H. Rauer, C. Catala, C. Aerts, T. Appourchaux, W. Benz, A. Brandeker, J. Christensen-Dalsgaard, M. Deleuil, L. Gizon, M. -J. Goupil, M. Güdel, E. Janot-Pacheco,… 展开作者
H. Rauer, C. Catala, C. Aerts, T. Appourchaux, W. Benz, A. Brandeker, J. Christensen-Dalsgaard, M. Deleuil, L. Gizon, M. -J. Goupil, M. Güdel, E. Janot-Pacheco, M. Mas-Hesse, I. Pagano, G. Piotto, D. Pollacco, N. C. Santos, A. Smith, J. -C., Suárez, R. Szabó, S. Udry, V. Adibekyan, Y. Alibert, J. -M. Almenara, P. Amaro-Seoane, M. Ammler-von Eiff, M. Asplund, E. Antonello, W. Ball, S. Barnes, F. Baudin, K. Belkacem, M. Bergemann, G. Bihain, A. C. Birch, X. Bonfils, I. Boisse, A. S. Bonomo, F. Borsa, I. M. Brandão, E. Brocato, S. Brun, M. Burleigh, R. Burston, J. Cabrera, S. Cassisi, W. Chaplin, S. Charpinet, C. Chiappini, R. P. Church, Sz. Csizmadia, M. Cunha, M. Damasso, M. B. Davies, H. J. Deeg, R. F. DÍaz, S. Dreizler, C. Dreyer, P. Eggenberger, D. Ehrenreich, P. Eigmüller, A. Erikson, R. Farmer, S. Feltzing, F. de Oliveira Fialho, P. Figueira, T. Forveille, M. Fridlund, R. A. García, P. Giommi, G. Giuffrida, M. Godolt, J. Gomes da Silva, T. Granzer, J. L. Grenfell, A. Grotsch-Noels, E. Günther, C. A. Haswell, A. P. Hatzes, G. Hébrard, S. Hekker, R. Helled, K. Heng, J. M. Jenkins, A. Johansen, M. L. Khodachenko, K. G. Kislyakova, W. Kley, U. Kolb, N. Krivova, F. Kupka, H. Lammer, A. F. Lanza, Y. Lebreton, D. Magrin, P. Marcos-Arenal, P. M. Marrese, J. P. Marques, J. Martins, S. Mathis, S. Mathur, S. Messina, A. Miglio, J. Montalban, M. Montalto, M. J. P. F. G. Monteiro, H. Moradi, E. Moravveji, C. Mordasini, T. Morel, A. Mortier, V. Nascimbeni, R. P. Nelson, M. B. Nielsen, L. Noack, A. J. Norton, A. Ofir, M. Oshagh, R. -M. Ouazzani, P. Pápics, V. C. Parro, P. Petit, B. Plez, E. Poretti, A. Quirrenbach, R. Ragazzoni, G. Raimondo, M. Rainer, D. R. Reese, R. Redmer, S. Reffert, B. Rojas-Ayala, I. W. Roxburgh, S. Salmon, A. Santerne, J. Schneider, J. Schou, S. Schuh, H. Schunker, A. Silva-Valio, R. Silvotti, I. Skillen, I. Snellen, F. Sohl, S. G. Sousa, A. Sozzetti, D. Stello, K. G. Strassmeier, M. Švanda, Gy. M. Szabó, A. Tkachenko, D. Valencia, V. van Grootel, S. D. Vauclair, P. Ventura, F. W. Wagner, N. A. Walton, J. Weingrill, S. C. Werner, P. J. Wheatley, K. Zwintz
备注：
63 pages, 17 figures, submitted to Experimental Astronomy (ExA)
PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture telescopes (32 with 25 sec readout cadence and 2 with 2.5 sec candence) providing a wide field-of-view (2232 deg2) and a large photometric magnitude range (4-16 mag). It focusses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to Earth-size by photometric transits, whose masses can then be determined by ground-based radial-velocity follow-up measurements. Asteroseismology will be performed for these bright stars to obtain highly accurate stellar parameters, including masses and ages. The combination of bright targets and asteroseismology results in high accuracy for the bulk planet parameters: 2%, 4-10% and 10% for planet radii, masses and ages, respectively. The planned baseline observing strategy includes two long pointings (2-3 years) to detect and bulk characterize planets reaching into the habitable zone (HZ) of solar-like stars and an additional step-and-stare phase to cover in total about 50% of the sky. PLATO 2.0 will observe up to 1,000,000 stars and detect and characterize hundreds of small planets, and thousands of planets in the Neptune to gas giant regime out to the HZ. It will therefore provide the first large-scale catalogue of bulk characterized planets with accurate radii, masses, mean densities and ages. This catalogue will include terrestrial planets at intermediate orbital distances, where surface temperatures are moderate. Coverage of this parameter range with statistical numbers of bulk characterized planets is unique to PLATO 2.0.
PlatoSim: An end-to-end PLATO camera simulator for modelling high-precision space-based photometry
KU Leuven（荷语鲁汶大学）；German Aerospace Center（德国航空航天中心）；Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CNRS（巴黎天文台、巴黎文理研究大学、索邦大学、巴黎西岱大学、法国国家科学研究中心）
Performance of AutoRegressive Planet Search methodology on simulated PLATO lightcurves
Penn State University（宾夕法尼亚州立大学）；Università di Padova（帕多瓦大学）；INAF, Osservatorio Astronomico di Padova（意大利国家天体物理研究所，帕多瓦天文台）；INAF, Osservatorio Astrofisico di Catania（意大利国家天体物理研究所，卡塔尼亚天文台）；University of Oxford（牛津大学）
Following up the Kepler field with PLATO: Transit Timing Performance
University of Warwick（华威大学）；Centre for Exoplanets and Habitability, University of Warwick（华威大学系外行星与宜居性中心）；Centre for Space Domain Awareness, University of Warwick（华威大学太空领域感知中心）；LIRA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS（巴黎天文台、PSL大学、索邦大学、巴黎西岱大学、CY塞尔吉巴黎大学、法国国家科学研究中心LIRA实验室）；Institute for Astronomy, KU Leuven（荷语鲁汶大学天文学研究所）；Isaac Newton Group of Telescopes（艾萨克·牛顿望远镜组）
Characterising transiting exoplanets at long orbital period: lessons learned for PLATO from 10 years of monitoring the HIP41378 system
Univ. Grenoble Alpes（格勒诺布尔阿尔卑斯大学）；CNRS（法国国家科学研究中心）；IPAG（天体物理学与行星学研究所）；Aix Marseille Univ（艾克斯-马赛大学）；CNES（法国国家空间研究中心）；LAM（拉奥朗实验室）；Department of Astronomy, University of Geneva（日内瓦大学天文系）
Assessing PLATO's Discovery Potential across Different Observing Strategies
University of Warwick（华威大学）；Isaac Newton Group of Telescopes（艾萨克·牛顿望远镜组）；University of British Columbia（不列颠哥伦比亚大学）；Institute of Space Research, German Aerospace Center (DLR)（德国航空航天中心空间研究所）；Freie Universitaet Berlin（柏林自由大学）；Observatoire astronomique de l’Université de Genève（日内瓦大学天文台）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯马赛大学、法国国家科学研究中心、法国国家空间研究中心）
The PLATO field selection process III. Selection of the Prime Sample for the LOPS2 field
INAF – Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Centro di Ateneo di Studi e Attività Spaziali “Giuseppe Colombo” (CISAS), Università degli Studi di Padova（帕多瓦大学空间研究与活动中心（CISAS））；Dipartimento di Fisica e Astronomia “Galileo Galilei”, Università degli Studi di Padova（帕多瓦大学伽利略·伽利雷物理与天文系）；INAF – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；SSDC-ASI（ASI SSDC）；INAF – Osservatorio Astrofisico di Catania（意大利国家天体物理研究所卡塔尼亚天文台）；Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institut für Weltraumforschung（德国航空航天中心空间研究所）
Outer Solar System Exploration: A Compelling and Unified Dual Mission Decadal Strategy for Exploring Uranus, Neptune, Triton, Dwarf Planets, and Small KBOs and Centaurs
PLATO input catalogs for technical calibration and fine guidance
Max Planck Institute for Solar System Research（马克斯·普朗克太阳系统研究所）；Freie Universität Berlin（柏林自由大学）；Università degli Studi di Padova（帕多瓦大学）；Osservatorio Astronomico di Padova, Istituto Nazionale di Astrofisica（帕多瓦天文台，意大利国家天体物理研究所）；Institute of Space Research, German Aerospace Center（德国航空航天中心空间研究所）；Italian National Institute of Astrophysics（意大利国家天体物理研究所）
Exoplanet Orbital Distribution around FGK Sun-like Host Stars I: planet occurrence rate derived from the Kepler Mission and theoretical interpretations from planet formation
University of Oslo（奥斯陆大学）；Harvard University（哈佛大学）；Natural History Museum, University of Oslo（奥斯陆大学自然历史博物馆）；Konkoly Observatory, HUN-REN CSFK（孔科利天文台，匈牙利研究网络科学院）
The PLATO Input Catalogue of targets (tPIC) for the first Long Pointing Field
Istituto Nazionale di Astrofisica – Osservatorio Astrofisico di Catania（意大利国家天体物理研究所-卡塔尼亚天文台）；Dipartimento di Fisica e Astronomia “Galileo Galilei”, Università degli Studi di Padova（帕多瓦大学伽利略·伽利雷物理与天文系）；Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Padova（意大利国家天体物理研究所-帕多瓦天文台）；Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Roma（意大利国家天体物理研究所-罗马天文台）；Space Science Data Center - ASI（ASI空间数据中心）；Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Palermo（意大利国家天体物理研究所-巴勒莫天文台）；Centro di Ateneo di Studi e Attività Spaziali “Giuseppe Colombo” (CISAS), Università degli Studi di Padova（帕多瓦大学朱塞佩·科洛莫太空研究与活动中心）；Deutsches Zentrum für Luft- und Raumfahrt (DLR)（德国航空航天中心）
Institut für Weltraumforschung, Deutsches Zentrum für Luft- und Raumfahrt（德国航空航天中心空间研究所）；Deutsches Zentrum für Luft- und Raumfahrt（德国航空航天中心）；Institut für Geologische Wissenschaften, Freie Universität Berlin（柏林自由大学地质科学研究所）；LIRA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Diderot, Sorbonne Paris Cité（巴黎天文台、巴黎文理研究大学、法国国家科学研究中心、索邦大学、巴黎第七大学、巴黎西岱大学联合实验室）；INAF, Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Centro di Ateneo di Studi e Attività Spaziali “Giuseppe Colombo” (CISAS), Università degli Studi di Padova（帕多瓦大学“朱塞佩·科洛姆博”太空研究与活动中心）；ESTEC, European Space Agency（欧洲空间局欧洲空间研究与技术中心）
Theoretical Reflectance Spectra of Earth-Like Planets through Their Evolutions: Impact of Clouds on the Detectability of Oxygen, Water, and Methane with Future Direct Imaging Missions
