再访后发座I星云中星系的HI性质
The HI properties of galaxies in the Coma I cloud revisited
摘要：
在小星系团内的预处理被提出来解释居住在富星系团中的星系的一些性质。目前工作的目的是看看预处理是否在附近的宇宙中起作用，在那里合并形成丰富的星系团的结构是相当大的。我们研究了属于后发座I云，一个协会的对象接近的室女星系团的大样本的晚型星系的HI气体性质。与先前所声称的相反，后发座I星云中的晚型星系并不缺乏HI气体（HI-def=0.06+-0.44）。如果后发座I星云代表了附近星系团中的落星系群，那么这一结果表明，在局部宇宙中，属于松散结构的晚型星系的演化与高速色散（>= 300 km/s）相关，与室女座等丰富的星系团有关，并没有受到预处理的显著扰动。
英文摘要：
Pre-processing within small groups has been proposed to explain several of the properties of galaxies inhabiting rich clusters. The aim of the present work is to see whether pre-processing is acting in the nearby universe, where the structures that are merging to form rich clusters are rather large and massive. We study the HI gas properties of a large sample of late-type galaxies belonging to the Coma I cloud, an association of objects close to the Virgo cluster. Contrary to what previously claimed, late-type galaxies in the Coma I cloud are not deficient in HI gas (HI-def=0.06+-0.44). If the Coma I cloud is representative of infalling groups in nearby clusters, this result suggests that, in the local universe, the evolution of late-type galaxies belonging to loose structures with high velocity dispersions (>= 300 km/s)associated to rich clusters such as Virgo is not significantly perturbed by pre-processing.
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