Probing galaxy-black hole co-evolution across cosmic time: predictions from next-generation observations and simulations

星系和它们中心的超大质量黑洞（SMBH）的共同演化在低红移下得到了最好的理解。我们通过动力学方法准确测量局部宇宙中SMBH质量的能力使我们能够将其与其宿主星系的性质进行比较，从而使我们目前了解两者如何共同进化。然而，我们对这种低红移下共同进化的驱动机制的理解仍然存在重大问题。此外，当我们移动到更高的红移时，通过动力学方法测量SMBH质量变得不那么准确，导致缺乏对中高红移的共同进化的理解。我们还不知道这种共同进化是否是红移的函数，是什么驱动了这种共同进化，以及可能导致这种共同进化的反馈过程。在未来的几个月里，我们将利用目前可用的高红移（z>7）星系（凯克Mosfire和VLT X-Shooter）的光谱观测，试图评估它们的性质和潜在的活动星系核（AGN）活动。然后将其结果与当前成熟的模拟（Illustris，IllustrisTNG和FABLE）进行比较，以更好地理解驱动这些属性的机制。在此之后，我们将试图评估星系淬火的主要驱动机制。现在已经很好地理解了，一个星系被恒星形成（SF）淬灭的概率主要取决于黑洞的质量。然而，有趣的评估是驱动这一点的机制：通过AGN风去除气体，星际介质加热或星系饥饿通过AGN喷流或风加热星系晕抑制SF效率。我们将在红移区域z>6、z ~ 2.5和z ~ 1.5对一系列类星体进行深阿塔卡马大型毫米波阵列（阿尔马）观测，使用各种发射线及其~ 100 GHz连续谱来追踪原子、分子和热气体，以探测类星体驱动外流的存在，环星系介质中的热晕或扩展的冷气体，以及这些淬火机制如何在宇宙时间内在日珥中变化。然后，我们将将这些结果与下一代模拟进行比较，以拼凑出不同红移下SMBH反馈的演变。这些模拟模拟SMBH反馈，辐射驱动的外流，射流和风，使我们能够跟踪SMBH反馈在宇宙时间内的变化。这些模拟将使我们不仅能够拍摄单个星系的快照，而且还可以观察它们从恒星形成到静止的演变，以及可能驱动这种演变的性质变化。

The co-evolution of galaxies and their central super-massive-black-holes (SMBHs) is best understood at low redshifts. Our ability to accurately measure the mass of SMBHs in the local universe through dynamical methods allows us to compare these to their host galaxies properties, leading to our current understanding of how the two co-evolve. However, significant problems remain with our understanding of the driving mechanisms of co-evolution at such low redshifts. In addition, as we move to higher redshifts SMBH mass measurements via dynamical methods become less accurate, leading to a lack of understanding of co-evolution at intermediate to high redshifts. We do not yet understand whether this co-evolution is a function of redshift, what drives this co-evolution and the feedback processes that may cause it. In the coming months we will use currently available spectroscopic observations of high redshift (z>7) galaxies (Keck Mosfire and VLT X-Shooter) in an attempt to evaluate their properties and potential active galactic nucleus (AGN) activity occurring within them. The results of this will then be compared to current well-established simulations (Illustris, IllustrisTNG and FABLE) to try to better understand the mechanisms driving these properties. Following this we will attempt to assess the primary driving mechanisms for galaxy quenching. It is now well understood that the probability that a galaxy has been quenched of star-formation (SF) depends primarily on black hole mass. The interesting assessment however is the mechanism that drives this: gas removal via AGN winds, SF efficiency suppression by inter-stellar medium heating or galaxy starvation by the heating of the galactic halo through AGN jets or winds. We will take deep Atacama Large Millimeter Array (ALMA) observations of a selection of quasars, in redshift regimes z>6, z ~ 2.5 and z ~ 1.5, using various emission lines and their ~ 100 GHz continuum to trace atomic, molecular and hot gas in order to probe the presence of either quasar driven outflows, the hot halo or extended cold gas in the circumgalactic medium and how these quenching mechanisms may change in prominence across cosmic time. We will then compare these results with next generation simulations to piece together the evolution of SMBH feedback across redshifts. These simulations model SMBH feedback, radiation driven outflows, jets and winds allowing us to track changes in SMBH feedback across cosmic time. These simulations will allow us to not only take snapshots of individual galaxies but to observe their evolution from star-forming to quiescent and the changes in their properties that potentially drive such an evolution.