VALIDATION OF KEPLER'S MULTIPLE PLANET CANDIDATES. III. LIGHT CURVE ANALYSIS AND ANNOUNCEMENT OF HUNDREDS OF NEW MULTI-PLANET SYSTEMS

By J. Rowe, S. Bryson, G. Marcy, Jack J. Lissauer, D. Jontof-Hutter, F. Mullally, R. Gilliland, Howard Issacson, Eric B. Ford, S. Howell and 19 more. 2014

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The Kepler mission has discovered more than 2500 exoplanet candidates in the first two years of spacecraft data, with approximately 40% of those in candidate multi-planet systems. The high rate of multiplicity combined with the low rate of identified false positives indicates that the multiplanet systems contain very few false positive signals due to other systems not gravitationally bound to the target star. False positives in the multi-planet systems are identified and removed, leaving behind a residual population of candidate multi-planet transiting systems expected to have a false positive rate less than 1%. We present a sample of 340 planetary systems that contain 851 planets that are validated to substantially better than the 99% confidence level; the vast majority of these have not been previously verified as planets. We expect ∼two unidentified false positives making our sample of planet very reliable. We present fundamental planetary properties of our sample based on a comprehensive analysis of Kepler light curves, ground-based spectroscopy, and high-resolution imaging. Since we do not require spectroscopy or high-resolution imaging for validation, some of our derived parameters for a planetary system may be systematically incorrect due to dilution from light due to additional stars in the photometric aperture. Nonetheless, our result nearly doubles the number verified exoplanets.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b2167e121beefea9f277cc169db64e551699931f

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Citations in the corpus

THE OCCURRENCE OF POTENTIALLY HABITABLE PLANETS ORBITING M DWARFS ESTIMATED FROM THE FULL KEPLER DATASET AND AN EMPIRICAL MEASUREMENT OF THE DETECTION SENSITIVITY (2015, methodology): “In those cases, we adopted the transit parameters found by Rowe et al. (2014) using a combined fit to the individual transit times and the planet properties.”
They are small worlds after all: revised properties of Kepler M dwarf stars and their planets (2015, result): “The fits from Swift et al. (2015) are generally consistent with those produced by the Kepler data validation fits (Rowe et al. 2014, 2015), with a median difference in RP /R∗ of just 0.2%, and 76% of RP /R∗ values agreeing within 1σ.”
How to Characterize Habitable Worlds and Signs of Life (2017, background): “Figure 5 shows all detected planets in the HZ as a function of the Teff of their host star and the incident stellar irradiation Seff; other recent lists of detected exoplanets can be found in the literature (e.g., Rowe et al. 2014, Kane et al. 2016).”
Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, neutral): “…1.117+0.040−0.049 1.632 +0.018 −0.009 0.361 +0.006 −0.010 4.056 +0.013 −0.010 3.183 +0.293 −0.202 6.23 +0.56 −1.23 413.44 +13.21 −12.61 Kepler-128 Xie (2014) 275 10586004 5770± 83 0.29±0.10 1.178+0.021−0.030 1.653 +0.009 −0.012 0.367 +0.004 −0.005 4.071 +0.005 −0.005 2.749 +0.151 −0.155 6.43…”
BREEDING SUPER-EARTHS AND BIRTHING SUPER-PUFFS IN TRANSITIONAL DISKS (2015, background): “Super-Earths are found orbiting ∼60% of FGK-type dwarfs with periods < 85 days (Howard et al. 2010; Batalha et al. 2013; Petigura et al. 2013; Dong & Zhu 2013; Fressin et al. 2013; Rowe et al. 2014).”
Precise Radial Velocities of Giant Stars VII. Occurrence Rate of Giant Extrasolar Planets as a Function of Mass and Metallicity (2014, background): “The rate of detection and confirmation of exoplanets has increased dramatically in the recent past, with almost one third of exoplanets confirmed in early 2014 alone (Rowe et al. 2014; Lissauer et al. 2014) and another third being discovered only during the last two years.”
PLANETARY CANDIDATES FROM THE FIRST YEAR OF THE K2 MISSION (2015, background): “…has been highly successful, finding thousands of planetary candidates (Borucki et al. 2011; Mullally et al. 2015), the majority of which are likely genuine transiting exoplanets (Morton & Johnson 2011; Morton 2012a; Fressin et al. 2013; Lissauer et al. 2012; Rowe et al. 2014; Santerne et al. 2015).”
AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS (2015, methodology): “We measured the properties of the five planets in a similar manner to that described in Rowe et al. (2014), who used the same transiting-planet model.”
THE KEPLER FOLLOW-UP OBSERVATION PROGRAM. I. A CATALOG OF COMPANIONS TO KEPLER STARS FROM HIGH-RESOLUTION IMAGING (2016, methodology): “…planet radii due to very uncertain stellar radii or unreliable transit fits by the Kepler pipeline (see, e.g., KOI 1298.02 and KOI 2092.03 with Rp of 39 and 30 R⊕, respectively, from the KOI table, which were validated as planets with radii of 1.82 R⊕ and 4.01R⊕, respectively; Rowe et al. 2014).”
One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c (2015, methodology): “The only system we could find with a closer normalised distance to resonance (defined in Lithwick et al. 2012), 4, was the Kepler-372cd pair (Rowe et al. 2014), where 4 is ∼0.0003, as compared to K2-19 with ∼0.0023.”
PLANETARY CANDIDATES OBSERVED BY KEPLER. VI. PLANET SAMPLE FROM Q1–Q16 (47 MONTHS) (2015, methodology): “Because the Lissauer et al. (2012) analysis does not include a treatment of nonastrophysical false alarms (Rowe et al. 2014), which is a concern for the outer most candidate, we do not claim K02194.”
ECCENTRICITY FROM TRANSIT PHOTOMETRY: SMALL PLANETS IN KEPLER MULTI-PLANET SYSTEMS HAVE LOW ECCENTRICITIES (2015, methodology): “Kepler-197 (KOI-623) contains four transiting planets with periods 5, 10, 15 and 25 days, which were validated statistically (Rowe et al. 2014; Lissauer et al. 2014).”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, background): “About 1 in 5 Sunlike stars harbor planets having radii of 1–4 R⊕ at distances of 0.05–0.3 AU (Howard et al. 2010; Batalha et al. 2013; Petigura et al. 2013; Dong & Zhu 2013; Fressin et al. 2013; Rowe et al. 2014).”
DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R⨁ SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR (2015, methodology): “…discoveries include Kepler-62e and f (Borucki et al. 2013), Kepler-186f (Quintana et al. 2014), a few among the multitude of planets reported by Rowe et al. (2014): Kepler-283c, Kepler-296e and f; and a set of small planets announced in Torres et al. (2015): Kepler-438b, Kepler-440b, and…”
TRANSIT TIMING OBSERVATIONS FROM KEPLER. IX. CATALOG OF THE FULL LONG-CADENCE DATA SET (2016, background): “(1) Cochran et al. (2011), (2) Xie (2014), (3) Rowe et al. (2014), (4) Lissauer et al. (2011a), (5) Ford et al. (2012a), (6) Steffen et al. (2012a), (7) Steffen et al. (2013), (8) Carter et al. (2012), (9) Kipping et al. (2014), (10) Holman et al. (2010), (11) Masuda (2014), (12) Fabrycky et al.…”
Identifying Exoplanets with Deep Learning: A Five-planet Resonant Chain around Kepler-80 and an Eighth Planet around Kepler-90 (2017, background): “…Borucki et al. 2011a,b; Batalha et al. 2013; Burke et al. 2014; Rowe et al. 2015; Mullally et al. 2015; Coughlin et al. 2016; Thompson et al. 2017; Rowe et al. 2014; Morton et al. 2016), and significantly improved our understanding of the population of small planets in the inner parts of…”
LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS (2015, methodology): “Eleven of these systems have been validated by Rowe et al. (2014) using statistical arguments from Lissauer et al. (2012, 2014) and Q1Q8 Kepler data.”