Volume 378, Number 2, November I 2001
|Page(s)||370 - 393|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 November 2001|
HI observations of loose galaxy groups
I. Data and global properties
DAEC, UMR CNRS 8631, Observatoire de Paris, Section de Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France e-mail: firstname.lastname@example.org; email@example.com
2 Unité Scientifique Nançay, USR CNRS B704, Observatoire de Paris, 18330 Nançay, France
3 Department of Physics and Astronomy, Texas Christian University, Box 298840, Fort Worth, TX 76129, USA e-mail: firstname.lastname@example.org
4 Astronomy Department, University of Madison-Wisconsin, 475 N. Charter St., Madison WI 53706-1582, USA e-mail: email@example.com; firstname.lastname@example.org
5 Faculté des Sciences et des Techniques, Université de Tours, Avenue Monge, 37000 Tours, France
Corresponding author: W. van Driel, email@example.com
Accepted: 4 September 2001
At Nançay, 21-cm H i line observations were made of 15 spiral-dominated loose groups of galaxies, divided into two samples: an "interacting" sample containing at least one pair of interacting galaxies, and a "control" sample having no optical evidence of interactions or morphological disturbances among the group members. The interacting sample consists of 62 galaxies representing 9 different groups, and the control sample contains 40 galaxies representing 6 groups. Of the 91 galaxy and galaxy pairs observed, 74 were detected, while upper limits were placed on the remaining 17 objects. These homogeneous H i data, which will be used in future analyses, provide comparative information on the H i content of groups and serve as a probe of the vicinity of the target spirals for H i clouds or very low surface brightness gas-rich galaxies.
Key words: galaxies: distances and redshifts / galaxies: general / galaxies: interactions / galaxies: ISM / radio lines: galaxies
© ESO, 2001
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