Modelling the spectral energy distribution of galaxies. I. Radiation fields and grain heating in the edge-on spiral NGC891

Details Modelling the spectral energy distribution of galaxies. I. Radiation fields and grain heating in the edge-on spiral NGC891 Modelling the spectral energy distribution of galaxies. I. Radiation fields and grain heating in the edge-on spiral NGC891

2000-08-06

arxiv.org/abs/astro-ph/0008098v1

Astronomy and Astrophysics

Astrophysics

15 pages, accepted for publication in Astronomy and Astrophysics

Scientific paper

We describe a new tool for the analysis of the UV to the sub-millimeter (sub-mm) spectral energy distribution (SED) of spiral galaxies. We use a consistent treatment of grain heating and emission, solve the radiation transfer problem for a finite disk and bulge, and self-consistently calculate the stochastic heating of grains placed in the resulting radiation field. We use this tool to analyse the well-studied nearby edge-on spiral galaxy NGC891. First we investigate whether the old stellar population in NGC891, along with a reasonable assumption about the young stellar population, can account for the heating of the dust and the observed far-infrared (FIR) and sub-mm emission. The dust distribution is taken from the model of Xilouris et al. (1999), who used only optical and near-IR observations to determine it. We have found that such a simple model cannot reproduce the SED of NGC891, especially in the sub-mm range. It underestimates by a factor of 2-4 the observed sub-mm flux. A number of possible explanations exist for the missing sub-mm flux. We investigate a few of them and demonstrate that one can reproduce the observed SED in the FIR and the sub-mm quite well, as well as the observed radial profile at 850 microns. For the models calculated we give the relative proportion of the dust radiation powered by the old and young stellar populations as a function of FIR/sub-mm wavelength. In all models we find that the dust is predominantly heated by the young stellar population.

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