TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE

By C. Burke, J. Christiansen, F. Mullally, S. Seader, D. Huber, J. Rowe, Jeff Coughlin, S. Thompson, J. Catanzarite, B. Clarke and 15 more. 2015

258 citations recorded by the source corpus.

We measure planet occurrence rates using the planet candidates discovered by the Q1-Q16 Kepler pipeline search. This study examines planet occurrence rates for the Kepler GK dwarf target sample for planet radii, 0.75 ≤ ?> R p ?> ≤ ?> 2.5 R ⨁ ?> , and orbital periods, 50 ≤ ?> P orb ?> ≤ ?> 300 days, with an emphasis on a thorough exploration and identification of the most important sources of systematic uncertainties. Integrating over this parameter space, we measure an occurrence rate of F0 = 0.77 planets per star, with an allowed range of 0.3 ≤ F 0 ≤ ?> 1.9. The allowed range takes into account both statistical and systematic uncertainties, and values of F0 beyond the allowed range are significantly in disagreement with our analysis. We generally find higher planet occurrence rates and a steeper increase in planet occurrence rates toward small planets than previous studies of the Kepler GK dwarf sample. Through extrapolation, we find that the one year orbital period terrestrial planet occurrence rate ζ 1.0 ?> = 0.1, with an allowed range of 0.01 ≤ ζ 1.0 ≤ ?> 2, where ζ 1.0 ?> is defined as the number of planets per star within 20% of the R p ?> and P orb ?> of Earth. For G dwarf hosts, the ζ 1.0 ?> parameter space is a subset of the larger &eegr; ⨁ ?> parameter space, thus ζ 1.0 ?> places a lower limit on &eegr; ⨁ ?> for G dwarf hosts. From our analysis, we identify the leading sources of systematics impacting Kepler occurrence rate determinations as reliability of the planet candidate sample, planet radii, pipeline completeness, and stellar parameters.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/95922b101ca7f7d211a75bfcca61cbf0bf48e409

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Citations in the corpus

Revised Stellar Properties of Kepler Targets for the Q1-17 (DR25) Transit Detection Run (2016, background): “…of detections allowed statistical studies of planet occurrence rates (e.g. Howard et al. 2012; Fressin et al. 2013; Dressing & Charbonneau 2015; Burke et al. 2015; Sil- 1 Space Science Institute, 4750 Walnut street Suite#205, Boulder, CO 80301, USA 2 Sydney Institute for Astronomy, School of…”
SPITZER OBSERVATIONS CONFIRM AND RESCUE THE HABITABLE-ZONE SUPER-EARTH K2-18b FOR FUTURE CHARACTERIZATION (2016, background): “…first telescope with the sensitivity to detect small planets in the habitable zones of sun-like stars, indicate that the occurrence rate for habitable Earths (“η⊕”) may be as high as 5-20% (Petigura et al. 2013; Foreman-Mackey et al. 2014; Silburt et al. 2015; Farr et al. 2015; Burke et al. 2015).”
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The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets (2017, unknown): “…& Shao (2011); Traub (2012); Howard et al. (2012); Fressin et al. (2013); Dong & Zhu (2013); Petigura et al. (2013); ForemanMackey et al. (2014); Burke et al. (2015); Dressing & Charbonneau (2015); Mulders et al. (2015). and with the occurrence of large planets (RP > 1.7 R⊕, P < 100 days).”
The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets (2017, background): “More recently, Burke et al. (2015) studied the occurrence of small, long-period planets.”
Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2 (2018, background): “Precise stellar classifications are also required to study the dynamics and evolution of planetary orbits (Kane et al. 2012; Sliski & Kipping 2014; Van Eylen & Albrecht 2015) and derive an accurate planet occurrence (e.g. Howard et al. 2012; Burke et al. 2015).”
The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets (2017, background): “Further work showed that Earth-size planets are common in and near the habitable zone (Petigura et al. 2013a; Dressing & Charbonneau 2015; Burke et al. 2015).”
The Exoplanet Population Observation Simulator. I. The Inner Edges of Planetary Systems (2018, background): “These results are consistent with the estimate of Γ⊕=60% for GK dwarfs by Burke et al. (2015), though we note that there is a large dispersion in the literature11 on habitable zone planet occurrence rates based on the adopted completeness correction, the method of extrapolation into the habitable…”
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The Gaia–Kepler Stellar Properties Catalog. I. Homogeneous Fundamental Properties for 186,301 Kepler Stars (2020, background): “…Fellow The first Kepler Stellar Properties Catalog (KSPC, Huber et al. 2014) was published to consolidate all of the follow-up work done for Kepler stars and improve the estimated planetary occurrence rates (e.g., Howard et al. 2012; Petigura et al. 2013; Burke et al. 2015; Fulton et al. 2017).”
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