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Borucki, Hans; Grötsch, Engelhardt; Wenzel, Barbara

doi:10.1007/978-1-4684-8118-1_7

Cited by 12 publications

(19 citation statements)

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“…Initial analyses of the published Kepler planet candidate catalogues, e.g. Borucki et al (2011b; referred to as B11 for the remainder of this paper), Catanzarite & Shao (2011), Youdin (2011), Howard et al (2012), Dong & Zhu (2013) and Fressin et al (2013) used various estimates of detection efficiency to constrain the occurrence rate of planets, jessie.christiansen@caltech.edu but as yet there is no definitive empirical measure of this value for the Kepler pipeline. Petigura, Howard & Marcy (2013; referred to as PHM13 for the remainder of this paper) used a custom-built pipeline to produce their own planet candidate sample from the Kepler data, which allowed them to directly quantify their detection efficiency and remove the uncertainties caused by estimating this quantity.…”

Section: Introductionmentioning

confidence: 99%

MEASURING TRANSIT SIGNAL RECOVERY IN THEKEPLERPIPELINE. II. DETECTION EFFICIENCY AS CALCULATED IN ONE YEAR OF DATA

Christiansen

Clarke

Burke

et al. 2015

ApJ

119

145

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The Kepler planet sample can only be used to reconstruct the underlying planet occurrence rate if the detection efficiency of the Kepler pipeline is known; here we present the results of a second experiment aimed at characterising this detection efficiency. We inject simulated transiting planet signals into the pixel data of ∼10,000 targets, spanning one year of observations, and process the pixels as normal. We compare the set of detections made by the pipeline with the expectation from the set of simulated planets, and construct a sensitivity curve of signal recovery as a function of the signal-to-noise of the simulated transit signal train. The sensitivity curve does not meet the hypothetical maximum detection efficiency, however it is not as pessimistic as some of the published estimates of the detection efficiency. For the FGK stars in our sample, the sensitivity curve is well fit by a gamma function with the coefficients a = 4.35 and b = 1.05. We also find that the pipeline algorithms recover the depths and periods of the injected signals with very high fidelity, especially for periods longer than 10 days. We perform a simplified occurrence rate calculation using the measured detection efficiency compared to previous assumptions of the detection efficiency found in the literature to demonstrate the systematic error introduced into the resulting occurrence rates. The discrepancies in the calculated occurrence rates may go some way towards reconciling some of the inconsistencies found in the literature.

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Section: Introductionmentioning

confidence: 99%

MEASURING TRANSIT SIGNAL RECOVERY IN THEKEPLERPIPELINE. II. DETECTION EFFICIENCY AS CALCULATED IN ONE YEAR OF DATA

Christiansen

Clarke

Burke

et al. 2015

ApJ

119

145

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“…The latter method has detected ∼100 planets, all of which have been confirmed by RV data (or transit timing, see Lissauer et al 2011). Many more transit candidates are reported by Borucki et al (2011) with the Kepler satellite.…”

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confidence: 85%

“…Through its first four months of operation, NASA's Kepler mission (Koch et al 2010) detected 83 transit candidates with transit depths of at least 5 mmag and periods shorter than 10 days (Borucki et al 2011). Given the Kepler target list of ∼160 000 stars (Koch et al 2010), this is an occurrence rate of 0.00052 short period transiting planets of this size per star.…”

Section: Yeti Target Selection Criteria and Transit Planet Detection mentioning

confidence: 99%

The Young Exoplanet Transit Initiative (YETI)

et al. 2011

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We present the Young Exoplanet Transit Initiative (YETI), in which we use several 0.2 to 2.6-m telescopes around the world to monitor continuously young (≤100 Myr), nearby (≤1 kpc) stellar clusters mainly to detect young transiting planets (and to study other variability phenomena on time-scales from minutes to years). The telescope network enables us to observe the targets continuously for several days in order not to miss any transit. The runs are typically one to two weeks long, about three runs per year per cluster in two or three subsequent years for about ten clusters. There are thousands of stars detectable in each field with several hundred known cluster members, e.g. in the first cluster observed, Tr-37, a typical cluster for the YETI survey, there are at least 469 known young stars detected in YETI data down to R = 16.5 mag with sufficient precision of 50 millimag rms (5 mmag rms down to R = 14.5 mag) to detect transits, so that we can expect at least about one young transiting object in this cluster. If we observe ∼10 similar clusters, we can expect to detect ∼10 young transiting planets with radius determinations. The precision given above is for a typical telescope of the YETI network, namely the 60/90-cm Jena telescope (similar brightness limit, namely within ±1 mag, for the others) so that planetary transits can be detected. For targets with a periodic transit-like light curve, we obtain spectroscopy to ensure that the star is young and that the transiting object can be sub-stellar; then, we obtain Adaptive Optics infrared images and spectra, to exclude other bright eclipsing stars in the (larger) optical PSF; we carry out other observations as needed to rule out other false positive scenarios; finally, we also perform spectroscopy to determine the mass of the transiting companion. For planets with mass and radius determinations, we can calculate the mean density and probe the internal structure. We aim to constrain planet formation models and their time-scales by discovering planets younger than ∼100 Myr and determining not only their orbital parameters, but also measuring their true masses and radii, which is possible so far only by the transit method. Here, we present an overview and first results.

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“…The disposition of KOI-1003 has changed several times over the course of the Kepler observations. In Borucki et al (2011b), the star was first listed as a Kepler candidate in the Q0-2 data release. The object retained a disposition of "candidate" in the Q1-6 data release (Batalha et al 2013), but Burke et al (2014) changed the disposition of the object to "not dispositioned."…”

Section: The Nature Of Koi-1003mentioning

confidence: 99%

Koi-1003: A New Spotted, Eclipsing Rs CVN Binary in the Kepler Field

Roettenbacher

Kane

Monnier

et al. 2016

ApJ

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Using the high-precision photometry from the Kepler space telescope, thousands of stars with stellar and planetary companions have been observed. The characterization of stars with companions is not always straightforward and can be contaminated by systematic and stellar influences on the light curves. Here, through a detailed analysis of starspots and eclipses, we identify KOI-1003 as a new, active RS CVn star-the first identified with data from Kepler. The Kepler light curve of this close binary system exhibits the system's primary transit, secondary eclipse, and starspot evolution of two persistent active longitudes. The near equality of the system's orbital and rotation periods indicates the orbit and primary star's rotation are nearly synchronized (P orb = 8.360613 ± 0.000003 days; P rot ∼ 8.23 days). By assuming the secondary star is on the main sequence, we suggest the system consists of a 1.45 +0.11 −0.19 M ⊙ subgiant primary and a 0.59 +0.03 −0.04 M ⊙ main-sequence companion. Our work gives a distance of 4400 ± 600 pc and an age of t = 3.0 −0.5 +2.0 Gyr, parameters which are discrepant with previous studies that included the star as a member of the open cluster NGC 6791.

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Cited by 12 publications

References 0 publications

MEASURING TRANSIT SIGNAL RECOVERY IN THEKEPLERPIPELINE. II. DETECTION EFFICIENCY AS CALCULATED IN ONE YEAR OF DATA

MEASURING TRANSIT SIGNAL RECOVERY IN THEKEPLERPIPELINE. II. DETECTION EFFICIENCY AS CALCULATED IN ONE YEAR OF DATA

The Young Exoplanet Transit Initiative (YETI)

Koi-1003: A New Spotted, Eclipsing Rs CVN Binary in the Kepler Field

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