利用Gemini NIFS对流向NGC4051 Seyfert核的分子气体流的作图
Mapping of the molecular gas inflow towards the Seyfert nucleus of NGC4051 using Gemini NIFS
摘要：
我们利用双子座近红外积分场光谱仪（NIFS）获得的近红外K波段光谱观测数据，以4.5 pc的采样率给出窄线塞弗特1星系NGC 4051内部~ 130 × 180 pc ^2的二维恒星和气体运动学。恒星自转曲线在离核仅55秒差距处的翻转，揭示了高度集中的引力势。核球的恒星速度色散约为60 km/s --这意味着核黑洞的质量约为10^6太阳质量--在核球内，速度色散较低的斑块表明存在较新的恒星形成区域。Brgamma发射线没有自转，也没有超过30 km/s的蓝移或红移，因此并不局限于星系平面。[CaVIII]冠状区域是紧凑的，但解决，在内部75 PC的延伸。它显示了最高的蓝移-高达-250公里/秒，以及最高的速度分散，解释为由于活动核的流出，支持靠近核的起源。从气体速度场中减去恒星速度场，可以分离出在H_2气体中观察到的非圆运动。最明显的运动学结构是两个核旋臂。我们将这些结构解释为流入的核，结果类似于以前的研究中，我们已经发现流运动沿核螺旋电离气体使用光学IFU观察。我们计算了沿着核旋臂的质量流入率，得到$ \dot{M}_{H_2} ~ 4 × 10 ^{-5} M_Sun/yr，这个值比驱动活动核所需的吸积率小~100倍。
英文摘要：
We present two-dimensional (2D) stellar and gaseous kinematics of the inner ~130x180 pc^2 of the Narrow Line Seyfert 1 galaxy NGC4051 at a sampling of 4.5 pc, from near-infrared K-band spectroscopic observations obtained with the Gemini's Near-infrared Integral Field Spectrograph (NIFS). The turnover of the stellar rotation curve at only ~55 pc from the nucleus, revealing a highly concentrated gravitational potential. The stellar velocity dispersion of the bulge is ~60 km/s -- implying on a nuclear black hole mass of ~10^6 M_sun -- within which patches of lower velocity dispersion suggest the presence of regions of more recent star formation. The Brgamma emission-line shows no rotation as well as no blueshifts or redshifts in excess of 30 km/s, and is thus not restricted to the galaxy plane. The [CaVIII] coronal region is compact but resolved, extending over the inner 75 pc. It shows the highest blueshifts -- of up to -250 km/s, and the highest velocity dispersions, interpreted as due to outflows from the active nucleus, supporting an origin close to the nucleus. Subtraction of the stellar velocity field from the gaseous velocity field has allowed us to isolate non-circular motions observed in the H_2 emitting gas. The most conspicuous kinematic structures are two nuclear spiral arms. We interpret these structures as inflows towards the nucleus, a result similar to those of previous studies in which we have found streaming motions along nuclear spirals in ionized gas using optical IFU observations. We have calculated the mass inflow rate along the nuclear spiral arms, obtaining $\dot{M}_{H_2} ~ 4x10^{-5} M_Sun/yr, value ~100 times smaller than the accretion rate necessary to power the active nucleus.
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