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星系演化的全貌：全色光度函数和金属的产生

A complete view of galaxy evolution: panchromatic luminosity functions and the generation of metals

Andrew W. Blain, Lee Armus, Frank Bertoldi, James Bock, Matt Bradford, C. Darren Dowell, Jason Glenn, Paul Goldsmith, Martin Harwit, George Helou, J. D. Smith, … 展开作者

Andrew W. Blain, Lee Armus, Frank Bertoldi, James Bock, Matt Bradford, C. Darren Dowell, Jason Glenn, Paul Goldsmith, Martin Harwit, George Helou, J. D. Smith, B. T. Soifer, Gordon Stacey, Joaquin Vieira, Min Yun, Jonas Zmuidzinas

备注：
A whitepaper submitted on 15th February 2009 in response to the call from the Astro2010 panel: astro2010.org; uploaded as an 8-page pdf file
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摘要：

星系是何时以及如何形成的，它们的金属是如何积累的？在过去的十年里，这已经从一个考古学问题转变为一个现场调查：现在有一个暗物质晕中星系演化的广阔图景：它们的质量，恒星，金属和超大质量黑洞。银河系的形成过程最活跃的地方已经被发现和研究，一直追溯到宇宙时间，当星系际介质（IGM）仍然基本上是中性的时候。然而，关于遥远星系中的星际介质（ISM）如何以及为什么冷却、加工、回收和富集恒星的金属，以及为活动星系核（AGN）提供燃料的细节仍然不确定。特别是，气体冷却到燃料星形成，以及最强烈活动区域的化学和物理学在光学波长下是隐藏的，但可以在中红外和远红外（IR）波长下看到和诊断。静止帧红外观测首先是重要的，以确定最明亮，有趣和重要的星系，其次是精确量化其总光度，最后是使用光谱跟踪恒星形成的分子和原子气体的条件。为了在宇宙中发现的各种环境和大尺度结构（从密集的星系团到最空旷的空洞）上绘制出这些过程，我们需要对z~5以外的数百万个星系进行深入、大面积调查的工具，以及详细的后续光谱学。必要的工具可以在技术上实现。在这里，我们概述了收集关键信息的要求，以建立，验证和挑战星系演化模型。

英文摘要：

When and how did galaxies form and their metals accumulate? Over the last decade, this has moved from an archeological question to a live investigation: there is now a broad picture of the evolution of galaxies in dark matter halos: their masses, stars, metals and supermassive blackholes. Galaxies have been found and studied in which these formation processes are taking place most vigorously, all the way back in cosmic time to when the intergalactic medium (IGM) was still largely neutral. However, the details of how and why the interstellar medium (ISM) in distant galaxies cools, is processed, recycled and enriched in metals by stars, and fuels active galactic nuclei (AGNs) remain uncertain. In particular, the cooling of gas to fuel star formation, and the chemistry and physics of the most intensely active regions is hidden from view at optical wavelengths, but can be seen and diagnosed at mid- & far-infrared (IR) wavelengths. Rest-frame IR observations are important first to identify the most luminous, interesting and important galaxies, secondly to quantify accurately their total luminosity, and finally to use spectroscopy to trace the conditions in the molecular and atomic gas out of which stars form. In order to map out these processes over the full range of environments and large-scale structures found in the universe - from the densest clusters of galaxies to the emptiest voids - we require tools for deep, large area surveys, of millions of galaxies out to z~5, and for detailed follow-up spectroscopy. The necessary tools can be realized technically. Here, we outline the requirements for gathering the crucial information to build, validate and challenge models of galaxy evolution.

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