On the origin of the 40-120 micron emission of galaxy disks: A comparison with H-alpha fluxes

Details On the origin of the 40-120 micron emission of galaxy disks: A comparison with H-alpha fluxes On the origin of the 40-120 micron emission of galaxy disks: A comparison with H-alpha fluxes

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987nascp2466..153p&link_type=abstract

Star formation in galaxies, Proceedings of a conference at the California Institute of Technology, Pasadena, California, June 16

Astronomy and Astrophysics

Astronomy

2

Astronomical Models, B Stars, Dust, Interstellar Radiation, O Stars, Spiral Galaxies, Star Formation, Emission Spectra, Far Infrared Radiation, H Alpha Line, H Ii Regions, Infrared Astronomy Satellite, Predictions, Star Formation Rate

Scientific paper

A comparison of 40 to 120 micron Infrared Astronomy Satellite (IRAS) fluxes with published H alpha and UBV photometry shows that the far infrared emission of galaxy disks consists of at least two components: a warm one associated with OB stars in HII-regions and young star-forming complexes, and a cooler one from dust in the diffuse, neutral interstellar medium, heated by the more general interstellar radiation field of the old disk population (a cirrus-like component). Most spiral galaxies are dominated by emission from the cooler component in this model. A significant fraction of the power for the cool component must originate with non-ionizing stars. For a normal spiral disk there is a substantial uncertainty in a star formation rate derived using either the H alpha or the far infrared luminosity.

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