On the origin of the radio emission in IRAS galaxies with high and ultrahigh luminosity - The starburst-AGN controversy

Details On the origin of the radio emission in IRAS galaxies with high and ultrahigh luminosity - The starburst-AGN controversy On the origin of the radio emission in IRAS galaxies with high and ultrahigh luminosity - The starburst-AGN controversy

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.259..709c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 259, no. 4, p. 709-724.

Astronomy and Astrophysics

Astronomy

44

Active Galactic Nuclei, Galactic Radiation, Infrared Astronomy Satellite, Radio Emission, Starburst Galaxies, Infrared Astronomy, Luminosity, Seyfert Galaxies

Scientific paper

The radio emission detected in high-luminosity and ultraluminous IRAS galaxies is explained here in terms of violent circumnuclear starbursts. The radio luminosities of the compact radio sources detected in the nearby circumnuclear starburst galaxies NGC 253 and M82 are consistent with their being a mixture of young radio SNe and old SNR. They must be intrinsically much brighter than the galactic SNR, i.e., radio hypernovae with peak luminosities 100 to 1000 times the luminosity of Cas A. In the starburst scenario, the radio luminosities of high-luminosity and ultraluminous IRAS galaxies (HLIRG and ULIRG) are dominated by the nonthermal radio emission associated with SNe and SNR. These SNe must be radio hypernovae for which SN1979c is a prototype. The observed FIR luminosities, q parameters, and Br-alpha luminosities in HLIRG and ULIRG are best explained by a Salpeter IMF with upper mass limit of 60 solar masses.

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