We present integral field spectroscopic observations of the nearby (z ∼ 0.03) dual active galactic nuclei (AGNs) Mrk 739, whose projected nuclear separation is ∼3.4 kpc, obtained with the Multi Unit Spectroscopic Explorer at the Very Large Telescope. We find that the galaxy has an extended AGN-ionized emission-line region extending up to ∼20 kpc away from the nuclei, while star-forming regions are more centrally concentrated within 2–3 kpc. We model the kinematics of the ionized gas surrounding the eastern nucleus using a circular disk profile, resulting in a peak velocity of at a distance of ∼1.2 kpc. The enclosed dynamical mass within 1.2 kpc is , ∼1000 times larger than the estimated supermassive black hole (SMBH) mass of Mrk 739E. The morphology and dynamics of the system are consistent with an early stage of the collision, where the foreground galaxy (Mrk 739W) is a young star-forming galaxy in an ongoing first passage with its background companion (Mrk 739E). Since the SMBH in Mrk 739W does not show evidence of being rapidly accreting, we claim that the northern spiral arms of Mrk 739W are ionized by the nuclear activity of Mrk 739E.

我们展示了附近 ( z ~ 0.03) 双活动星系核 (AGNs) Mrk 739 的积分场光谱观测，其预计核间距为 ~3.4 kpc，由甚大望远镜的多单元光谱探测器获得。我们发现该星系有一个扩展的 AGN 电离发射线区域，从原子核延伸到约 20 kpc，而恒星形成区域更集中在 2-3 kpc 内。我们使用圆盘轮廓模拟围绕东原子核的电离气体的运动学，从而在~ 1.2 kpc 的距离处产生峰值速度。1.2 kpc 范围内的封闭动力质量为, 比估计的 Mrk 739E 的超大质量黑洞 (SMBH) 质量大 1000 倍。该系统的形态和动力学与碰撞的早期阶段一致，其中前景星系（Mrk 739W）是一个年轻的恒星形成星系，与背景伴星（Mrk 739E）正在进行第一次通道。由于 Mrk 739W 中的 SMBH 没有显示出快速吸积的证据，我们声称 Mrk 739W 的北旋臂被 Mrk 739E 的核活动电离。