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Date and Time of the Query: 2019-06-17 T04:34:03 PDT
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For refcode 2005ApJ...628..137V:
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2005ApJ...628..137V The Low End of the Supermassive Black Hole Mass Function: Constraining the Mass of a Nuclear Black Hole in NGC 205 via Stellar Kinematics Monica Valluri, Laura Ferrarese, David Merritt, and Charles L. Joseph Abstract. Hubble Space Telescope (HST) images and spectra of the nucleated dwarf elliptical galaxy NGC 205 are combined with three-integral axisymmetric dynamical models to constrain the mass M_BH_ of a putative nuclear black hole. This is only the second attempt, after M33, to use resolved stellar kinematics to search for a nuclear black hole with mass below 10^6^ solar masses. We are unable to identify a best-fit value of M_BH_ in NGC 205; however, the data impose a upper limit of 2.2x10^4^ M_sun_ (1 {sigma} confidence) and an upper limit of 3.8x10^4^ M_sun_ (3 {sigma} confidence). This upper limit is consistent with the extrapolation of the M_BH_-{sigma} relation to the M_BH_<10^6^ M_sun_ regime. If we assume that NGC 205 and M33 both contain nuclear black holes, the upper limits on M_BH_ in the two galaxies imply a slope of ~5.5 or greater for the M_BH_-{sigma} relation. We use our three-integral models to evaluate the relaxation time and stellar collision time in NGC 205; T_r_ is ~10^8^ yr or less in the nucleus, and T_coll_~10^11^ yr. The low value of T_r_ is consistent with core collapse having already occurred, but we are unable to draw conclusions from nuclear morphology about the presence or absence of a massive black hole. Keywords: Galaxies: Elliptical and Lenticular, cD, Galaxies: Nuclei, Galaxies: Structure, Stellar Dynamics
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