Measuring the Masses of Supermassive Black Holes
Measuring the Masses of Supermassive Black Holes
复制标题
DOI：
10.1007/s11214-013-9987-4
复制
发表时间：
2014-09
影响因子：
10.3
通讯作者：
B. Peterson
中科院分区：
文献类型：
--
作者：
B. Peterson
超大质量黑洞位于大多数（如果不是全部）大质量星系的中心：活动星系和静止星系之间的差异是由于质量吸积率和辐射效率的差异，而不是它们是否有核黑洞。在这方面的贡献，测量超大质量黑洞的质量的方法进行了讨论，重点是混响映射，这是最普遍适用于吸积超大质量黑洞，特别是遥远的类星体的时间分辨率可以用作角分辨率的替代品。间接方法的基础上的缩放关系混响映射研究，也讨论了沿着其目前的局限性。
Supermassive black holes reside at the centers of most, if not all, massive galaxies: the difference between active and quiescent galaxies is due to differences in mass accretion rate and radiative efficiency rather than whether or not they have nuclear black holes. In this contribution, methods for measuring the masses of supermassive black holes are discussed, with emphasis on reverberation mapping which is most generally applicable to accreting supermassive black holes and, in particular, to distant quasars where time resolution can be used as a surrogate for angular resolution. Indirect methods based on scaling relationships from reverberation mapping studies are also discussed, along with their current limitations.