论文标题
阿尔玛时代的高红移星形成
High-redshift star formation in the ALMA era
论文作者
论文摘要
Atacama大毫米/亚毫米阵列（ALMA）目前正在改变我们对遥远（$ Z \ gtrsim1 $）宇宙中星系星系的看法。 Before ALMA, most of what we knew about dust-obscured star formation in distant galaxies was limited to the brightest submillimetre sources$-$the so-called submillimetre galaxies (SMGs)$-$and even the information on those sources was sparse, with resolved (i.e., sub-galactic) observations of the obscured star formation and gas reservoirs typically restricted to the most extreme and/or strongly镜头来源。从2011年的早期科学作品开始开始，最近九年的ALMA观察结果引入了一个新时代，以研究高红移之星形成。 Alma凭借其长基线，允许观察到远处的尘埃式恒星形成，其棱角分辨率可与$ - $甚至超过$ - $ - 最佳当前光学望远镜。凭借其带宽和频率覆盖范围，它通过针对性的随访和偶然的检测/盲线扫描提供了这些遥远星系中相关分子和原子气体的前所未有的观察。最后，与以前的（亚）毫米阵列相比，它的灵敏度飞跃，它通过对颜色/质量选择的星系群和专用的深层领域的统计研究，使这些强大的灰尘/气体示踪剂的检测更远地降低了光度的功能。我们审查了Alma在其科学运营的前九年中对高红移（$ Z \ GTRSIM1 $）星系星系的灰尘和气体的理解的主要进步，我们重点介绍了Alma在未来的几年中可能回答的有趣问题。
The Atacama Large Millimetre/submillimetre Array (ALMA) is currently in the process of transforming our view of star-forming galaxies in the distant ($z\gtrsim1$) universe. Before ALMA, most of what we knew about dust-obscured star formation in distant galaxies was limited to the brightest submillimetre sources$-$the so-called submillimetre galaxies (SMGs)$-$and even the information on those sources was sparse, with resolved (i.e., sub-galactic) observations of the obscured star formation and gas reservoirs typically restricted to the most extreme and/or strongly lensed sources. Starting with the beginning of early science operations in 2011, the last nine years of ALMA observations have ushered in a new era for studies of high-redshift star formation. With its long baselines, ALMA has allowed observations of distant dust-obscured star formation with angular resolutions comparable to$-$or even far surpassing$-$the best current optical telescopes. With its bandwidth and frequency coverage, it has provided an unprecedented look at the associated molecular and atomic gas in these distant galaxies through targeted follow-up and serendipitous detections/blind line scans. Finally, with its leap in sensitivity compared to previous (sub-)millimetre arrays, it has enabled the detection of these powerful dust/gas tracers much further down the luminosity function through both statistical studies of color/mass-selected galaxy populations and dedicated deep fields. We review the main advances ALMA has helped bring about in our understanding of the dust and gas properties of high-redshift ($z\gtrsim1$) star-forming galaxies during these first nine years of its science operations, and we highlight the interesting questions that may be answered by ALMA in the years to come.
