Taking Census of Massive, Star-Forming Galaxies formed<1 Gyr After the Big Bang
Taking Census of Massive, Star-Forming Galaxies formed<1 Gyr After the Big Bang
复制标题
对大爆炸后小于 1 吉里形成的巨大恒星形成星系进行普查
DOI：
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发表时间：
2019
期刊：
影响因子：
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通讯作者：
J. Zavala
中科院分区：
文献类型：
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作者：
C. Casey;P. Capak;J. Staguhn;L. Armus;A. Blain;M. Béthermin;J. Champagne;A. Cooray;K. Coppin;P. Drew;E. Dwek;S. Finkelstein;Maximilien Franco;J. Geach;J. Hodge;M. Koprowski;C. Lagos;D. Narayanan;A. Pope;D. Sanders;I. Shivaei;S. Toft;J. Vieira;F. Walter;K. Whitaker;M. Yun;J. Zavala
二十年来，人们一直致力于单碟和干涉毫米波天空测量，以推断尘埃恒星形成星系（dsfg， SFR>100M $_\odot$ yr $^{-1}$）在宇宙时间内的体积密度。虽然在宇宙恒星形成的高峰期（$z\sim2$）附近，被遮蔽的星系主导着宇宙恒星的形成，但在$z\sim2.5$之外，这种被严重遮蔽的星系对宇宙恒星形成的贡献是未知的，这与通过近红外深空和地面铅笔束巡天研究的莱曼-破星系（LBGs）种群相比，研究得很好。解开$z>3$以外的dsfg的体积密度，特别是在大爆炸后的前1 Gyr内，对于解决早期宇宙星系形成的关键开放问题至关重要：(1)宇宙在前几个Gyr内的综合恒星形成速率密度是多少，以及它在低质量星系（如莱曼-破星系）和高质量星系（如dsfg和类星体宿主星系）之间是如何分布的？(2)第一个大质量星系是如何以及在哪里聚集的？(3)关于宇宙大爆炸后<1 Gyr的尘埃产生机制（如超新星、AGB恒星、ISM中的颗粒生长），最极端的dsfg能告诉我们什么？我们总结了未来十年解决这些问题所需的观察类型。
Two decades of effort have been poured into both single-dish and interferometric millimeter-wave surveys of the sky to infer the volume density of dusty star-forming galaxies (DSFGs, with SFR>100M$_\odot$ yr$^{-1}$) over cosmic time. Though obscured galaxies dominate cosmic star-formation near its peak at $z\sim2$, the contribution of such heavily obscured galaxies to cosmic star-formation is unknown beyond $z\sim2.5$ in contrast to the well-studied population of Lyman-break galaxies (LBGs) studied through deep, space- and ground-based pencil beam surveys in the near-infrared. Unlocking the volume density of DSFGs beyond $z>3$, particularly within the first 1 Gyr after the Big Bang is critical to resolving key open questions about early Universe galaxy formation: (1) What is the integrated star-formation rate density of the Universe in the first few Gyr and how is it distributed among low-mass galaxies (e.g. Lyman-break galaxies) and high-mass galaxies (e.g. DSFGs and quasar host galaxies)? (2) How and where do the first massive galaxies assemble? (3) What can the most extreme DSFGs teach us about the mechanisms of dust production (e.g. supernovae, AGB stars, grain growth in the ISM)<1 Gyr after the Big Bang? We summarize the types of observations needed in the next decade to address these questions.