为射电星系的中央引擎提供燃料。III。3C 293的分子气和恒星形成效率
Fueling the central engine of radio galaxies. III. Molecular gas and star formation efficiency of 3C 293
摘要：
目的。我们调查的AGN反馈的不同表现形式的演变，强大的无线电源3C 293及其对宿主星系，其中窝藏年轻的恒星形成区域和快速流出的HI和电离气体的分子气体的影响。方法.我们利用高空间分辨率的CO（1-0）和CO（2-1）谱线以及IRAM PdBI的3和1 mm连续谱线研究了3C 293分子气体的分布和运动学。我们绘制了3C 293的分子气体，并将其与宿主的尘埃和恒星形成图像进行了比较。我们在CO运动学中寻找流出运动的签名，并重新检查HI光谱中流出气体的证据。我们还利用文献中所有可用的SFR示踪剂推导了宿主的恒星形成率（SFR）和效率（SFE），并将其与年轻和进化的射电星系以及正常恒星形成星系的SFE进行了比较。结果CO（1-0）发射谱线表明，3C 293中的分子气体分布在一个质量为2.2E10Msun的弯曲盘上，该盘围绕活动星系核旋转，直径为21 kpc。我们的数据表明，尘埃和恒星的形成显然与CO盘有关。CO（2-1）辐射位于活动星系核周围直径为7 kpc的内部区域，与CO（1-0）盘的内部一致。CO（1-0）和CO（2-1）光谱都表明，在3C 293的中心区域存在一个与盘相关的吸收体。在冷分子气体中，我们没有探测到任何快速（>500 km/s）的外流运动。3C 293的宿主显示出符合Kennicutt-Schmidt定律的SFE。演化的射电星系的明显低的SFE可能是由于低估了SFR和/或高估了这些源中的分子气体密度。我们在3C 293的分子气体中没有发现活动星系核反馈的信号。
英文摘要：
Aims. We investigate the different manifestations of AGN feedback in the evolved, powerful radio source 3C293 and their impact on the molecular gas of its host galaxy, which harbors young star-forming regions and fast outflows of HI and ionized gas. Methods. We study the distribution and kinematics of the molecular gas of 3C293 using high spatial resolution observations of the CO(1-0) and CO(2-1) lines, and the 3 and 1mm continuum taken with the IRAM PdBI. We mapped the molecular gas of 3C293 and compared it with the dust and star-formation images of the host. We searched for signatures of outflow motions in the CO kinematics, and reexamined the evidence of outflowing gas in the HI spectra. We also derived the star formation rate (SFR) and efficiency (SFE) of the host with all available SFR tracers from the literature, and compared them with the SFE of young and evolved radio galaxies and normal star-forming galaxies. Results. The CO(1-0) emission line shows that the molecular gas in 3C293 is distributed along a massive (2.2E10 Msun) warped disk with diameter of 21 kpc that rotates around the AGN. Our data show that the dust and the star formation are clearly associated with the CO disk. The CO(2-1) emission is located in the inner 7 kpc (diameter) region around the AGN, coincident with the inner part of the CO(1-0) disk. Both the CO(1-0) and CO(2-1) spectra reveal the presence of an absorber against the central regions of 3C293 that is associated with the disk. We do not detect any fast (>500 km/s) outflow motions in the cold molecular gas. The host of 3C293 shows an SFE consistent with the Kennicutt-Schmidt law. The apparently low SFE of evolved radio galaxies may be caused by an underestimation of the SFR and/or an overestimation of the molecular gas densities in these sources. We find no signatures of AGN feedback in the molecular gas of 3C293.
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