Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2

Berger, Travis A.; Huber, Daniel; Gaidos, Eric; Saders, Jennifer L. van

doi:10.3847/1538-4357/aada83

Cited by 298 publications

(438 citation statements)

References 97 publications

(154 reference statements)

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“…We aim at targets of dwarfs, removing giant stars with an empirical T eff − g log relation determined by Ciardi et al (2011). Binaries labeled by Berger et al (2018) were also excluded. To select F-to K-type stars, we use T eff in the range of 3800-7200 K. To place a lower limit on the quality of the individual observations, the S/Ns at the blue end of the spectra are higher than 10.…”

Section: Discussionmentioning

confidence: 99%

Magnetic Activity of F-, G-, and K-type Stars in the LAMOST–Kepler Field

Zhang

et al. 2020

ApJS

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Monitoring chromospheric and photospheric indexes of magnetic activity can provide valuable information, especially the interaction between different parts of the atmosphere and their response to magnetic fields. We extract chromospheric indexes, S and + R HK , for 59,816 stars from LAMOST spectra in the LAMOST-Kepler program, and photospheric index, R eff , for 5575 stars from Kepler light curves. The log R eff shows positive correlation with log + R HK . We estimate the power-law indexes between R eff and + R HK for F-, G-, and K-type stars, respectively. We also confirm the dependence of both chromospheric and photospheric activity on stellar rotation. Ca II H and K emissions and photospheric variations generally decrease with increasing rotation periods for stars with rotation periods exceeding a few days. The power-law indexes in exponential decay regimes show different characteristics in the two activity-rotation relations. The updated largest sample including the activity proxies and reported rotation periods provides more information to understand the magnetic activity for cool stars.

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Section: Discussionmentioning

confidence: 99%

Magnetic Activity of F-, G-, and K-type Stars in the LAMOST–Kepler Field

Zhang

et al. 2020

ApJS

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“…Unsurprisingly, the K2 pipeline is far more prone to transit depth reduction. However, both of these offsets (Kepler and K2 ) are smaller than the average planet radius uncertainty (∼ 10%; Berger et al 2018). Knowing that this offset falls within the normal radius uncertainty, Figure 14 shows the mode of this offset distribution is located at 1, we do not apply this correction to our candidate parameters.…”

Section: Planet Radiusmentioning

confidence: 96%

Scaling K2. II. Assembly of a Fully Automated C5 Planet Candidate Catalog Using EDI-Vetter

Zink

Hardegree-Ullman

Christiansen

et al. 2020

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We present a uniform transiting exoplanet candidate list for Campaign 5 of the K2 mission. This catalog contains 75 planets with 7 multi-planet systems (5 double, 1 triple, and 1 quadruple planet system). Within the range of our search, we find 8 previously undetected candidates with the remaining 66 candidates overlapping 51% of the Kruse et al. study that manually vet Campaign 5 candidates. In order to vet our potential transit signals, we introduce the Exoplanet Detection Identification Vetter (EDI-Vetter), which is a fully automated program able to determine if a transit signal should be labeled as a false positive or a planet candidate. This automation allows us to create a statistically uniform catalog, ideal for planet occurrence rate measurements. When tested, the vetting software is able to ensure our sample is 94.2% reliable against systematic false positives. Additionally, we inject artificial transits at the light-curve-level of the raw K2 data and find the maximum completeness of our pipeline is 70% before vetting and 60% after vetting. For convenience of future occurrence rate studies, we include measurements of stellar noise (CDPP) and the three-transit window function for each target. This study is part of a larger survey of the K2 data set and the methodology which will be applied to the entirety of the K2 data set.

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“…For the tranet sample, Zhu et al (2018) used the Kepler Data Release 24, while we used the final Data Release 25. For the star sample, they select ∼ 30,000 solar-type stars based on a wide temperature range (T eff =4700-6500 K) and a cut on surface gravity (log g > 4) given by LAMOST (Luo et al 2015), while our result in Figure 8 is for ∼ 10,000 solar-type stars selected from the HR diagram (Berger et al 2018) with a narrower temperature range (T eff ∼ 5700 − 5900 K). Second, the models are different.…”

Section: α As a Function Of T Effmentioning

confidence: 99%

Occurrence and Architecture of Kepler Planetary Systems as Functions of Stellar Mass and Effective Temperature

Jun

Xie

Zhou

2020

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The Kepler mission has discovered thousands of exoplanets around various stars with different spectral types (M, K, G, and F) and thus different masses and effective temperatures. Previous studies have shown that the planet occurrence rate, in terms of the average number of planets per star, drops with increasing stellar effective temperature (T eff ). In this paper, with the final Kepler Data Release (DR25) catalog, we revisit the relation between stellar effective temperature (as well as mass) and planet occurrence, but in terms of the fraction of stars with planets and the number of planets per planetary system (i.e., planet multiplicity). We find that both the fraction of stars with planets and planet multiplicity decrease with increasing stellar temperature and mass. Specifically, about 75% late-type stars (T eff < 5000 K) have Kepler -like planets with an average planet multiplicity of ∼2.8, while for early-type stars (T eff > 6500 K), this fraction and the average multiplicity fall down to ∼35% and ∼1.8, respectively. The decreasing trend in the fraction of stars with planets is very significant with ∆AIC> 30, though the trend in planet multiplicity is somewhat tentative with ∆AIC∼ 5. Our results also allow us to derive the dispersion of planetary orbital inclinations in relationship with stellar effective temperature. Interestingly, it is found to be similar to the well-known trend between obliquity and stellar temperature, indicating that the two trends might have a common origin.

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Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2

Cited by 298 publications

References 97 publications

Magnetic Activity of F-, G-, and K-type Stars in the LAMOST–Kepler Field

Magnetic Activity of F-, G-, and K-type Stars in the LAMOST–Kepler Field

Scaling K2. II. Assembly of a Fully Automated C5 Planet Candidate Catalog Using EDI-Vetter

Occurrence and Architecture of Kepler Planetary Systems as Functions of Stellar Mass and Effective Temperature

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