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EDP Sciences, Astronomy & Astrophysics, (541), p. L5, 2012

DOI: 10.1051/0004-6361/201118615

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Herschel/SPIRE observations of the dusty disk of NGC 4244

Journal article published in 2012 by Bw W. Holwerda, S. Bianchi ORCID, T. Böker, D. Radburn-Smith, Rs S. de Jong, Maarten Baes ORCID, Pc C. van der Kruit, M. Xilouris, Karl D. Gordon ORCID, Jj J. Dalcanton
This paper is made freely available by the publisher.
This paper is made freely available by the publisher.

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Abstract

We present Herschel/SPIRE images at 250, 350, and 500 mu m of NGC 4244, a typical low-mass, disk-only and edge-on spiral galaxy. The dust disk is clumpy and shows signs of truncation at the break radius of the stellar disk. This disk coincides with the densest part of the Hi disk. We compare the spectral energy distribution (SED), including the new SPIRE fluxes, to 3D radiative transfer models; a smooth model disk and a clumpy model with embedded heating. Each model requires a very high value for the dust scale-length (h(d) = 2-5 h(*)), higher dust masses than previous models of NGC 4244 (M-d = 0.47-1.39 x 10(7) M-circle dot) and a face-on optical depth of tau(f.o.)(V) = 0.4-1.12, in agreement with previous disk opacity studies. The vertical scales of stars and dust are similar. The clumpy model much better mimics the general morphology in the sub-mm images and the general SED. The inferred gas-to-dust mass ratio is compatible with those of similar low-mass disks. The relatively large radial scale-length of the dust disk points to radial mixing of the dusty ISM within the stellar disk. The large vertical dust scale and the clumpy dust distribution of our SED model are both consistent with a scenario in which the vertical structure of the ISM is dictated by the balance of turbulence and self-gravity.