A Quintet of Black Hole Mass Determinations

(10) LBT Observatory; (11) Institut d'Astronomie et d'Astrophysique; (2) Department of Astronomy; (3) National Optical Astronomy Observatory; (4) Department of Physics; (5) Department of Physics; (6) Universitaets-Sternwarte der Ludwig-Maximilians-Universit\"at; (7) Observatories of the Carnegie Institution of Washington; (8) University of California Observatories/Lick Observatory; (9) Department of Astronomy

A Quintet of Black Hole Mass Determinations

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arxiv 0901.4162 v2 pith:KS6FISOW submitted 2009-01-27 astro-ph.GA astro-ph.CO

Kayhan Gultekin (1) , Douglas O. Richstone (1) , Karl Gebhardt (2) , Tod R. Lauer (3) , Jason Pinkney (4) , M. C. Aller (5) , Ralf Bender (6) , Alan Dressler (7)

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S. M. Faber (8) Alexei V. Filippenko (9) Richard Green (10) Luis C. Ho (7) John Kormendy (2) Christos Siopis (11) ((1) Dept. of Astronomy University of Michigan (2) Department of Astronomy University of Texas (3) National Optical Astronomy Observatory (4) Department of Physics Astronomy Ohio Northern University (5) Department of Physics Institute of Astronomy ETH Zurich (6) Universitaets-Sternwarte der Ludwig-Maximilians-Universität (7) Observatories of the Carnegie Institution of Washington (8) University of California Observatories/Lick Observatory Board of Studies in Astronomy Astrophysics University of California Santa Cruz (9) Department of Astronomy Berkeley (10) LBT Observatory University of Arizona (11) Institut d'Astronomie et d'Astrophysique Université Libre de Bruxelles)

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classification astro-ph.GA astro-ph.CO

keywords blackgalaxyholemassesaxisymmetricgalaxieshubblem-sigma

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We report five new measurements of central black hole masses based on STIS and WFPC2 observations with the Hubble Space Telescope and on axisymmetric, three-integral, Schwarzschild orbit-library kinematic models. We selected a sample of galaxies within a narrow range in velocity dispersion that cover a range of galaxy parameters (including Hubble type and core/power-law surface density profile) where we expected to be able to resolve the galaxy's sphere of influence based on the predicted value of the black hole mass from the M-sigma relation. We find masses in units of 10^8 solar masses for the following galaxies: NGC 3585, M_BH = 3.4 (+1.5, -0.6); NGC 3607, M_BH = 1.2 (+0.4, -0.4); NGC 4026, M_BH = 2.1 (+0.7, -0.4); and NGC 5576, M_BH = 1.8 (+0.3, -0.4), all significantly excluding M_BH = 0. For NGC 3945, M_BH = 0.09 (+0.17, -0.21), which is significantly below predictions from M-sigma and M-L relations and consistent with M_BH = 0, though the presence of a double bar in this galaxy may present problems for our axisymmetric code.

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