An Upper Limit on the Mass of the Black Hole in Ursa Minor Dwarf Galaxy

• Published in: Astrophysical journal. Letters Vol. 699; no. 2; pp. L113 - L117
• Main Authors: Lora, V, Sánchez-Salcedo, F. J, Raga, A. C, Esquivel, A
• Format: Journal Article
• Language: English
• Published: IOP Publishing 01.07.2009
• ISSN: 1538-4357; 0004-637X; 2041-8205; 1538-4357
• DOI: 10.1088/0004-637X/699/2/L113

The well-established correlations between the mass of massive black holes (BHs) in the nuclei of most studied galaxies and various global properties of their hosting galaxy lend support to the idea that dwarf galaxies and globular clusters could also host a BH in their centers. Direct kinematic detection of BHs in dwarf spheroidal (dSph) galaxies is seriously hindered by the small number of stars inside the gravitational influence region of the BH. The aim of this Letter is to establish an upper dynamical limit on the mass of the putative BH in the Ursa Minor (UMi) dSph galaxy. We present direct N-body simulations of the tidal disruption of the dynamical fossil observed in UMi, with and without a massive BH. We find that the observed substructure is incompatible with the presence of a massive BH of (2-3) X 104 M within the core of UMi. These limits are consistent with the extrapolation of the M BH- Delta *s relation to the M BH < 106 M regime. We also show that the BH may be off-center with respect to the center of symmetry of the whole galaxy.