THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES
THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES
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DOI：
10.1088/0004-637x/809/1/77
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发表时间：
2015-06
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通讯作者：
P. Sullivan;J. Winn;Z. Berta-Thompson;D. Charbonneau;D. Deming;C. Dressing;D. Latham;A. Levine;P. McCullough;T. Morton;G. Ricker;R. Vanderspek;D. Woods
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作者：
P. Sullivan;J. Winn;Z. Berta-Thompson;D. Charbonneau;D. Deming;C. Dressing;D. Latham;A. Levine;P. McCullough;T. Morton;G. Ricker;R. Vanderspek;D. Woods
凌日系外行星巡天卫星（TESS）是美国国家航空航天局（NASA）资助的一项探索者任务，它将对凌越明亮主恒星的行星进行广域巡天观测。在此，我们预测TESS将探测到的凌星行星的特性，以及产生假阳性光度信号的食双星（EB星）。这些预测基于对附近恒星群体的蒙特卡罗模拟、从开普勒任务得出的行星出现率，以及TESS相机的光度性能和天空覆盖模型。我们预计TESS将从2×10⁵颗预选目标恒星中发现大约1700颗凌星行星。这其中包括556颗半径小于地球两倍的行星，其中419颗由M型矮星承载，137颗由FGK型矮星承载。大约130颗半径为地球半径（R⊕）的行星其主恒星的视星等Ks将亮于9等。大约48颗半径为R⊕的行星位于宜居带（0.2）内或附近；其中有2到7颗这样的行星其主恒星亮于Ks = 9等。我们还预计大约会探测到1100颗半径为2 - 4R⊕的行星，以及67颗半径大于4R⊕的行星。在预选目标恒星之外的恒星周围也能探测到更多半径大于2R⊕的行星，因为TESS还将以30分钟的间隔提供全帧图像。行星探测伴随着1000多个天体物理学假阳性结果。我们讨论了如何利用TESS数据和地基观测来区分假阳性结果和真实行星。我们还讨论了后续观测以测量TESS行星的质量和大气层的前景。
The Transiting Exoplanet Survey Satellite (TESS) is a NASA-sponsored Explorer mission that will perform a wide-field survey for planets that transit bright host stars. Here, we predict the properties of the transiting planets that TESS will detect along with the EB stars that produce false-positive photometric signals. The predictions are based on Monte Carlo simulations of the nearby population of stars, occurrence rates of planets derived from Kepler, and models for the photometric performance and sky coverage of the TESS cameras. We expect that TESS will find approximately 1700 transiting planets from 2 × 10 5 ?> pre-selected target stars. This includes 556 planets smaller than twice the size of Earth, of which 419 are hosted by M dwarf stars and 137 are hosted by FGK dwarfs. Approximately 130 of the R planets will have host stars brighter than K s = 9 ?> . Approximately 48 of the planets with R lie within or near the habitable zone ( 0.2 ); between 2 and 7 such planets have host stars brighter than K s = 9 ?> . We also expect approximately 1100 detections of planets with radii 2–4 R ⨁ ?> , and 67 planets larger than 4 R ⨁ ?> . Additional planets larger than 2 R ⨁ ?> can be detected around stars that are not among the pre-selected target stars, because TESS will also deliver full-frame images at a 30-minute cadence. The planet detections are accompanied by over 1000 astrophysical false positives. We discuss how TESS data and ground-based observations can be used to distinguish the false positives from genuine planets. We also discuss the prospects for follow-up observations to measure the masses and atmospheres of the TESS planets.