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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 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 Bouma, L.G.; Hartman, J.D.; Brahm, R.; Evans, P.; Collins, K.A.; Zhou, G.; Sarkis, P.; Quinn, S.N.; de Leon, J.; Livingston, J.; Bergmann, C.; Stassun, K.G.; Bhatti, W.; Winn, J.N.; Bakos, G.A.; Abe, L.; Crouzet, N.; Dransfield, G.; Guillot, T.; Marie-Sainte, W.; Mekarnia, D.; Triaud, A.H.M.J.; Tinney, C.G.; Henning, T.; Espinoza, N.; Jordan, A.; Barbieri, M.; Nandakumar, S.; Trifonov, T.; Vines, J.I.; Vuckovic, M.; Ziegler, C.; Law, N.; Mann, A.W.; Ricker, G.R.; Vanderspek, R.; Seager, S.; Jenkins, J.M.; Burke, C.J.; Dragomir, D.; Levine, A.M.; Quintana, E.V.; Rodriguez, J.E.; Smith, J.C.; Wohler, B.
Title Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602 Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 5 Pages 20 pp
Keywords
Abstract We report the discovery of TOI 837b and its validation as a transiting planet. We characterize the system using data from the NASA Transiting Exoplanet Survey Satellite mission, the ESA Gaia mission, ground-based photometry from El Sauce and ASTEP400, and spectroscopy from CHIRON, FEROS, and Veloce. We find that TOI 837 is a T = 9.9 mag G0/F9 dwarf in the southern open cluster IC 2602. The star and planet are therefore 35(-5)(+11) million years old. Combining the transit photometry with a prior on the stellar parameters derived from the cluster color-magnitude diagram, we find that the planet has an orbital period of 8.3 days and is slightly smaller than Jupiter (R-p = 0.77(0.07)(+0.09) R-Jup). From radial velocity monitoring, we limit M-p sin i to less than 1.20 M-Jup (3 sigma). The transits either graze or nearly graze the stellar limb. Grazing transits are a cause for concern, as they are often indicative of astrophysical false-positive scenarios. Our follow-up data show that such scenarios are unlikely. Our combined multicolor photometry, high-resolution imaging, and radial velocities rule out hierarchical eclipsing binary scenarios. Background eclipsing binary scenarios, though limited by speckle imaging, remain a 0.2% possibility. TOI 837b is therefore a validated adolescent exoplanet. The planetary nature of the system can be confirmed or refuted through observations of the stellar obliquity and the planetary mass. Such observations may also improve our understanding of how the physical and orbital properties of exoplanets change in time.
Address [Bouma, L. G.; Hartman, J. D.; Bhatti, W.; Winn, J. N.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08540 USA, Email: luke@astro.princeton.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:000585065500001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1260
Permanent link to this record
 

 
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 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
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 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
Permanent link to this record
 

 
Author Carmichael, T.W.; Quinn, S.N.; Mustill, A.J.; Huang, C.; Zhou, G.; Persson, C.M.; Nielsen, L.D.; Collins, K.A.; Ziegler, C.; Collins, K.I.; Rodriguez, J.E.; Shporer, A.; Brahm, R.; Mann, A.W.; Bouchy, F.; Fridlund, M.; Stassun, K.G.; Hellier, C.; Seidel, J.V.; Stalport, M.; Udry, S.; Pepe, F.; Ireland, M.; Zerjal, M.; Briceno, C.; Law, N.; Jordan, A.; Espinoza, N.; Henning, T.; Sarkis, P.; Latham, D.W.
Title Two Intermediate-mass Transiting Brown Dwarfs from the TESS Mission Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 1 Pages 15 pp
Keywords Brown dwarfs; Radial velocity; Transit photometry; Spectroscopy; Photometry; Substellar companion stars
Abstract We report the discovery of two intermediate-mass transiting brown dwarfs (BDs), TOI-569b and TOI-1406b, from NASA's Transiting Exoplanet Survey Satellite mission. TOI-569b has an orbital period of P = 6.55604 0.00016 days, a mass of M-b = 64.1 1.9 , and a radius of R-b = 0.75 0.02 . Its host star, TOI-569, has a mass of M-star = 1.21 0.05, a radius of R-star = 1.47 0.03 dex, and an effective temperature of T-eff = 5768 110 K. TOI-1406b has an orbital period of P = 10.57415 0.00063 days, a mass of M-b = 46.0 2.7 , and a radius of R-b = 0.86 0.03 . The host star for this BD has a mass of M-star = 1.18 0.09 a radius of R-star = 1.35 0.03 dex, and an effective temperature of T-eff = 6290 100 K. Both BDs are in circular orbits around their host stars and are older than 3 Gyr based on stellar isochrone models of the stars. TOI-569 is one of two slightly evolved stars known to host a transiting BD (the other being KOI-415). TOI-1406b is one of three known transiting BDs to occupy the mass range of 40-50 and one of two to have a circular orbit at a period near 10 days (with the first being KOI-205b). Both BDs have reliable ages from stellar isochrones, in addition to their well-constrained masses and radii, making them particularly valuable as tests for substellar isochrones in the BD mass-radius diagram.
Address [Carmichael, Theron W.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA, Email: tcarmich@cfa.harvard.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:000549117200001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1179
Permanent link to this record
 

 
Author Carone, L.; Molliere, P.; Zhou, YF.; Bouwman, J.; Yan, F.; Baeyens, R.; Apai, D.; Espinoza, N.; Rackham, BV.; Jordan, A.; Angerhausen, D.; Decin, L.; Lendl, M.; Venot, O.; Henning, T.
Title Indications for very high metallicity and absence of methane in the eccentric exo-Saturn WASP-117b Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 646 Issue Pages A168
Keywords methods: observational; planets and satellites: atmospheres
Abstract Aims. We investigate the atmospheric composition of the long-period (P-orb = 10 days) eccentric exo-Saturn WASP-117b. WASP-117b could be similar in atmospheric temperature and chemistry to WASP-107b. In mass and radius, WASP-117b is similar to WASP-39b, which allows a comparative study of these planets.Methods. We analyzed a near-infrared transmission spectrum of WASP-117b taken with the Hubble Space Telescope (HST) WFC3 G141, which was reduced with two independent pipelines. High-resolution measurements were taken with VLT/ESPRESSO in the optical.Results. We report the robust (3 sigma) detection of a water spectral feature. In a 1D atmosphere model with isothermal temperature, uniform cloud deck, and equilibrium chemistry, the Bayesian evidence of a retrieval analysis of the transmission spectrum indicates a preference for a high atmospheric metallicity

[Fe/H] = 2.58(-0.37)(+0.26)

[Fe/H]=2.58-0.37+0.26 and clear skies. The data are also consistent with a lower metallicity composition [Fe/H] < 1.75 and a cloud deck between 10(-2.2) and 10(-5.1) bar, but with weaker Bayesian preference. We retrieve a low CH4 abundance of <10(-4) volume fraction within 1 sigma and <2 x 10(-1) volume fraction within 3<sigma>. We cannot constrain the equilibrium temperature between theoretically imposed limits of 700 and 1000 K. Further observations are needed to confirm quenching of CH4 with K-zz >= 10(8) cm(2) s(-1). We report indications of Na and K in the VLT/ESPRESSO high-resolution spectrum with substantial Bayesian evidence in combination with HST data.
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:000624484900001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1353
Permanent link to this record
 

 
Author Dawson, RI.; Huang, CLX.; Brahm, R.; Collins, KA.; Hobson, MJ.; Jordan, A.; Dong, JY.; Korth, J.; Trifonov, T.; Abe, L.; Agabi, A.; Bruni, I.; Butler, RP.; Barbieri, M.; Collins, KI.; Conti, DM.; Crane, JD.; Crouzet, N.; Dransfield, G.; Evans, P.; Espinoza, N.; Gan, TJ.; Guillot, T.; Henning, T.; Lissauer, JJ.; Jensen, ELN.; Sainte, WM.; Mekarnia, D.; Myers, G.; Nandakumar, S.; Relles, HM.; Sarkis, P.; Torres, P.; Shectman, S.; Schmider, FX.; Shporer, A.; Stockdale, C.; Teske, J.; Triaud, AHMJ.; Wang, SX.; Ziegler, C.; Ricker, G.; Vanderspek, R.; Latham, DW.; Seager, S.; Winn, J.; Jenkins, JM.; Bouma, LG.; Burt, JA.; Charbonneau, D.; Levine, AM.; McDermott, S.; McLean, B.; Rose, ME.; Vanderburg, A.; Wohler, B.
Title Precise Transit and Radial-velocity Characterization of a Resonant Pair: The Warm Jupiter TOI-216c and Eccentric Warm Neptune TOI-216b Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 4 Pages 161
Keywords
Abstract TOI-216 hosts a pair of warm, large exoplanets discovered by the TESS mission. These planets were found to be in or near the 2:1 resonance, and both of them exhibit transit timing variations (TTVs). Precise characterization of the planets' masses and radii, orbital properties, and resonant behavior can test theories for the origins of planets orbiting close to their stars. Previous characterization of the system using the first six sectors of TESS data suffered from a degeneracy between planet mass and orbital eccentricity. Radial-velocity measurements using HARPS, FEROS, and the Planet Finder Spectrograph break that degeneracy, and an expanded TTV baseline from TESS and an ongoing ground-based transit observing campaign increase the precision of the mass and eccentricity measurements. We determine that TOI-216c is a warm Jupiter, TOI-216b is an eccentric warm Neptune, and that they librate in 2:1 resonance with a moderate libration amplitude of deg, a small but significant free eccentricity of for TOI-216b, and a small but significant mutual inclination of 12-39 (95% confidence interval). The libration amplitude, free eccentricity, and mutual inclination imply a disturbance of TOI-216b before or after resonance capture, perhaps by an undetected third planet.
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 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000625759900001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1363
Permanent link to this record
 

 
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 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 Gill, S.; Wheatley, P.J.; Cooke, B.F.; Jordan, A.; Nielsen, L.D.; Bayliss, D.; Anderson, D.R.; Vines, J.I.; Lendl, M.; Acton, J.S.; Armstrong, D.J.; Bouchy, F.; Brahm, R.; Bryant, E.M.; Burleigh, M.R.; Casewell, S.L.; Eigmuller, P.; Espinoza, N.; Gillen, E.; Goad, M.R.; Grieves, N.; Gunther, M.N.; Henning, T.; Hobson, M.J.; Hogan, A.; Jenkins, J.S.; McCormac, J.; Moyano, M.; Osborn, H.P.; Pollacco, D.; Queloz, D.; Rauer, H.; Raynard, L.; Rojas, F.; Sarkis, P.; Smith, A.M.S.; Pinto, M.T.; Tilbrook, R.H.; Udry, S.; Watson, C.A.; West, R.G.
Title NGTS-11 b (TOI-1847 b): A Transiting Warm Saturn Recovered from a TESS Single-transit Event Type
Year 2020 Publication Astrophysical Journal Letters Abbreviated Journal Astrophys. J. Lett.
Volume 898 Issue 1 Pages 6 pp
Keywords
Abstract We report the discovery of NGTS-11 b (=TOI-1847b), a transiting Saturn in a 35.46 day orbit around a mid K-type star (T-eff = 5050 +/- 80 K). We initially identified the system from a single-transit event in a TESS full-frame image light curve. Following 79 nights of photometric monitoring with an NGTS telescope, we observed a second full transit of NGTS-11 b approximately one year after the TESS single-transit event. The NGTS transit confirmed the parameters of the transit signal and restricted the orbital period to a set of 13 discrete periods. We combined our transit detections with precise radial-velocity measurements to determine the true orbital period and measure the mass of the planet. We find NGTS-11 b has a radius of 0.817 +/-(0.028)(0.032) R-Jup, a mass of 0.344 +/-(0.092)(0.073) M-Jup, and an equilibrium temperature of just 435 +/-(34)(32) K, making it one of the coolest known transiting gas giants. NGTS-11 b is the first exoplanet to be discovered after being initially identified as a TESS single-transit event, and its discovery highlights the power of intense photometric monitoring in recovering longer-period transiting exoplanets from single-transit events.
Address [Gill, Samuel; Wheatley, Peter J.; Armstrong, David J.; Bryant, Edward M.; Pollacco, Don] Univ Warwick, Ctr Exoplanets & Habitabil, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England, Email: samuel.gill@warwick.ac.uk
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 2041-8205 ISBN Medium
Area Expedition Conference
Notes WOS:000553513300001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1213
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Author Hartman, J.D.; Jordan, A.; Bayliss, D.; Bakos, G.A.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Henning, T.; Mancini, L.; Penev, K.; Rabus, M.; Sarkis, P.; Suc, V.; de Val-Borro, M.; Zhou, G.; Crane, J.D.; Shectman, S.; Teske, J.K.; Wang, S.X.; Butler, R.P.; Lazar, J.; Papp, I.; Sari, P.; Anderson, D.R.; Hellier, C.; West, R.G.; Barkaoui, K.; Pozuelos, F.J.; Jehin, E.; Gillon, M.; Nielsen, L.; Lendl, M.; Udry, S.; Ricker, G.R.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Christiansen, J.; Crossfield, I.J.M.; Henze, C.E.; Jenkins, J.M.; Smith, J.C.; Ting, E.B.
Title HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b: Four Warm Giant Planets Transiting K Dwarfs Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 159 Issue 4 Pages 23 pp
Keywords Exoplanets; Extrasolar gas giants; Hot Jupiters; Transits
Abstract We report the discovery of four transiting giant planets around K dwarfs. The planets HATS-47b, HATS-48Ab, HATS49b, and HATS-72b have masses of 0.369+ 0.0210.031MJ, 0.243+ 0.0300.022 MJ, 0.353+ 0.0270.038 MJ, and 0.1254. 0.0039 MJ, respectively, and radii of 1.117. 0.014 RJ, 0.800. 0.015 RJ, 0.765. 0.013 RJ, and 0.7224. 0.0032 RJ, respectively. The planets orbit close to their host stars with orbital periods of 3.9228 days, 3.1317 days, 4.1480 days, and 7.3279 days, respectively. The hosts are main-sequence K dwarfs with masses of 0.674+ 0.0120.016.M, 0.7279. 0.0066.M, 0.7133. 0.0075.M, and 0.7311. 0.0028, and with V-band magnitudes of V = 14.829. 0.010, 14.35. 0.11, 14.998. 0.040 and 12.469. 0.010. The super-Neptune HATS-72b (a.k.a. WASP-191b and TOI 294.01) was independently identified as a transiting planet candidate by the HATSouth, WASP, and TESS surveys, and we present a combined analysis of all of the data gathered by each of these projects (and their follow-up programs). An exceptionally precise mass is measured for HATS-72b thanks to high-precision radial velocity (RV) measurements obtained with VLT/ESPRESSO, FEROS, HARPS, and Magellan/PFS. We also incorporate TESS observations of the warm Saturn-hosting systems HATS-47 (a.k.a. TOI.1073.01), HATS-48A, and HATS-49. HATS-47 was independently identified as a candidate by the TESS team, while the other two systems were not previously identified from the TESS data. The RV orbital variations are measured for these systems using Magellan/PFS. HATS-48A has a resolved 5.. 4 neighbor in Gaia.DR2, which is a common-proper-motion binary star companion to HATS-48A with a mass of 0.22.M and a current projected physical separation of similar to 1400 au.
Address [Hartman, J. D.; Bakos, G. A.; Bhatti, W.; Csubry, Z.; Winn, Joshua N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA, Email: jhartman@astro.princeton.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:000522443100001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1155
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Author Jordan, A.; Bakos, G.A.; Bayliss, D.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Hartman, J.D.; Henning, T.; Mancini, L.; Penev, K.; Rabus, M.; Sarkis, P.; Suc, V.; de Val-Borro, M.; Zhou, G.; Butler, R.P.; Teske, J.; Crane, J.; Shectman, S.; Tan, T.G.; Thompson, I.; Wallace, J.J.; Lazar, J.; Papp, I.; Sari, P.
Title HATS-37Ab and HATS-38b: Two Transiting Hot Neptunes in the Desert* Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 5 Pages 14 pp
Keywords Exoplanets; Hot Neptunes
Abstract We report the discovery of two transiting Neptunes by the HATSouth survey. The planet HATS-37Ab has a mass of 0.099 +/- 0.042 MJ (31.5.+/-.13.4M(circle dot)) and a radius of 0.606 +/- 0.016 R-J, and is on a P = 4.3315 day orbit around a V = 12.266 +/- 0.030 mag, 0.843(-0.012)(+0.017)M(circle dot) star with a radius of 0.877(-0.012)(+0.019) R-circle dot We also present evidence that the star HATS-37A has an unresolved stellar companion HATS-37B, with a photometrically estimated mass of 0.654 +/- 0.033.M-circle dot The planet HATS-38b has a mass of 0.074. 0.011MJ (23.5 +/- 3.5M(circle dot)) and a radius of 0.614 +/- 0.017 R-J, and is on a P = 4.3750 day orbit around a V = 12.411 +/- 0.030 mag, 0.890(-0.012)(+0.016) M-circle dot star with a radius of 1.105 +/- 0.016.R-circle dot Both systems appear to be old, with isochrone-based ages of 11.46(-1.45)(+0.79) Gyr, and 11.89 +/- 0.60 Gyr, respectively. Both HATS-37Ab and HATS-38b lie in the Neptune desert and are thus examples of a population with a low occurrence rate. They are also among the lowest-mass planets found from ground-based wide-field surveys to date.
Address [Jordan, A.; Brahm, R.; Suc, V] Univ Adolfo Ibanez, Fac Ingn & Ciencias, Av Diagonal Tones 2640, Santiago, Chile, Email: andres.jordan@uai.cl
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:000584931800001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1261
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Author Jordan, A.; Brahm, R.; Espinoza, N.; Henning, T.; Jones, M.I.; Kossakowski, D.; Sarkis, P.; Trifonov, T.; Rojas, F.; Torres, P.; Drass, H.; Nandakumar, S.; Barbieri, M.; Davis, A.; Wang, S.H.; Bayliss, D.; Bouma, L.; Dragomir, D.; Eastman, J.D.; Daylan, T.; Guerrero, N.; Barclay, T.; Ting, E.B.; Henze, C.E.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.; Jenkins, J.M.; Wittenmyer, R.A.; Bowler, B.P.; Crossfield, I.; Horner, J.; Kane, S.R.; Kielkopf, J.F.; Morton, T.D.; Plavchan, P.; Tinney, C.G.; Addison, B.; Mengel, M.W.; Okumura, J.; Shahaf, S.; Mazeh, T.; Rabus, M.; Shporer, A.; Ziegler, C.; Mann, A.W.; Hart, R.
Title TOI-677b: A Warm Jupiter (P=11.2 days) on an Eccentric Orbit Transiting a Late F-type Star Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 159 Issue 4 Pages 10 pp
Keywords Exoplanets; Extrasolar gas giants; Exoplanet astronomy; Transit photometry; Radial velocity; Planet hosting stars
Abstract We report the discovery of TOI-677.b, first identified as a candidate in light curves obtained within Sectors 9 and 10 of the Transiting Exoplanet Survey Satellite (TESS) mission and confirmed with radial velocities. TOI-677.b has a mass of M-p = 1.236(-0.067)(+0.069) M-J, a radius of R-P = 1.170 +/- 0.03 R-J, and orbits its bright host star (V=.9.8 mag) with an orbital period of 11.23660 +/- 0.00011 d, on an eccentric orbit with e = 0.435 +/- 0.024. The host star has a mass of M-star = 1.181 +/- 0.058 M-circle dot, a radius of R. = 1.28(-0.03)(+0.03) R-circle dot, an age of 2.92(-0.73)(+0.80) Gyr and solar metallicity, properties consistent with a main-sequence late-F star with T-eff = 6295 +/- 77 K. We find evidence in the radial velocity measurements of a secondary long-term signal, which could be due to an outer companion. The TOI-677.b system is a well-suited target for Rossiter-Mclaughlin observations that can constrain migration mechanisms of close-in giant planets.
Address [Jordan, Andres] Univ Adolfo Ibanez, Fac Ingn & Ciencias, Ave Diagonal Torres 2640, Santiago, Chile
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:000521218500001 Approved
Call Number UAI @ eduardo.moreno @ Serial 1129
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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 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
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Author Lendl, M.; Bouchy, F.; Gill, S.; Nielsen, L.D.; Turner, O.; Stassun, K.; Acton, J.S.; Anderson, D.R.; Armstrong, D.J.; Bayliss, D.; Belardi, C.; Bryant, E.M.; Burleigh, M.R.; Chaushev, A.; Casewell, S.L.; Cooke, B.F.; Eigmuller, P.; Gillen, E.; Goad, M.R.; Gunther, M.N.; Hagelberg, J.; Jenkins, J.S.; Louden, T.; Marmier, M.; McCormac, J.; Moyano, M.; Pollacco, D.; Raynard, L.; Tilbrook, R.H.; Udry, S.; Vines, J.I.; West, R.G.; Wheatley, P.J.; Ricker, G.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.; Jenkins, J.M.; Addison, B.; Briceno, C.; Brahm, R.; Caldwell, D.A.; Doty, J.; Espinoza, N.; Goeke, B.; Henning, T.; Jordan, A.; Krishnamurthy, A.; Law, N.; Morris, R.; Okumura, J.; Mann, A.W.; Rodriguez, J.E.; Sarkis, P.; Schlieder, J.; Twicken, J.D.; Villanueva, S.; Wittenmyer, R.A.; Wright, D.J.; Ziegler, C.
Title TOI-222: a single-transit TESS candidate revealed to be a 34-d eclipsing binary with CORALIE, EulerCam, and NGTS Type
Year 2020 Publication Monthly Notices Of The Royal Astronomical Society Abbreviated Journal Mon. Not. Roy. Astron. Soc.
Volume 492 Issue 2 Pages 1761-1769
Keywords techniques: photometric; stars: individual: TOI-222; planetary systems
Abstract We report the period, eccentricity, and mass determination for the Transiting Exoplanet Survey Satellite (TESS) single-transit event candidate TOI-222, which displayed a single 3000 ppm transit in the TESS 2-min cadence data from Sector 2. We determine the orbital period via radial velocity measurements (P = 33.9 d), which allowed for ground-based photometric detection of two subsequent transits. Our data show that the companion to TOI-222 is a low-mass star, with a radius of 0.18(-0.10)(+0.39) R-circle dot and a mass of 0.23 +/- 0.01 M-circle dot. This discovery showcases the ability to efficiently discover long-period systems from TESS single-transit events using a combination of radial velocity monitoring coupled with high-precision ground-based photometry.
Address [Lendl, Monika; Bouchy, Francois; Nielsen, Louise D.; Turner, Oliver; Hagelberg, Janis; Marmier, Maxime; Udry, Stephane] Univ Geneva, Observ Geneve, 51 Ch Maillettes, CH-1290 Sauverny, Switzerland, Email: monika.lendl@unige.ch
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:000512297600016 Approved
Call Number UAI @ eduardo.moreno @ Serial 1107
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Author Mancini, L.; Sarkis, P.; Henning, T.; Bakos, G.A.; Bayliss, D.; Bento, J.; Bhatti, W.; Brahm, R.; Csubry, Z.; Espinoza, N.; Hartman, J.; Jordan, A.; Penev, K.; Rabus, M.; Suc, V.; de Val-Borro, M.; Zhou, G.; Chen, G.; Damasso, M.; Southworth, J.; Tan, T.G.
Title The highly inflated giant planet WASP-174b Type
Year 2020 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 633 Issue Pages 12 pp
Keywords planetary systems; stars: fundamental parameters; stars: individual: WASP-174; techniques: photometric; techniques: radial velocities; methods: data analysis
Abstract Context. The transiting exoplanetary system WASP-174 was reported to be composed by a main-sequence F star (V = 11.8 mag) and a giant planet, WASP-174b (orbital period P-orb = 4.23 days). However only an upper limit was placed on the planet mass (<1.3 M-Jup), and a highly uncertain planetary radius (0.7-1.7 R-Jup) was determined.Aims. We aim to better characterise both the star and the planet and precisely measure their orbital and physical parameters.Methods. In order to constrain the mass of the planet, we obtained new measurements of the radial velocity of the star and joined them with those from the discovery paper. Photometric data from the HATSouth survey and new multi-band, high-quality (precision reached up to 0.37 mmag) photometric follow-up observations of transit events were acquired and analysed for getting accurate photometric parameters. We fit the model to all the observations, including data from the TESS space telescope, in two different modes: incorporating the stellar isochrones into the fit, and using an empirical method to get the stellar parameters. The two modes resulted to be consistent with each other to within 2<sigma>.Results. We confirm the grazing nature of the WASP-174b transits with a confidence level greater than 5 sigma, which is also corroborated by simultaneously observing the transit through four optical bands and noting how the transit depth changes due to the limb-darkening effect. We estimate that approximate to 76% of the disk of the planet actually eclipses the parent star at mid-transit of its transit events. We find that WASP-174b is a highly-inflated hot giant planet with a mass of M-p = 0.330 +/- 0.091 M-Jup and a radius of R-p = 1.435 +/- 0.050 R-Jup, and is therefore a good target for transmission-spectroscopy observations. With a density of rho (p) = 0.135 +/- 0.042 g cm(-3), it is amongst the lowest-density planets ever discovered with precisely measured mass and radius.
Address [Mancini, L.] Univ Roma Tor Vergata, Dept Phys, Via Ric Sci 1, I-00133 Rome, Italy, Email: lmancini@roma2.infn.it
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:000505741300005 Approved
Call Number UAI @ eduardo.moreno @ Serial 1093
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Author Mireles, I.; Shporer, A.; Grieves, N.; Zhou, G.; Gunther, M.N.; Brahm, R.; Ziegler, C.; Stassun, K.G.; Huang, C.X.; Nielsen, L.; dos Santos, L.A.; Udry, S.; Bouchy, F.; Ireland, M.; Wallace, A.; Sarkis, P.; Henning, T.; Jordan, A.; Law, N.; Mann, A.W.; Paredes, L.A.; James, H.S.; Jao, W.C.; Henry, T.J.; Butler, R.P.; Rodriguez, J.E.; Yu, L.; Flowers, E.; Ricker, G.R.; Latham, D.W.; Vanderspek, R.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Furesz, G.; Hesse, K.; Quintana, E.V.; Rose, M.E.; Smith, J.C.; Tenenbaum, P.; Vezie, M.; Yahalomi, D.A.; Zhan, Z.C.
Title TOI 694b and TIC 220568520b: Two Low-mass Companions near the Hydrogen-burning Mass Limit Orbiting Sun-like Stars Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 3 Pages 13 pp
Keywords Low mass stars; M dwarf stars; Eclipsing binary stars
Abstract We report the discovery of TOI 694 b and TIC 220568520 b, two low-mass stellar companions in eccentric orbits around metal-rich Sun-like stars, first detected by the Transiting Exoplanet Survey Satellite (TESS). TOI 694 b has an orbital period of 48.05131 +/- 0.00019 days and eccentricity of 0.51946 +/- 0.00081, and we derive a mass of 89.0 +/- 5.3 M-Jup (0.0849 +/- 0.0051 M-circle dot) and radius of 1.111 +/- 0.017 R-Jup (0.1142 +/- 0.0017 R-circle dot). TIC 220568520 b has an orbital period of 18.55769 +/- 0.00039 days and eccentricity of 0.0964 +/- 0.0032, and we derive a mass of 107.2 +/- 5.2 M-Jup (0.1023 +/- 0.0050 M-circle dot) and radius of 1.248 +/- 0.018 R-Jup (0.1282 +/- 0.0019 R-circle dot). Both binary companions lie close to and above the hydrogen-burning mass threshold that separates brown dwarfs and the lowest-mass stars, with TOI 694 b being 2s above the canonical mass threshold of 0.075 M-circle dot. The relatively long periods of the systems mean that the magnetic fields of the low-mass companions are not expected to inhibit convection and inflate the radius, which according to one leading theory is common in similar objects residing in short-period tidally synchronized binary systems. Indeed we do not find radius inflation for these two objects when compared to theoretical isochrones. These two new objects add to the short but growing list of low-mass stars with well-measured masses and radii, and highlight the potential of the TESS mission for detecting such rare objects orbiting bright stars.
Address [Mireles, Ismael; Shporer, Avi; Guenther, Maximilian N.; Huang, Chelsea X.; Yu, Liang; Ricker, George R.; Vanderspek, Roland; Seager, Sara; Furesz, Gabor] MIT, Dept Phys, Cambridge, MA 02139 USA
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:000565724400001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1253
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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 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 Rodriguez, JE.; Quinn, SN.; Zhou, G.; Vanderburg, A.; Nielsen, LD.; Wittenmyer, RA.; Brahm, R.; Reed, PA.; Huang, CLX.; Vach, S.; Ciardi, DR.; Oelkers, RJ.; Stassun, KG.; Hellier, C.; Gaudi, BS.; Eastman, JD.; Collins, KA.; Bieryla, A.; Christian, S.; Latham, DW.; Carleo, I.; Wright, DJ.; Matthews, E.; Gonzales, EJ.; Ziegler, C.; Dressing, CD.; Howell, SB.; Tan, TG.; Wittrock, J.; Plavchan, P.; McLeod, KK.; Baker, D.; Wang, GV.; Radford, DJ.; Schwarz, RP.; Esposito, M.; Ricker, GR.; Vanderspek, RK.; Seager, S.; Winn, JN.; Jenkins, JM.; Addison, B.; Anderson, DR.; Barclay, T.; Beatty, TG.; Berlind, P.; Bouchy, F.; Bowen, M.; Bowler, BP.; Brasseur, CE.; Briceno, C.; Caldwell, DA.; Calkins, ML.; Cartwright, S.; Chaturvedi, P.; Chaverot, G.; Chimaladinne, S.; Christiansen, JL.; Collins, KI.; Crossfield, IJM.; Eastridge, K.; Espinoza, N.; Esquerdo, GA.; Feliz, DL.; Fenske, T.; Fong, W.; Gan, TJ.; Giacalone, S.; Gill, H.; Gordon, L.; Granados, A.; Grieves, N.; Guenther, EW.; Guerrero, N.; Henning, T.; Henze, CE.; Hesse, K.; Hobson, MJ.; Horner, J.; James, DJ.; Jensen, ELN.; Jimenez, M.; Jordan, A.; Kane, SR.; Kielkopf, J.; Kim, K.; Kuhn, RB.; Latouf, N.; Law, NM.; Levine, AM.; Lund, MB.; Mann, AW.; Mao, SD.; Matson, RA.; Mengel, MW.; Mink, J.; Newman, P.; O'Dwyer, T.; Okumura, J.; Palle, E.; Pepper, J.; Quintana, EV.; Sarkis, P.; Savel, AB.; Schlieder, JE.; Schnaible, C.; Shporer, A.; Sefako, R.; Seidel, JV.; Siverd, RJ.; Skinner, B.; Stalport, M.; Stevens, DJ.; Stibbards, C.; Tinney, CG.; West, RG.; Yahalomi, DA.; Zhang, H.
Title TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 4 Pages 194
Keywords Exoplanet astronomy; Exoplanet migration; Exoplanet detection methods; Exoplanets; Transits; Radial velocity; Direct imaging
Abstract We present the discovery and characterization of five hot and warm Jupiters-TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b ( TIC 139375960)-based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size (R-P = 1.01-1.77 R-J) and have masses that range from 0.85 to 6.33 M-J. The host stars of these systems have F and G spectral types (5595 <= T-eff <= 6460 K) and are all relatively bright (9.5 < V < 10.8, 8.2 < K < 9.3), making them well suited for future detailed characterization efforts. Three of the systems in our sample (TOI-640 b, TOI-1333 b, and TOI-1601 b) orbit subgiant host stars (log g < 4.1). TOI-640 b is one of only three known hot Jupiters to have a highly inflated radius (R-P > 1.7 R-J, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of 6.31(-0.30)(+) (0.28) M-J and a statistically significant, nonzero orbital eccentricity of e = 0.074(-0.022)(+) (0.021). This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA's TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals.
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Notes WOS:000632893600001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1358
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Author Schlecker, M.; Kossakowski, D.; Brahm, R.; Espinoza, N.; Henning, T.; Carone, L.; Molaverdikhani, K.; Trifonov, T.; Molliere, P.; Hobson, MJ.; Jordan, A.; Rojas, FI.; Klahr, H.; Sarkis, P.; Bakos, GA.; Bhatti, W.; Osip, D.; Suc, V.; Ricker, G.; Vanderspek, R.; Latham, DW.; Seager, S.; Winn, JN.; Jenkins, JM.; Vezie, M.; Villasenor, JN.; Rose, ME.; Rodriguez, DR.; Rodriguez, JE.; Quinn, SN.; Shporer, A.
Title A highly eccentric warm jupiter orbiting TIC 237913194 Type
Year 2020 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 160 Issue 6 Pages 275
Keywords Exoplanet astronomy; Transit photometry; Radial velocity; Exoplanet dynamics; Exoplanet atmospheres; Exoplanet structure; Hot Jupiters; Extrasolar gas giants
Abstract The orbital parameters of warm Jupiters serve as a record of their formation history, providing constraints on formation scenarios for giant planets on close and intermediate orbits. Here, we report the discovery of TIC.237913194b, detected in full-frame images from Sectors 1 and 2 of the Transiting Exoplanet Survey Satellite (TESS), ground-based photometry (Chilean-Hungarian Automated Telescope, Las Cumbres Observatory Global Telescope), and Fiber-fed Extended Range Optical Spectrograph radial velocity time series. We constrain its mass to M-P = 1.942(-0.091)(+0.091) M-J and its radius to R-P = 1.117(-0.047)(+0.054) R-J, implying a bulk density similar to Neptune's. It orbits a G-type star (M-* = 1.026(-0.055)(+0.057) M-circle dot, V = 12.1 mag) with a period of 15.17 days on one of the most eccentric orbits of all known warm giants (e approximate to 0.58). This extreme dynamical state points to a past interaction with an additional, undetected massive companion. A tidal evolution analysis showed a large tidal dissipation timescale, suggesting that the planet is not a progenitor for a hot Jupiter caught during its high-eccentricity migration. TIC.237913194b further represents an attractive opportunity to study the energy deposition and redistribution in the atmosphere of a warm Jupiter with high eccentricity.
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Call Number UAI @ alexi.delcanto @ Serial 1286
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Author Sha, LZ.; Huang, CLX.; Shporer, A.; Rodriguez, JE.; Vanderburg, A.; Brahm, R.; Hagelberg, J.; Matthews, EC.; Ziegler, C.; Livingston, JH.; Stassun, KG.; Wright, DJ.; Crane, JD.; Espinoza, N.; Bouchy, F.; Bakos, GA.; Collins, KA.; Zhou, GR.; Bieryla, A.; Hartman, JD.; Wittenmyer, RA.; Nielsen, LD.; Plavchan, P.; Bayliss, D.; Sarkis, P.; Tan, TG.; Cloutier, R.; Mancini, L.; Jordan, A.; Wang, SR.; Henning, T.; Narita, N.; Penev, K.; Teske, JK.; Kane, SR.; Mann, AW.; Addison, BC.; Tamura, M.; Horner, J.; Barbieri, M.; Burt, JA.; Diaz, MR.; Crossfield, IJM.; Dragomir, D.; Drass, H.; Feinstein, AD.; Zhang, H.; Hart, R.; Kielkopf, JF.; Jensen, ELN.; Montet, BT.; Ottoni, G.; Schwarz, RP.; Rojas, F.; Nespral, D.; Torres, P.; Mengel, MW.; Udry, S.; Zapata, A.; Snoddy, E.; Okumura, J.; Ricker, GR.; Vanderspek, RK.; Latham, DW.; Winn, JN.; Seager, S.; Jenkins, JM.; Colon, KD.; Henze, CE.; Krishnamurthy, A.; Ting, EB.; Vezie, M.; Villanueva, S.
Title TOI-954 b and K2-329 b: Short-period Saturn-mass Planets that Test whether Irradiation Leads to Inflation Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 161 Issue 2 Pages 82
Keywords STARS; 1ST; ALGORITHM; RADIUS; HOST; NAOS; RICH
Abstract We report the discovery of two short-period Saturn-mass planets, one transiting the G subgiant TOI-954 (TIC 44792534, V = 10.343, T = 9.78) observed in TESS sectors 4 and 5 and one transiting the G dwarf K2-329 (EPIC 246193072, V = 12.70, K = 10.67) observed in K2 campaigns 12 and 19. We confirm and characterize these two planets with a variety of ground-based archival and follow-up observations, including photometry, reconnaissance spectroscopy, precise radial velocity, and high-resolution imaging. Combining all available data, we find that TOI-954 b has a radius of 0.852(-0.062)(+0.053) R-J and a mass of 0.174(-0.017)(+0.018) M-J and is in a 3.68 day orbit, while K2-329 b has a radius of 0.774(-0.024)(+0.026) R-J and a mass if 0.260(-0.022)(+0.020) M-J and is in a 12.46 day orbit. As TOI-954 b is 30 times more irradiated than K2-329 b but more or less the same size, these two planets provide an opportunity to test whether irradiation leads to inflation of Saturn-mass planets and contribute to future comparative studies that explore Saturn-mass planets at contrasting points in their lifetimes.
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Call Number UAI @ alexi.delcanto @ Serial 1327
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