A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology
We present Kepler exoplanet occurrence rates for planets between 0.5 and 16 R _⊕ and between 1 and 400 days. To measure occurrence, we use a nonparametric method via a kernel density estimator and use bootstrap random sampling for uncertainty estimation. We use a full characterization of completenes...
| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/acebc8 |
| _version_ | 1797694412021563392 |
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| author | Anne Dattilo Natalie M. Batalha Steve Bryson |
| author_facet | Anne Dattilo Natalie M. Batalha Steve Bryson |
| author_sort | Anne Dattilo |
| collection | DOAJ |
| description | We present Kepler exoplanet occurrence rates for planets between 0.5 and 16 R _⊕ and between 1 and 400 days. To measure occurrence, we use a nonparametric method via a kernel density estimator and use bootstrap random sampling for uncertainty estimation. We use a full characterization of completeness and reliability measurements from the Kepler Data Release 25 catalog, including detection efficiency, vetting completeness, astrophysical reliability, and false alarm reliability. We also include more accurate and homogeneous stellar radii from Gaia Data Release 2. In order to see the impact of these final Kepler properties, we revisit benchmark exoplanet occurrence rate measurements from the literature. We compare our measurements with previous studies to both validate our method and observe the dependence of these benchmarks on updated stellar and planet properties. For FGK stars, between 0.5 and 16 R _⊕ and between 1 and 400 days, we find an occurrence of 1.52 ± 0.08 planets per star. We investigate the dependence of occurrence as a function of radius, orbital period, and stellar type and compare with previous studies with excellent agreement. We measure the minimum of the radius valley to be ${1.78}_{-0.16}^{+0.14}$ R _⊕ for FGK stars and find it to move to smaller radii for cooler stars. We also present new measurements of the slope of the occurrence cliff at 3–4 R _⊕ , and find that the cliff becomes less steep at long orbital period. Our methodology will enable us to constrain theoretical models of planet formation and evolution in the future. |
| first_indexed | 2024-03-12T02:57:30Z |
| format | Article |
| id | doaj.art-cedcfd8680084e5c8ee0b64a6c592e27 |
| institution | Directory Open Access Journal |
| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-03-12T02:57:30Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-cedcfd8680084e5c8ee0b64a6c592e272023-09-03T15:13:00ZengIOP PublishingThe Astronomical Journal1538-38812023-01-01166312210.3847/1538-3881/acebc8A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. MethodologyAnne Dattilo0https://orcid.org/0000-0002-1092-2995Natalie M. Batalha1https://orcid.org/0000-0002-7030-9519Steve Bryson2https://orcid.org/0000-0003-0081-1797Department of Astronomy and Astrophysics, University of California Santa Cruz , Santa Cruz, CA 95064, USA ; adattilo@ucsc.eduDepartment of Astronomy and Astrophysics, University of California Santa Cruz , Santa Cruz, CA 95064, USA ; adattilo@ucsc.eduNASA Ames Research Center , Moffett Field, CA 94035, USAWe present Kepler exoplanet occurrence rates for planets between 0.5 and 16 R _⊕ and between 1 and 400 days. To measure occurrence, we use a nonparametric method via a kernel density estimator and use bootstrap random sampling for uncertainty estimation. We use a full characterization of completeness and reliability measurements from the Kepler Data Release 25 catalog, including detection efficiency, vetting completeness, astrophysical reliability, and false alarm reliability. We also include more accurate and homogeneous stellar radii from Gaia Data Release 2. In order to see the impact of these final Kepler properties, we revisit benchmark exoplanet occurrence rate measurements from the literature. We compare our measurements with previous studies to both validate our method and observe the dependence of these benchmarks on updated stellar and planet properties. For FGK stars, between 0.5 and 16 R _⊕ and between 1 and 400 days, we find an occurrence of 1.52 ± 0.08 planets per star. We investigate the dependence of occurrence as a function of radius, orbital period, and stellar type and compare with previous studies with excellent agreement. We measure the minimum of the radius valley to be ${1.78}_{-0.16}^{+0.14}$ R _⊕ for FGK stars and find it to move to smaller radii for cooler stars. We also present new measurements of the slope of the occurrence cliff at 3–4 R _⊕ , and find that the cliff becomes less steep at long orbital period. Our methodology will enable us to constrain theoretical models of planet formation and evolution in the future.https://doi.org/10.3847/1538-3881/acebc8ExoplanetsExoplanet formationExoplanet astronomyExoplanet evolutionTransit photometry |
| spellingShingle | Anne Dattilo Natalie M. Batalha Steve Bryson A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology The Astronomical Journal Exoplanets Exoplanet formation Exoplanet astronomy Exoplanet evolution Transit photometry |
| title | A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology |
| title_full | A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology |
| title_fullStr | A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology |
| title_full_unstemmed | A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology |
| title_short | A Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology |
| title_sort | unified treatment of kepler occurrence to trace planet evolution i methodology |
| topic | Exoplanets Exoplanet formation Exoplanet astronomy Exoplanet evolution Transit photometry |
| url | https://doi.org/10.3847/1538-3881/acebc8 |
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