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Carleo, I.; Gandolfi, D.; Barragan, O.; Livingston, J.H.; Persson, C.M.; Lam, K.W.F.; Vidotto, A.; Lund, M.B.; D'Angelo, C.V.; Collins, K.A.; Fossati, L.; Howard, A.W.; Kubyshkina, D.; Brahm, R.; Oklopcic, A.; Molliere, P.; Redfield, S.; Serrano, L.M.; Dai, F.; Fridlund, M.; Borsa, F.; Korth, J.; Esposito, M.; Diaz, M.R.; Nielsen, L.D.; Hellier, C.; Mathur, S.; Deeg, H.J.; Hatzes, A.P.; Benatti, S.; Rodler, F.; Alarcon, J.; Spina, L.; Santos, A.R.G.; Georgieva, I.; Garcia, R.A.; Gonzalez-Cuesta, L.; Ricker, G.R.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Albrecht, S.; Batalha, N.M.; Beard, C.; Boyd, P.T.; Bouchy, F.; Burt, J.A.; Butler, R.P.; Cabrera, J.; Chontos, A.; Ciardi, D.R.; Cochran, W.D.; Collins, K.I.; Crane, J.D.; Crossfield, I.; Csizmadia, S.; Dragomir, D.; Dressing, C.; Eigmuller, P.; Endl, M.; Erikson, A.; Espinoza, N.; Fausnaugh, M.; Feng, F.B.; Flowers, E.; Fulton, B.; Gonzales, E.J.; Grieves, N.; Grziwa, S.; Guenther, E.W.; Guerrero, N.M.; Henning, T.; Hidalgo, D.; Hirano, T.; Hjorth, M.; Huber, D.; Isaacson, H.; Jones, M.; Jordan, A.; Kabath, P.; Kane, S.R.; Knudstrup, E.; Lubin, J.; Luque, R.; Mireles, I.; Narita, N.; Nespral, D.; Niraula, P.; Nowak, G.; Palle, E.; Patzold, M.; Petigura, E.A.; Prieto-Arranz, J.; Rauer, H.; Robertson, P.; Rose, M.E.; Roy, A.; Sarkis, P.; Schlieder, J.E.; Segransan, D.; Shectman, S.; Skarka, M.; Smith, A.M.S.; Smith, J.C.; Stassun, K.; Teske, J.; Twicken, J.D.; Van Eylen, V.; Wang, S.R.; Weiss, L.M.; Wyttenbach, A. |

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Title |
The Multiplanet System TOI-421* |
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Year |
2020 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
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Volume |
160 |
Issue |
3 |
Pages |
23 pp |
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We report the discovery of a warm Neptune and a hot sub-Neptune transiting TOI-421 (BD-14 1137, TIC 94986319), a bright (V = 9.9) G9 dwarf star in a visual binary system observed by the Transiting Exoplanet Survey Satellite (TESS) space mission in Sectors 5 and 6. We performed ground-based follow-up observations-comprised of Las Cumbres Observatory Global Telescope transit photometry, NIRC2 adaptive optics imaging, and FIbre-fed Echelle Spectrograph, CORALIE, High Accuracy Radial velocity Planet Searcher, High Resolution echelle Spectrometer, and Planet Finder Spectrograph high-precision Doppler measurements-and confirmed the planetary nature of the 16 day transiting candidate announced by the TESS team. We discovered an additional radial velocity signal with a period of five days induced by the presence of a second planet in the system, which we also found to transit its host star. We found that the inner mini-Neptune, TOI-421 b, has an orbital period of P-b = 5.19672 +/- 0.00049 days, a mass of M-b = 7.17 +/- 0.66 M-circle plus, and a radius of R-b = R-circle plus, whereas the outer warm Neptune, TOI-421 c, has a period of P-c = 16.06819 +/- 0.00035 days, a mass of M-c = 16.42(-1.04)(+1.06)M(circle plus), a radius of R-c = 5.09(-0.15)(+0.16)R(circle plus), and a density of rho(c) = 0.685(-0.072)(+0.080) cm(-3). With its characteristics, the outer planet (rho(c) = 0.685(-0.0072)(+0.080) cm(-3)) is placed in the intriguing class of the super-puffy mini-Neptunes. TOI-421 b and TOI-421 c are found to be well-suited for atmospheric characterization. Our atmospheric simulations predict significant Ly alpha transit absorption, due to strong hydrogen escape in both planets, as well as the presence of detectable CH4 in the atmosphere of TOI-421 c if equilibrium chemistry is assumed. |
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[Carleo, Ilaria; Redfield, Seth] Wesleyan Univ, Astron Dept, Middletown, CT 06459 USA, Email: icarleo@wesleyan.edu |
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Iop Publishing Ltd |
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0004-6256 |
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WOS:000561609000001 |
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UAI @ alexi.delcanto @ |
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1254 |
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Espinoza, N.; Brahm, R.; Henning, T.; Jordan, A.; Dorn, C.; Rojas, F.; Sarkis, P.; Kossakowski, D.; Schlecker, M.; Diaz, M.R.; Jenkins, J.S.; Aguilera-Gomez, C.; Jenkins, J.M.; Twicken, J.D.; Collins, K.A.; Lissauer, J.; Armstrong, D.J.; Adibekyan, V.; Barrado, D.; Barros, S.C.C.; Battley, M.; Bayliss, D.; Bouchy, F.; Bryant, E.M.; Cooke, B.F.; Demangeon, O.D.S.; Dumusque, X.; Figueira, P.; Giles, H.; Lillo-Box, J.; Lovis, C.; Nielsen, L.D.; Pepe, F.; Pollaco, D.; Santos, N.C.; Sousa, S.G.; Udry, S.; Wheatley, P.J.; Turner, O.; Marmier, M.; Segransan, D.; Ricker, G.; Latham, D.; Seager, S.; Winn, J.N.; Kielkopf, J.F.; Hart, R.; Wingham, G.; Jensen, E.L.N.; Helminiak, K.G.; Tokovinin, A.; Briceno, C.; Ziegler, C.; Law, N.M.; Mann, A.W.; Daylan, T.; Doty, J.P.; Guerrero, N.; Boyd, P.; Crossfield, I.; Morris, R.L.; Henze, C.E.; Chacon, A.D. |

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Title |
HD 213885b: a transiting 1-d-period super-Earth with an Earth-like composition around a bright (V=7.9) star unveiled by TESS |
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Year |
2020 |
Publication |
Monthly Notices Of The Royal Astronomical Society |
Abbreviated Journal |
Mon. Not. Roy. Astron. Soc. |
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Volume |
491 |
Issue |
2 |
Pages |
2982-2999 |
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techniques: photometric; techniques: radial velocities; planets and satellites: detection; planets and satellites: fundamental parameters; planets and satellites: individual: TOI-141, TIC 403224672, HD213885 |
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We report the discovery of the 1.008-d, ultrashort period (USP) super-EarthHD213885b (TOI141b) orbiting the bright (V= 7.9) star HD 213885 (TOI-141, TIC 403224672), detected using photometry from the recently launched TESS mission. Using FEROS, HARPS, and CORALIE radial velocities, we measure a precise mass of 8.8 +/- 0.6M. for this 1.74 +/- 0.05 R. exoplanet, which provides enough information to constrain its bulk composition – similar to Earth's but enriched in iron. The radius, mass, and stellar irradiation of HD 213885b are, given our data, very similar to 55 Cancri e, making this exoplanet a good target to perform comparative exoplanetology of short period, highly irradiated super-Earths. Our precise radial velocities reveal an additional 4.78-d signal which we interpret as arising from a second, non-transiting planet in the system, HD 213885c, whoseminimum mass of 19.9 +/- 1.4M. makes it consistent with being a Neptune-mass exoplanet. The HD 213885 system is very interesting from the perspective of future atmospheric characterization, being the second brightest star to host an USP transiting super-Earth (with the brightest star being, in fact, 55 Cancri). Prospects for characterization with present and future observatories are discussed. |
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[Espinoza, Nestor] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA, Email: nespinoza@stsci.edu |
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Oxford Univ Press |
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English |
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0035-8711 |
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WOS:000512302100105 |
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UAI @ eduardo.moreno @ |
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1106 |
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Kaye, L.; Vissapragada, S.; Gunther, M.N.; Aigrain, S.; Mikal-Evans, T.; Jensen, E.L.N.; Parviainen, H.; Pozuelos, F.J.; Abe, L.; Acton, J.S.; Agabi, A.; Alves, D.R.; Anderson, D.R.; Armstrong, D.J.; Barkaoui, K.; Barragan, O.; Benneke, B.; Boyd, P.T.; Brahm, R.; Bruni, I.; Bryant, E.M.; Burleigh, M.R.; Casewell, S.L.; Ciardi, D.; Cloutier, R.; Collins, K.A.; Collins, K.I.; Conti, D.M.; Crossfield, I.J.M.; Crouzet, N.; Daylan, T.; Dragomir, D.; Dransfield, G.; Fabrycky, D.; Fausnaugh, M.; Gan, T.J.; Gill, S.; Gillon, M.; Goad, M.R.; Gorjian, V.; Greklek-McKeon, M.; Guerrero, N.; Guillot, T.; Jehin, E.; Jenkins, J.S.; Lendl, M.; Kamler, J.; Kane, S.R.; Kielkopf, J.F.; Kunimoto, M.; Marie-Sainte, W.; McCormac, J.; Mekarnia, D.; Morales, F.Y.; Moyano, M.; Palle, E.; Parmentier, V; Relles, H.M.; Schmider, F.X.; Schwarz, R.P.; Seager, S.; Smith, A.M.S.; Tan, T.G.; Taylor, J.; Triaud, A.H.M.J.; Twicken, J.D.; Udry, S.; Vines, J.I.; Wang, G.; Wheatley, P.J.; Winn, J.N. |

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Title |
Transit timings variations in the three-planet system: TOI-270 |
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Year |
2022 |
Publication |
Monthly Notices Of The Royal Astronomical Society |
Abbreviated Journal |
Mon. Not. Roy. Astron. Soc. |
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Volume |
510 |
Issue |
4 |
Pages |
5464-5485 |
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planets and satellites: composition; planets and satellites: formation; planets and satellites: fundamental parameters |
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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 similar to 10 min and a super-period of similar to 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 M-b = 1.48 +/- 0.18 M-circle plus, M-c = 6.20 +/- 0.31 M-circle plus, and M-d = 4.20 +/- 0.16 M-circle plus for planets b, c, and d, respectively. We also detect small but significant eccentricities for all three planets : e(b) = 0.0167 +/- 0.0084, e(c) = 0.0044 +/- 0.0006, and e(d) = 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. |
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0035-8711 |
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WOS:000764893900001 |
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UAI @ alexi.delcanto @ |
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1552 |
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