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Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1

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posted on 2017-02-24, 12:21 authored by Michaël Gillon, Amaury H. M. J. Triaud, Brice-Olivier Demory, Emmanuël Jehin, Eric Agol, Katherine M. Deck, Susan M. Lederer, Julien de Wit, Artem Burdanov, James G. Ingalls, Emeline Bolmont, Jeremy Leconte, Sean N. Raymond, Franck Selsis, Martin Turbet, Khalid Barkaoui, Adam Burgasser, Matthew R. Burleigh, Sean J. Carey, Aleksander Chaushev, Chris M. Copperwheat, Laetitia Delrez, Catarina S. Fernandes, Daniel L. Holdsworth, Enrico J. Kotze, Valérie Van Grootel, Yaseen Almleaky, Zouhair Benkhaldoun, Pierre Magain, Didier Queloz
One aim of modern astronomy is to detect temperate, Earth-like exoplanets that are well suited for atmospheric characterization. Recently, three Earth-sized planets were detected that transit (that is, pass in front of) a star with a mass just eight per cent that of the Sun, located 12 parsecs away 1. The transiting configuration of these planets, combined with the Jupiter-like size of their host star—named TRAPPIST-1—makes possible in-depth studies of their atmospheric properties with present-day and future astronomical facilities 1, 2, 3. Here we report the results of a photometric monitoring campaign of that star from the ground and space. Our observations reveal that at least seven planets with sizes and masses similar to those of Earth revolve around TRAPPIST-1. The six inner planets form a near-resonant chain, such that their orbital periods (1.51, 2.42, 4.04, 6.06, 9.1 and 12.35 days) are near-ratios of small integers. This architecture suggests that the planets formed farther from the star and migrated inwards 4, 5. Moreover, the seven planets have equilibrium temperatures low enough to make possible the presence of liquid water on their surfaces 6, 7, 8.



Nature, 2017, 542(5), pp. 456-460

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/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy


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The conversion of the ut times of the photometric measurements to the BJDTDB system was performed using the online program created by J. Eastman and distributed at utc2bjd.html. The MCMC software used to analyse the photometric data is a custom Fortran 90 code that can be obtained from M.G. on reasonable request. The n-body integration codes TTVFast, TTVFaster, and Mercury are freely available online at, TTVFaster, and To realize Fig. 2a, we relied on TEPCAT, an online catalogue of transiting planets maintained by J. Southworth (;The Spitzer data that support our findings are available from the Spitzer Heritage Archive database ( Source Data for Fig. 1 and Extended Data Figs 1, 2, 3, 4 are available online. The other datasets generated and/or analysed during the present study are available from M.G. on reasonable request.;The file associated with this record is under embargo until 6 months after publication, in accordance with the publisher's self-archiving policy. The full text may be available through the publisher links provided above.



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