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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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2020 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
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Volume |
160 |
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3 |
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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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English |
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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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Nowak, G.; Palle, E.; Gandolfi, D.; Deeg, HJ.; Hirano, T.; Barragan, O.; Kuzuhara, M.; Dai, F.; Luque, R.; Persson, CM.; Fridlund, M.; Johnson, MC.; Korth, J.; Livingston, JH.; Grziwa, S.; Mathur, S.; Hatzes, AP.; Prieto-Arranz, J.; Nespral, D.; Hidalgo, D.; Hjorth, M.; Albrecht, S.; Van Eylen, V.; Lam, KWF.; Cochran, WD.; Esposito, M.; Csizmadia, S.; Guenther, EW.; Kabath, P.; Blay, P.; Brahm, R.; Jordan, A.; Espinoza, N.; Rojas, F.; Barris, NC.; Rodler, F.; Sobrino, RA.; Cabrera, J.; Carleo, I.; Chaushev, A.; de Leon, J.; Eigmuller, P.; Endl, M.; Erikson, A.; Fukui, A.; Georgieva, I.; Gonzalez-Cuesta, L.; Knudstrup, E.; Lund, MN.; Rodriguez, PM.; Murgas, F.; Narita, N.; Niraula, P.; Patzold, M.; Rauer, H.; Redfield, S.; Ribas, I.; Skarka, M.; Smith, AMS.; Subjak, J. |
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Title |
K2-280 b – a low density warm sub-Saturn around a mildly evolved star |
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2020 |
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MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY |
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Mon. Not. Roy. Astron. Soc. |
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497 |
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4 |
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4423-4435 |
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techniques: photometric; techniques: radial velocities; techniques: spectroscopic; planets and satellites: detection; stars: individual: (EPIC 216494238, K2-280) |
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We present an independent discovery and detailed characterization of K2-280 b, a transiting low density warm sub-Saturn in a 19.9-d moderately eccentric orbit (e = 0.35(-0.04)(+0.05)) from K2 campaign 7. A joint analysis of high precision HARPS, HARPS-N, and FIES radial velocity measurements and K2 photometric data indicates that K2-280 b has a radius of R-b = 7.50 +/- 0.44 R-circle plus and a mass of M-b = 37.1 +/- 5.6 M-circle plus, yielding a mean density of rho(b) = 0.48(-0.10)(+0.13) g cm(-3). The host star is a mildly evolved G7 star with an effective temperature of T-eff = 5500 +/- 100 K, a surface gravity of log g(star) = 4.21 +/- 0.05 (cgs), and an iron abundance of [Fe/H] = 0.33 +/- 0.08 dex, and with an inferred mass of M-star = 1.03 +/- 0.03 M-circle dot and a radius of R-star = 1.28 +/- 0.07 R-circle dot. We discuss the importance of K2-280 b for testing formation scenarios of sub-Saturn planets and the current sample of this intriguing group of planets that are absent in the Solar system. |
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0035-8711 |
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UAI @ alexi.delcanto @ |
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1276 |
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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. |
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Title |
TESS Delivers Five New Hot Giant Planets Orbiting Bright Stars from the Full-frame Images |
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Year |
2021 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
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Volume |
161 |
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4 |
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194 |
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Exoplanet astronomy; Exoplanet migration; Exoplanet detection methods; Exoplanets; Transits; Radial velocity; Direct imaging |
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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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WOS:000632893600001 |
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UAI @ alexi.delcanto @ |
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1358 |
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