Volume 479, Number 2, February IV 2008
|Page(s)||603 - 624|
|Section||Online catalogs and data|
|Published online||04 December 2007|
Canes Venatici I cloud of galaxies seen in the Hα line
Special Astrophysical Observatory, Russian Academy of Sciences, N. Arkhyz, KChR, 369167, Russia e-mail: firstname.lastname@example.org
Accepted: 25 September 2007
We present results of Hα imaging for 42 galaxies in the nearby low-density cloud Canes Venatici I, populated mainly by late-type objects. Estimates of the Hα flux and integrated star formation rate () are now available for all 78 known members of this scattered system, spanning a large range in luminosity, surface brightness, HI content and . Distributions of the CVnI galaxies versus their , blue absolute magnitude and total hydrogen mass, are given in comparison with those for a population of the nearby virialized group around M 81. We found no essential correlation between star formation activity in a galaxy and its density environment. The bulk of CVnI galaxies had enough time to generate their baryon mass with the observed . Most of them also possess a supply of gas that is sufficient to maintain their observed s during the next Hubble time.
Key words: galaxies: evolution / galaxies: ISM / galaxies: dwarf
© ESO, 2008
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