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Author 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 (down) 649 Issue Pages A26
Keywords HOT SUPER-EARTHS; TESS INPUT CATALOG; RADIUS DISTRIBUTION; MASS; SYSTEM; MODEL; STARS; MIGRATION; DYNAMICS; TOOL
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)</textual-form>

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.
Address
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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Author Grieves, N.; Nielsen, LD.; Vines, JI.; Bryant, EM.; Gill, S.; Bouchy, F.; Lendl, M.; Bayliss, D.; Eigmueller, P.; Segransan, D.; Acton, JS.; Anderson, DR.; Burleigh, MR.; Casewell, SL.; Chaushev, A.; Cooke, BF.; Gillen, E.; Goad, MR.; Gunther, MN.; Henderson, BA.; Hogan, A.; Jenkins, JS.; Alves, DR.; Jordan, A.; McCormac, J.; Moyano, M.; Queloz, D.; Raynard, L.; Seidel, JV.; Smith, AMS.; Tilbrook, RH.; Udry, S.; West, RG.; Wheatley, PJ.
Title NGTS-13b: a hot 4.8 Jupiter-mass planet transiting a subgiant star Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume (down) 647 Issue Pages A180
Keywords planets and satellites: detection; planets and satellites: individual: NGTS-13b; techniques: photometric; techniques: radial velocities
Abstract We report the discovery of the massive hot Jupiter NGTS-13b by the Next Generation Transit Survey (NGTS). The V = 12.7 host star is likely in the subgiant evolutionary phase with logg(*) = 4.04 +/- 0.05, T-eff = 5819 +/- 73 K, M-* = 1.30(-0.18)(+0.11) M-circle dot, and R-* = 1.79 +/- 0.06 R-circle dot. The NGTS detected a transiting planet with a period of P = 4.12 days around the star, which was later validated with the Transiting Exoplanet Survey Satellite (TESS; TIC 454069765). We confirm the planet using radial velocities from the CORALIE spectrograph. Using NGTS and TESS full-frame image photometry combined with CORALIE radial velocities, we determine NGTS-13b to have a radius of R-P = 1.142 +/- 0.046 R-Jup, a mass of M-P = 4.84 +/- 0.44 M-Jup, and an eccentricity of e = 0.086 +/- 0.034. Previous studies have suggested that similar to 4 M-Jup may be the border separating two formation scenarios (e.g., core accretion and disk instability) and that massive giant planets share similar formation mechanisms as lower-mass brown dwarfs. NGTS-13b is just above 4 M-Jup, making it an important addition to the statistical sample needed to understand the differences between various classes of substellar companions. The high metallicity of NGTS-13, [Fe/H] = 0.25 +/- 0.17, does not support previous suggestions that massive giants are found preferentially around lower metallicity host stars, but NGTS-13b does support findings that more massive and evolved hosts may have a higher occurrence of close-in massive planets than lower-mass unevolved stars.
Address
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 ISBN Medium
Area 0004-6361 Expedition Conference
Notes WOS:000636753900003 Approved
Call Number UAI @ alexi.delcanto @ Serial 1372
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Author Nielsen, L.D.; Brahm, R.; Bouchy, F.; Espinoza, N.; Turner, O.; Rappaport, S.; Pearce, L.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Acton, J.S.; Bakos, G.; Barclay, T.; Barkaoui, K.; Bhatti, W.; Briceno, C.; Bryant, E.M.; Burleigh, M.R.; Ciardi, D.R.; Collins, K.A.; Collins, K.I.; Cooke, B.F.; Csubry, Z.; dos Santos, L.A.; Eigmuller, P.; Fausnaugh, M.M.; Gan, T.; Gillon, M.; Goad, M.R.; Guerrero, N.; Hagelberg, J.; Hart, R.; Henning, T.; Huang, C.X.; Jehin, E.; Jenkins, J.S.; Jordan, A.; Kielkopf, J.F.; Kossakowski, D.; Lavie, B.; Law, N.; Lendl, M.; de Leon, J.P.; Lovis, C.; Mann, A.W.; Marmier, M.; McCormac, J.; Mori, M.; Moyano, M.; Narita, N.; Osip, D.; Otegi, J.F.; Pepe, F.; Pozuelos, F.J.; Raynard, L.; Relles, H.M.; Sarkis, P.; Segransan, D.; Seidel, J.V.; Shporer, A.; Stalport, M.; Stockdale, C.; Suc, V.; Tamura, M.; Tan, T.G.; Tilbrook, R.H.; Ting, E.B.; Trifonov, T.; Udry, S.; Vanderburg, A.; Wheatley, P.J.; Wingham, G.; Zhan, Z.; Ziegler, C.
Title Three short-period Jupiters from TESS: HIP 65Ab, TOI-157b, and TOI-169b Type
Year 2020 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume (down) 639 Issue Pages 17 pp
Keywords planets and satellites: detection; planets and satellites: individual: TOI-129; planets and satellites: individual: HIP 65A; planets and satellites: individual: TOI-157
Abstract We report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V = 11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 +/- 0.078 M-J planet in a grazing transit configuration with an impact parameter of b = 1.17(-0.08)(+0.10) b=1.17-0.08+0.10 . As a result the radius is poorly constrained, 2.03(-0.49)(+0.61)R(J) 2.03-0.49+0.61 RJ . The planet's distance to its host star is less than twice the separation at which it would be destroyed by Roche lobe overflow. It is expected to spiral into HIP 65A on a timescale ranging from 80 Myr to a few gigayears, assuming a reduced tidal dissipation quality factor of Q(s)(') = 10(7) – 10(9) Qs ' =107-109 . We performed a full phase-curve analysis of the TESS data and detected both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass of 1.18 +/- 0.13 M-J and a radius of 1.29 +/- 0.02 R-J. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V = 12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V = 12.4 G-type star. It has a mass of 0.79 +/- 0.06 M-J and a radius of 1.09(-0.05)(+0.08)R(J) 1.09-0.05+0.08<mml:msub>RJ . Despite having the longest orbital period (P = 2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with [Fe / H] ranging from 0.18 to0.24.
Address [Nielsen, L. D.; Bouchy, F.; Turner, O.; dos Santos, L. A.; Hagelberg, J.; Lavie, B.; Lendl, M.; Lovis, C.; Marmier, M.; Otegi, J. F.; Pepe, F.; Segransan, D.; Seidel, J., V; Stalport, M.; Udry, S.] Univ Geneva, Geneva Observ, Chemin Mailettes 51, CH-1290 Versoix, Switzerland, Email: louise.nielsen@unige.ch
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:000554478300001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1215
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Author 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 (down) 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 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.
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 Type
Year 2020 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume (down) 491 Issue 2 Pages 2982-2999
Keywords techniques: photometric; techniques: radial velocities; planets and satellites: detection; planets and satellites: fundamental parameters; planets and satellites: individual: TOI-141, TIC 403224672, HD213885
Abstract 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.
Address [Espinoza, Nestor] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA, Email: nespinoza@stsci.edu
Corporate Author Thesis
Publisher Oxford Univ Press Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0035-8711 ISBN Medium
Area Expedition Conference
Notes WOS:000512302100105 Approved
Call Number UAI @ eduardo.moreno @ Serial 1106
Permanent link to this record
 

 
Author Kossakowski, D.; Espinoza, N.; Brahm, R.; Jordan, A.; Henning, T.; Rojas, F.; Kurster, M.; Sarkis, P.; Schlecker, M.; Pozuelos, F.J.; Barkaoui, K.; Jehin, E.; Gillon, M.; Matthews, E.; Horch, E.P.; Ciardi, D.R.; Crossfield, I.J.M.; Gonzales, E.; Howell, S.B.; Matson, R.; Schlieder, J.; Jenkins, J.; Ricker, G.; Seager, S.; Winn, J.N.; Li, J.; Rose, M.E.; Smith, J.C.; Dynes, S.; Morgan, E.; Villasenor, J.N.; Charbonneau, D.; Jaffe, T.; Yu, L.; Bakos, G.; Bhatti, W.; Bouchy, F.; Collins, K.A.; Collins, K.I.; Csubry, Z.; Evans, P.; Jensen, E.L.N.; Lovis, C.; Marmier, M.; Nielsen, L.D.; Osip, D.; Pepe, F.; Relles, H.M.; Segransan, D.; Shporer, A.; Stockdale, C.; Suc, V.; Turner, O.; Udry, S.
Title TOI-150b and TOI-163b: two transiting hot Jupiters, one eccentric and one inflated, revealed by TESS near and at the edge of the JWST CVZ Type
Year 2019 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume (down) 490 Issue 1 Pages 1094-1110
Keywords techniques: photometric; planets and satellites: detection; stars: individual: HD271181; stars: individual: TIC 179317684; stars: individual: TIC 271893367; stars: individual: TYC9191-519-1
Abstract We present the discovery of TYC9191-519-1b (TOI-150b, TIC 271893367) and HD271181b (TOI-163b, TIC 179317684), two hot Jupiters initially detected using 30-min cadence Transiting Exoplanet Survey Satellite (TESS) photometry from Sector 1 and thoroughly characterized through follow-up photometry (CHAT, Hazelwood, LCO/CTIO, El Sauce, TRAPPIST-S), high-resolution spectroscopy (FEROS, CORALIE), and speckle imaging (Gemini/DSSI), confirming the planetary nature of the two signals. A simultaneous joint fit of photometry and radial velocity using a new fitting package JULIET reveals that TOI-150b is a 1.254 +/- 0.016 R-J, massive (2.61(-0.12)(+0.19) M-J) hot Jupiter in a 5.857-d orbit, while TOI-163b is an inflated (R-P = 1.478(-0.029)(+0.022) R-J, M-P = 1.219 +/- 0.11 M-J) hot Jupiter on a P = 4.231-d orbit; both planets orbit F-type stars. A particularly interesting result is that TOI-150b shows an eccentric orbit (e = 0.262(-0.037)(+0.045)), which is quite uncommon among hot Jupiters. We estimate that this is consistent, however, with the circularization time-scale, which is slightly larger than the age of the system. These two hot Jupiters are both prime candidates for further characterization – in particular, both are excellent candidates for determining spin-orbit alignments via the Rossiter-McLaughlin (RM) effect and for characterizing atmospheric thermal structures using secondary eclipse observations considering they are both located closely to the James Webb Space Telescope (JWST) Continuous Viewing Zone (CVZ).
Address [Kossakowski, Diana; Espinoza, Nestor; Henning, Thomas; Kuerster, Martin; Sarkis, Paula; Schlecker, Martin] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany, Email: kossakowski@mpia.dc
Corporate Author Thesis
Publisher Oxford Univ Press Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0035-8711 ISBN Medium
Area Expedition Conference
Notes WOS:000496922300078 Approved
Call Number UAI @ eduardo.moreno @ Serial 1076
Permanent link to this record
 

 
Author 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.
Title The Multiplanet System TOI-421* Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume (down) 160 Issue 3 Pages 23 pp
Keywords
Abstract 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.
Address [Carleo, Ilaria; Redfield, Seth] Wesleyan Univ, Astron Dept, Middletown, CT 06459 USA, Email: icarleo@wesleyan.edu
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000561609000001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1254
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Author Brahm, R.; Nielsen, L.D.; Wittenmyer, R.A.; Wang, S.H.; Rodriguez, J.E.; Espinoza, N.; Jones, M.I.; Jordan, A.; Henning, T.; Hobson, M.; Kossakowski, D.; Rojas, F.; Sarkis, P.; Schlecker, M.; Trifonov, T.; Shahaf, S.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Addison, B.C.; Bakos, G.A.; Bhatti, W.; Bayliss, D.; Berlind, P.; Bieryla, A.; Bouchy, F.; Bowler, B.P.; Briceno, C.; Brown, T.M.; Bryant, E.M.; Caldwell, D.A.; Charbonneau, D.; Collins, K.A.; Davis, A.B.; Esquerdo, G.A.; Fulton, B.J.; Guerrero, N.M.; Henze, C.E.; Hogan, A.; Horner, J.; Huang, C.X.; Irwin, J.; Kane, S.R.; Kielkopf, J.; Mann, A.W.; Mazeh, T.; McCormac, J.; McCully, C.; Mengel, M.W.; Mireles, I.; Okumura, J.; Plavchan, P.; Quinn, S.N.; Rabus, M.; Saesen, S.; Schlieder, J.E.; Segransan, D.; Shiao, B.; Shporer, A.; Siverd, R.J.; Stassun, K.G.; Suc, V.; Tan, T.G.; Torres, P.; Tinney, C.G.; Udry, S.; Vanzi, L.; Vezie, M.; Vines, J.I.; Vuckovic, M.; Wright, D.J.; Yahalomi, D.A.; Zapata, A.; Zhang, H.; Ziegler, C.
Title TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume (down) 160 Issue 5 Pages 14 pp
Keywords Exoplanet detection methods; Transit photometry; Radial velocity; Exoplanet astronomy
Abstract We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481.b and TOI-892.b have similar radii (0.99.+/-.0.01 R-J and 1.07.+/-.0.02 R-J, respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53.+/-.0.03 MJ versus 0.95.+/-.0.07 MJ, respectively). Both planets orbit metal-rich stars ([Fe H] = + 0.26. 0.05 dex and [Fe H] = +0.24. 0.05 for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a M*=.1.14.+/-.0.02 M., R*=.1.66.+/-.0.02 R. G-type star (T-eff = 5735 +/- 72 K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892 on the other hand, is a F-type dwarf star (T-eff = 6261 +/- 80 K), which has a mass of M*=.1.28.+/-.0.03 M-circle dot and a radius of R*=.1.39.+/-.0.02 R-circle dot. TOI-481.b and TOI-892.b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.
Address [Brahm, Rafael; Jordan, Andres; Suc, Vincent] Univ Adolfo Ibanez, Santiago, Chile, Email: rbrahm@gmail.com
Corporate Author Thesis
Publisher Iop Publishing Ltd Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000584302400001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1263
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