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Carleo, I.; Gandolfi, D.; Barragan, O.; Livingston, J.H.; Persson, C.M.; Lam, K.W.F.; Vidotto, A.; Lund, M.B.; D'Angelo, C.V.; Collins, K.A.; Fossati, L.; Howard, A.W.; Kubyshkina, D.; Brahm, R.; Oklopcic, A.; Molliere, P.; Redfield, S.; Serrano, L.M.; Dai, F.; Fridlund, M.; Borsa, F.; Korth, J.; Esposito, M.; Diaz, M.R.; Nielsen, L.D.; Hellier, C.; Mathur, S.; Deeg, H.J.; Hatzes, A.P.; Benatti, S.; Rodler, F.; Alarcon, J.; Spina, L.; Santos, A.R.G.; Georgieva, I.; Garcia, R.A.; Gonzalez-Cuesta, L.; Ricker, G.R.; Vanderspek, R.; Latham, D.W.; Seager, S.; Winn, J.N.; Jenkins, J.M.; Albrecht, S.; Batalha, N.M.; Beard, C.; Boyd, P.T.; Bouchy, F.; Burt, J.A.; Butler, R.P.; Cabrera, J.; Chontos, A.; Ciardi, D.R.; Cochran, W.D.; Collins, K.I.; Crane, J.D.; Crossfield, I.; Csizmadia, S.; Dragomir, D.; Dressing, C.; Eigmuller, P.; Endl, M.; Erikson, A.; Espinoza, N.; Fausnaugh, M.; Feng, F.B.; Flowers, E.; Fulton, B.; Gonzales, E.J.; Grieves, N.; Grziwa, S.; Guenther, E.W.; Guerrero, N.M.; Henning, T.; Hidalgo, D.; Hirano, T.; Hjorth, M.; Huber, D.; Isaacson, H.; Jones, M.; Jordan, A.; Kabath, P.; Kane, S.R.; Knudstrup, E.; Lubin, J.; Luque, R.; Mireles, I.; Narita, N.; Nespral, D.; Niraula, P.; Nowak, G.; Palle, E.; Patzold, M.; Petigura, E.A.; Prieto-Arranz, J.; Rauer, H.; Robertson, P.; Rose, M.E.; Roy, A.; Sarkis, P.; Schlieder, J.E.; Segransan, D.; Shectman, S.; Skarka, M.; Smith, A.M.S.; Smith, J.C.; Stassun, K.; Teske, J.; Twicken, J.D.; Van Eylen, V.; Wang, S.R.; Weiss, L.M.; Wyttenbach, A. |
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Title |
The Multiplanet System TOI-421* |
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Year |
2020 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
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Volume |
160 |
Issue |
3 |
Pages |
23 pp |
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We report the discovery of a warm Neptune and a hot sub-Neptune transiting TOI-421 (BD-14 1137, TIC 94986319), a bright (V = 9.9) G9 dwarf star in a visual binary system observed by the Transiting Exoplanet Survey Satellite (TESS) space mission in Sectors 5 and 6. We performed ground-based follow-up observations-comprised of Las Cumbres Observatory Global Telescope transit photometry, NIRC2 adaptive optics imaging, and FIbre-fed Echelle Spectrograph, CORALIE, High Accuracy Radial velocity Planet Searcher, High Resolution echelle Spectrometer, and Planet Finder Spectrograph high-precision Doppler measurements-and confirmed the planetary nature of the 16 day transiting candidate announced by the TESS team. We discovered an additional radial velocity signal with a period of five days induced by the presence of a second planet in the system, which we also found to transit its host star. We found that the inner mini-Neptune, TOI-421 b, has an orbital period of P-b = 5.19672 +/- 0.00049 days, a mass of M-b = 7.17 +/- 0.66 M-circle plus, and a radius of R-b = R-circle plus, whereas the outer warm Neptune, TOI-421 c, has a period of P-c = 16.06819 +/- 0.00035 days, a mass of M-c = 16.42(-1.04)(+1.06)M(circle plus), a radius of R-c = 5.09(-0.15)(+0.16)R(circle plus), and a density of rho(c) = 0.685(-0.072)(+0.080) cm(-3). With its characteristics, the outer planet (rho(c) = 0.685(-0.0072)(+0.080) cm(-3)) is placed in the intriguing class of the super-puffy mini-Neptunes. TOI-421 b and TOI-421 c are found to be well-suited for atmospheric characterization. Our atmospheric simulations predict significant Ly alpha transit absorption, due to strong hydrogen escape in both planets, as well as the presence of detectable CH4 in the atmosphere of TOI-421 c if equilibrium chemistry is assumed. |
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[Carleo, Ilaria; Redfield, Seth] Wesleyan Univ, Astron Dept, Middletown, CT 06459 USA, Email: icarleo@wesleyan.edu |
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Iop Publishing Ltd |
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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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Eberhardt, J.; Trifonov, T.; Kurster, M.; Stock, S.; Henning, T.; Wollbold, A.; Reffert, S.; Lee, M.H.; Zechmeister, M.; Rodler, F.; Zakhozhay, O.; Heeren, P.; Gandolfi, D.; Barragan, O.; Pinto, M.T.; Wolthoff, V.; Sarkis, P.; Brems, S.S. |
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Title |
Dynamical Architecture of the HD 107148 Planetary System |
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Year |
2022 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
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Volume |
163 |
Issue |
5 |
Pages |
198 |
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Keywords |
LOMB-SCARGLE PERIODOGRAM; EXTRA-SOLAR PLANETS; RADIAL-VELOCITIES; ORBITAL SOLUTIONS; CARMENES SEARCH; M DWARFS; COMPANIONS; PRECISION; STARS; EXOPLANETS |
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We present an independent Doppler validation and dynamical orbital analysis of the two-planet system HD 107148, which was recently announced in Rosenthal et al. Our detailed analyses are based on literature HIRES data and newly obtained HARPS and CARMENES radial-velocity (RV) measurements as part of our survey in search for additional planets around single-planet systems. We perform a periodogram analysis of the available HIRES and HARPS precise RVs and stellar activity indicators. We do not find any apparent correlation between the RV measurements and the stellar activity indicators, thus linking the two strong periodicities to a moderately compact multiplanet system. We carry out orbital fitting analysis by testing various one- and two-planet orbital configurations and studying the posterior probability distribution of the fitted parameters. Our results solidify the existence of a Saturn-mass planet (HD 107148b, discovered first) with a period of P (b) similar to 77.2 days and a second, eccentric (e (c) similar to 0.4), Neptune-mass exoplanet (HD 107148c) with an orbital period of P (c) similar to 18.3 days. Finally, we investigate the two-planet system's long-term stability and overall orbital dynamics with the posterior distribution of our preferred orbital configuration. Our N-body stability simulations show that the system is long-term stable and exhibits large secular osculations in eccentricity but in no particular mean motion resonance configuration. The HD 107148 system, consisting of a solar-type main-sequence star with two giant planets in a rare configuration, features a common proper-motion white dwarf companion and is therefore a valuable target for understanding the formation and evolution of planetary systems. |
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0004-6256 |
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WOS:000778725000001 |
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UAI @ alexi.delcanto @ |
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1562 |
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Kaye, L.; Vissapragada, S.; Gunther, M.N.; Aigrain, S.; Mikal-Evans, T.; Jensen, E.L.N.; Parviainen, H.; Pozuelos, F.J.; Abe, L.; Acton, J.S.; Agabi, A.; Alves, D.R.; Anderson, D.R.; Armstrong, D.J.; Barkaoui, K.; Barragan, O.; Benneke, B.; Boyd, P.T.; Brahm, R.; Bruni, I.; Bryant, E.M.; Burleigh, M.R.; Casewell, S.L.; Ciardi, D.; Cloutier, R.; Collins, K.A.; Collins, K.I.; Conti, D.M.; Crossfield, I.J.M.; Crouzet, N.; Daylan, T.; Dragomir, D.; Dransfield, G.; Fabrycky, D.; Fausnaugh, M.; Gan, T.J.; Gill, S.; Gillon, M.; Goad, M.R.; Gorjian, V.; Greklek-McKeon, M.; Guerrero, N.; Guillot, T.; Jehin, E.; Jenkins, J.S.; Lendl, M.; Kamler, J.; Kane, S.R.; Kielkopf, J.F.; Kunimoto, M.; Marie-Sainte, W.; McCormac, J.; Mekarnia, D.; Morales, F.Y.; Moyano, M.; Palle, E.; Parmentier, V; Relles, H.M.; Schmider, F.X.; Schwarz, R.P.; Seager, S.; Smith, A.M.S.; Tan, T.G.; Taylor, J.; Triaud, A.H.M.J.; Twicken, J.D.; Udry, S.; Vines, J.I.; Wang, G.; Wheatley, P.J.; Winn, J.N. |
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Title |
Transit timings variations in the three-planet system: TOI-270 |
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Year |
2022 |
Publication |
Monthly Notices Of The Royal Astronomical Society |
Abbreviated Journal |
Mon. Not. Roy. Astron. Soc. |
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Volume |
510 |
Issue |
4 |
Pages |
5464-5485 |
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Keywords |
planets and satellites: composition; planets and satellites: formation; planets and satellites: fundamental parameters |
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We present ground- and space-based photometric observations of TOI-270 (L231-32), a system of three transiting planets consisting of one super-Earth and two sub-Neptunes discovered by TESS around a bright (K-mag = 8.25) M3V dwarf. The planets orbit near low-order mean-motion resonances (5:3 and 2:1) and are thus expected to exhibit large transit timing variations (TTVs). Following an extensive observing campaign using eight different observatories between 2018 and 2020, we now report a clear detection of TTVs for planets c and d, with amplitudes of similar to 10 min and a super-period of similar to 3 yr, as well as significantly refined estimates of the radii and mean orbital periods of all three planets. Dynamical modelling of the TTVs alone puts strong constraints on the mass ratio of planets c and d and on their eccentricities. When incorporating recently published constraints from radial velocity observations, we obtain masses of M-b = 1.48 +/- 0.18 M-circle plus, M-c = 6.20 +/- 0.31 M-circle plus, and M-d = 4.20 +/- 0.16 M-circle plus for planets b, c, and d, respectively. We also detect small but significant eccentricities for all three planets : e(b) = 0.0167 +/- 0.0084, e(c) = 0.0044 +/- 0.0006, and e(d) = 0.0066 +/- 0.0020. Our findings imply an Earth-like rocky composition for the inner planet, and Earth-like cores with an additional He/H2O atmosphere for the outer two. TOI-270 is now one of the best constrained systems of small transiting planets, and it remains an excellent target for atmospheric characterization. |
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0035-8711 |
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WOS:000764893900001 |
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UAI @ alexi.delcanto @ |
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1552 |
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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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K2-280 b – a low density warm sub-Saturn around a mildly evolved star |
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2020 |
Publication |
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY |
Abbreviated Journal |
Mon. Not. Roy. Astron. Soc. |
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Volume |
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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UAI @ alexi.delcanto @ |
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1276 |
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Trifonov, T.; Wollbold, A.; Kurster, M.; Eberhardt, J.; Stock, S.; Henning, T.; Reffert, S.; Butler, R.P.; Vogt, S.S.; Reiners, A.; Lee, M.H.; Bitsch, B.; Zechmeister, M.; Rodler, F.; Perdelwitz, V.; Tal-Or, L.; Rybizki, J.; Heeren, P.; Gandolfi, D.; Barragan, O.; Zakhozhay, O.; Sarkis, P.; Pinto, M.T.; Kossakowski, D.; Wolthoff, V.; Brems, S.S.; Passegger, V.M. |
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A New Third Planet and the Dynamical Architecture of the HD33142 HD 33142 Planetary System |
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2022 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
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Volume |
164 |
Issue |
4 |
Pages |
156 |
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GAS GIANT PLANETS; STELLAR PARAMETERS; STARS; EVOLUTION; MASS; SEARCH; DWARF; II; MIGRATION; EXOPLANET |
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Based on recently-taken and archival HARPS, FEROS, and HIRES radial velocities (RVs), we present evidence for a new planet orbiting the first ascent red giant star HD 33142 (with an improved mass estimate of M1.52 +/- 0.03 M-circle dot), already known to host two planets. We confirm the Jovian-mass planets HD 33142b and c, with periods of P-b = 330.0(-0.4)(+0.4) days and P-c = 810. 2(-4.2)(+3.8) days and minimum dynamical masses of m(b) sin i =1.26(-0.05)(+0.05) M-Jup and m(c) sin i = 0.89(-0.05)(+0.06) M-Jup, respectively. Furthermore, our periodogram analysis of the precise RVs shows strong evidence for a short-period Doppler signal in the residuals of a two-planet Keplerian fit, which we interpret as a third, Saturn-mass planet with m(d) sin i = 0.20(-)(0.03)(+0.02) M-Jup in a close-in orbit with an orbital period of P-d = 89.9(-0.1)(+0.1) days. We study the dynamical behavior of the three-planet system configuration with an N-body integration scheme, finding it to be long-term stable with the planets alternating between low and moderate eccentricity episodes. We also perform N-body simulations, including stellar evolution and second-order dynamical effects such as planet-stellar tides and stellar mass loss on the way to the white dwarf phase. We find that planets HD 33142b, c, and d are likely to be engulfed near the tip of the red giant branch phase due to tidal migration. These results make the HD 33142 system an essential benchmark for planet population statistics of the multiple-planet systems found around evolved stars. |
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0004-6256 |
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WOS:000856534500001 |
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UAI @ alexi.delcanto @ |
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1651 |
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