Issue |
A&A
Volume 378, Number 2, November I 2001
|
|
---|---|---|
Page(s) | 370 - 393 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20011241 | |
Published online | 15 November 2001 |
HI observations of loose galaxy groups
I. Data and global properties
1
DAEC, UMR CNRS 8631, Observatoire de Paris, Section de Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France e-mail: wim.vandriel@obspm.fr; delphine.ragaigne@obspm.fr
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: p.marcum@tcu.edu
4
Astronomy Department, University of Madison-Wisconsin, 475 N. Charter St., Madison WI 53706-1582, USA e-mail: jsg@astro.wisc.edu; ewilcots@astro.wisc.edu
5
Faculté des Sciences et des Techniques, Université de Tours, Avenue Monge, 37000 Tours, France
Corresponding author: W. van Driel, wim.vandriel@obspm.fr
Received:
24
July
2001
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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