The TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets*

Yee, Samuel W.; Winn, Joshua N.; Hartman, J. D.; Bouma, Luke G.; Zhou, George; Quinn, Samuel N.; Latham, David W.; Bieryla, Allyson; Rodriguez, Joseph E.; Collins, Karen A.; Owen, Alfaro,; Barkaoui, Khalid; Beard, Corey; Belinski, A. A.; Benkhaldoun, Z.; Benni, Paul; Bernacki, Krzysztof; W., Boyle, Andrew; Butler, R. Paul; Caldwell, Douglas A.; Chontos, Ashley; Christiansen, Jessie L.; Ciardi, David R.; Collins, Kevin I.; Conti, Dennis M.; Crane, Jeffrey D.; Daylan, Tansu; Dressing, Courtney D.; Eastman, Jason D.; Essack, Zahra; Evans, P.; Everett, Mark E.; Fajardo-Acosta, S. B.; Forés-Toribio, Raquel; Furlan, Elise; Ghachoui, Mourad; Gillon, M.; Hellier, C.; Helm, Ian; Howard, Andrew W.; Howell, Steve B.; Isaacson, Howard; Jehin, Emmanuël; Jenkins, Jon M.; Jensen, Eric L. N.; Kielkopf, John F.; Laloum, Didier; Naunet, Leonhardes-Barboza,; Lewin, Pablo; Logsdon, Sarah E.; Polanski, Alex S.; Lund, Michael B.; MacDougall, Mason G.; Mann, Andrew W.; Massey, Bob; McLeod, Kim K.; Muñoz, J. A.; Newman, Patrick; Orlov, V. G.; Plavchan, Peter; Pozuelos, F. J.; Radford, Don J.; Reefe, Michael; Ricker, G.; Rudat, Alexander; Safonov, Boris; Schwarz, Richard P.; Schweiker, Heidi; Scott, Nicholas J.; Winn, Joshua N.; Shectman, Stephen; Stockdale, Chris; Tan, T. G.; Teske, Johanna; Thomas, Neil; Timmermans, Mathilde; Vanderspek, R.; Vermilion, David; Watanabe, David; Weiss, Lauren M.; West, R. G.; Zandt, Judah Van; Żejmo, M.; Ziegler, Carl

doi:10.3847/1538-4365/aca286

Cited by 19 publications

(6 citation statements)

References 159 publications

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“…Due to this small number, the timescale for the decline of the NPPS is still consistent with a wide range of values. Our framework can be extended to transit surveys and will also be useful to investigate HJ samples that are more than an order of magnitude larger (e.g., Yee et al 2023). Such applications would provide a more precise age dependence of the NPPS and might also reveal the age dependence of the mass-period distribution of HJs; in this work, we ignored a possible stellar parameter dependence of the shape of f (x|γ, z); (i.e., m and p in Equation (17) do not depend on stellar parameters), but this assumption may be relaxed with a larger sample.…”

Section: Implications For Past and Future Survey Resultsmentioning

confidence: 99%

Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age

Miyazaki,

Masuda

2023

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We investigate how the occurrence rate of giant planets (minimum mass > 0.3 M Jup) around Sun-like stars depends on the age, mass, and metallicity of their host stars. We develop a hierarchical Bayesian framework to infer the number of planets per star (NPPS) as a function of both planetary and stellar parameters. The framework fully takes into account the uncertainties in the latter by utilizing the posterior samples for the stellar parameters obtained by fitting stellar isochrone models to the spectroscopic parameters, Gaia DR3 parallaxes, and 2MASS K s-band magnitudes adopting a certain bookkeeping prior. We apply the framework to 46 Doppler giants found around a sample of 382 Sun-like stars from the California Legacy Survey catalog that publishes spectroscopic parameters and search completeness for all the surveyed stars. We find evidence that the NPPS of hot Jupiters (orbital period P = 1–10 days) decreases roughly in the latter half of the main sequence over the timescale of  ( Gyr ) , while that of cold Jupiters (P = 1–10 yr) does not. Assuming that this decrease is real and caused by tidal orbital decay, the modified stellar tidal quality factor Q ⋆ ′ is implied to be  ( 10 6 ) for a Sun-like main-sequence star orbited by a Jupiter-mass planet with P ≈ 3 days.

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Section: Implications For Past and Future Survey Resultsmentioning

confidence: 99%

Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age

Miyazaki,

Masuda

2023

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“…Using a more complete sample of planets would reduce the possibility that a large number of undetected planets exist that have a different metallicity/period distribution. Constructing a magnitudelimited sample of hot Jupiters is the goal of the Grand Unified Hot Jupiter Survey (Yee et al 2022(Yee et al , 2023. Although this goal has not yet been achieved, completeness has been substantially increased over the last few years.…”

Section: Sample Completenessmentioning

confidence: 99%

“…We decided to augment the NEA-based sample with 16 hot Jupiters described only in preprints (Anderson et al 2014;Bakos et al 2016;Anderson et al 2018;Brown et al 2019;Sha et al 2022;Rodriguez et al 2023;Yee et al 2023) at the time of archive query, and 22 that will be described in forthcoming papers by J.Schulte et al (2023, in preparation), S. W.Yee et al (2023, in preparation), andS. N.Quinn et al (2023, in preparation) that meet the same criteria on planet and stellar properties described in Section 2.…”

Section: Sample Completenessmentioning

confidence: 99%

“…We and others have been assembling a magnitude-limited sample of several hundred transiting hot Jupiters (P < 10 days), by combining the past two decades of discoveries with new discoveries from the NASA Transiting Exoplanet Survey Satellite (TESS; Ricker et al 2015). Our contribution goes by the name of the Grand Unified Hot Jupiter Survey (Yee et al 2022(Yee et al , 2023. Objects in this sample orbit brighter stars and have been vetted more thoroughly than the Kepler sample, while being more complete and homogeneous than the collection studied by Hellier et al (2017).…”

Section: Introductionmentioning

confidence: 99%

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The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity

Yee

Winn

2023

ApJL

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The probability that a Sun-like star has a close-orbiting giant planet (period ≲1 yr) increases with stellar metallicity. Previous work provided evidence that the period distribution of close-orbiting giant planets is also linked to metallicity, hinting that there two formation/evolution pathways for such objects, one of which is more probable in high-metallicity environments. Here, we check for differences in the period distribution of hot Jupiters (P < 10 days) as a function of host star metallicity, drawing on a sample of 232 transiting hot Jupiters and homogeneously derived metallicities from Gaia Data Release 3. We found no evidence for any metallicity dependence; the period distributions of hot Jupiters around metal-poor and metal-rich stars are indistinguishable. As a byproduct of this study, we provide transformations between metallicities from the Gaia Radial Velocity Spectrograph and from traditional high-resolution optical spectroscopy of main-sequence FGK stars.

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“…Third, for CoRoT-22, Kepler-1502, TOI-1937 A b, and TOI-4145 A b, which have inconsistent age measurements and lack of stellar rotation measurements, we can hardly validate their age. Additionally, Yee et al (2023) suspect that TOI-1937 A and TOI-4145 A may be the field star because of the poorly constrained cluster membership identification. Therefore, we directly exclude these four systems.…”

Section: Age Validationmentioning

confidence: 99%

Understanding the Planetary Formation and Evolution in Star Clusters (UPiC). I. Evidence of Hot Giant Exoplanets Formation Timescales

Dai,

Liu,

Yang

et al. 2023

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Planets in young star clusters could shed light on planet formation and evolution since star clusters can provide accurate age estimation. However, the number of transiting planets detected in clusters was only ∼30, too small for statistical analysis. Thanks to the unprecedented high-precision astrometric data provided by Gaia DR2 and Gaia DR3, many new open clusters (OCs) and comoving groups have been identified. The Understanding Planetary Formation and Evolution in Star Clusters project aims to find observational evidence and interpret how planets form and evolve in cluster environments. In this work, we cross match the stellar catalogs of new OCs and comoving groups with confirmed planets and candidates. We carefully remove false positives and obtain the biggest catalog of planets in star clusters up to now, which consists of 73 confirmed planets and 84 planet candidates. After age validation, we obtain the radius–age diagram of these planets/candidates. We find an increment in the fraction of hot Jupiters (HJs) around 100 Myr and attribute the increment to the flyby-induced high-e migration in star clusters. An additional small bump of the fraction of HJs after 1 Gyr is detected, which indicates the formation timescale of HJ around field stars is much larger than that in star clusters. Thus, stellar environments play important roles in the formation of HJs. The hot Neptune desert occurs around 100 Myr in our sample. A combination of photoevaporation and high-e migration may sculpt the hot Neptune desert in clusters.

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The TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets*

Cited by 19 publications

References 159 publications

Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age

Evidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age

The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity

Understanding the Planetary Formation and Evolution in Star Clusters (UPiC). I. Evidence of Hot Giant Exoplanets Formation Timescales

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