2005MNRAS.363L..21B

An extended Hi cloud (VIRGOHi21) with an Hi mass of ∼10⁸M_☉ and no apparent optical counterpart was recently discovered in the Virgo cluster. In order to understand the origin of physical properties of apparently isolated Hi clouds like VIRGOHi21, we numerically investigate physical properties of tidal Hi debris that were formed by galaxy-galaxy interactions in clusters of galaxies. Our hydrodynamical simulations demonstrate that tidal debris with total Hi masses of 10⁸-10⁹M_☉can have (1) a wide spread of Hi velocities (>200km/s), (2) a small mass fraction of stars (∼10 per cent), and (3) a mean B-band surface brightness of the stellar components fainter than 30 mag/arcsec2. These results suggest that VIRGOHi21, which lies at a projected distance of ∼150 kpc from the one-armed, Hi-rich spiral galaxy M99 (NGC 4254), is tidal debris. We propose that the comparison between the simulated and the observed velocity fields of Hi clouds allows us to better understand their nature and origin (e.g. whether they are just tidal debris or are `dark galaxies' that have Hi gas only and are embedded within dark matter haloes).