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

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 away1. 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 facilities1,2,3. 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 inwards4,5. Moreover, the seven planets have equilibrium temperatures low enough to make possible the presence of liquid water on their surfaces6,7,8.

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Space Sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Allée du 6 Août 19C, Bat. B5C, Liège, 4000, BelgiumMichaël Gillon, Emmanuël Jehin, Artem Burdanov, Laetitia Delrez, Catarina S. Fernandes, Valérie Van Grootel & Pierre Magain

Space Sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Allée du 6 Août 19C, Bat. B5C, Liège, 4000, Belgium

Michaël Gillon, Emmanuël Jehin, Artem Burdanov, Laetitia Delrez, Catarina S. Fernandes, Valérie Van Grootel & Pierre Magain

Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UKAmaury H. M. J. Triaud

Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK

Amaury H. M. J. Triaud

University of Bern, Center for Space and Habitability, Sidlerstrasse 5, Bern, CH-3012, SwitzerlandBrice-Olivier Demory

University of Bern, Center for Space and Habitability, Sidlerstrasse 5, Bern, CH-3012, Switzerland

Cavendish Laboratory, JJ Thomson Avenue, Cambridge, CB3 0HE, UKBrice-Olivier Demory, Laetitia Delrez & Didier Queloz

Cavendish Laboratory, JJ Thomson Avenue, Cambridge, CB3 0HE, UK

Brice-Olivier Demory, Laetitia Delrez & Didier Queloz

Astronomy Department, University of Washington, Seattle, 98195, Washington, USAEric Agol

Astronomy Department, University of Washington, Seattle, 98195, Washington, USA

NASA Astrobiology Institute’s Virtual Planetary Laboratory, Seattle, 98195, Washington, USAEric Agol

NASA Astrobiology Institute’s Virtual Planetary Laboratory, Seattle, 98195, Washington, USA

Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, 91125, California, USAKatherine M. Deck

Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, 91125, California, USA

NASA Johnson Space Center, 2101 NASA Parkway, Houston, 77058, Texas, USASusan M. Lederer

NASA Johnson Space Center, 2101 NASA Parkway, Houston, 77058, Texas, USA

Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, 02139, Massachusetts, USAJulien de Wit

Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, 02139, Massachusetts, USA

Spitzer Science Center, California Institute of Technology, 1200 E California Boulevard, Mail Code 314-6, Pasadena, 91125, California, USAJames G. Ingalls & Sean J. Carey

Spitzer Science Center, California Institute of Technology, 1200 E California Boulevard, Mail Code 314-6, Pasadena, 91125, California, USA

James G. Ingalls & Sean J. Carey

Department of Mathematics, NaXys, University of Namur, 8 Rempart de la Vierge, Namur, 5000, BelgiumEmeline Bolmont

Department of Mathematics, NaXys, University of Namur, 8 Rempart de la Vierge, Namur, 5000, Belgium

Laboratoire AIM Paris-Saclay, CEA/DRF–CNRS–Univ. Paris Diderot - IRFU/SAp, Centre de Saclay, Gif-sur-Yvette, F- 91191, Cedex, FranceEmeline Bolmont

Laboratoire AIM Paris-Saclay, CEA/DRF–CNRS–Univ. Paris Diderot - IRFU/SAp, Centre de Saclay, Gif-sur-Yvette, F- 91191, Cedex, France

Laboratoire d'astrophysique de Bordeaux, Université Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, F-33615, FranceJeremy Leconte, Sean N. Raymond & Franck Selsis

Laboratoire d'astrophysique de Bordeaux, Université Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, F-33615, France

Jeremy Leconte, Sean N. Raymond & Franck Selsis

Laboratoire de Météorologie Dynamique, Sorbonne Universités, UPMC Univ Paris 06, CNRS, 4 Place Jussieu, Paris, 75005, FranceMartin Turbet

Laboratoire de Météorologie Dynamique, Sorbonne Universités, UPMC Univ Paris 06, CNRS, 4 Place Jussieu, Paris, 75005, France

Laboratoire LPHEA, Oukaimeden Observatory, Cadi Ayyad University/FSSM, Marrakesh, BP 2390, MoroccoKhalid Barkaoui & Zouhair Benkhaldoun

Laboratoire LPHEA, Oukaimeden Observatory, Cadi Ayyad University/FSSM, Marrakesh, BP 2390, Morocco

Khalid Barkaoui & Zouhair Benkhaldoun

Center for Astrophysics and Space Science, University of California San Diego, La Jolla, 92093, California, USAAdam Burgasser

Center for Astrophysics and Space Science, University of California San Diego, La Jolla, 92093, California, USA

Department of Physics and Astronomy, Leicester Institute for Space and Earth Observation, University of Leicester, Leicester, LE1 7RH, UKMatthew R. Burleigh & Aleksander Chaushev

Department of Physics and Astronomy, Leicester Institute for Space and Earth Observation, University of Leicester, Leicester, LE1 7RH, UK

Matthew R. Burleigh & Aleksander Chaushev

Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, UKChris M. Copperwheat

Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, UK

Jeremiah Horrocks Institute, University of Central Lancashire, Preston, PR1 2HE, UKDaniel L. Holdsworth

Jeremiah Horrocks Institute, University of Central Lancashire, Preston, PR1 2HE, UK

South African Astronomical Observatory, PO Box 9, Observatory, 7935, South AfricaEnrico J. Kotze

South African Astronomical Observatory, PO Box 9, Observatory, 7935, South Africa

Space and Astronomy Department, Faculty of Science, King Abdulaziz University, Jeddah, 21589, Saudi ArabiaYaseen Almleaky

Space and Astronomy Department, Faculty of Science, King Abdulaziz University, Jeddah, 21589, Saudi Arabia

King Abdullah Centre for Crescent Observations and Astronomy, Makkah Clock, Mecca, 24231, Saudi ArabiaYaseen Almleaky

King Abdullah Centre for Crescent Observations and Astronomy, Makkah Clock, Mecca, 24231, Saudi Arabia

Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, CH-1290 Sauverny, SwitzerlandDidier Queloz

Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, CH-1290 Sauverny, Switzerland

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M.G. leads the ultracool dwarf transit survey that uses the TRAPPIST telescope and led the photometric follow-up of the star TRAPPIST-1; he also planned and analysed most of the observations, led their scientific exploitation, and wrote most of the manuscript. A.H.M.J.T. led the observational campaign using the La Palma telescopes (the Liverpool Telescope, LT, and William Herschel Telescope, WHT). C.M.C. managed the scheduling of the LT observations, and Ar.B. performed the photometric analysis of the resulting LT and WHT images. B.-O.D. led the TTV/dynamical simulations. E.A. and K.M.D. performed independent analyses of the transit timings. J.G.I. and S.J.C. helped to optimize the Spitzer observations. B.-O.D., J.G.I. and J.d.W. performed independent analyses of the Spitzer data. M.G., E.J., L.D., Ar.B., P.M., K.B., Y.A. and Z.B. performed the TRAPPIST observations and their analysis. S.M.L. obtained the director’s discretionary time on UKIRT, and, with E.J., managed the preparation of the UKIRT observations. M.T., J.L., F.S., E.B. and S.N.R. carried out atmospheric modelling for the planets and worked on the theoretical interpretation of their properties. V.V.G. managed the SAAO observations performed by C.S.F., M.R.B., D.L.H., A.C. and E.J.K. All co-authors assisted with writing the manuscript. A.H.M.J.T. prepared most of the figures.

Correspondence to

Michaël Gillon.

The authors declare no competing financial interests.

Reviewer Information Nature thanks D. Deming and I. Snellen for their contribution to the peer review of this work.

Extended data figures and tables

Extended Data Figure 1 Light curve of a triple transit of planets c, e and f.

The black points show the differential photometric measurements extracted from VLT/HAWK-I images taken on 11 December 2015, with the formal 1σ errors shown as vertical lines. The best-fit triple-transit model is shown as a red line. Possible configurations of the planets relative to the stellar disc are shown below the light curve for three different times (red, planet c; yellow, planet e; green, planet f). The relative positions and sizes of the planets, as well as the impact parameters, correspond to the values in Table 1.

Extended Data Figure 2 Transit light curve for planets d and e.

The black points show the photometric measurements, binned per 0.005 days (7.2 min). The error for each bin (shown as a vertical line) was computed as the 1σ error on the average. These light curves are divided by their best-fit instrumental models and by the best-fit transit models of other planets (for multiple transits). The best-fit transit models are shown as solid lines. The light curves are period-folded on the best-fit transit ephemeris given in Table 1, their relative shifts on the x-axis reflecting TTVs due to planet–planet interactions (see text). The epoch of the transit and the facility used to observe it are indicated above each light curve.

Extended Data Figure 3 Transit light curves for planets f and g.

As for Extended Data Fig. 2, but for planets f and g.

Extended Data Figure 4 TTVs measured for planets b, c, d, e, f and g.

For each planet, the best-fit TTV model computed with the n-body numerical integration code Mercury52 is shown as a red line. The 1 σ errors of the transit timing measurements are shown as vertical lines.

PowerPoint slide for Fig. 1 (download PPT )

PowerPoint slide for Fig. 2 (download PPT )

Source data to Fig. 1 (download XLSX )

Source data to Extended Data Fig. 2 (download XLSX )

Source data to Extended Data Fig. 3 (download XLSX )

Source data to Extended Data Fig. 4 (download XLSX )

Source data to Extended Data Fig. 5 (download XLSX )

Gillon, M., Triaud, A., Demory, BO. et al. Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1.

Nature 542, 456–460 (2017). https://doi.org/10.1038/nature21360

Received: 21 November 2016

Received: 21 November 2016

Accepted: 21 December 2016

Accepted: 21 December 2016

Published: 23 February 2017

Published: 23 February 2017

Issue date: 23 February 2017

Issue date: 23 February 2017

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