CASASOLA, V, CASSARÀ, LP, BIANCHI, S, VERSTOCKEN, S, XILOURIS, E, MAGRINI, L, SMITH, M, DE LOOZE, I, GALAMETZ, M, MADDEN, SC, BAES, M, CLARK, C, DAVIES, J, DE VIS, P, EVANS, R, FRITZ, J, GALLIANO, F, JONES, AP, MOSENKOV, AV, VIAENE, S and YSARD, N (2017). Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies. Astronomy & Astrophysics, 605, A18.
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Abstract
Aims. The purpose of this work is the characterization of the radial distribution of dust, stars, gas, and star-formation rate (SFR) in a sub-sample of 18 face-on spiral galaxies extracted from the DustPedia sample. Methods. This study is performed by exploiting the multi-wavelength DustPedia database, from ultraviolet (UV) to sub-millimeter bands, in addition to molecular (12CO) and atomic (Hi) gas maps and metallicity abundance information available in the literature. We fitted the surface-brightness profiles of the tracers of dust and stars, the mass surface-density profiles of dust, stars, molecular gas, and total gas, and the SFR surface-density profiles with an exponential curve and derived their scale-lengths. We also developed a method to solve for the CO-to-H2 conversion factor (αCO) per galaxy by using dust- and gas-mass profiles. Results. Although each galaxy has its own peculiar behavior, we identified a common trend of the exponential scale-lengths versus wavelength. On average, the scale-lengths normalized to the B-band 25 mag/arcsec2 radius decrease from UV to 70 μm, from 0.4 to 0.2, and then increase back up to ~0.3 at 500 microns. The main result is that, on average, the dust-mass surface-density scale-length is about 1.8 times the stellar one derived from IRAC data and the 3.6 μm surface brightness, and close to that in the UV. We found a mild dependence of the scale-lengths on the Hubble stage T: the scale-lengths of the Herschel bands and the 3.6 μm scale-length tend to increase from earlier to later types, the scale-length at 70 μm tends to be smaller than that at longer sub-mm wavelength with ratios between longer sub-mm wavelengths and 70 μm that decrease with increasing T. The scale-length ratio of SFR and stars shows a weak increasing trend towards later types. Our αCO determinations are in the range (0.3−9) M⊙ pc-2 (K km s-1)-1, almost invariant by using a fixed dust-to-gas ratio mass (DGR) or a DGR depending on metallicity gradient.
Item Type: | Article |
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Uncontrolled Keywords: | 0201 Astronomical And Space Sciences; Astronomy & Astrophysics |
Identification Number: | https://doi.org/10.1051/0004-6361/201731020 |
Page Range: | A18 |
SWORD Depositor: | Symplectic Elements |
Depositing User: | Symplectic Elements |
Date Deposited: | 05 Mar 2019 15:57 |
Last Modified: | 18 Mar 2021 06:31 |
URI: | https://shura.shu.ac.uk/id/eprint/23985 |
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