We use Gemini Near-Infrared Integral Field Spectrograph (NIFS) observations of the inner 3.5 × 3.5 kpc2 of the radio galaxy Cygnus A to map the gas excitation and kinematics at a spatial resolution of 200 pc. The emission of the ionized gas shows a biconical morphology, with half-opening angle of 45○ and oriented along the position angle of the radio jet. Coronal line emission is seen within the cone, up to 1.75 kpc from the nucleus, with higher ionization gas observed in the easterly side. The H2 and [Fe ii] emission lines are consistent with excitation by the central AGN, with some contribution of shocks to the south-west of the nucleus. The gas visual extinction and electron density are larger than those from optical-based measurements, consistent with the fact that near-IR observations penetrate deeply into the gas emission structure, probing denser and more obscured regions. The gas kinematics shows two components: (i) a rotating disc with kinematic position angle of Ψ0 = 21○ ± 2○, seen both in ionized and molecular gas, and (ii) outflows with velocities of up to 600 km s−1 observed within the ionization cone in ionized gas and restricted to inner 0.5 arcsec in molecular gas. The mass outflow rate in ionized gas is in the range $\sim \! 100\!-\!280\, {\rm M_\odot \, yr^{-1}}$ and the kinetic power of the outflow corresponds to 0.3–3.3 per cent of the AGN bolometric luminosity, indicating that the outflows in Cygnus A may be effective in suppressing star formation.

中文翻译：

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天鹅座 A 中部区域强大的多相流出物

我们使用双子星近红外积分场光谱仪 (NIFS) 对射电星系 Cygnus A 内部 3.5 × 3.5 kpc2 的观测，以 200 pc 的空间分辨率绘制气体激发和运动学图。电离气体的发射呈双锥形态，半开角为 45°，并沿射流的位置角定向。在锥体内可以看到日冕线发射，距核最多 1.75 kpc，在东侧观察到较高的电离气体。H2 和[Fe ii] 发射线与中央活动星系核的激发一致，其中有一些冲击对核西南的贡献。气体视觉消光和电子密度大于基于光学的测量值，这与近红外观测深入到气体发射结构中的事实一致，探测更密集和更模糊的区域。气体运动学显示两个组成部分：(i) 运动学位置角为 Ψ0 = 21○ ± 2○ 的旋转圆盘，在电离气体和分子气体中均可见，以及 (ii) 观察到的流出速度高达 600 km s-1在电离气体的电离锥内，在分子气体中限制在 0.5 弧秒内。电离气体的质量流出速率在 $\sim \! 100\!-\!280\, {\rm M_\odot \, yr^{-1}}$ 和流出的动能对应于活动星系核辐射光度的 0.3-3.3%，表明流出在天鹅座 A 可能有效抑制恒星的形成。(ii) 在电离气体的电离锥内观察到速度高达 600 km s-1 的流出物，并且限制在分子气体的内部 0.5 弧秒内。电离气体的质量流出速率在 $\sim \! 100\!-\!280\, {\rm M_\odot \, yr^{-1}}$ 和流出的动能对应于活动星系核辐射光度的 0.3-3.3%，表明流出在天鹅座 A 可能有效抑制恒星的形成。(ii) 在电离气体的电离锥内观察到速度高达 600 km s-1 的流出物，并且限制在分子气体的内部 0.5 弧秒内。电离气体的质量流出速率在 $\sim \! 100\!-\!280\, {\rm M_\odot \, yr^{-1}}$ 和流出的动能对应于活动星系核辐射光度的 0.3-3.3%，表明流出在天鹅座 A 可能有效抑制恒星的形成。