喷流驱动的冷气外流的位置和影响：3C 293的情况
The location and impact of jet-driven outflows of cold gas: the case of 3C293
摘要：
附近的射电星系3C 293是一小群检测到中性氢极端外流的天体之一。然而，由于先前观测的空间分辨率有限，无法确定外流的确切位置。在这封信中，我们提出了新的更高分辨率的VLA观测该射电源的中心区域，并检测到一个快速流出的HI与FWZI速度为Δv~1200 km/s的内部无线电喷流，约0.5 kpc的中央核心以西。我们调查可能的机制，可以产生所观察到的HI流出，并得出结论，它是由无线电射流驱动。然而，这种中性氢的流出位于原子核的相对侧，与先前在该物体中检测到的电离气体的流出相反。我们计算出的质量流出率在8-50太阳质量/年的范围内，对应于注入ISM的动能功率为1.38x10^{42} - 1.00x10^{43} erg/s或爱丁顿光度的0.01%-0.08%。这使得它刚好在一些星系演化模拟所要求的范围之外，因为AGN的负反馈可以有效地阻止星系内的恒星形成。
英文摘要：
The nearby radio galaxy 3C293 is one of a small group of objects where extreme outflows of neutral hydrogen have been detected. However, due to the limited spatial resolution of previous observations, the exact location of the outflow was not able to be determined. In this letter, we present new higher resolution VLA observations of the central regions of this radio source and detect a fast outflow of HI with a FWZI velocity of Δv~1200 km/s associated with the inner radio jet, approximately 0.5 kpc west of the central core. We investigate possible mechanisms which could produce the observed HI outflow and conclude that it is driven by the radio-jet. However, this outflow of neutral hydrogen is located on the opposite side of the nucleus to the outflow of ionised gas previously detected in this object. We calculate a mass outflow rate in the range of 8-50 solar masses/yr corresponding to a kinetic energy power injected back into the ISM of 1.38x10^{42} - 1.00x10^{43} erg/s or 0.01 - 0.08 percent of the Eddington luminosity. This places it just outside the range required by some galaxy evolution simulations for negative feedback from the AGN to be effective in halting star-formation within the galaxy.
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