The far-infrared continuum spectrum of the Milky Way explained by a dust and gas model

Details The far-infrared continuum spectrum of the Milky Way explained by a dust and gas model The far-infrared continuum spectrum of the Milky Way explained by a dust and gas model

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996el.....34...69s&link_type=abstract

Europhysics Letters, Volume 34, Issue 1, pp. 69-74 (1996).

Physics

4

Scientific paper

The far-infrared continuum spectra observed in the FIRAS-COBE mission are explained by a one-component dust source in the Galaxy and a cold excess due to radiation of molecular hydrogen gas in the outer Galaxy. The dust model is based on an empirically tested temperature-dependent mass absorption coefficient and a reasonable dust density distribution close to the galactic plane. The temperature of the dust along the line of sight is determined by a fit curve. The gas source is conceivable as a small part of cold molecular hydrogen and helium gas in the outer Galaxy which is only observable in a small temperature interval at 11 K and at corresponding (equilibrium ) condensation densities of about 4.5·1018 cm-3. It is assumed that the high densities occur in very small and short-living inhomogeneities of the fractal-structured gas due to self-gravitation, turbulence and starting condensation in the elementary fragments, i.e. the gas is at a stage close to star formation. Preliminary tests show that the gas sources are very likely correlated with the well-known HI sources in the outer Galaxy. The gas sources contribute to the spectra still at latitudes up to |b| < 25 30 degrees, while the instrument noise is larger at higher latitudes.

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