用Gemini近红外积分场谱仪探测Mrk 1157活动核的馈电和反馈
Feeding and feedback in the active nucleus of Mrk 1157 probed with Gemini Near-Infrared Integral-Field Spectrograph
摘要：
我们已经映射了恒星和气体的运动学，以及发射线通量分布和比率，从内部450 pc半径的Mrk 1157，使用2D近红外光谱与双子座NIFS获得的空间分辨率为35 pc。恒星速度场呈现旋转模式，零速度曲线呈离散的S形。酒吧的存在也支持所观察到的旋转场和模型的圆形轨道之间的残差映射在普卢默潜在的。恒星速度色散图显示了一个低σ值（50- 60 km/s）的部分环，距离核心250 pc，被来自星系核球的较高σ值所包围，起源于运动学上较冷的区域，伴随着最近的恒星形成。球核的速度色散（100 km/s）意味着一个质量为8.3 × 10^6 M_Sun的黑洞。发射线通量分布最沿PA=27/153度延伸，达到至少450 pc从核和以下的方向观察到在以前的光学发射线[OIII]成像和无线电喷流。H_2分子的发射主要是由热过程控制的，这主要是由于活性核的X射线加热。[FeII]激发有较大的贡献，从无线电喷流产生的冲击，证明了线比图和速度色散图，这表明与无线电结构的空间相关性。气体运动学显示了两个组成部分，一个是由于位于星系平面的气体，另一个是由于流出的气体，流出的气体靠近天空平面，因此延伸到高纬度，因为星系平面相对于天空平面倾斜45度。在平面内旋转的气体在H_2和Pa-β发射中占主导地位，而流出气体在[Fe Ⅱ]发射中占主导地位。从流出速度和隐含的几何形状，我们估计的离子化气体的流出质量率为6M_sun/yr。
英文摘要：
We have mapped the stellar and gaseous kinematics, as well as the emission-line flux distributions and ratios, from the inner 450pc radius of Mrk1157, using 2D near-IR spectra obtained with the Gemini NIFS at a spatial resolution of 35pc. The stellar velocity field shows a rotation pattern, with a discrete S-shaped zero velocity curve. The presence of a bar is also supported by the residual map between the observed rotation field and a model of circular orbits in a Plummer potential. The stellar velocity dispersion map presents a partial ring of low-sigma values (50-60km/s) at 250pc from the nucleus surrounded by higher sigma values from the galaxy bulge, originated in kinematically colder regions with recent star formation. The velocity dispersion of the bulge (100km/s) implies in a black hole mass of 8.3x10^6M_Sun. Emission-line flux distributions are most extended along PA=27/153deg, reaching at least 450pc from the nucleus and following the orientation observed in previous optical emission-line [OIII] imaging and radio jet. The molecular H_2 emission is dominated by thermal processes, mainly due to X-ray heating by the active nucleus. The [FeII] excitation has a larger contribution from shocks produced by the radio jet, as evidenced by the line-ratio maps and velocity dispersion map, which show spatial correlation with the radio structures. The gaseous kinematics shows two components, one due to gas located in the galaxy plane and another in outflow, which is oriented close to the plane of the sky, thus extending to high latitudes, as the galaxy plane is inclined by 45deg relative to the plane of the sky. The gas rotating in the plane dominates the H_2 and Pa-beta emission, while the gas in outflow is observed predominantly in [FeII] emission. From the outflow velocities and implied geometry, we estimate an outflow mass rate of 6M_sun/yr for the ionised gas.
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