TRANSIT TIMING OBSERVATIONS FROM
                    <i>KEPLER</i>
                    . VIII. CATALOG OF TRANSIT TIMING MEASUREMENTS OF THE FIRST TWELVE QUARTERS

Mazeh, T.; Nachmani, Gil; Holczer, Tomer; Fabrycky, Daniel C.; Ford, Eric B.; Sanchis-Ojeda, Roberto; Sokol, G. V.; Rowe, Jason F.; Zucker, S.; Agol, Eric; Carter, Joshua A.; Lissauer, Jack J.; Quintana, Elisa V.; Ragozzine, Darin; Steffen, Jason H.; Welsh, William F.

doi:10.1088/0067-0049/208/2/16

Cited by 174 publications

(226 citation statements)

References 43 publications

(42 reference statements)

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“…This rate is substantially higher than that reported by Mazeh et al (2013), who find 130 KOIs with significant TTVs out of a total sample of 1897 i.e., (6.9 ± 0.6)%. This is incompatible with the rate seen for the TSAs beyond the inner edge of the habitable zone (as defined by Zsom et al 2013) at a level of 3.2 σ, meaning coincidental sample selection is highly improbable to be responsible.…”

Section: Ttv Systemscontrasting

confidence: 65%

“…Additionally, KOI-1174.01, KOI-490.02, andKOI-1274.01 (also known as Kepler-421b; Kipping et al 2014b) have fewer than three visible transits and were rejected. Finally, KOI-902.01 was reported by Mazeh et al (2013) to display high-amplitude (100 minutes) and long-period (3 years) TTVs, which are uncharacteristic of exomoons (Kipping 2009a), and so was also rejected. This resulted in the 16 KOIs listed in Table 1.…”

Section: Target Selection Automaticmentioning

confidence: 99%

“…This is incompatible with the rate seen for the TSAs beyond the inner edge of the habitable zone (as defined by Zsom et al 2013) at a level of 3.2 σ, meaning coincidental sample selection is highly improbable to be responsible. However, the sample studied by Mazeh et al (2013) casts a much wider net than the carefully selected targets of TSA. Specifically, this rate is for the 2321 KOIs in the Borucki et al (2011Borucki et al ( , 2012 catalogs with a SNR > 2.5 (giving 1960 KOIs) exhibiting 7 or more transits in the first 12 quarters of data (giving 1897 KOIs).…”

Section: Ttv Systemsmentioning

confidence: 99%

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THE HUNT FOR EXOMOONS WITHKEPLER(HEK). V. A SURVEY OF 41 PLANETARY CANDIDATES FOR EXOMOONS

Kipping

Schmitt²,

Huang

et al. 2015

ApJ

109

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We present a survey of 41 Kepler Objects of Interest (KOIs) for exomoons using Bayesian photodynamics, more than tripling the number of KOIs surveyed with this technique. We find no compelling evidence for exomoons although 13 KOIs yield spurious detections driven by instrumental artifacts, stellar activity, and/or perturbations from unseen bodies. Regarding the latter, we find seven KOIs exhibiting >5 σ evidence of transit timing variations, including the "mega-Earth" Kepler-10c, likely indicating an additional planet in that system. We exploit the moderately large sample of 57 unique KOIs surveyed to date to infer several useful statistics. For example, although there is a diverse range in sensitivities, we find that we are sensitive to Pluto-Charon mass-ratio systems for ;40% of KOIs studied and Earth-Moon mass-ratios for 1 in 8 cases. In terms of absolute mass, our limits probe down to 1.7 Ganymede masses, with a sensitivity to Earth-mass moons for 1 in 3 cases studied and to the smallest moons capable of sustaining an Earth-like atmosphere (0.3 M ⊕ ) for 1 in 4. Despite the lack of positive detections to date, we caution against drawing conclusions yet, since our most interesting objects remain under analysis. Finally, we point out that had we searched for the photometric transit signals of exomoons alone, rather than using photodynamics, we estimate that 1 in 4 KOIs would have erroneously been concluded to harbor exomoons due to residual time correlated noise in the Kepler data, posing a serious problem for alternative methods.

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Section: Ttv Systemscontrasting

confidence: 65%

Section: Target Selection Automaticmentioning

confidence: 99%

Section: Ttv Systemsmentioning

confidence: 99%

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THE HUNT FOR EXOMOONS WITHKEPLER(HEK). V. A SURVEY OF 41 PLANETARY CANDIDATES FOR EXOMOONS

Kipping

Schmitt²,

Huang

et al. 2015

ApJ

109

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show abstract

“…The TPS algorithm assumes equally spaced transits and fails to find the most extreme TTV cases. The QATS algorithm (Carter et al 2013) is better tuned to find such systems, and Mazeh et al (2013) provides a recent catalog of such systems detected with Kepler. Other complicated systems such as circumbinary planets (e.g., Doyle et al 2011) are typically also not detected.…”

Section: Caveatsmentioning

confidence: 99%

PLANETARY CANDIDATES OBSERVED BY KEPLER . VI. PLANET SAMPLE FROM Q1–Q16 (47 MONTHS)

Mullally

Coughlin

Thompson

et al. 2015

ApJS

Self Cite

259

224

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We present the sixth catalog of Kepler candidate planets based on nearly four years of high precision photometry. This catalog builds on the legacy of previous catalogs released by the Kepler project and includes 1493 new Kepler Objects of Interest (KOIs) of which 554 are planet candidates, and 131 of these candidates have best-fit radii <1.5 Å R . This brings the total number of KOIs and planet candidates to 7348 and 4175 respectively. We suspect that many of these new candidates at the low signal-to-noise ratio limit may be false alarms created by instrumental noise, and discuss our efforts to identify such objects. We re-evaluate all previously published KOIs with orbital periods of >50 days to provide a consistently vetted sample that can be used to improve planet occurrence rate calculations. We discuss the performance of our planet detection algorithms, and the consistency of our vetting products. The full catalog is publicly available at the NASA Exoplanet Archive.

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“…Given the length of our observation period, we cannot make any conclusion about more distant companions. In addition, Mazeh et al (2013) report no significant transit timing variations for this target. The high-eccentricity migration scenario cannot be favored yet.…”

Section: Koi-614bmentioning

confidence: 78%

SOPHIE velocimetry ofKeplertransit candidates

Almenara

Damiani

Bouchy

et al. 2015

A&A

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We report the validation and characterization of three new transiting exoplanets using SOPHIE radial velocities: KOI-614b, KOI-206b, and KOI-680b. KOI-614b has a mass of 2.86 ± 0.35 M Jup and a radius of 1.13 +0.26−0.18 R Jup , and it orbits a G0, metallic ([Fe/H] = 0.35 ± 0.15) dwarf in 12.9 days. Its mass and radius are familiar and compatible with standard planetary evolution models, so it is one of the few known transiting planets in this mass range to have an orbital period over ten days. With an equilibrium temperature of T eq = 1000 ± 45 K, this places KOI-614b at the transition between what is usually referred to as "hot" and "warm" Jupiters. KOI-206b has a mass of 2.82 ± 0.52 M Jup and a radius of 1.45 ± 0.16 R Jup , and it orbits a slightly evolved F7-type star in a 5.3-day orbit. It is a massive inflated hot Jupiter that is particularly challenging for planetary models because it requires unusually large amounts of additional dissipated energy in the planet. On the other hand, KOI-680b has a much lower mass of 0.84 ± 0.15 M Jup and requires less extra-dissipation to explain its uncommonly large radius of 1.99 ± 0.18 R Jup . It is one of the biggest transiting planets characterized so far, and it orbits a subgiant F9-star well on its way to the red giant stage, with an orbital period of 8.6 days. With host stars of masses of 1.46 ± 0.17 M and 1.54 ± 0.09 M , respectively, KOI-206b, and KOI-680b are interesting objects for theories of formation and survival of short-period planets around stars more massive than the Sun. For those two targets, we also find signs of a possible distant additional companion in the system.

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TRANSIT TIMING OBSERVATIONS FROM KEPLER . VIII. CATALOG OF TRANSIT TIMING MEASUREMENTS OF THE FIRST TWELVE QUARTERS

Cited by 174 publications

References 43 publications

THE HUNT FOR EXOMOONS WITHKEPLER(HEK). V. A SURVEY OF 41 PLANETARY CANDIDATES FOR EXOMOONS

THE HUNT FOR EXOMOONS WITHKEPLER(HEK). V. A SURVEY OF 41 PLANETARY CANDIDATES FOR EXOMOONS

PLANETARY CANDIDATES OBSERVED BY KEPLER . VI. PLANET SAMPLE FROM Q1–Q16 (47 MONTHS)

SOPHIE velocimetry ofKeplertransit candidates

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