MEASURING TRANSIT SIGNAL RECOVERY IN THE<i>KEPLER</i>PIPELINE. II. DETECTION EFFICIENCY AS CALCULATED IN ONE YEAR OF DATA

Christiansen, Jessie L.; Clarke, Bruce; Burke, Christopher J.; Seader, Shawn; Jenkins, Jon M.; Twicken, Joseph D.; Catanzarite, Joseph; Smith, Jeffrey C.; Batalha, Natalie M.; Haas, Michael R.; Thompson, Susan E.; Campbell, Jennifer R.; Sabale, Anima; Uddin, Akm Kamal

doi:10.1088/0004-637x/810/2/95

Cited by 120 publications

(152 citation statements)

References 36 publications

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“…Characterizing p det as a function of S/N has been addressed in several previous works (e.g., Fressin et al 2013;Petigura et al 2013;Christiansen et al 2015). This is a challenging problem, which depends on how a complex, multi-stage transit pipeline performs in the face of correlated, non-stationary, and non-Gaussian photometric noise.…”

Section: Completenessmentioning

confidence: 99%

The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets

et al. 2018

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Probing the connection between a star's metallicity and the presence and properties of any associated planets offers an observational link between conditions during the epoch of planet formation and mature planetary systems. We explore this connection by analyzing the metallicities of Kepler target stars and the subset of stars found to host transiting planets. After correcting for survey incompleteness, we measure planet occurrence: the number of planets per 100 stars with a given metallicity M. Planet occurrence correlates with metallicity for some, but not all, planet sizes and orbital periods. For warm super-Earths having P=10-100days and R P =1.0-1.7R Å , planet occurrence is nearly constant over metallicities spanning −0.4 to +0.4dex. We find 20 warm super-Earths per 100 stars, regardless of metallicity. In contrast, the occurrence of warm sub-Neptunes (R P = 1.7-4.0 R Å ) doubles over that same metallicity interval, from 20 to 40 planets per 100 stars. We model the distribution of planets as, where β characterizes the strength of any metallicity correlation. This correlation steepens with decreasing orbital period and increasing planet size. + -+ . High metallicities in protoplanetary disks may increase the mass of the largest rocky cores or the speed at which they are assembled, enhancing the production of planets larger than 1.7R Å . The association between high metallicity and short-period planets may reflect disk density profiles that facilitate the inward migration of solids or higher rates of planet-planet scattering.

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Section: Completenessmentioning

confidence: 99%

The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets

et al. 2018

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“…(The upper script C refers to the completeness.) This has been thoroughly studied in Christiansen et al (2013Christiansen et al ( , 2015. In particular, they find that the detection efficiency of EGPs transiting bright, solar-type dwarfs is better than 95% over orbital periods up to 400 days (Christiansen et al, priv.…”

Section: Survey Correctionsmentioning

confidence: 99%

“…Together with the pipeline completeness (Christiansen et al 2013(Christiansen et al , 2015, this information is needed to accurately assess the underlying occurrence of planets, down to Earth-size planets in the habitable zone. The latter is the main objective of the Kepler prime mission (Borucki et al 2009;Batalha 2014).…”

Section: Comparison With Other False-positive Rate Estimatesmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Tsantaki

et al. 2016

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While giant extrasolar planets have been studied for more than two decades now, there are still some open questions as to their dominant formation and migration processes, as well as to their atmospheric evolution in different stellar environments. In this paper, we study a sample of giant transiting exoplanets detected by the Kepler telescope with orbital periods up to 400 days. We first defined a sample of 129 giant-planet candidates that we followed up with the SOPHIE spectrograph (OHP, France) in a 6-year radial velocity campaign. This allowed us to unveil the nature of these candidates and to measure a false-positive rate of 54.6 ± 6.5% for giant-planet candidates orbiting within 400 days of period. Based on a sample of confirmed or likely planets, we then derived the occurrence rates of giant planets in different ranges of orbital periods. The overall occurrence rate of giant planets within 400 days is 4.6 ± 0.6%. We recovered, for the first time in the Kepler data, the different populations of giant planets reported by radial velocity surveys. Comparing these rates with other yields, we find that the occurrence rate of giant planets is lower only for hot Jupiters but not for the longer-period planets. We also derive a first measurement of the occurrence rate of brown dwarfs in the brown-dwarf desert with a value of 0.29 ± 0.17%. Finally, we discuss the physical properties of the giant planets in our sample. We confirm that giant planets receiving moderate irradiation are not inflated, but we find that they are on average smaller than predicted by formation and evolution models. In this regime of low-irradiated giant planets, we find a possible correlation between their bulk density and the iron abundance of the host star, which needs more detections to be confirmed.

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“…Current and future studies with injection/recovery tests similar to those performed for Kepler (Petigura et al 2013;Christiansen et al 2015) will help resolve this discrepancy between accuracy and precision in measuring transit depths with K2.…”

Section: Is K2-97b Inflated?mentioning

confidence: 99%

K2-97b: A (RE-?)INFLATED PLANET ORBITING A RED GIANT STAR

et al. 2016

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Strongly irradiated giant planets are observed to have radii larger than thermal evolution models predict. Although these inflated planets have been known for over 15 years, it is unclear whether their inflation is caused by thedeposition of energy from the host staror theinhibited cooling of the planet. These processes can be distinguished if the planet becomes highly irradiated only when the host star evolves onto the red giant branch. We report the discovery of K2-97b, a 1.31±0.11 R J , 1.10±0.11 M J planet orbiting a 4.20±0.14 R e , 1.16±0.12 M e red giant star with an orbital period of 8.4 days. We precisely constrained stellar and planetary parameters by combining asteroseismology, spectroscopy, and granulation noise modeling along with transit and radial velocity measurements. The uncertainty in planet radius is dominated by systematic differences in transit depth, which we measure to be up to 30% between different light-curve reduction methods. Our calculations indicate the incident flux on this planet was -+ 60140 times the incident flux on Earth, while the star was on the main sequence. Previous studies suggest that this incident flux is insufficient to delay planetary cooling enough to explain the present planet radius. This system thus provides the first evidence that planets may be inflated directly by incident stellar radiation rather than by delayed loss of heat from formation. Further studies of planets around red giant branch stars will confirm or contradict this hypothesisand may reveal a new class of re-inflated planets.

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

Cited by 120 publications

References 36 publications

The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets

The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets

SOPHIE velocimetry ofKeplertransit candidates

K2-97b: A (RE-?)INFLATED PLANET ORBITING A RED GIANT STAR

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