van Kampen Eelco, Bakx Tom, De Breuck Carlos, Chen Chian-Chou, Dannerbauer Helmut, Magnelli Benjamin, Montenegro-Montes Francisco Miguel, Okumura Teppei, Pu Sy-Yin, Rybak Matus, Saintonge Amelie, Cicone Claudia, Hatziminaoglou Evanthia, Hilhorst Juliëtte, Klaassen Pamela, Lee Minju, Lovell Christopher C, Lundgren Andreas, Di Mascolo Luca, Mroczkowski Tony, Sommovigo Laura, Booth Mark, Cordiner Martin A, Ivison Rob, Johnstone Doug, Liu Daizhong, Maccarone Thomas J, Smith Matthew, Thelen Alexander E, Wedemeyer Sven
European Southern Observatory, Garching bei München, Bayern, 85748, Germany.
Department of Space, Earth, & Environment, Chalmers University of Technology, Gothenberg, SE-412 96, Sweden.
Open Res Eur. 2024 Jun 24;4:122. doi: 10.12688/openreseurope.17445.1. eCollection 2024.
During the most active period of star formation in galaxies, which occurs in the redshift range 1 3, strong bursts of star formation result in significant quantities of dust, which obscures new stars being formed as their UV/optical light is absorbed and then re-emitted in the infrared, which redshifts into the mm/sub-mm bands for these early times. To get a complete picture of the high- galaxy population, we need to survey a large patch of the sky in the sub-mm with sufficient angular resolution to resolve all galaxies, but we also need the depth to fully sample their cosmic evolution, and therefore obtain their redshifts using direct mm spectroscopy with a very wide frequency coverage. This requires a large single-dish sub-mm telescope with fast mapping speeds at high sensitivity and angular resolution, a large bandwidth with good spectral resolution and multiplex spectroscopic capabilities. The proposed 50-m Atacama Large Aperture Submillimeter Telescope (AtLAST) will deliver these specifications. We discuss how AtLAST allows us to study the whole population of high-z galaxies, including the dusty star-forming ones which can only be detected and studied in the sub-mm, and obtain a wealth of information for each of these up to 7: gas content, cooling budget, star formation rate, dust mass, and dust temperature. We present worked examples of surveys that AtLAST can perform, both deep and wide, and also focused on galaxies in proto-clusters. In addition we show how such surveys with AtLAST can measure the growth rate f and the Hubble constant with high accuracy, and demonstrate the power of the line-intensity mapping method in the mm/sub-mm wavebands to constrain the cosmic expansion history at high redshifts, as good examples of what can uniquely be done by AtLAST in this research field.
在星系中恒星形成最活跃的时期，即红移范围在1至3之间时，强烈的恒星形成爆发会产生大量尘埃，这些尘埃会遮蔽正在形成的新恒星，因为它们的紫外/光学光被吸收，然后在红外波段重新发射，在早期这些红外光会红移到毫米/亚毫米波段。为了全面了解高红移星系群体，我们需要在亚毫米波段对大片天空进行勘测，要有足够的角分辨率来分辨所有星系，同时我们还需要足够的深度来充分采样它们的宇宙演化，因此要使用具有非常宽频率覆盖范围的直接毫米波光谱学来获取它们的红移。这需要一台大型单 dish 亚毫米波望远镜，具备高灵敏度、角分辨率下的快速测绘速度，大带宽、良好的光谱分辨率以及多路光谱能力。提议中的50米阿塔卡马大型毫米波望远镜（AtLAST）将满足这些规格要求。我们将讨论AtLAST如何使我们能够研究高红移星系的整个群体，包括那些只能在亚毫米波段被探测和研究的尘埃恒星形成星系，并获取这些星系直至红移为7的丰富信息：气体含量、冷却预算、恒星形成率、尘埃质量和尘埃温度。我们给出了AtLAST能够进行的勘测工作示例，包括深度和广度勘测，以及针对原星系团中星系的聚焦勘测。此外，我们展示了利用AtLAST进行的此类勘测如何高精度测量生长率f和哈勃常数，并展示了毫米波/亚毫米波波段线强度映射方法在约束高红移宇宙膨胀历史方面的能力，这些都是AtLAST在该研究领域能够独特完成的很好示例。
