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

星系及其中心的超大质量黑洞（SMBHs）的共同演化在低红移时得到了最好的理解。我们通过动力学方法精确测量本地宇宙中SMBHs质量的能力使我们能够将其与宿主星系的特性进行比较，从而使我们目前对两者如何共同演化的理解。然而，我们对如此低红移的共同进化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的质量变得不那么精确，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一个功能，是什么驱动了这种共同进化，以及可能导致这种进化的反馈过程。在接下来的几个月里，我们将使用目前可用的高红移（z bbbb7）星系的光谱观测（Keck Mosfire和VLT X-Shooter），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，以试图更好地理解驱动这些属性的机制。接下来，我们将尝试评估星系猝灭的主要驱动机制。现在人们已经很清楚，一个星系的恒星形成（SF）被熄灭的可能性主要取决于黑洞的质量。然而，有趣的评估是驱动这一现象的机制：通过AGN风去除气体，通过星际介质加热抑制SF效率，或者通过AGN喷流或风加热星系晕导致星系饥饿。我们将利用阿塔卡马大型毫米波阵列（ALMA）对红移区z >.6、z ~ 2.5和z ~ 1.5的一系列类星体进行深入观测，利用各种发射谱线及其~ 100 GHz连续谱线来追踪原子、分子和热气体，以探测类星体驱动的外流、热晕或环星系介质中延伸的冷气体的存在，以及这些淬灭机制如何在宇宙时间内发生显著变化。然后，我们将把这些结果与下一代模拟结果进行比较，以拼凑出跨红移的SMBH反馈的演变。这些模拟模拟了SMBH反馈、辐射驱动的流出、喷流和风，使我们能够在宇宙时间内跟踪SMBH反馈的变化。这些模拟不仅可以让我们拍摄单个星系的快照，还可以观察它们从恒星形成到静止的演变过程，以及它们的属性变化，这些变化可能会推动这种演变。

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.