Kostov, VB, Powell, BP, Orosz, JA, Welsh, WF, Cochran, W, Collins, KA, Endl, M, Hellier, C, Latham, DW, MacQueen, P, Pepper, J, Quarles, B, Sairam, L, Torres, G, Wilson, RF, Bergeron, S, Boyce, P, Bieryla, A, Buchheim, R, Ben Christiansen, C, Ciardi, DR, Collins, KI, Conti, DM, Dixon, S, Guerra, P, Haghighipour, N, Herman, J, Hintz, EG, Howard, WS, Jensen, ELN, Kielkopf, JF, Kruse, E, Law, NM, Martin, D, Maxted, PFL, Montet, BT, Murgas, F, Nelson, M, Olmschenk, G, Otero, S, Quimby, R, Richmond, M, Schwarz, RP, Shporer, A, Stassun, KG, Stephens, DC, Triaud, AHMJ, Ulowetz, J, Walter, BS, Wiley, E, Wood, D, Yenawine, M, Agol, E, Barclay, T, Beatty, TG, Boisse, I, Caldwell, DA, Christiansen, J, Colon, KD, Deleuil, M, Doyle, L, Fausnaugh, M, Furesz, G, Gilbert, EA, Hebrard, G, James, DJ, Jenkins, J, Kane, SR, Jr, KRC, Kopparapu, R, Li, G, Lissauer, JJ, Lund, MB, Majewski, SR, Mazeh, T, Quinn, SN, Quintana, E, Ricker, G, Rodriguez, JE, Rowe, J, Santerne, A, Schlieder, J, Seager, S, Standing, MR, Stevens, DJ, Ting, EB, Vanderspek, R and Winn, JN (2021) TIC 172900988: A Transiting Circumbinary Planet Detected in One Sector of TESS Data. The Astronomical Journal, 162 (6). ISSN 0004-6256

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We report the first discovery of a transiting circumbinary planet detected from a single sector of Transiting Exoplanet Survey Satellite (TESS) data. During Sector 21, the planet TIC 172900988b transited the primary star and then five days later it transited the secondary star. The binary is itself eclipsing, with a period P ≈ 19.7 days and an eccentricity e ≈ 0.45. Archival data from ASAS-SN, Evryscope, KELT, and SuperWASP reveal a prominent apsidal motion of the binary orbit, caused by the dynamical interactions between the binary and the planet. A comprehensive photodynamical analysis of the TESS, archival and follow-up data yields stellar masses and radii of M1 = 1.2384 ±0.0007 M⊙ and R1 = 1.3827 ± 0.0016 R⊙ for the primary and M2 = 1.2019 ± 0.0007 M⊙ and R2 = 1.3124 ±0.0012 R⊙ for the secondary. The radius of the planet is R3 = 11.25 ± 0.44 R⊕ (1.004 ± 0.039RJup). The planet's mass and orbital properties are not uniquely determined—there are six solutions with nearly equal likelihood. Specifically, we find that the planet's mass is in the range of 824 ≲ M3 ≲ 981 M⊕ (2.65 ≲ M3 ≲ 3.09MJup), its orbital period could be 188.8, 190.4, 194.0, 199.0, 200.4, or 204.1 days, and the eccentricity is between 0.02 and 0.09. At V = 10.141 mag, the system is accessible for high-resolution spectroscopic observations, e.g., the Rossiter–McLaughlin effect and transit spectroscopy.

Item Type: Article
Additional Information: The final version of this accepted manuscript and all relevant information related to it, including copyrights, can be found online via the publisher website via; https://iopscience.iop.org/article/10.3847/1538-3881/ac223a
Subjects: Q Science > Q Science (General)
Q Science > QA Mathematics
Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB799 Stars
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Related URLs:
Depositing User: Symplectic
Date Deposited: 30 Nov 2021 14:35
Last Modified: 10 Nov 2022 01:30
URI: https://eprints.keele.ac.uk/id/eprint/10322

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