The Mass Relation Between The Black Hole And The Bulge For AGN

The core of the active galaxy is known as Active Galactic Nuclei (ab.AGN), which has bright and dense nuclei, with polarized non-heat continuous radiation in radio, optical and X-ray band. There exists strong atomic and ionic emission, with the ability to send out more energetic photons than normal galaxies. Quasars and Seyfert galaxies are two types of AGN. Quasars are the most luminous AGNs, while Seyfert galaxies are dimmer. Two models can explain the AGN well: Black-Hole Disk Model and Uniformed Model. The Black-Hole Disk Model makes it easier to explain the difficulty by high luminosity and small scale of AGN, while better to explain how the angle momentum moved to the outer. Uniformed Model thinks that the classification of AGN strongly ties to the orientation of observing. The differences of AGN are all decided by orientation. Observers seeing from different direction will obtain different type of AGN.The existence of central supermassive black holes (SMBHs) in AGN is widely accepted. Using the reverberating mapping method, we obtained the SMBHs masses of Quasars and Seyfert galaxies. It is found that there exists a tight correlation between the SMBHs and their host galaxies. The SMBH mass is proportional to the mass of the host bulge (hereafter SMBH/Bulge relation), with an average SMBH-to-bulge mass ratio of a constant, and a nearly, linear SMBH/Bulge relation. However, some groups found a nonlinear SMBH/Bulge mass relation, suggesting that the mean SMBH-to-bulge mass ratio is therefore not a universal constant, which is related to the bulge mass. It is found that the central SMBH mass is not only related to the bulge luminosity, but also to the bulge velocity dispersion.Using the bulge data from AGNs image decomposition, we calculate the ratio of...