The identification of galaxies with "overly massive" black holes requires two measurements: a black hole mass (M-bh) and a host spheroid mass (M-sph,M-*). Here we provide our measurements for NGC. 1277. Our structural decomposition reveals that NGC. 1277 is dominated by a "classical" spheroid with a Srsic index n. =. 5.3, a half-light radius R-e,R-major = 2.1 kpc, and a stellar mass of 2.7 x 10(11) M-circle dot (using M-*/L-V = 11.65, Martin-Navarro et. al.). Thismass is an order of magnitude greater than originally reported. Using the latest M-bh-n, M-bh-M-sph,M-,M- and M-bh-sigma relations, the expected black hole mass is, respectively, (0.57(-0.40)(+1.29)) x 10(9) M-circle dot, (1.58(-1.13)(+4.04)) x 10(9) M-circle dot, (2.27(-1.44)(+4.04)) x 10(9) M-circle dot (using sigma = 300 km s(-1)) for which the "sphere-of-influence" is 0.'' 31. Our new kinematical maps obtained from laser guide star assisted, adaptive optics on the Keck I Telescope dramatically reaffirm the presence of the inner, nearly edge-on, disk seen in the galaxy image. We also report that this produces a large velocity shear (similar to 400 km s(-1)) across the inner 0.'' 2 (70 pc) plus elevated values of root sigma(2)+ V-2 across the inner (+/- 3.'' 8) x (+/- 0.'' 6) region of the galaxy. Our new multi-Gaussian expansion (MGE) models and Jeans Anisotropic MGE analysis struggled to match this extended component. Our optimal black hole mass, albeit a probable upper limit because of the disk is 1.2 x 10(9) M-circle dot (M/L-V = 12.3). This is an order of magnitude smaller than originally reported and 4 times smaller than recently reported. It gives an M-bh/M-sph,M-* ratio of 0.45% in agreement with the median (approximate to 0.5%) and range (0.1%-5.0%) observed in non-dwarf, early-type galaxies. This result highlights the need for caution with inner disks.

A NORMAL SUPERMASSIVE BLACK HOLE in NGC 1277 / Graham, Alister W.; Durré, Mark; Savorgnan, Giulia A. D.; Medling, Anne M.; Batcheldor, Dan; Scott, Nicholas; Watson, Beverly; Marconi, Alessandro. - In: THE ASTROPHYSICAL JOURNAL. - ISSN 0004-637X. - ELETTRONICO. - 819:(2016), pp. 43-56. [10.3847/0004-637X/819/1/43]

A NORMAL SUPERMASSIVE BLACK HOLE in NGC 1277

MARCONI, ALESSANDRO
2016

Abstract

The identification of galaxies with "overly massive" black holes requires two measurements: a black hole mass (M-bh) and a host spheroid mass (M-sph,M-*). Here we provide our measurements for NGC. 1277. Our structural decomposition reveals that NGC. 1277 is dominated by a "classical" spheroid with a Srsic index n. =. 5.3, a half-light radius R-e,R-major = 2.1 kpc, and a stellar mass of 2.7 x 10(11) M-circle dot (using M-*/L-V = 11.65, Martin-Navarro et. al.). Thismass is an order of magnitude greater than originally reported. Using the latest M-bh-n, M-bh-M-sph,M-,M- and M-bh-sigma relations, the expected black hole mass is, respectively, (0.57(-0.40)(+1.29)) x 10(9) M-circle dot, (1.58(-1.13)(+4.04)) x 10(9) M-circle dot, (2.27(-1.44)(+4.04)) x 10(9) M-circle dot (using sigma = 300 km s(-1)) for which the "sphere-of-influence" is 0.'' 31. Our new kinematical maps obtained from laser guide star assisted, adaptive optics on the Keck I Telescope dramatically reaffirm the presence of the inner, nearly edge-on, disk seen in the galaxy image. We also report that this produces a large velocity shear (similar to 400 km s(-1)) across the inner 0.'' 2 (70 pc) plus elevated values of root sigma(2)+ V-2 across the inner (+/- 3.'' 8) x (+/- 0.'' 6) region of the galaxy. Our new multi-Gaussian expansion (MGE) models and Jeans Anisotropic MGE analysis struggled to match this extended component. Our optimal black hole mass, albeit a probable upper limit because of the disk is 1.2 x 10(9) M-circle dot (M/L-V = 12.3). This is an order of magnitude smaller than originally reported and 4 times smaller than recently reported. It gives an M-bh/M-sph,M-* ratio of 0.45% in agreement with the median (approximate to 0.5%) and range (0.1%-5.0%) observed in non-dwarf, early-type galaxies. This result highlights the need for caution with inner disks.
2016
819
43
56
Graham, Alister W.; Durré, Mark; Savorgnan, Giulia A. D.; Medling, Anne M.; Batcheldor, Dan; Scott, Nicholas; Watson, Beverly; Marconi, Alessandro
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Utilizza questo identificatore per citare o creare un link a questa risorsa: https://hdl.handle.net/2158/1039099
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