标题： Abell 1835星团中心星系中的恒星爆发：超大质量黑洞爆发调节星系形成的案例研究 显示英文标题

标题： The Starburst in the Abell 1835 Cluster Central Galaxy: A Case Study of Galaxy Formation Regulated by an Outburst from a Supermassive Black Hole

摘要： 我们展示了对Abell 1835星团中心cD星系中的恒星爆发的光学、X射线和无线电分析。围绕该星系的密集气体正在辐射X射线，其亮度约为1E45尔格/秒，这与每年约1000到2000个太阳质量的冷却率一致。然而，钱德拉和XMM-Newton观测发现，每年低于约2 keV的气体冷却量不到200个太阳质量，这一水平与cD星系当前的恒星形成率（100-180个太阳质量/年）一致。必须有一种或多种加热机制（反馈）来补充剩余的辐射损失。超新星爆炸产生的热通量和热传导单独作用无法做到这一点。然而，来自活动星系核爆发的一对X射线空腔在过去4000万年内向周围气体沉积了大约1.7E60尔格的能量。相应的喷流功率为1.4E45尔格/秒，足以抵消大部分冷却气体的辐射损失。喷流功率比无线电同步辐射功率高出约4000倍，使这个源成为已知最不具辐射效率的无线电源之一。大的喷流功率意味着在过去的4000万年左右，cD星系的超大质量黑洞以每年约0.3个太阳质量的平均速率吸积物质，这仅仅是10E9个太阳质量黑洞的爱丁顿吸积率的一小部分。通过恒星形成和通过吸积增长的球状体增长率的比例与附近休眠星系中球状体和中央黑洞质量之间的（Magorrian）关系斜率一致。在这个系统中，净冷却、加热（反馈）和冷却汇（恒星形成）之间的一致性解决了传统冷却流模型的主要反对意见。 显示英文摘要

摘要： We present an optical, X-ray, and radio analysis of the starburst in the Abell 1835 cluster's central cD galaxy. The dense gas surrounding the galaxy is radiating X-rays with a luminosity of ~1E45 erg/s consistent with a cooling rate of ~1000-2000 solar masses per year. However, Chandra and XMM-Newton observations find less than 200 solar masses per year of gas cooling below ~2 keV, a level that is consistent with the cD's current star formation rate of 100-180 solar masses per year. One or more heating agents (feedback) must then be replenishing the remaining radiative losses. The heat fluxes from supernova explosions and thermal conduction alone are unable to do so. However, a pair of X-ray cavities from an AGN outburst has deposited ~1.7E60 erg into the surrounding gas over the past 40 Myr. The corresponding jet power 1.4E45 erg/sec is enough to offset most of the radiative losses from the cooling gas. The jet power exceeds the radio synchrotron power by ~4000 times, making this one of the most radiatively inefficient radio sources known. The large jet power implies that the cD's supermassive black hole accreted at a mean rate of ~0.3 solar masses per year over the last 40 Myr or so, which is a small fraction of the Eddington accretion rate for a 10E9 solar mass black hole. The ratio of the bulge growth rate through star formation and the black hole growth rate through accretion is consistent with the slope of the (Magorrian) relationship between bulge and central black hole mass in nearby quiescent galaxies. The consistency between net cooling, heating (feedback), and the cooling sink (star formation) in this system resolves the primary objection to traditional cooling flow models. (abridged)