Ultraviolet Imaging Telescope Observations of H{\small{II}} Regions in M74

Details Ultraviolet Imaging Telescope Observations of H{\small{II}} Regions in M74 Ultraviolet Imaging Telescope Observations of H{\small{II}} Regions in M74

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.4302o&link_type=abstract

American Astronomical Society, 183rd AAS Meeting, #43.02; Bulletin of the American Astronomical Society, Vol. 25, p.1356

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Scientific paper

M74 (NGC 628) is an ScI galaxy which is viewed nearly face-on with many well-defined \hii regions. We report individual UV fluxes of over 160 \hii regions in M74, as imaged by the Ultraviolet Imaging Telescope during the Astro-1 mission in December, 1990. We compare the \hii region fluxes in the near-UV (2490 Angstroms) and far-UV (1520 Angstroms) with each other and with the fluxes measured in the B, R and Hα bands. Preliminary results indicate that emission from \hii regions directly contributes 30% of all UV flux. We also compare the locations and the morphologies of individual \hii emission features in the near-UV and Hα . The average displacement between an \hii region's near-UV emission peak and its Hα emission peak is approximately 3 arcseconds and is measurably greater than the uncertainty which may be attributed to known sources of error. Because the UV image sources are generally reflection nebulae while the Hα sources are ionized gas, this comparison gives valuable information about the relative locations of these two ISM components.

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