2001/03/20 by Martin Zwaan, M. A. Zwaan · 1 citation
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy group #Local Group #Milky Way #Physics #Satellite galaxy #Star formation #Telescope #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2001.04514.x
published as Mon.Not.Roy.Astron.Soc. 325 (2001) 1142 · 7 pages, 4 figures, accepted for publication in MNRAS
arxiv created 2001/03/20 · openalex publication_date 2001/08/11 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Five galaxy groups with properties similar to those of the Local Group have been surveyed for H i clouds with the Arecibo Telescope. In total 300 pointings have been observed on grids of approximately 2.5×1.5 Mpc2 centred on the groups. The 4.5σ detection limit on the minimal detectable H i masses is approximately 7×106 M⊙(H0=65 km s−1 Mpc−1). All detections could be attributed to optical galaxies; no significant detections of H i clouds have been made. This null result leads to the conclusion that the total H i mass of intragroup clouds must be less than 10 per cent of the total H i mass of galaxy groups and less than 0.05 per cent of the dynamical mass. The recent hypothesis that Galactic high-velocity clouds are Local Group satellite galaxies is highly inconsistent with these observations.