低功率喷流与星际介质耦合及盘面扰动：侧向 Seyfert 星系 NGC 4388
Low-power jet-ISM coupling and disk-plane perturbations in the edge-on Seyfert galaxy NGC 4388
- Università di Firenze（佛罗伦萨大学）
- INAF - Arcetri Astrophysical Observatory（意大利国家天体物理研究所-阿切特里天文台）
- Scuola Normale Superiore（比萨高等师范学院）
- Center for Physical Sciences and Technology（物理与技术研究中心）
- Instituto de Alta Investigación, Universidad de Tarapacá（塔拉帕卡大学高级研究所）
- Dipartimento di Fisica e Astronomia, Università di Bologna（博洛尼亚大学物理与天文系）
- INAF – Istituto di Radioastronomia（意大利国家天体物理研究所无线电天文研究所）
- European Southern Observatory（欧洲南方天文台）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究通过VLT/MUSE和VLA观测，发现侧向星系NGC 4388中低功率射电喷流与星际介质有效耦合，产生双锥外流和盘面扰动，证实喷流反馈不受方向限制。
AI中文摘要：
活动星系核（AGN）可能通过辐射驱动风和准直喷流调节星系演化，但它们的相对影响以及与星际介质（ISM）的耦合仍不确定。我们研究了邻近（$D\sim$ 17 Mpc）Seyfert 2 星系 NGC 4388 中的电离气体，该星系拥有一个星系尺度（$\sim$1.6 kpc）、低功率（$\sim1.4~\times~10^{42}~erg~s^{-1}$）的双极射电喷流，其投影方向大致垂直于其侧向盘。我们分析了来自VLT/MUSE自适应光学宽场模式的光学积分场光谱观测，并辅以追踪喷流的VLA射电数据。我们绘制了电离气体发射、运动学、激发和尘埃消光图。我们使用MOKA3D运动学模型重建了去投影的三维外流几何和速度场，并估计了其质量和能量。电离气体显示出一个旋转盘和一个kpc尺度的双锥外流。我们测量到总电离外流质量约为$10^6~M_\odot$，质量外流率约为$0.2~M_\odot$~yr$^{-1}$，动能功率约为$3\times10^{40}~erg~s^{-1}$，相对于喷流动能和辐射驱动的核风功率，耦合效率约为$1\\%$，表明这两种机制中的任何一种都可能驱动外流。我们探测到沿星系盘面延伸（$\sim$2 kpc）的气体速度弥散增强，其方向垂直于外流和喷流轴。这些区域的光学线比与激波激发一致。与ALMA CO(2-1)发射的空间对应关系较弱，而增强的恒星速度弥散排除了纯喷流解释。我们报告了首个观测证据，表明即使是一个几乎垂直于星系盘的低功率射电喷流也能有效地与ISM耦合，这表明喷流诱导的扰动是AGN反馈的重要渠道，无论喷流方向如何。
英文摘要：
Active galactic nuclei (AGN) may regulate galaxy evolution through radiatively driven winds and collimated jets, but their relative impact and coupling to the interstellar medium (ISM) remain uncertain. We investigate the ionized gas in the nearby ($D\sim$ 17 Mpc) Seyfert 2 galaxy NGC 4388, hosting a galaxy-scale ($\sim$1.6 kpc), low-power ($\sim1.4~\times~10^{42}~erg~s^{-1}$) bipolar radio jet projected roughly perpendicular to its edge-on disk. We analyze optical integral-field spectroscopic observations from the Wide Field Mode with adaptive optics of VLT/MUSE, complemented by VLA radio data tracing the jet. We map ionized-gas emission, kinematics, excitation, and dust attenuation. We reconstruct the de-projected 3D outflow geometry and velocity field using the MOKA3D kinematic model, and estimate its mass and energetics. The ionized gas shows a rotating disk and a kpc-scale biconical outflow. We measure a total ionized outflow mass of $\sim10^6~M_\odot$, a mass outflow rate of $\sim0.2~M_\odot$~yr$^{-1}$, and a kinetic power of $\sim3\times10^{40}~erg~s^{-1}$, which gives a coupling efficiency of $\sim1\%$ relative to both the jet kinetic and the radiation-driven nuclear wind power, indicating that either mechanism could drive the outflow. We detect an extended ($\sim$2 kpc) enhancement of the gas velocity dispersion along the galaxy disk plane, oriented perpendicular to the outflow and jet axes. These regions show optical line ratios consistent with shock excitation. The spatial correspondence with ALMA CO(2-1) emission is marginal, while enhanced stellar velocity dispersion prevents an exclusive jet interpretation. We report the first observational evidence that even a low-power radio jet oriented nearly perpendicular to the galaxy disk can efficiently couple with the ISM, suggesting that jet-induced perturbations are an important AGN feedback channel regardless of jet orientation.
