M31核的三维开普勒轨道叠加模型
Three-dimensional Keplerian orbit-superposition models of the nucleus of M31
摘要：
我们提出了三维偏心盘模型的M31的核心，模拟光盘作为一个线性组合的厚环的无质量的恒星轨道上的潜在的中央黑洞。我们的模型是Peiris和Tremaine的参数模型的非参数概括。该模型再现观测到的WFPC2光度，详细的线的视线速度分布从STIS观测沿P1和P2，连同定性特征的绿洲运动学地图。我们证实了Peiris和Tremaine的发现，即强烈排除核盘与M31较大盘对齐的可能性。我们的最佳模型相对于M31的视线倾斜57度，位置角为55度。它的中心有一个质量为10^8太阳质量的黑洞，当从三维角度观察时，黑洞周围的恒星密度明显增加。在我们的模型中的轨道偏心率的分布是类似的Peiris & Tremaine的模型，但我们发现显着不同的倾角分布，这可能提供有价值的线索盘的起源。
英文摘要：
We present three-dimensional eccentric disc models of the nucleus of M31, modelling the disc as a linear combination of thick rings of massless stars orbiting in the potential of a central black hole. Our models are nonparametric generalisations of the parametric models of Peiris & Tremaine. The models reproduce well the observed WFPC2 photometry, the detailed line-of-sight velocity distributions from STIS observations along P1 and P2, together with the qualitative features of the OASIS kinematic maps. We confirm Peiris & Tremaine's finding that nuclear discs aligned with the larger disc of M31 are strongly ruled out. Our optimal model is inclined at 57 degrees with respect to the line of sight of M31 and has a position angle of 55 degrees. It has a central black hole of mass 10^8 solar masses, and, when viewed in three dimensions, shows a clear enhancement in the density of stars around the black hole. The distribution of orbit eccentricities in our models is similar to Peiris & Tremaine's model, but we find significantly different inclination distributions, which might provide valuable clues to the origin of the disc.
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