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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/862
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dc.contributor.authorOmar, A.-
dc.contributor.authorDwarakanath, K.S.-
dc.date.accessioned2005-12-26T08:52:28Z-
dc.date.available2005-12-26T08:52:28Z-
dc.date.issued2005-
dc.identifier.citationJournal of Astrophysics and Astronomy, 2005, Vol. 26, p.71-88.en
dc.identifier.issn0250-6335-
dc.identifier.urihttp://hdl.handle.net/2289/862-
dc.description.abstractThe HI content of galaxies in the Eridanus group is studied using the GMRT observations and the HIPASS data. A significant HI deficiency up to a factor of 2-3 is observed in galaxies in the high galaxy density regions. The HI deficiency in galaxies is observed to be directly correlated to the local projected galaxy density, and inversely correlated to the lineof-sight radial velocity. Furthermore, galaxies with larger optical diameters are predominantly in the lower galaxy density regions. It is suggested that the HI deficiency in Eridanus is due to tidal interactions. In some galaxies, evidences of tidal interactions are seen. An important implication is that significant evolution of galaxies can take place in the group environment. In the hierarchical way of formation of clusters via mergers of groups, a fraction of the observed HI deficiency in clusters could have originated in groups. The co-existence of S0s and severely HI deficient galaxies in the Eridanus group suggests that tidal interaction is likely to be an effective mechanism for transforming spirals to S0s.en
dc.format.extent1025399 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherIndian Academy of Sciences, Bangalore, India.en
dc.rightsIndian Academy of Sciences, Bangalore, India.en
dc.subjectGalaxy: evolution—galaxiesen
dc.subjectgroups,clusters—individualen
dc.subjectEridanus—radiolinesen
dc.subjectHI 21cm-lineen
dc.titleThe HI content of the Eridanus group of galaxiesen
dc.typeArticleen
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