L 500). We find a significant trend between SFR/L 500 and Tc , implying that the flux of hard UV photons relative to the amount of dust is significantly contributing to the heating of the cold, or diffuse, dust component. We also see a trend between L 3.6/L 500 and ЮВ, indicating that the old stellar population contributes to the heating at far-IR/submillimeter wavelengths. Finally, we find that when ЮВ is held constant, Tc exhibits a strongly decreasing radial trend, illustrating that the shape of the far-IR SED is changing radially through a galaxy, thus confirming on a sample almost double in size the trends observed in Galametz et al.

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