Scaling K2. III. Comparable Planet Occurrence in the FGK Samples of Campaign 5 and Kepler

Zink, Jon K.; Hardegree-Ullman, Kevin K.; Christiansen, Jessie L.; Petigura, Erik A.; Dressing, Courtney D.; Schlieder, Joshua E.; Ciardi, David R.; Crossfield, Ian J. M.

doi:10.3847/1538-3881/aba123

Cited by 17 publications

(27 citation statements)

References 80 publications

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“…Looking forward to new surveys, the introduction of data from missions such as K2 (e.g. Howell et al 2014;Zink et al 2020) and TESS (e.g. Ricker et al 2015) are encouraging for this avenue of model comparison.…”

Section: Discussionmentioning

confidence: 99%

Photoevaporation vs. core-powered mass-loss: model comparison with the 3D radius gap

Rogers,

Gupta,

Owen

et al. 2021

Preprint

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The EUV/X-ray photoevaporation and core-powered mass-loss models are both capable of reproducing the bimodality in the sizes of small, close-in exoplanets observed by the Kepler space mission, often referred to as the "radius gap". However, it is unclear which of these two mechanisms dominates the atmospheric mass-loss which is likely sculpting the radius gap. In this work, we propose a new method of differentiating between the two models, which relies on analysing the radius gap in 3D parameter space. Using models for both mechanisms, and by performing synthetic transit surveys we predict the size and characteristics of a survey capable of discriminating between the two models. We find that a survey of 5000 planets, with a wide range in stellar mass and measurement uncertainties at a 5% level is sufficient. Our methodology is robust against moderate false positive contamination of 10%. We perform our analysis on two surveys (which do not satisfy our requirements): the California Kepler Survey and the Gaia-Kepler Survey and find, unsurprisingly, that both data-sets are consistent with either model. We propose a hypothesis test to be performed on future surveys which can robustly ascertain which of the two mechanisms formed the radius gap, provided one dominates over the other.

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Section: Discussionmentioning

confidence: 99%

Photoevaporation vs. core-powered mass-loss: model comparison with the 3D radius gap

Rogers,

Gupta,

Owen

et al. 2021

Preprint

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“…The observations will also be critical in future analyses of K2 and TESS exoplanet demographics and occurrence rates (e.g., Hardegree-Ullman et al, 2020;Zink et al, 2020). The HRI observations allow true planet radii to be included in these analysis.…”

Section: Discussionmentioning

confidence: 99%

Follow-Up and Validation of K2 and TESS Planetary Systems With Keck NIRC2 Adaptive Optics Imaging

Schlieder

Gonzales

Ciardi

et al. 2021

Front. Astron. Space Sci.

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High resolution imaging (HRI) is a critical part of the transiting exoplanet follow-up and validation process. HRI allows previously unresolved stellar companions and background blends to be resolved, vetting false positive signals and improving the radii measurements of true planets. Through a multi-semester Keck NIRC2 adaptive optics imaging program, we have pursued HRI of K2 and TESS candidate planet host systems to provide the transiting exoplanet community with necessary data for system validation and characterization. Here we present a summary of our ongoing program that includes an up to date list of targets observed, a description of the observations and data reduction, and a discussion of planetary systems validated by the community using these data. This observing program has been key in NASA's K2 and TESS missions reaching their goals of identifying new exoplanets ideal for continued follow-up observations to measure their masses and investigate their atmospheres. Once processed, all observations presented here are available as calibrated images and resulting contrast curves through the Exoplanet Follow-up Observing Program (ExoFOP) website. We encourage members of the exoplanet community to use these data products in their ongoing planetary system validation and characterization efforts.

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“…by using the K2 stellar sample, that spans a larger field of view and higher Galactic latitudes, and therefore contains more halo and thick-disk stars (e.g. Zink et al 2020), and the TESS input catalogue (Boley et al 2021).…”

Section: Discussionmentioning

confidence: 99%

Exoplanets in the Galactic context: Planet occurrence rates in the thin disk, thick disk and stellar halo of Kepler stars

Bashi,

Zucker

2021

Preprint

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In order to gain a better understanding of planet formation and evolution, it is important to examine the statistics of exoplanets in the Galactic context. By combining information on stellar elemental abundances and kinematics, we constructed separate samples of Kepler stars according to their affiliation to the Galactic components of thin disk, thick disk and stellar halo. Using a Bayesian analysis with conjugate priors, we then investigated how planet occurrence rates differ in different regions of planet properties. We find that young, slow and metal-rich stars, associated mainly with the thin disk, host on average more planets (especially close-in super Earths) compared to the old, fast and metal-poor thick disk stars. We further assess the dependence between stellar properties such as spectral type and metallicity, and planet occurrence rates. The trends we find agree with those found by other authors as well. We argue that in the Galactic context, these are probably not the main properties that affect planet occurrence rates, but rather the dynamical history of stars, and especially stellar age and kinematics, impact the current distribution of planets in the Galaxy.

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Scaling K2. III. Comparable Planet Occurrence in the FGK Samples of Campaign 5 and Kepler

Cited by 17 publications

References 80 publications

Photoevaporation vs. core-powered mass-loss: model comparison with the 3D radius gap

Photoevaporation vs. core-powered mass-loss: model comparison with the 3D radius gap

Follow-Up and Validation of K2 and TESS Planetary Systems With Keck NIRC2 Adaptive Optics Imaging

Exoplanets in the Galactic context: Planet occurrence rates in the thin disk, thick disk and stellar halo of Kepler stars

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