| Records |
| 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 |
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| 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 |
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Iop Publishing Ltd |
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English |
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0004-6256 |
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WOS:000584931800001 |
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UAI @ alexi.delcanto @ |
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1261 |
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| Author |
Trifonov, T.; Brahm, R.; Espinoza, N.; Henning, T.; Jordan, A.; Nesvorny, D.; Dawson, R.I.; Lissauer, J.J.; Lee, M.H.; Kossakowski, D.; Rojas, F.I.; Hobson, M.J.; Sarkis, P.; Schlecker, M.; Bitsch, B.; Bakos, G.A.; Barbieri, M.; Bhatti, W.; Butler, R.P.; Crane, J.D.; Nandakumar, S.; Diaz, M.R.; Shectman, S.; Teske, J.; Torres, P.; Suc, V.; Vines, J.I.; Wang, S.R.X.; Ricker, G.R.; Shporer, A.; Vanderburg, A.; Dragomir, D.; Vanderspek, R.; Burke, C.J.; Daylan, T.; Shiao, B.; Jenkins, J.M.; Wohler, B.; Seager, S.; Winn, J.N. |
| Title |
A Pair of Warm Giant Planets near the 2:1 Mean Motion Resonance around the K-dwarf Star TOI-2202* |
Type |
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| Year |
2021 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
| Volume |
162 |
Issue |
6 |
Pages |
283 |
| Keywords |
EARTH-SIZED PLANET; SUPER-EARTH; HOT JUPITERS; TESS; SYSTEMS; TRANSIT; NEPTUNE; MODEL; PERIODOGRAM; SCATTERING |
| Abstract |
TOI-2202 b is a transiting warm Jovian-mass planet with an orbital period of P = 11.91 days identified from the Full Frame Images data of five different sectors of the TESS mission. Ten TESS transits of TOI-2202 b combined with three follow-up light curves obtained with the CHAT robotic telescope show strong transit timing variations (TTVs) with an amplitude of about 1.2 hr. Radial velocity follow-up with FEROS, HARPS, and PFS confirms the planetary nature of the transiting candidate (a (b) = 0.096 +/- 0.001 au, m (b) = 0.98 +/- 0.06 M (Jup)), and a dynamical analysis of RVs, transit data, and TTVs points to an outer Saturn-mass companion (a (c) = 0.155 +/- 0.002 au, m (c) = 0.37 +/- 0.10 M (Jup)) near the 2:1 mean motion resonance. Our stellar modeling indicates that TOI-2202 is an early K-type star with a mass of 0.82 M (circle dot), a radius of 0.79 R (circle dot), and solar-like metallicity. The TOI-2202 system is very interesting because of the two warm Jovian-mass planets near the 2:1 mean motion resonance, which is a rare configuration, and their formation and dynamical evolution are still not well understood. |
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0004-6256 |
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| Notes |
WOS:000725244600001 |
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UAI @ alexi.delcanto @ |
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1511 |
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| Author |
Trifonov, T.; Brahm, R.; Jordan, A.; Hartogh, C.; Henning, T.; Hobson, M.J.; Schlecker, M.; Howard, S.; Reichardt, F.; Espinoza, N.; Lee, M.H.; Nesvorny, D.; Rojas, F.I.; Barkaoui, K.; Kossakowski, D.; Boyle, G.; Dreizler, S.; Kurster, M.; Heller, R.; Guillot, T.; Triaud, A.H.M.J.; Abe, L.; Agabi, A.; Bendjoya, P.; Crouzet, N.; Dransfield, G.; Gasparetto, T.; Gunther, M.N.; Marie-Sainte, W.; Mekarnia, D.; Suarez, O.; Teske, J.; Butler, R.P.; Crane, J.D.; Shectman, S.; Ricker, G.R.; Shporer, A.; Vanderspek, R.; Jenkins, J.M.; Wohler, B.; Collins, K.A.; Collins, K.I.; Ciardi, D.R.; Barclay, T.; Mireles, I.; Seager, S.; Winn, J.N. |
| Title |
TOI-2525 b and c: A Pair of Massive Warm Giant Planets with Strong Transit Timing Variations Revealed by TESS |
Type |
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| Year |
2023 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
| Volume |
165 |
Issue |
4 |
Pages |
179 |
| Keywords |
HOT JUPITERS; EXOPLANET SURVEY; SUPER-EARTH; LOW-DENSITY; SYSTEMS; NEPTUNE; STAR; II.; POPULATION; MIGRATION |
| Abstract |
The K-type star TOI-2525 has an estimated mass of M = 0.849(-0.033)(+0.024) M-circle dot and radius of R = 0.785(-0.007)(+0.007) R-circle dot observed by the TESS mission in 22 sectors (within sectors 1 and 39). The TESS light curves yield significant transit events of two companions, which show strong transit timing variations (TTVs) with a semiamplitude of similar to 6 hr. We performed TTV dynamical and photodynamical light-curve analysis of the TESS data combined with radial velocity measurements from FEROS and PFS, and we confirmed the planetary nature of these companions. The TOI-2525 system consists of a transiting pair of planets comparable to Neptune and Jupiter with estimated dynamical masses of m(b) = 0.088(-0.004)(+0.005) and m(c) = 0.709(-0.033)(+0.034) M-Jup, radii of r(b) = 0.88(-0.02)(+0.02) and r(c) = 0.98(-0.02)(+0.02) R-Jup, and orbital periods of P-b = 23.288(-0.002)(+0.001) and P-c = 49.260(-0.001)(+0.001) days for the inner and outer planet, respectively. The period ratio is close to the 2:1 period commensurability, but the dynamical simulations of the system suggest that it is outside the mean-motion resonance (MMR) dynamical configuration. Object TOI-2525 b is among the lowest-density Neptune-mass planets known to date, with an estimated median density of rho(b) = 0.174(-0.015)(+0.016) g cm(-3). The TOI-2525 system is very similar to the other K dwarf systems discovered by TESS, TOI-2202 and TOI-216, which are composed of almost identical K dwarf primaries and two warm giant planets near the 2:1 MMR. |
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0004-6256 |
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WOS:000960020200001 |
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UAI @ alexi.delcanto @ |
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1835 |
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