Transit timings variations in the three-planet system: TOI-270

Laurel Kaye, Shreyas Vissapragada, Maximilian N. Günther, Suzanne Aigrain, Thomas Mikal-Evans, Eric L.N. Jensen, Hannu Parviainen, Francisco J. Pozuelos, Lyu Abe, Jack S. Acton, Abdelkrim Agabi, Douglas R. Alves, David R. Anderson, David J. Armstrong, Khalid Barkaoui, Oscar Barragán, Björn Benneke, Patricia T. Boyd, Rafael Brahm, Ivan BruniEdward M. Bryant, Matthew R. Burleigh, Sarah L. Casewell, David Ciardi, Ryan Cloutier, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J.M. Crossfield, Nicolas Crouzet, Tansu Daylan, Diana Dragomir, Georgina Dransfield, Daniel Fabrycky, Michael Fausnaugh, Gábor Fuurész, Tianjun Gan, Samuel Gill, Michaël Gillon, Michael R. Goad, Varoujan Gorjian, Michael Greklek-Mckeon, Natalia Guerrero, Tristan Guillot, Emmanuël Jehin, J. S. Jenkins, Monika Lendl, Jacob Kamler, Stephen R. Kane, John F. Kielkopf, Michelle Kunimoto, Wenceslas Marie-Sainte, James Mccormac, Djamel Mékarnia, Farisa Y. Morales, Maximiliano Moyano, Enric Palle, Vivien Parmentier, Howard M. Relles, François Xavier Schmider, Richard P. Schwarz, S. Seager, Alexis M.S. Smith, Thiam Guan Tan, Jake Taylor, Amaury H.M.J. Triaud, Joseph D. Twicken, Stephane Udry, J. I. Vines, Gavin Wang, Peter J. Wheatley, Joshua N. Winn

Research output: Contribution to journalArticlepeer-review

4 Scopus citations

Abstract

We present ground- and space-based photometric observations of TOI-270 (L231-32), a system of three transiting planets consisting of one super-Earth and two sub-Neptunes discovered by TESS around a bright (K-mag = 8.25) M3V dwarf. The planets orbit near low-order mean-motion resonances (5:3 and 2:1) and are thus expected to exhibit large transit timing variations (TTVs). Following an extensive observing campaign using eight different observatories between 2018 and 2020, we now report a clear detection of TTVs for planets c and d, with amplitudes of ∼10 min and a super-period of ∼3 yr, as well as significantly refined estimates of the radii and mean orbital periods of all three planets. Dynamical modelling of the TTVs alone puts strong constraints on the mass ratio of planets c and d and on their eccentricities. When incorporating recently published constraints from radial velocity observations, we obtain masses of Mb=1.48± 0.18, M⊕, Mc=6.20± 0.31, M⊕, and Md=4.20± 0.16, M⊕ for planets b, c, and d, respectively. We also detect small but significant eccentricities for all three planets: eb = 0.0167 ± 0.0084, ec = 0.0044 ± 0.0006, and ed = 0.0066 ± 0.0020. Our findings imply an Earth-like rocky composition for the inner planet, and Earth-like cores with an additional He/H2O atmosphere for the outer two. TOI-270 is now one of the best constrained systems of small transiting planets, and it remains an excellent target for atmospheric characterization.

Original languageEnglish
Pages (from-to)5464-5485
Number of pages22
JournalMonthly Notices of the Royal Astronomical Society
Volume510
Issue number4
DOIs
StatePublished - 1 Mar 2022
Externally publishedYes

Keywords

  • planets and satellites: composition
  • planets and satellites: formation
  • planets and satellites: fundamental parameters

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