An HI survey of six Local Group analogs: I. Survey description and the search for high-velocity clouds

Details An HI survey of six Local Group analogs: I. Survey description and the search for high-velocity clouds An HI survey of six Local Group analogs: I. Survey description and the search for high-velocity clouds

2007-03-12

arxiv.org/abs/astro-ph/0703279v1

Astrophys.J.662:959-968,2007

Astronomy and Astrophysics

Astrophysics

10 pages, ApJ accepted

Scientific paper

10.1086/517986

We have conducted an HI 21 cm emission-line survey using the Parkes 20cm multibeam instrument and the Australia Telescope Compact Array (ATCA) of six loose groups of galaxies chosen to be analogs to the Local Group. The goal of this survey is to make a census of the HI-rich galaxies and high-velocity clouds (HVCs) within these groups and compare these populations with those in the Local Group. The Parkes observations covered the entire volume of each group with a rms M(HI) sensitivity of 4-10x10^5 M(sun) per 3.3 km/s channel. All potential sources detected in the Parkes data were confirmed with ATCA observations at ~2' resolution and the same M(sun) sensitivity. All the confirmed sources have associated stellar counterparts; no starless HI clouds--HVC analogs--were found in the six groups. In this paper, we present a description of the survey parameters, its sensitivity and completeness. Using the population of compact HVCs (CHVCs) around the Milky Way as a template coupled with the detailed knowledge of our survey parameters, we infer that our non-detection of CHVC analogs implies that, if similar populations exist in the six groups studied, the CHVCs must be clustered within 90 kpc of group galaxies, with average M(HI) < 4x10^5 M(sun) at the 95% confidence level. The corollary is that the same must apply to Milky Way CHVCs. This is consistent with our previous results from a smaller sample of groups, and in accordance with recent observational and theoretical constraints from other authors. These results confirm that there is very little neutral matter around galaxies, and that any substantial reservoir of baryons must be in other phases.

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