K2-99: a subgiant hosting a transiting warm Jupiter in an eccentric orbit and a long-period companion

Smith, A. M. S.; Gandolfi, D.; Barragán, Oscar; Bowler, Brendan P.; Csizmadia, Sz.; Endl, Michael; Fridlund, M.; Grziwa, S.; Guenther, E. W.; Hatzes, A. P.; Nowak, G.; Albrecht, S.; Alonso, R.; Cabrera, J.; Cochran, William D.; Deeg, H. J.; Cusano, F.; Eigmüller, Philipp; Erikson, A.; Hidalgo, D.; Hirano, Teruyuki; Johnson, Marshall C.; Korth, J.; Mann, Andrew W.; Narita, Norio; Nespral, D.; Πάλλη, Ε.; Pätzold, M.; Prieto-Arranz, J.; Rauer, H.; Ribas, I.; Tingley, B.; Wolthoff, V.

doi:10.1093/mnras/stw2487

Cited by 52 publications

(12 citation statements)

References 66 publications

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“…The Gelman-Rubin statistic (e.g., Croll 2006) is used to check the convergence of chains. For detailed descriptions of TLCM, we refer the reader to the following works: Csizmadia et al (2011Csizmadia et al ( , 2015, Smith et al (2017).…”

Section: Updating Transit Parametersmentioning

confidence: 99%

It Takes Two Planets in Resonance to Tango around K2-146

Lam

Korth

Masuda

et al. 2020

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K2-146 is a cool, 0.358M  dwarf that was found to host a mini-Neptune with a 2.67 day period. The planet exhibited strong transit timing variations (TTVs) of greater than 30 minutes, indicative of the presence of an additional object in the system. Here we report the discovery of the previously undetected outer planet in the system, K2-146 c, using additional photometric data. K2-146 c was found to have a grazing transit geometry and a 3.97 day period. The outer planet was only significantly detected in the latter K2 campaigns presumably because of precession of its orbital plane. The TTVs of K2-146 b and c were measured using observations spanning a baseline of almost 1200 days. We found strong anti-correlation in the TTVs, suggesting the two planets are gravitationally interacting. Our TTV and transit model analyses revealed that K2-146 b has a radius of 2.25±0.10 Å R and a mass of 5.6±0.7 Å M , whereas K2-146 c has a radius of -+ 2.59 0.39 1.81 ÅR and a mass of 7.1±0.9 Å M . The inner and outer planets likely have moderate eccentricities of e=0.14±0.07 and 0.16±0.07, respectively. Long-term numerical integrations of the two-planet orbital solution show that it can be dynamically stable for at least 2 Myr. We show that the resonance angles of the planet pair are librating, which may be an indication that K2-146 b and c are in a 3:2 mean motion resonance. The orbital architecture of the system points to a possible convergent migration origin.

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Section: Updating Transit Parametersmentioning

confidence: 99%

It Takes Two Planets in Resonance to Tango around K2-146

Lam

Korth

Masuda

et al. 2020

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“…The observation that the radii of giant planets increase with incident stellar irradiation hints that giant planet inflation is intimately linked to irradiation (Burrows et al 2000;Bodenheimer et al 2001;Lopez & Fortney 2016). We can distinguish between these two classes of models by studying warm Jupiters around stars that have recently evolved off the main sequence (e.g., Shporer et al 2017;Smith et al 2017). The irradiation levels experienced by warm Jupiters around main-sequence stars are not high enough to cause inflation, but as their host stars move up the subgiant and red-giant branches, they will experience enormous increases in their irradiation levels.…”

Section: Introductionmentioning

confidence: 99%

Two Warm, Low-density Sub-Jovian Planets Orbiting Bright Stars in K2 Campaigns 13 and 14

Rodriguez

Eastman

et al. 2018

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We report the discovery of two planets transiting the bright stars HD 89345 (EPIC 248777106, V=9.376, K=7.721) in K2 Campaign 14 and HD 286123 (EPIC 247098361, V=9.822, K=8.434) in K2 Campaign 13. Both stars are G-type stars, one of which is at or near the end of its main-sequence lifetime, and the other is just over halfway through its main-sequence lifetime. HD 89345 hosts a warm sub-Saturn (0.66R J , 0.11M J , T eq =1100 K) in an 11.81 day orbit. The planet is similar in size to WASP-107b, which falls in the transition region between ice giants and gas giants. HD 286123 hosts a Jupiter-sized, low-mass planet (1.06R J , 0.39 M J , T eq =1000 K) in an 11.17 day, mildly eccentric orbit, with e=0.255±0.035. Given that they orbit relatively evolved main-sequence stars and have orbital periods longer than 10 days, these planets are interesting candidates for studies of gas planet evolution, migration, and (potentially) reinflation. Both planets have spent their entire lifetimes near the proposed stellar irradiation threshold at which giant planets become inflated, and neither shows any sign of radius inflation. They probe the regime where inflation begins to become noticeable and are valuable in constraining planet inflation models. In addition, the brightness of the host stars, combined with large atmospheric scale heights of the planets, makes these two systems favorable targets for transit spectroscopy to study their atmospheres and perhaps provide insight into the physical mechanisms that lead to inflated hot Jupiters.

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“…These planets were discovered and characterized as part of the KESPRINT collaboration to find planets using K2. Our team has confirmed and characterized over two dozen transiting planets using K2, including hot Jupiters (e.g., Grziwa et al 2016;Hirano et al 2016b;Johnson et al 2016), longer-period giant planets (e.g., Smith et al 2017;Van Eylen et al 2018), ultra-short-period planets (e.g., Dai et al 2017;Smith et al 2018), multiplanet systems (e.g., Gandolfi et al 2017;Niraula et al 2017), as well as other planets (e.g., Narita et al 2017).…”

Section: Introductionmentioning

confidence: 93%

K2-260 b: a hot Jupiter transiting an F star, and K2-261 b: a warm Saturn around a bright G star

Johnson

Dai

Justesen

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the discovery and confirmation of two new transiting giant planets from the Kepler extended mission K2. K2-260 b is a hot Jupiter transiting a V = 12.7 F6V star in K2 Field 13, with a mass and radius of M = 1.39 +0.05 −0.06 M and R = 1.69 ± 0.03 R . The planet has an orbital period of P = 2.627 days, and a mass and radius of M P = 1.42 +0.31 −0.32 M J and R P = 1.552 +0.048 −0.057 R J . This is the first K2 hot Jupiter with a detected secondary eclipse in the Kepler bandpass, with a depth of 71 ± 15 ppm, which we use to estimate a geometric albedo of A g ∼ 0.2. We also detected a candidate stellar companion at 0.6" from K2-260; we find that it is very likely physically associated with the system, in which case it would be an M5-6V star at a projected separation of ∼ 400 AU. K2-261 b is a warm Saturn transiting a bright (V = 10.5) G7IV/V star in K2 Field 14. The host star is a metal-rich ([Fe/H]= 0.36 ± 0.06), mildly evolved 1.10 +0.01 −0.02 M star with R = 1.65 ± 0.04 R . Thanks to its location near the main sequence turn-off, we can measure a relatively precise age of 8.8 +0.4 −0.3 Gyr. The planet has P = 11.633 days, M P = 0.223 ± 0.031 M J , and R P = 0.850 +0.026 −0.022 R J , and its orbit is eccentric (e = 0.39 ± 0.15). Its brightness and relatively large transit depth make this one of the best known warm Saturns for follow-up observations to further characterize the planetary system.

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K2-99: a subgiant hosting a transiting warm Jupiter in an eccentric orbit and a long-period companion

Cited by 52 publications

References 66 publications

It Takes Two Planets in Resonance to Tango around K2-146

It Takes Two Planets in Resonance to Tango around K2-146

Two Warm, Low-density Sub-Jovian Planets Orbiting Bright Stars in K2 Campaigns 13 and 14

K2-260 b: a hot Jupiter transiting an F star, and K2-261 b: a warm Saturn around a bright G star

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