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| Cool Gas deposited by X-ray Cooling Flows |
| 2009-07-24 | 编辑：星系宇宙学研究中心 | 【大 中 小】【打印】【关闭】 |
Speaker:
Prof. Jeremy Lim (Hong Kong University)
Time:
3:00pm, July 24
Location:
Large conf. room, 3rd floor
Abstract：
Galaxy clusters are permeated by hot X-ray-emitting gas.In relaxed clusters, the Xray gas around the cluster center is predicted to cool rapidly thereby resulting in a X-ray cooling flow.All subsequent searches, however, have foundmuch less cool gas than predicted, even in cases where molecular gas with masses of 10^9-10^11 Msun have been detected.Today, radio jets from the AGN in the central giant elliptical galaxy are believed to reheat the surrounding X-ray gas, mitigating if not entirely quenching the X-ray cooling flow.Here, I review the properties of the cool gas in the central giant elliptical galaxy of the Perseus Cluster, the X-ray-brightest cluster in the sky.I present a detailed study of its molecular gas, revealing for the first time that this gas is concentrated in multiple radial filaments unlike that seen in any other elliptical galaxy.I show that the molecular gas appears to be radially infalling, contrary to that expected if this gas has been accreted from a merger, but as would be expected if it originates from a X-ray cooling flow.I show tentative evidence that the molecular gas may be responsible for fueling the AGN in the central elliptical galaxy, completing a feedback loop of cooling and reheating of the X-ray gas. |
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