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http://hdl.handle.net/20.500.12386/30710
Titolo: | A Normal Supermassive Black Hole in NGC 1277 | Autori: | Graham, Alister W. Durré, Mark Savorgnan, Giulia A. D. Medling, Anne M. Batcheldor, Dan Scott, Nicholas Watson, Beverly Marconi, Alessandro |
Data pubblicazione: | 2016 | Rivista: | THE ASTROPHYSICAL JOURNAL | Numero: | 819 | Fascicolo: | 1 | Da pagina:: | 43 | Abstract: | The identification of galaxies with “overly massive” black holes requires two measurements: a black hole mass (M<SUB>bh</SUB>) and a host spheroid mass ({M}<SUB>{{sph,\ast </SUB>}}). Here we provide our measurements for NGC 1277. Our structural decomposition reveals that NGC 1277 is dominated by a “classical” spheroid with a Sérsic index n = 5.3, a half-light radius {R}<SUB>{{e,major</SUB>}}=2.1 {{kpc}}, and a stellar mass of 2.7× {10}<SUP>11</SUP>\quad {M}<SUB>☉ </SUB> (using {M}<SUB>*</SUB>/{L}<SUB>V</SUB>=11.65, Martín-Navarro et al.). This mass is an order of magnitude greater than originally reported. Using the latest M<SUB>bh</SUB>-n, M<SUB>bh</SUB>-{M}<SUB>{{sph,\ast </SUB>}}, and M<SUB>bh</SUB>-σ relations, the expected black hole mass is, respectively, ({0.57}<SUB>-0.40</SUB><SUP>+1.29</SUP>)× {10}<SUP>9</SUP>\quad {M}<SUB>☉ </SUB>, ({1.58}<SUB>-1.13</SUB><SUP>+4.04</SUP>)× {10}<SUP>9</SUP>\quad {M}<SUB>☉ </SUB>, and ({2.27}<SUB>-1.44</SUB><SUP>+4.04</SUP>)× {10}<SUP>9</SUP>\quad {M}<SUB>☉ </SUB> (using σ = 300 km s<SUP>-1</SUP>) 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 (∼400 km s<SUP>-1</SUP>) across the inner 0.″2 (70 pc) plus elevated values of \sqrt{{σ }<SUP>2</SUP>+{V}<SUP>2</SUP>} across the inner (+/- 3\buildrel{\prime\prime}\over{.} 8)× (+/- 0\buildrel{\prime\prime}\over{.} 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 × 10<SUP>9</SUP> M<SUB>☉</SUB> (M/{L}<SUB>V</SUB>=12.3). This is an order of magnitude smaller than originally reported and 4 times smaller than recently reported. It gives an {M}<SUB>{{bh</SUB>}}/{M}<SUB>{{sph,\ast </SUB>}} ratio of 0.45% in agreement with the median (≈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. | URI: | http://hdl.handle.net/20.500.12386/30710 | URL: | https://iopscience.iop.org/article/10.3847/0004-637X/819/1/43 | ISSN: | 0004-637X | DOI: | 10.3847/0004-637X/819/1/43 | Bibcode ADS: | 2016ApJ...819...43G | Fulltext: | open |
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