| Abstract | H I 21-cm line observations of 24 Virgo cluster (VC) spirals are used to compare the H I contents of 56 spirals later than Sb in the VC area with those of another 110 galaxies of the same types, either isolated or members of small groups. The VC spirals are shown to be H I deficient, the deficiency being limited to the VC proper (12 degrees in extent), and amounting to a factor of 2.2 plus or minus 0.3 on the average. In addition, individual deficiencies of Virgo spirals have a dispersion lower than a factor of 2, and the H I content of VC galaxies is related to morphology (anemic spirals with smooth arms having less gas than others). Evidence suggests that the abnormally low H I contents have been provoked by the combined effects of galactic collisions and the interaction between the galaxies and the intracluster gas. |
