IBISCO调查：Seyfert星系Markarian 509的多相盘和风
The IBISCO survey: I. Multiphase discs and winds in the Seyfert galaxy Markarian 509
摘要：
我们提出了分析的ALMA CO（2-1）发射线和潜在的1.2毫米连续的Mrk 509与空间分辨率为270 pc。这个Seyfert 1.5星系在光学上被归类为一个球状体，已知拥有一个电离盘，一个星暴环，以及在核和星系尺度上的电离气体风。由CO（2-1）我们估计了位于5.2 kpc大小的圆盘内的分子气体质量$M_{H_2}=1.7\times 10^9\, \rm M_{\odot}$，$M_{dyn}$ =（2.0 $\pm$ 1.1）$\times$ $10^{10}\, \rm M_{\odot}$，倾斜于$44\pm10$ °。圆盘内的分子气体分数为$μ_{gas}=5\%$。在r=700 pc内的核区域中的气体运动学表明存在翘曲的核盘。无论是存在的一个分子盘与正在进行的恒星形成的星暴环，和一个小合并的签名，是在协议的情况下，星系合并产生气体不稳定，饲料恒星形成和活动星系核活动。空间分辨的Toomre Q-参数的分子盘是在$Q_{gas}=0.5-10$的范围内，并表明，光盘是边缘不稳定的整个星爆环，稳定的核和在一个不平衡的环状结构位于星爆环内。我们发现复杂的分子气体运动学和显着的运动学扰动在两个位置，一个在300秒差距内的核心，和一个1.4千秒差距的高$Q_{gas}$，我们解释为分子风的区域。总分子流出速率在6.4-17.0 $\rm M_\odot/yr$的范围内。分子风总动能与活动星系核驱动的多相动量守恒风一致，$\dot{P}_{of}/\dot{P}_{rad}$在0.06-0.5之间。内分子风与电离风的空间重叠，以及它们相似的速度表明，在一个多相活动星系核驱动风的冷却序列。
英文摘要：
We present the analysis of the ALMA CO(2-1) emission line and the underlying 1.2 mm continuum of Mrk509 with spatial resolution of 270 pc. This local Seyfert 1.5 galaxy, optically classified as a spheroid, is known to host a ionised disc, a starburst ring, and ionised gas winds on both nuclear and galactic scales. From CO(2-1) we estimate a molecular gas mass $M_{H_2}=1.7\times 10^9\, \rm M_{\odot}$, located within a disc of size 5.2 kpc, with $M_{dyn}$=(2.0$\pm$1.1) $\times$ $10^{10}\, \rm M_{\odot}$ inclined at $44\pm10$ deg. The molecular gas fraction within the disc is $μ_{gas}=5\%$. The gas kinematics in the nuclear region within r=700 pc suggests the presence of a warped nuclear disc. Both the presence of a molecular disc with ongoing star-formation in a starburst ring, and the signatures of a minor merger, are in agreement with the scenario where galaxy mergers produce gas destabilization, feeding both star-formation and AGN activity. The spatially-resolved Toomre Q-parameter across the molecular disc is in the range $Q_{gas}=0.5-10$, and shows that the disc is marginally unstable across the starburst ring, and stable at nucleus and in a lopsided ring-like structure located inside of the starburst ring. We find complex molecular gas kinematics and significant kinematics perturbations at two locations, one within 300 pc from the nucleus, and one 1.4 kpc away close to the region with high $Q_{gas}$, that we interpret as molecular winds. The total molecular outflow rate is in the range 6.4-17.0 $\rm M_\odot/yr$. The molecular wind total kinetic energy is consistent with a multiphase momentum-conserving wind driven by the AGN with $\dot{P}_{of}/\dot{P}_{rad}$ in the range 0.06-0.5. The spatial overlap of the inner molecular wind with the ionised wind, and their similar velocity suggest a cooling sequence within a multiphase AGN driven wind.
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