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dc.creatorMcConnell, Nicholas J.en_US
dc.creatorMa, Chung-Peien_US
dc.creatorGraham, James R.en_US
dc.creatorGebhardt, Karlen_US
dc.creatorLauer, Tod R.en_US
dc.creatorWright, Shelley A.en_US
dc.creatorRichstone, Douglas O.en_US
dc.date.accessioned2016-04-28T22:21:32Z
dc.date.available2016-04-28T22:21:32Z
dc.date.issued2011-02en
dc.identifierdoi:10.15781/T2952B
dc.identifier.citationMcConnell, Nicholas J., Chung-Pei Ma, James R. Graham, Karl Gebhardt, Tod R. Lauer, Shelley A. Wright, and Douglas O. Richstone. "The Black Hole Mass in the Brightest Cluster Galaxy NGC 6086." The Astrophysical Journal, Vol. 728, No. 2 (Feb., 2011): 100.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35188
dc.description.abstractWe present the first direct measurement of the central black hole mass, M-center dot, in NGC 6086, the Brightest Cluster Galaxy (BCG) in A2162. Our investigation demonstrates for the first time that stellar-dynamical measurements of M-center dot in BCGs are possible beyond the nearest few galaxy clusters. We observed NGC 6086 with laser guide star adaptive optics and the integral-field spectrograph (IFS) OSIRIS at the W. M. Keck Observatory and with the seeing-limited IFS GMOS-N at Gemini Observatory North. We combined the IFS data sets with existing major-axis kinematics and used axisymmetric stellar orbit models to determine M-center dot and the R-band stellar mass-to-light ratio, M-*/LR. We find M-center dot = 3.6(-1.1)(+1.7) x 10(9) M-circle dot and M-*/L-R = 4.6(-0.7)(+0.3) M-circle dot L-circle dot(-1) (68% confidence) from models using the most massive dark matter halo allowed within the gravitational potential of the host cluster. Models fitting only IFS data confirm M-center dot similar to 3x10(9) M circle dot and M-*/L-R similar to 4M(circle dot) L-circle dot(-1), with weak dependence on the assumed dark matter halo structure. When data out to 19 kpc are included, the unrealistic omission of dark matter causes the best-fit black hole mass to decrease dramatically, to 0.6 x 10(9) M-circle dot, and the best-fit stellar mass-to-light ratio to increase to 6.7 M circle dot L-(c),R(-1) . The latter value is at further odds with stellar population studies favoring M-*/L-R similar to 2M(circle dot) L-circle dot(-1) . Biases from dark matter omission could extend to dynamical models of other galaxies with stellar cores, and revised measurements of M-center dot could steepen the empirical scaling relationships between black holes and their host galaxies.en_US
dc.description.sponsorshipNSF AST-1009663, 0908639en_US
dc.description.sponsorshipNSF Center for Adaptive Optics AST 98-76783en_US
dc.description.sponsorshipMiller Institute for Basic Research in Science, the University of California, Berkeleyen_US
dc.description.sponsorshipW. M. Keck Foundationen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectgalaxies: elliptical and lenticular, cden_US
dc.subjectgalaxies: individual (ngcen_US
dc.subject6086)en_US
dc.subjectgalaxies: kinematics and dynamicsen_US
dc.subjectgalaxies: nucleien_US
dc.subjecthubble-space-telescopeen_US
dc.subjectaxisymmetrical dynamical modelsen_US
dc.subjectadaptive opticsen_US
dc.subjectsystemen_US
dc.subjectdark-matter haloen_US
dc.subjectto-light ratioen_US
dc.subjectelliptic galaxiesen_US
dc.subjectvelocityen_US
dc.subjectdispersionsen_US
dc.subjectstellar populationsen_US
dc.subjectfundamental planeen_US
dc.subjectmultiobjecten_US
dc.subjectspectrographen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Black Hole Mass In The Brightest Cluster Galaxy NGC 6086en_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.Filename2011_02_blackhole.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/728/2/100en_US
dc.contributor.utaustinauthorGebhardt, Karlen_US
dc.relation.ispartofserialAstrophysical Journalen_US


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