Images in the rocket ultraviolet - Star formation and extinction in the M51 system

Details Images in the rocket ultraviolet - Star formation and extinction in the M51 system Images in the rocket ultraviolet - Star formation and extinction in the M51 system

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...352...55b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 352, March 20, 1990, p. 55-67.

Astronomy and Astrophysics

Astronomy

17

Interstellar Extinction, Spiral Galaxies, Star Formation, Ultraviolet Astronomy, Brightness Distribution, Galactic Nuclei, H Ii Regions, Images, Rocket-Borne Instruments

Scientific paper

UV images of M51 with up to 15 arcsec resolution were obtained by a rocket-borne telescope. The bandwidth was 970 A with maximum response at 2650 A. The two most prominent features of M51 in the UV are the bright central region and a region of intense star formation about 2.5 NE of the nucleus toward the companion NGC 5195. This complex is the source of 20 percent of the total UV flux in M51. The companion is much less prominent in the UV than in optical bands. Spiral arms show much higher contrast in UV and U bands than in the R band. The nuclear region in the UV band shows clumped emission from probable star-forming regions, possibly associated with the inner Lindblad resonance. These regions are probably the UV counterparts of FIR sources discovered in an EW scan across the nucleus. UV/U colors of most bright H II regions with known extinction are consistent with O star spectra reddened by amounts estimated from radio and Balmer line measurements. However, some of the brightest H II regions have redder UV/U colors, probably indicating the presence of cooler stars which contribute in the U band. CO and IR observations indicate that the companion NGC 5195 may be a reddened starburst in spite of its faintness in the UV.

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