The black hole mass of NGC 4151. II. Stellar dynamical measurement from near-infrared integral field spectroscopy

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dc.contributor.authorOnken, Christopher
dc.contributor.authorValluri, Monica
dc.contributor.authorBrown, Jonathan S
dc.contributor.authorMcGregor, Peter
dc.contributor.authorPeterson, Bradley M
dc.contributor.authorBentz, Misty C
dc.contributor.authorFerrarese, Laura
dc.contributor.authorPogge, R W
dc.contributor.authorVestergaard, Marianne
dc.contributor.authorStorchi-Bergmann, Thaisa
dc.contributor.authorRiffel, Rogemar A
dc.date.accessioned2015-12-13T22:30:39Z
dc.date.issued2014
dc.date.updated2015-12-11T08:55:16Z
dc.description.abstractWe present a revised measurement of the mass of the central black hole (M BH) in the Seyfert 1 galaxy NGC 4151. The new stellar dynamical mass measurement is derived by applying an axisymmetric orbit-superposition code to near-infrared integral field data obtained using adaptive optics with the Gemini Near-infrared Integral Field Spectrograph (NIFS). When our models attempt to fit both the NIFS kinematics and additional low spatial resolution kinematics, our results depend sensitively on how χ2 is computed - probably a consequence of complex bar kinematics that manifest immediately outside the nuclear region. The most robust results are obtained when only the high spatial resolution kinematic constraints in the nuclear region are included in the fit. Our best estimates for the black hole mass and H-band mass-to-light ratio are M BH ∼ 3.76 ± 1.15 × 107 M ⊙ (1σ error) and Υ⊙ H ∼ 0.34 ± 0.03 M ⊙/L ⊙ (3σ error), respectively (the quoted errors reflect the model uncertainties). Our black hole mass measurement is consistent with estimates from both reverberation mapping () and gas kinematics (; 1σ errors), and our best-fit mass-to-light ratio is consistent with the photometric estimate of Υ⊙ H = 0.4 ± 0.2 M ⊙/L ⊙. The NIFS kinematics give a central bulge velocity dispersion σc = 116 ± 3 km s-1, bringing this object slightly closer to the M BH-σ relation for quiescent galaxies. Although NGC 4151 is one of only a few Seyfert 1 galaxies in which it is possible to obtain a direct dynamical black hole mass measurement - and thus, an independent calibration of the reverberation mapping mass scale - the complex bar kinematics makes it less than ideally suited for this purpose.
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/74931
dc.publisherIOP Publishing
dc.rightsAuthor/s retain copyrighten_AU
dc.sourceAstrophysical Journal, The
dc.titleThe black hole mass of NGC 4151. II. Stellar dynamical measurement from near-infrared integral field spectroscopy
dc.typeJournal article
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.issue1
local.bibliographicCitation.lastpage20
local.bibliographicCitation.startpage1
local.contributor.affiliationOnken, Christopher , College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationValluri, Monica, University of Michigan
local.contributor.affiliationBrown, Jonathan S, University of Michigan
local.contributor.affiliationMcGregor, Peter, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationPeterson, Bradley M, Ohio State University
local.contributor.affiliationBentz, Misty C, Georgia State University
local.contributor.affiliationFerrarese, Laura, Herzberg Institute of Astrophysics
local.contributor.affiliationPogge, R W, Ohio State University
local.contributor.affiliationVestergaard, Marianne, University of Arizona
local.contributor.affiliationStorchi-Bergmann, Thaisa, Universidade Federal do Rio Grande do Sul
local.contributor.affiliationRiffel, Rogemar A, Universidade Federal de Santa Maria
local.contributor.authoremailu4606113@anu.edu.au
local.contributor.authoruidOnken, Christopher , u4606113
local.contributor.authoruidMcGregor, Peter, u8401248
local.description.notesImported from ARIES
local.identifier.absfor020100 - ASTRONOMICAL AND SPACE SCIENCES
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciences
local.identifier.ariespublicationU3488905xPUB4382
local.identifier.citationvolume791
local.identifier.doi10.1088/0004-637X/791/1/37
local.identifier.scopusID2-s2.0-84905215059
local.identifier.thomsonID000339657700037
local.identifier.uidSubmittedByU3488905
local.type.statusPublished Version

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