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Tracing interactions in HCGs through the H I1

Published online by Cambridge University Press:  12 April 2016

L. Verdes-Montenegro ,
M. S. Yun ,
B. A. Williams ,
W. K. Huchtmeier ,
A. Del Olmo  and
J. Perea
L. Verdes-Montenegro
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Apdo. Correos 3004, E-18080 Granada, Spain; lourdes@iaa.es
M. S. Yun
Affiliation:
National Radio Astronomy Observatory, 2P. O. Box 0, Socorro, NM 87801, USA; myun@aoc.nrao.edu
B. A. Williams
Affiliation:
University of Delaware, Newark, Delaware, USAbaw@udel.edu
W. K. Huchtmeier
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germanyhuchtmeier@mpifr-bonn.mpg.de
A. Del Olmo
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Apdo. Correos 3004, E-18080 Granada, Spain; chony@iaa.es, jaime@iaa.es
J. Perea
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Apdo. Correos 3004, E-18080 Granada, Spain; chony@iaa.es, jaime@iaa.es

Abstract

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We present a global study of Hɪ spectral line mapping for 16 Hickson Compact Groups (HCGs) combining new and unpublished VLA data, plus the analysis of the Hɪ content of individual galaxies. Sixty percent of the groups show morphological and kinematical signs of perturbations (from multiple tidal features to concentration of the Hɪ in a single enveloping cloud) and sixty five of the resolved galaxies are found to be Hɪ deficient with respect to a sample of isolated galaxies. In total, 77% of the groups suffer interactions among all its members which provides strong evidence of their reality. We find that dynamical evolution does not always produce Hɪ deficiency, but when this deficiency is observed, it appears to correlate with a high group velocity dispersion and in some cases with the presence of a first-ranked elliptical. The X-ray data available for our sample are not sensitive enough for a comparison with the Hɪ mass; however this study does suggest a correlation between Hɪ deficiency and hot gas since velocity dispersions are known from the literature to correlate with X-ray luminosity.

Type
Part 2. Properties of Small Groups
Information
International Astronomical Union Colloquium , Volume 174: Small Galaxy Groups , 2000 , pp. 167 - 173
Copyright
Copyright © Astronomical Society of the Pacific 2000

Footnotes

2

The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

1

Based on observations made with the VLA operated by the National Radio Astronomy Observatory and on data taken using ALFOSC, which is owned by the Instituto de Astrofísica de Andalucía (IAA) and operated at the Nordic Optical Telescope under agreement between IAA and the NBIfA of the Astronomical Observatory of Copenhagen.

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