The benchmark black hole in NGC 4258 : dynamical models from high-resolution two-dimensional stellar kinematics

• Autor(a) principal: Drehmer, Daniel Alf
• Data de Publicação: 2015
• Outros Autores: Storchi-Bergmann, Thaisa, Ferrari, Fabricio, Cappellari, Michele, Riffel, Rogemar André
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/126983
• topic: Nucleo galatico; Dinamica estelar; Buracos negros; Masers astronômicos; Galaxies: individual: NGC 4258; Galaxies: kinematics and dynamics

NGC 4258 is the galaxy with the most accurate (maser-based) determination for the mass of the supermassive black hole (SMBH) in its nucleus. In this work, we present a two-dimensional mapping of the stellar kinematics in the inner 3.0 arcsec × 3.0 arcsec = 100 pc × 100 pc of NGC 4258 using adaptive-optics observations obtained with the Near-Infrared Integral Field Spectrograph of the Gemini North telescope at an ≈0.11 arcsec (4 pc) angular resolution. The observations resolve the radius of influence of the SMBH, revealing an abrupt increase in the stellar velocity dispersion within ≈10 pc from the nucleus, consistent with the presence of an SMBH there. Assuming that the galaxy nucleus is in a steady state and that the velocity dispersion ellipsoid is aligned with a cylindrical coordinate system, we constructed a Jeans anisotropic dynamical model to fit the observed kinematics distribution. Our dynamical model assumes that the galaxy has axial symmetry and is constructed using the multi-Gaussian expansion method to parametrize the observed surface brightness distribution. The Jeans dynamical model has three free parameters: the mass of the central SMBH (M•), the mass– luminosity ratio ( k = M/L) of the galaxy and the anisotropy of the velocity distribution. We test two types of models: one with constant velocity anisotropy, and another with variable anisotropy. The model that best reproduces the observed kinematics was obtained considering that the galaxy has radially varying anisotropy, being the best-fitting parameters with 3σ significanceM• = 4.8+0.8 −0.9 × 107M and k = 4.1+0.4 −0.5. This value for the mass of the SMBH is just 25 per cent larger than that of the maser determination and 50 per cent larger that a previous stellar dynamical determination obtained via Schwarzschild models for long-slit data that provides an SMBH mass 15 per cent lower than the maser value.