English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

(Abridged) NASA's Kepler mission has provided several thousand transitingplanet candidates, yet only a small subset have been confirmed as true planets.Therefore, the most fundamental question about these candidates is the fractionof bona fide planets. Estimating the rate of false positives of the overallKepler sample is necessary to derive the planet occurrence rate. We present theresults from two large observational campaigns that were conducted with theSpitzer telescope during the the Kepler mission. These observations arededicated to estimating the false positive rate (FPR) amongst the Keplercandidates. We select a sub-sample of 51 candidates, spanning wide ranges instellar, orbital and planetary parameter space, and we observe their transitswith Spitzer at 4.5 microns. We use these observations to measures thecandidate's transit depths and infrared magnitudes. A bandpass-dependent depthalerts us to the potential presence of a blending star that could be the sourceof the observed eclipse: a false-positive scenario. For most of the candidates(85%), the transit depths measured with Kepler are consistent with the depthsmeasured with Spitzer as expected for planetary objects, while we find that themost discrepant measurements are due to the presence of unresolved stars thatdilute the photometry. The Spitzer constraints on their own yield FPRs between5-40%, depending on the KOIs. By considering the population of the Kepler fieldstars, and by combining follow-up observations (imaging) when available, wefind that the overall FPR of our sample is low. The measured upper limit on theFPR of our sample is 8.8% at a confidence level of 3 sigma. This observationalresult, which uses the achromatic property of planetary transit signals that isnot investigated by the Kepler observations, provides an independent indicationthat Kepler's false positive rate is low.

Low False-Positive Rate of Kepler Candidates Estimated From A Combination Of Spitzer And Follow-Up Observations