ABSTRACT The identification of galaxies with "overly massive" black holes requires two measurements: a black hole mass (Mbh) and a host spheroid mass ( ). 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 , and a stellar mass of (using , Martín-Navarro et al.). This mass is an order of magnitude greater than originally reported. Using the latest Mbh-n, Mbh- , and Mbh- relations, the expected black hole mass is, respectively, ( , ( , and ( (using = 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 (∼400 km s−1) across the inner 0 2 (70 pc) plus elevated values of across the inner 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 × 109 M ( ). This is an order of magnitude smaller than originally reported and 4 times smaller than recently reported. It gives an 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.