M_（bh）-sigma图的稠密核星团扩展
Extending the M_(bh)-sigma diagram with dense nuclear star clusters
摘要：
摘要：对于已知黑洞质量M_bh的星系，给出了4个新的核星团质量M_nc和7个质量上限。结合64个有直接M_bh测量值的星系样本（其中13个星系现在有M_nc测量值，而不仅仅是上限值）和29个有M_nc测量值和速度色散σ的矮星系，我们构造了一个（M_bh + M_nc）-σ图。考虑到主要的干星系合并事件保持了M_bh/L的比值，并且考虑到亮星系的L ~ σ ^[5]，我们首先注意到观测结果M_bh ~ σ ^[5]与预期是一致的。对于较暗的椭圆星系，已知L ~ σ ^[2]，并假设M_nc/L比值为常数（Ferrarese等人），M_nc ~ σ ^2的预期值与我们新的观测结果M_nc ~ σ ^{1.57 \pm 0.24}大体一致。然而，这个指数是在对比的值~4，这已经在以前的报告和解释的调节反馈机制从恒星风。
英文摘要：
Abridged: Four new nuclear star cluster masses, M_nc, plus seven upper limits, are provided for galaxies with previously determined black hole masses, M_bh. Together with a sample of 64 galaxies with direct M_bh measurements, 13 of which additionally now have M_nc measurements rather than only upper limits, plus an additional 29 dwarf galaxies with available M_nc measurements and velocity dispersions sigma, an (M_bh + M_nc)-sigma diagram is constructed. Given that major dry galaxy merger events preserve the M_bh/L ratio, and given that L ~ sigma^5 for luminous galaxies, it is first noted that the observation M_bh ~ sigma^5 is consistent with expectations. For the fainter elliptical galaxies it is known that L ~ sigma^2, and assuming a constant M_nc/L ratio (Ferrarese et al.), the expectation that M_nc ~ sigma^2 is in broad agreement with our new observational result that M_nc ~ sigma^{1.57\pm0.24}. This exponent is however in contrast to the value of ~4 which has been reported previously and interpreted in terms of a regulating feedback mechanism from stellar winds.
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