How elevated is the dynamical-to-stellar mass ratio of the ultra-compact dwarf S999?
arXiv:1502.06598 · doi:10.1093/mnras/stv389
Abstract
Here we present new Keck ESI high-resolution spectroscopy and deep archival HST/ACS imaging for S999, an ultra-compact dwarf in the vicinity of M87, which was claimed to have an extremely high dynamical-to-stellar mass ratio. Our data increase the total integration times by a factor of 5 and 60 for spectroscopy and imaging, respectively. This allows us to constrain the stellar population parameters for the first time (simple stellar population equivalent age Gyr; ; ). Assuming a Kroupa stellar initial mass function, the stellar population parameters and luminosity ( mag) yield a stellar mass of , which we also find to be consistent with near-infrared data. Via mass modelling, with our new measurements of velocity dispersion ( km s) and size ( pc), we obtain an elevated dynamical-to-stellar mass ratio (with a range ). Furthermore, we analyse the surface brightness profile of S999, finding only a small excess of light in the outer parts with respect to the fitted Sérsic profile, and a positive colour gradient. Taken together these observations suggest that S999 is the remnant of a much larger galaxy that has been tidally stripped. If so, the observed elevated mass ratio may be caused by mechanisms related to the stripping process: the existence of an massive central black hole or internal kinematics that are out of equilibrium due to the stripping event. Given the observed dynamical-to-stellar mass ratio we suggest that S999 is an ideal candidate to search for the presence of an overly massive central black hole.
arXiv comment16 pages, 5 figures, accepted for publication in MNRAS
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