Spectral Energy Distributions of Dusty Galaxies

Details Spectral Energy Distributions of Dusty Galaxies Spectral Energy Distributions of Dusty Galaxies

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000isass..14..155t&link_type=abstract

The Institute of Space and Astronautical Science Report SP No. 14, p.155-162.

Astronomy and Astrophysics

Astronomy

Galaxies, Clusters, Intracluster Medium, Dust, Infrared

Scientific paper

We present a model of spectral energy distributions (SEDs). This model employs two processes of dust heating: heating by radiation and heating by hot gas. The radiation fields and the resulting SEDs are calculated by a software code that treats the radiative transfer by assuming spherical symmetry. Using a dust model with a mixture of graphite, silicate and PAHs, we reproduce the standard extinction curve and the spectrum of the cirrus emission in the Galaxy. The temperature fluctuation of dust particles is taken into account wherever the enthalpy of a dust particle that corresponds to the equilibrium temperature in a given radiation field is less than the energy of one UV photon. We derived the SEDs of a starburst galaxy (M82), an elliptical galaxy (NGC2768) and a cluster of galaxies (the Coma cluster). The derived age of M82 is 500 Myr when the V-band optical depth, tauV, is 3.5. In the optically thin case, such as NGC2768, the spatial distribution of dust in the galaxy is derived from the SED fitting, by fixing the size of galaxy. We conclude that the spatial distribution of dust is the same as that of stars in NGC2768. The 120 micron emission from the Coma cluster detected by ISO is reproduced by the model with tauV = 0.002. It is found that dust particles in the intracluster space is mainly heated by the hot X-ray emitting gas, although the heating by the intracluster radiation field is important for the spectrum at the submillimeter and longer wavelengths.

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