The H I disk of UGC 7175

Details The H I disk of UGC 7175 The H I disk of UGC 7175

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aj....104..563l&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 104, no. 2, Aug. 1992, p. 563-568.

Astronomy and Astrophysics

Astronomy

3

Galactic Rotation, Galactic Structure, Irregular Galaxies, Seyfert Galaxies, Astronomical Models, Brightness Distribution, Emission Spectra, H Lines, Red Shift, Very Large Array (Vla)

Scientific paper

UGC 7175 is an S-Irr galaxy near NGC 4151 and NGC 4145 in redshift (1000-1150 km/s) and position. Arp (1977) found an optical bridge between UGC 7175 and a smaller, adjacent (30 arcsec) system at z = 0.098, and ascribed the horned or antennalike morphology of UGC 7175 to a physical interaction between the latter two systems. The H I in UGC 7175 was serendipitously synthesized and is shown here to be simply described by a highly inclined, flat, rotating disk oriented along the optical image of UGC 7175. There are no clear effects which might be ascribed to interaction between the two systems of discordant redshift in this experiment. The H I synthesis could, however, be repeated more purposefully with very much higher sensitivity.

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