论文标题
测量凸耳星系NGC 4546的超质量黑洞的质量
Measuring the mass of the supermassive black hole of the lenticular galaxy NGC 4546
论文作者
论文摘要
大多数带有结构良好的凸起的星系在其中心都有一个超级质量的黑洞（SMBH）。 Stellar kinematics models applied to adaptive optics (AO) assisted integral field unit observations are well-suited to measure the SMBH mass ($M_{BH}$) and also the total mass-to-light ratio [$(M/L)_{TOT}$] and possible anisotropies in the stellar velocity distribution in the central region of galaxies.在这项工作中，我们使用了新的AO辅助近红外积分磁场光谱仪（NIFS）观测值以及来自Hubble Space Space望远镜NGC 4546的Hubble Space Legacy档案的光度数据数据，以确定其SMBH质量。为此，我们应用了牛仔的各向异性建模（JAM）方法，以适合恒星结构的视线$（\ overline {v^2_ {los}}）$的平均第二速度矩。此外，我们还获得了$（m/l）_ {tot} $和经典的各向异性参数$β_z$ = 1 - （$σ_z$/$σ_r$）$^2 $在200 $ \ times $ \ times $ \ times $ \ times $ \ times $ 200 $ 200 pc $^2 $的视图中。使用惩罚的像素拟合（{\ sc ppxf}）技术为该星系建造了恒星径向速度和速度分散剂的地图。我们应用了多高斯膨胀程序以适合恒星亮度分布。 Using JAM, the best-fitting model for $\overline{v^2_{los}}$ of the stellar structure was obtained with $(M/L)_{TOT}$ = 4.34$\pm$0.07 (Johnson's R band), $M_{BH}$ = (2.56$\pm$0.16)$\times$10$^8$ M$_\odot$ and $β_z$ = -0.015 $ \ pm $ 0.03（3 $σ$置信度）。通过这些结果，我们发现NGC 4546遵循$ m_ {bh} $ $ \ times $ $σ$关系。我们还测量了该对象1 Arcsec的半径内的中央速度分散，为$σ_C$ = 241 $ \ pm $ 2 km S $^{ - 1} $。
Most galaxies with a well-structured bulge host a supermassive black hole (SMBH) in their centre. Stellar kinematics models applied to adaptive optics (AO) assisted integral field unit observations are well-suited to measure the SMBH mass ($M_{BH}$) and also the total mass-to-light ratio [$(M/L)_{TOT}$] and possible anisotropies in the stellar velocity distribution in the central region of galaxies. In this work, we used new AO assisted Near-Infrared Integral Field Spectrometer (NIFS) observations and also photometric data from the Hubble Space Telescope Legacy Archive of the galaxy NGC 4546 in order to determine its SMBH mass. To do this, we applied the Jeans Anisotropic Modelling (JAM) method to fit the average second velocity moment in the line of sight $(\overline{v^2_{los}})$ of the stellar structure. In addition, we also obtained $(M/L)_{TOT}$ and the classical anisotropy parameter $β_z$=1--($σ_z$/$σ_R$)$^2$ for this object within a field of view of 200$\times$200 pc$^2$. Maps of the stellar radial velocity and of the velocity dispersion were built for this galaxy using the penalized pixel fitting ({\sc ppxf}) technique. We applied the Multi Gaussian Expansion procedure to fit the stellar brightness distribution. Using JAM, the best-fitting model for $\overline{v^2_{los}}$ of the stellar structure was obtained with $(M/L)_{TOT}$ = 4.34$\pm$0.07 (Johnson's R band), $M_{BH}$ = (2.56$\pm$0.16)$\times$10$^8$ M$_\odot$ and $β_z$ = --0.015$\pm$0.03 (3$σ$ confidence level). With these results, we found that NGC 4546 follows the $M_{BH}$ $\times$ $σ$ relation. We also measured the central velocity dispersion within a radius of 1 arcsec of this object as $σ_c$ = 241$\pm$2 km s$^{-1}$.
