Multimessenger Signatures of Massive Black Holes in Dwarf Galaxies
Multimessenger Signatures of Massive Black Holes in Dwarf Galaxies
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DOI：
10.1093/mnras/sty2842
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发表时间：
2018-06
影响因子：
4.8
通讯作者：
J. Bellovary;Colleen M. Cleary;F. Munshi;M. Tremmel;C. Christensen;A. Brooks;T. Quinn
中科院分区：
文献类型：
--
作者：
J. Bellovary;Colleen M. Cleary;F. Munshi;M. Tremmel;C. Christensen;A. Brooks;T. Quinn
最近在矮星系中发现的大质量黑洞（MBH）表明，它们可能比以前想象的更常见。系统搜索揭示了更多的候选人，但这一过程可以通过模拟预测来加速。我们对几个高分辨率的宇宙学放大模拟进行了研究，重点是在z = 0处拥有大质量黑洞的矮星系，目的是确定黑洞何时最可观察。较大的矮星系比质量较低的矮星系更有可能拥有MBH。大约50%的矮星系中的MBH并不位于星系中心，而是在距离星系中心几千秒差距的范围内徘徊。在整个宇宙时间内，矮星中MBH的吸积光度都很低，使得它们极难被探测到。然而，这些MBH的合并历史是最佳的引力波探测丽莎。
Recent discoveries of massive black holes (MBHs) in dwarf galaxies suggest that they may have a more common presence than once thought. Systematic searches are revealing more candidates, but this process could be accelerated by predictions from simulations. We perform a study of several high-resolution, cosmological, zoom-in simulations focusing on dwarf galaxies that host massive black holes at z = 0, with the aim of determining when the black holes are most observable. Larger dwarf galaxies are more likely to host MBHs than those of lower mass. About 50% of the MBHs in dwarfs are not centrally located, but rather are wandering within a few kpc of the galaxy center. The accretion luminosities of MBHs in dwarfs are low throughout cosmic time, rendering them extremely difficult to detect. However, the merger history of these MBHs is optimal for gravitational wave detection by LISA.