Advanced Technology Large-Aperture Space Telescope (ATLAST): A Technology Roadmap for the Next Decade
Marc Postman, Vic Argabright, Bill Arnold, David Aronstein, Paul Atcheson, Morley Blouke, Tom Brown, Daniela Calzetti, Webster Cash, Mark Clampin, Dave Content,… 展开作者
Marc Postman, Vic Argabright, Bill Arnold, David Aronstein, Paul Atcheson, Morley Blouke, Tom Brown, Daniela Calzetti, Webster Cash, Mark Clampin, Dave Content, Dean Dailey, Rolf Danner, Rodger Doxsey, Dennis Ebbets, Peter Eisenhardt, Lee Feinberg, Andrew Fruchter, Mauro Giavalisco, Tiffany Glassman, Qian Gong, James Green, John Grunsfeld, Ted Gull, Greg Hickey, Randall Hopkins, John Hraba, Tupper Hyde, Ian Jordan, Jeremy Kasdin, Steve Kendrick, Steve Kilston, Anton Koekemoer, Bob Korechoff, John Krist, John Mather, Chuck Lillie, Amy Lo, Rick Lyon, Peter McCullough, Gary Mosier, Matt Mountain, Bill Oegerle, Bert Pasquale, Lloyd Purves, Cecelia Penera, Ron Polidan, Dave Redding, Kailash Sahu, Babak Saif, Ken Sembach, Mike Shull, Scott Smith, George Sonneborn, David Spergel, Phil Stahl, Karl Stapelfeldt, Harley Thronson, Gary Thronton, Jackie Townsend, Wesley Traub, Steve Unwin, Jeff Valenti, Robert Vanderbei, Michael Werner, Richard Wesenberg, Jennifer Wiseman, Bruce Woodgate
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22 pages, RFI submitted to Astro2010 Decadal Committee
The Advanced Technology Large-Aperture Space Telescope (ATLAST) is a set of mission concepts for the next generation of UVOIR space observatory with a primary aperture diameter in the 8-m to 16-m range that will allow us to perform some of the most challenging observations to answer some of our most compelling questions, including "Is there life elsewhere in the Galaxy?" We have identified two different telescope architectures, but with similar optical designs, that span the range in viable technologies. The architectures are a telescope with a monolithic primary mirror and two variations of a telescope with a large segmented primary mirror. This approach provides us with several pathways to realizing the mission, which will be narrowed to one as our technology development progresses. The concepts invoke heritage from HST and JWST design, but also take significant departures from these designs to minimize complexity, mass, or both.
Our report provides details on the mission concepts, shows the extraordinary scientific progress they would enable, and describes the most important technology development items. These are the mirrors, the detectors, and the high-contrast imaging technologies, whether internal to the observatory, or using an external occulter. Experience with JWST has shown that determined competitors, motivated by the development contracts and flight opportunities of the new observatory, are capable of achieving huge advances in technical and operational performance while keeping construction costs on the same scale as prior great 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）
Expanding the Horizon of Black Hole Imaging with AtLAST
Heriot-Watt University（赫瑞-瓦特大学）；University of Naples Federico II（那不勒斯费德里科二世大学）；MSSL, University College London（伦敦大学学院太空与气候物理研究所）；Yamaguchi University（山口大学）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）；Nagoya City University（名古屋市立大学）；Massachusetts Institute of Technology Haystack Observatory（麻省理工学院海斯塔克观测站）；Niigata University（新潟大学）；Instituto de Astrofísica de Andalucía, IAA-CSIC（安达卢西亚天体物理研究所）；University of Lancashire（兰开夏大学）
Simulation-based dynamic pointing analysis of AtLAST under wind loading and fast-scan conditions
OHB Digital Connect（OHB数字连接）；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））；Institute of Theoretical Astrophysics, University of Oslo（奥斯陆大学理论天体物理研究所）
Characterization of sensitivity and responses of a 2-element prototype wavefront sensor for millimeter-wave adaptive optics attached to the Nobeyama 45 m telescope
我们报告的结果的原型波前传感器的性能表征毫米自适应光学（MAO）安装在Nobeyama 45米射电望远镜。微弧氧化是实现未来大口径亚毫米波望远镜的关键部件，如大型亚毫米波望远镜（LST）或阿塔卡玛大口径亚毫米波望远镜（AtLAST）。然而，微弧氧化的困难在于，在孔径上以~10 μ m的精度实时感测波前变形。我们的波前传感器工作在20 GHz的测量主镜表面的某个位置到放置20 GHz相干接收器的焦点之间的无线电路径长度。与2元件的原型，我们采样的两个位置上的主镜表面（在半径为5米和16米）在10 Hz的采样率。然后，通过对两个光路进行微分，得到两个位置之间的多余光程长度（EPL）。EPL的功率谱密度示出三个分量：低频漂移（1/f^n）、振荡和白噪声。比较了不同风况下的EPL测量结果，发现前两种现象可能是由望远镜结构的风荷载引起的。白噪声的功率对应于EPL测量中8 μ m的1西格玛统计误差。8 um r.m.s.对于LST和AtLAST所需的镜面精度（~20-40 μ m r.m.s.）而言是重要的，这表明，我们的技术也是有用的，为未来的大口径亚毫米望远镜。
Photonic Integrated Circuits for the Habitable Worlds Observatory: Science Drivers, Material Platforms, Arrayed-Waveguide Spectrographs, and a Space-Qualification Roadmap
Leibniz Institute for Astrophysics Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）
PROVIDENCE: a ground station for space observation
ONERA – The French Aerospace Lab（法国航空航天实验室）；LAM, Laboratoire d'Astrophysique de Marseille（马赛天体物理学实验室）；OHP, Observatoire de Haute-Provence（上普罗旺斯天文台）；EMBASE；BETEM；TMT Observatory（三十米望远镜天文台）；Rubin Observatory（鲁宾天文台）；Iridescence-group（Iridescence小组）
