Computer Science
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205..224t&link_type=abstract
Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at
Computer Science
Scientific paper
Subarcsecond radio and infrared observations have recently revealed a class of luminous, obscured, and often optically thick HII regions associated with extremely large young clusters in nearby galaxies. VLA images of radio continuum emission in starburst and Wolf-Rayet galaxies show nebulae that are bright and dense, with ne ~ 103- 104 cm-3. The densities are characteristic of compact HII regions, but these nebulae are orders of magnitude larger than Galactic compact HII regions. The ionizing fluxes as well as the sizes and densities of the nebulae require the excitation equivalent of several thousand O stars within regions of 1-50 pc extent. From the O star population we estimate that the clusters are likely to have at least 100,000 stars, and as many as 106 stars. These very large clusters, possible protoglobular clusters, are likely to represent the conditions under which globular clusters form. The radio results have been confirmed with mid-infrared imaging at subarcsecond resolution, using the Long Wavelength Spectrometer on the Keck Telescope. The nebulae are also bright in the mid-infrared, and can often account for a significant fraction of the total IR luminosity of the parent galaxy. The prototype for these ``supernebulae" is the large, obscured cluster in the dwarf galaxy NGC 5253.
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