IRAS and ground-based observations of star formation regions in the Magellanic clouds

Details IRAS and ground-based observations of star formation regions in the Magellanic clouds IRAS and ground-based observations of star formation regions in the Magellanic clouds

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987nascp2466..241e&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

Energy Distribution, Interstellar Matter, Luminosity, Magellanic Clouds, Star Formation, Far Infrared Radiation, Flux Density, H Ii Regions, Infrared Astronomy Satellite, Space Surveillance (Ground Based)

Scientific paper

The Infrared Astronomy Satellite (IRAS) detected several hundred individual regions of star formation in the Large and Small Magellanic Clouds. Nearly two dozen of the brightest such sources were searched for from the ground at 10 microns; most of these were located and measured at wavelengths from 0.6 to 20 microns. Three principle results emerge from this study: First, the IRAS data show that star formation is considerably less active in the SMC than in the LMC, relative either to mass, luminosity, or H I content. The reduced activity in the SMC is consistent with the smaller amount of molecular material inferred from CO observations. Second, the sizes of the objects range from less than a few arcsecs (objects which look like extremely compact HII regions, with little or no extended radio, optical, or infrared emission) to some tens of arcsecs across (giant HII regions, of which the largest and brightest is 30 Doradus). Third, there are no obvious differences in the characteristics of the central portions of the LMC and SMC sources; all look like Galactic H II regions of similar luminosity.

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