Mark Booth, Pamela Klaassen, Claudia Cicone, Tony Mroczkowski, Martin A. Cordiner, Luca Di Mascolo, Doug Johnstone, Eelco van Kampen, Minju M. Lee, Daizhong Liu… 展开作者
Mark Booth, Pamela Klaassen, Claudia Cicone, Tony Mroczkowski, Martin A. Cordiner, Luca Di Mascolo, Doug Johnstone, Eelco van Kampen, Minju M. Lee, Daizhong Liu, John Orlowski-Scherer, Amélie Saintonge, Matthew W. L. Smith, Alexander Thelen, Sven Wedemeyer, Kazunori Akiyama, Stefano Andreon, Doris Arzoumanian, Tom J. L. C. Bakx, Caroline Bot, Geoffrey Bower, Roman Brajša, Chian-Chou Chen, Elisabete da Cunha, David Eden, Stefano Ettori, Brandt Gaches, Evanthia Hatziminaoglou, Patricia Luppe, Benjamin Magnelli, Jonathan P. Marshall, Francisco Miguel Montenegro-Montes, Michael Niemack, Conor Nixon, Imke de Pater, Yvette Perrott, Sandra I. Raimundo, Elena Redaelli, Anita Richards, Matus Rybak, Nikolina Šarčević, Dmitry Semenov, Silvia Spezzano, Sundar Srinivasan, Thomas Stanke, Paola Andreani, Maria T. Beltrán, Bryan J. Butler, Sebastiano Cantalupo, Miguel Chavez Dagostino, Ana Duarte-Cabral, Bjorn Emonts, Leigh Fletcher, Dale E. Gary, Stanislav Gunar, Alvaro Hacar, Bendix Hagedorn, Tomek Kaminski, Fiona Kirton, Katherine de Kleer, Eduard Kontar, Yi-Jehng Kuan, John Lightfoot, Enrique Lopez-Rodriguez, Andreas Lundgren, Stefanie N. Milam, Atul Mohan, Raphael Moreno, Galina G. Motorina, Arielle Moullet, Kate Pattle, Alberto Pellizzoni, Nicolas Peretto, Joanna Ramasawmy, Claudio Ricci, Andrew J. Rigby, Álvaro Sánchez-Monge, Maryam Saberi, Masumi Shimojo, Aurora Simionescu, Mark Thompson, Alessio Traficante, Cristian Vignali, Stephen M. White
Submillimeter and millimeter wavelengths provide a unique view of the Universe, from the gas and dust that fills and surrounds galaxies to the chromosphere of our own Sun. Current single-dish facilities have presented a tantalising view of the brightest (sub-)mm sources, and interferometers have provided the exquisite resolution necessary to analyse the details in small fields, but there are still many open questions that cannot be answered with current facilities. In this report we summarise the science that is guiding the design of the Atacama Large Aperture Submillimeter Telescope (AtLAST). We demonstrate how tranformational advances in topics including star formation in high redshift galaxies, the diffuse circumgalactic medium, Galactic ecology, cometary compositions and solar flares motivate the need for a 50m, single-dish telescope with a 1-2 degree field of view and a new generation of highly multiplexed continuum and spectral cameras. AtLAST will have the resolution to drastically lower the confusion limit compared to current single-dish facilities, whilst also being able to rapidly map large areas of the sky and detect extended, diffuse structures. Its high sensitivity and large field of view will open up the field of submillimeter transient science by increasing the probability of serendipitous detections. Finally, the science cases listed here motivate the need for a highly flexible operations model capable of short observations of individual targets, large surveys, monitoring programmes, target of opportunity observations and coordinated observations with other observatories. AtLAST aims to be a sustainable, upgradeable, multipurpose facility that will deliver orders of magnitude increases in sensitivity and mapping speeds over current and planned submillimeter observatories.
Science drivers and requirements for an Advanced Technology Large Aperture Space Telescope (ATLAST): Implications for technology development and synergies with other future facilities
The Atacama Large Aperture Submillimeter Telescope (AtLAST): enabling large-scale sub-mm science beyond 2030
Institute of Theoretical Astrophysics, University of Oslo（奥斯陆大学理论天体物理研究所）；Institute of Space Sciences (ICE-CSIC)（空间科学研究所（ICE-CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院（IEEC））；Instituto de Astrofísica de Canarias (IAC)（加那利群岛天体物理研究所（IAC））；Departamento de Astrofísica, Universidad de La Laguna（拉古纳大学天体物理学系）；European Southern Observatory (ESO)（欧洲南方天文台（ESO））；OHB Digital Connect（OHB数字连接公司）；Department of Technology Systems, University of Oslo（奥斯陆大学技术系统系）；MPIfR（马克斯·普朗克射电天文研究所）；UK Astronomy Technology Centre, Royal Observatory Edinburgh（英国天体技术中心，爱丁堡皇家天文台）；IPARCOS-UCM, Universidad Complutense de Madrid（马德里康普顿斯大学IPARCOS研究中心）；Department of EEC Engineering, University of Pretoria（比勒陀利亚大学电气工程与电子工程系）；University of Tokyo（东京大学）；INAF Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；Nagoya University（名古屋大学）；Rosseland Centre for Solar Physics, University of Oslo（奥斯陆大学罗斯兰太阳物理中心）；ESO（欧洲南方天文台）；ICREA（加泰罗尼亚卓越研究奖计划）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、AIM）；TU Delft（代尔夫特理工大学）
The Colorado Ultraviolet Transit Experiment (CUTE) Mission Overview
大气逃逸是影响许多行星结构、组成和演化的基本过程。逃逸的信号在靠近的气态系外行星上是可以探测到的，这些行星围绕明亮的恒星运行，这是由于它们的母恒星发出了高水平的极紫外线辐射。科罗拉多紫外线凌日实验（CUTE）是一个立方体卫星飞行任务，旨在利用近紫外线恒星亮度分布对附近近距离行星的扩展大气层进行调查。CUTE的有效载荷是一个放大NUV（2479~--~3306 Ang）摄谱仪，由一个矩形卡塞格伦望远镜（206 mm x 84 mm）馈电;光谱图记录在一个背照式紫外增强CCD上。科学有效载荷集成到6 U Blue Canyon Technology XB 1总线中。CUTE于2021年9月27日发射到极地低地球轨道，并在在轨调试期后一直在进行这项凌日光谱调查。本文介绍了任务的动机，发展道路，并展示了小卫星进行这类科学的潜力，提出初步的在轨科学观测。主要的科学任务将于2022~--~2023年进行，公开的数据档案将于2023年上线。
The LMT 2 Millimeter Receiver System (B4R). I. Overview and Results of Science Demonstration
National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；The Graduate University for Advanced Studies (SOKENDAI)（高级研究院（SOKENDAI））；The University of Electro-Communications（电气通信大学）；Keio University（庆应义塾大学）；Kitami Institute of Technology（北见工业大学）；Nagoya University（名古屋大学）；The University of Tokyo（东京大学）；Osaka Metropolitan University（大阪公立大学）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Kyushu Kyoritsu University（九州桐生大学）；Chalmers University of Technology（查尔姆斯理工大学）；The Institute of Statistical Mathematics（统计数学研究所）
The InfraRed Imaging Spectrograph (IRIS) for TMT: Overview of innovative science programs
IRIS（红外成像光谱仪）是为未来30米望远镜（TMT）设计的第一台轻型近红外衍射极限成像仪和积分场光谱仪。IRIS经过优化，可以在宇宙时间的很大一部分进行天文学研究，从我们的太阳系到遥远的新形成的星系（Barton等人[1]）。我们提出了一系列创新的科学案例，这些案例是IRIS在即将到来的太空和地面望远镜时代所独有的。我们专注于直接成像的系外行星大气的积分场光谱学，探索银河系中心的基础物理，测量10^4到10^10 Msun的超大质量黑洞质量，年轻恒星形成星系（1 < z < 5）和第一轻星系（6 < z < 12）的分辨光谱学，以及强引力透镜源的分辨光谱学来测量暗物质子结构。对于这些科学案例中的每一个，我们都使用IRIS模拟器（Wright et al. [2]，Do et al. [3]）来探索IRIS功能。为了突出独特的IRIS功能，我们还更新了积分场摄谱仪（IFS）在所有五个宽带滤波器（Z，Y，J，H，K）中的点和分辨源灵敏度，以实现每spatial 0.004”的最小空间尺度。我们简要地讨论了未来的发展计划的数据减少管道和快速查看软件的IRIS仪器套件。
MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys
Tsinghua University（清华大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Pengcheng Laboratory（鹏城实验室）；École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
The DSA/Chronoscope fast radio burst survey: forecasts and science overview
Harvard & Smithsonian（哈佛大学与史密森尼学会）；California Institute of Technology（加州理工学院）；The Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Cornell University（康奈尔大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；University of Arizona（亚利桑那大学）；Northwestern University（西北大学）；University of California, Berkeley（加州大学伯克利分校）；Massachusetts Institute of Technology（麻省理工学院）
VAPOLA -- A multi-year, multi-band polarization survey of AGN and Sgr A* at mm wavelengths with ALMA I. Survey Overview and Science-Ready Archival Products
Università degli Studi di Cagliari（卡利亚里大学）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；University of Balearic Islands（巴利阿里群岛大学）；Institute of the Balearic Islands (IAIB)（巴利阿里群岛研究所）；Health Research Institute of the Balearic Islands (IdISBa)（巴利阿里群岛健康研究所）；Universidade São Paulo, Instituto de Astronomia, Geofísica e Ciéencias Atmosféricas（圣保罗大学天文、地球物理与大气科学研究所）；INAF-Istituto di Radioastronomia（意大利国家天体物理研究所射电天文学研究所）；INAF–Italian Centre for Astronomical Archive（意大利天体物理研究所意大利天文档案中心）
Prime Focus Spectrograph on the Subaru Telescope: Overview of Science Operations
National Astronomical Observatory of Japan（日本国立天文台）；Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学）；Subaru Telescope, National Astronomical Observatory of Japan（昴星团望远镜，日本国立天文台）
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）
SVOM/VT: Instrument Overview, Science Objectives, and First-Year Performance
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Xi’an Institute of Optics and Precision Mechanics, Chinese Academy of Sciences（中国科学院西安光学精密机械研究所）
