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Author (up) Astudillo-Defru, N.; Cloutier, R.; Wang, S.X.; Teske, J.; Brahm, R.; Hellier, C.; Ricker, G.; Vanderspek, R.; Latham, D.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Collins, K.A.; Stassun, K.G.; Ziegler, C.; Almenara, J.M.; Anderson, D.R.; Artigau, E.; Bonfils, X.; Bouchy, F.; Briceno, C.; Butler, R.P.; Charbonneau, D.; Conti, D.M.; Crane, J.; Crossfield, I.J.M.; Davies, M.; Delfosse, X.; Diaz, R.F.; Doyon, R.; Dragomir, D.; Eastman, J.D.; Espinoza, N.; Essack, Z.; Feng, F.; Figueira, P.; Forveille, T.; Gan, T.; Glidden, A.; Guerrero, N.; Hart, R.; Henning, T.; Horch, E.P.; Isopi, G.; Jenkins, J.S.; Jordan, A.; Kielkopf, J.F.; Law, N.; Lovis, C.; Mallia, F.; Mann, A.W.; de Medeiros, J.R.; Melo, C.; Mennickent, R.E.; Mignon, L.; Murgas, F.; Nusdeo, D.A.; Pepe, F.; Relles, H.M.; Rose, M.; Santos, N.C.; Segransan, D.; Shectman, S.; Shporer, A.; Smith, J.C.; Torres, P.; Udry, S.; Villasenor, J.; Winters, J.G.; Zhou, G.
Title A hot terrestrial planet orbiting the bright M dwarf L 168-9 unveiled by TESS Type
Year 2020 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 636 Issue Pages 13 pp
Keywords stars: individual L 168-9; planetary systems; stars: late-type; techniques:photometric; techniques: radial velocities
Abstract We report the detection of a transiting super-Earth-sized planet (R = 1.39 +/- 0.09 R-circle plus) in a 1.4-day orbit around L 168-9 (TOI-134), a bright M1V dwarf (V = 11, K = 7.1) located at 25.15 +/- 0.02 pc. The host star was observed in the first sector of the Transiting Exoplanet Survey Satellite (TESS) mission. For confirmation and planet mass measurement purposes, this was followed up with ground-based photometry, seeing-limited and high-resolution imaging, and precise radial velocity (PRV) observations using the HARPS and Magellan/PFS spectrographs. By combining the TESS data and PRV observations, we find the mass of L 168-9 b to be 4.60 +/- 0.56 M-circle plus and thus the bulk density to be 1.74(-0.33)(+0.44) times higher than that of the Earth. The orbital eccentricity is smaller than 0.21 (95% confidence). This planet is a level one candidate for the TESS mission's scientific objective of measuring the masses of 50 small planets, and it is one of the most observationally accessible terrestrial planets for future atmospheric characterization.
Address [Astudillo-Defru, N.] Univ Catolica Santisima Concepcion, Dept Matemat & Fis Aplicadas, Alonso de Rivera 2850, Concepcion, Chile, Email: nastudillo@ucsc.cl
Corporate Author Thesis
Publisher Edp Sciences S A Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 1432-0746 ISBN Medium
Area Expedition Conference
Notes WOS:000528572600001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1144
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Author (up) Leleu, A.; Alibert, Y.; Hara, N.C.; Hooton, M. J.; Wilson, T.G.; Robutel, P.; Delisle, J.B.; Laskar, J .; Hoyer, S.; Lovis, C.; Bryant, E.M.; Ducrot, E.; Cabrera, J.; Delrez, L.; Acton, J.S.; Adibekyan, V.; Allart, R.; Prieto, C.A.; Alonso, R.; Alves, D.; Anderson, D.R.; Angerhausen, D.; Escude, G.A.; Asquier, J.; Barrado, D.; Barros, S.C.C.; Baumjohann, W.; Bayliss, D.; Beck, M.; Beck, T.; Bekkelien, A.; Benz, W.; Billot, N.; Bonfanti, A.; Bonfils, X.; Bouchy, F.; Bourrier, V.; Boue, G.; Brandeker, A.; Broeg, C.; Buder, M.; Burdanov, A.; Burleigh, M.R.; Barczy, T.; Cameron, A.C.; Chamberlain, S.; Charnoz, S.; Cooke, B.F.; Van Damme, C.C.; Correia, A.C.M.; Cristiani, S.; Damasso, M.; Davies, M.B.; Deleuil, M.; Demangeon, O.D.S.; Demory, B.O.; Di Marcantonio, P.; Di Persio, G.; Dumusque, X.; Ehrenreich, D.; Erikson, A.; Figueira, P.; Fortier, A.; Fossati, L.; Fridlund, M.; Futyan, D.; Gandolfi, D.; Munoz, A.G.; Garcia, L.J.; Gill, S.; Osorio, M.R.Z.; Gillen, E.; Gillon, M.; Goad, M.R.; Hernandez, J.I.G.; Guedel, M.; Haldemann, J.; Henderson, B.; Heng, K.; Hogan, A.E.; Isaak, K.; Jehin, E.; Jenkins, J.S.; Jordan, A.; Kiss, L.; Kristiansen, M.H.; Lam, K.; Lavie, B.; des Etangs, A.L.; Lendl, M.; Lillo-Box, J.; Lo Curto, G.; Magrin, D.; Martins, C.J.A.P.; Maxted, P.F.L.; McCormac, J.; Mehner, A.; Micela, G.; Molaro, P.; Moyano, M.; Murray, C.A.; Nascimbeni, V.; Nunes, N.J.; Olofsson, G.; Osborn, H.P.; Oshagh, M.; Ottensamer, R.; Pagano, I.; Palle, E.; Pedersen, P.P.; Pepe, F.A.; Persson, C.M.; Peter, G.; Piotto, G.; Polenta, G.; Pollacco, D.; Poretti, E.; Pozuelos, F.J.; Queloz, D.; Ragazzoni, R.; Rando, N.; Ratti, F.; Rauer, H.; Raynard, L.; Rebolo, R.; Reimers, C.; Ribas, I.; Santos, N.C.; Scandariato, G.; Schneider, J.; Sebastian, D.; Sestovic, M.; Simon, A.E.; Smith, A.M.S.; Sousa, S.G.; Sozzetti, A.; Steller, M.; Mascareno, A.S.; Szabo, G.M.; Segransan, D.; Thomas, N.; Thompson, S.; Tilbrook, R.H.; Triaud, A.; Turner, O.; Udry, S.; Van Grootel, V.; Venus, H.; Verrecchia, F.; Vines, J.I.; Walton, N.A.; West, R.G.; Wheatley, P.J.; Wolter, D.
Title Six transiting planets and a chain of Laplace resonances in TOI-178 Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 649 Issue Pages A26
Abstract Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at the possible presence of a near 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from


1.152-0.070+0.073 to

2.87(-0.13)(+0.14)</textual-form> 2.87-0.13+0.14 Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from

1.02(-0.23)(+0.28)</textual-form> 1.02-0.23+0.28 to

0.177(-0.061)(+0.055)</textual-form> 0.177-0.061+0.055 times the Earth's density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 (H = 8.76 mag, J = 9.37 mag, V = 11.95 mag) allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes.
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6361 ISBN Medium
Area Expedition Conference
Notes WOS:000655036600001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1416
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