标题： NGC3227活跃星系核中的恒星形成星环和动态黑洞质量 显示英文标题

标题： The Star-Forming Torus and Stellar Dynamical Black Hole Mass in the Seyfert 1 Nucleus of NGC3227

摘要： 我们报告了利用VLT（甚大望远镜）SINFONI自适应光学积分场K波段光谱仪对活动星系核 Seyfert 1 星系 NGC3227 核心的分辨率为0.085"（7 pc）的R~4300观测数据。 我们展示了发射线和吸收特征的形态学及动力学特性，并首次基于空间解析的恒星动力学推导出一个 Seyfert 1 核心区域黑洞的质量。 我们显示核区气体具有大约10^{24}-10^{25}cm^{-2}的平均柱密度，并且几何上较厚，这与标准“分子环”模型一致。 我们讨论了哪些加热过程可能负责维持环面的垂直高度。 我们也解析了核区恒星分布，并发现距离活动星系核（AGN）几秒差距范围内存在过一次强烈的恒星爆发，最近的一次爆发始于约40百万年前但现在已经停止。 距离AGN 30 pc范围内的恒星当前亮度约为3×10^9L_sun，与AGN亮度相当。 基于各自尺度的比较，我们认为恒星形成发生在遮蔽环内。 最后，我们首次基于恒星动力学从边缘分辨出 Seyfert 1 核心区域的黑洞质量。 我们应用施瓦西轨道叠加模型到我们的完整二维数据并推导黑洞质量，同时仔细关注经常不确定的输入参数：大尺度凸起及其质量-光度比；核区近期恒星形成及其质量-光度比；气体质量对势能的贡献；以及倾角。 我们的模型得出黑洞质量在1σ范围内的值为M_{BH} = 7×10^6-2×10^7M_sun。 显示英文摘要

摘要： We report R~4300 VLT SINFONI adaptive optics integral field K-band spectroscopy of the nucleus of the Seyfert 1 galaxy NGC3227 at a spatial resolution of 0.085" (7pc). We present the morphologies and kinematics of emission lines and absorption features, and give the first derivation of a black hole mass in a Seyfert 1 nucleus from spatially resolved stellar dynamics. We show that the gas in the nucleus has a mean column density of order 10^{24}-10^{25}cm^{-2} and that it is geometrically thick, in agreement with the standard `molecular torus' scenario. We discuss which heating processes may be responsible for maintaining the vertical height of the torus. We have also resolved the nuclear stellar distribution, and find that within a few parsecs of the AGN there has been an intense starburst, the most recent episode of which began ~40Myr ago but has now ceased. The current luminosity of stars within 30pc of the AGN, ~3x10^9L_sun, is comparable to that of the AGN. Based on a comparison of the respective size scales, we argue that the star formation has been occuring in the obscuring torus. Finally, we present the first derivation of a black hole mass in a Seyfert 1 nucleus from stellar dynamics which marginally spatially resolve the black hole's sphere of influence. We apply Schwarzschild orbit superposition models to our full 2-dimensional data and derive the mass of the black hole, paying careful attention to the input parameters which are often uncertain: the contribution of the large scale bulge and its mass-to-light ratio; the recent star formation in the nucleus and its mass-to-light ratio; the contribution of the gas mass to the potential; and the inclination. Our models yield a 1sigma range for the black hole mass of M_{BH} = 7x10^6-2x10^7M_sun.