Graham, Alister W.Alister W.GrahamDurré, MarkMarkDurréSavorgnan, Giulia A. D.Giulia A. D.SavorgnanMedling, Anne M.Anne M.MedlingBatcheldor, DanDanBatcheldorScott, NicholasNicholasScottWatson, BeverlyBeverlyWatsonMarconi, AlessandroAlessandroMarconi2021-03-152021-03-1520160004-637Xhttp://hdl.handle.net/20.500.12386/30710The 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.STAMPAenArticle10.3847/0004-637X/819/1/432-s2.0-84960983639000372303400043https://iopscience.iop.org/article/10.3847/0004-637X/819/1/432016ApJ...819...43GFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_8 Formation and evolution of galaxies