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Optical Counterparts to Galaxies in the Cen A Group Discovered by HIPASS

Published online by Cambridge University Press:  05 March 2013

Patricia M. Knezek
Patricia M. Knezek*
Affiliation:
Department of Physics and Astronomy, The Johns Hopkins University, Bloomberg Center, Baltimore, MD 21218–2695, USA; [email protected] Visiting Astronomer, Cerro Tololo Inter-American Observatory, operated by AURA, Inc. under contract to the National Science Foundation
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Abstract

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We have completed a 21-cm survey of a 600 square degree region of the Centaurus A group of galaxies at a redshift of ∼500 km s−1 as part of a larger survey of the entire southern sky. This group of galaxies was recently the subject of a separate and thorough optical survey (Côté et al. 1997), and thus presented an ideal comparison for us to test the survey performance. We have identified 10 new group members to add to the 21 already known in our survey area. Six of the new members are previously uncatalogued galaxies, while four were catalogued but assumed not to be group members. Including the seven known members outside of our survey area, this brings the total known number of Cen A members to 38. All of the new HI detections have optical counterparts, most being intrinsically very faint (MB > –13·0), late-type low surface brightness dwarfs. Most of the new members have HI masses only a few times our survey limit of 107M☉ at an assumed distance for the group of 3·5 Mpc, and are extremely gas-rich, with a median MHI/LB > 1. Our limiting HI sensitivity was actually slightly worse than the HI follow-up observations of the Côté et al. optical survey, yet we have already increased the known number of group members by 50% using an HIsurvey technique. While we have increased the known number of members by ∼50%, these new members contribute <4% to its light.

Keywords

galaxies: generalgalaxies: luminosity function, mass functiongalaxies: statistics
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 16 , Issue 1 , 1999 , pp. 60 - 65
Copyright
Copyright © Astronomical Society of Australia 1999

References

Banks, G., et al. 1999, ApJ, submittedGoogle Scholar
Barnes, D. G., Staveley-Smith, L., Ye, T., & Oosterloo, T. 1998, in Astronomical Data Analysis Software and Systems VII, ed. Albrecht, R. et al. (San Francisco: ASP), 145, 89 Google Scholar
Côté, S., Freeman, K. C., Carnigan, C., & Quinn, P. 1997, AJ, 114, 1313 Google Scholar
de Vaucouleurs, G. 1979, AJ, 84, 1270 Google Scholar
de Vaucouleurs, G., et al. 1991, Third Reference Catalogue of Bright Galaxies (New York: Springer)Google Scholar
Graham, J. A. 1979, ApJ, 232, 60 Google Scholar
Hui, X., et al. 1993, ApJ, 414, 463 Google Scholar
Landolt, A. U. 1992, AJ, 104, 340 Google Scholar
Lang, K. R. 1980, Astrophysical Formulae (Berlin: Springer)Google Scholar
Mateo, M. L. 1998, ARAA, 36, 435 CrossRefGoogle Scholar
Matthews, L., & Gallagher, J. 1996, AJ, 111, 1098 CrossRefGoogle Scholar
Matthews, L., & Gallagher, J. 1997, AJ, 114, 1899 Google Scholar
Richter, O.-G., Sackett, P. D., & Sparke, L. S. 1994, AJ, 107, 99 Google Scholar
Sandage, A., et al. 1994, ApJ, 425, 14 Google Scholar
Schechter, P. 1976, ApJ, 203, 297 Google Scholar
Staveley-Smith, L., et al. 1996, PASA, 13, 243 Google Scholar
van den Bergh, S. 1992, A&A, 264, 75 Google Scholar
van Gorkom, J. H., van der Hulst, J. M., Haschick, A. D., & Tubbs, A. D. 1990, AJ, 99, 1781 Google Scholar
Wakker, B. 1991, A&AS, 90, 495 Google Scholar
Yahil, A., Tammann, G., & Sandage, A. 1977, ApJ, 217, 903 Google Scholar