Transit timing observations from Kepler - III. : Confirmation of four multiple planet systems by a Fourier-domain study of anticorrelated transit timing variations

By J. Steffen, D. Fabrycky, Eric B. Ford, J. Carter, J. D'esert, F. Fressin, M. Holman, Jack J. Lissauer, A. Moorhead, J. Rowe and 64 more. 2012

136 citations recorded by the source corpus.

We present a method to confirm the planetary nature of objects in systems with multiple transiting exoplanet candidates. This method involves a Fourier-domain analysis of the deviations in the transit times from a constant period that result from dynamical interactions within the system. The combination of observed anticorrelations in the transit times and mass constraints from dynamical stability allow us to claim the discovery of four planetary systems, Kepler-25, Kepler-26, Kepler-27 and Kepler-28, containing eight planets and one additional planet candidate.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/aa18188a0141e7285491d925c6a4888436d02202

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Charbonneau
2. Timothy Morton
3. Jon Fortney
4. G. Marcy
5. J. Winn
6. J. Johnson
7. E. Petigura
8. C. Dressing

In Instrumentation

1. D. Charbonneau
2. Timothy Morton
3. G. Marcy
4. Jon Fortney
5. E. Petigura
6. J. Winn
7. C. Dressing
8. J. Southworth

Citations in the corpus

• ECCENTRICITY FROM TRANSIT PHOTOMETRY: SMALL PLANETS IN KEPLER MULTI-PLANET SYSTEMS HAVE LOW ECCENTRICITIES (2015, background): “Kepler-25 (KOI-244) contains two planets in a near 2:1 resonance, discovered due to their anti-correlated TTVs (Steffen et al. 2012).”
• AN EFFICIENT AUTOMATED VALIDATION PROCEDURE FOR EXOPLANET TRANSIT CANDIDATES (2012, background): “…may be used to dynamically confirm the planets in the system (Holman et al. 2010; Lissauer et al. 2011; Cochran et al. 2011; Fabrycky et al. 2012; Ford et al. 2012; Steffen et al. 2012), but the number of systems for which this is feasible is still an overwhelming minority of all the candidates.”
• PASTIS: Bayesian extrasolar planet validation. I. General framework, models, and performance (2014, methodology): “…in the timing of transits due to the mutual gravitational influence of the planets can be used to measure their masses (for some successful examples of the application of this technique, see Holman et al. 2010a; Lissauer et al. 2011; Fabrycky et al. 2012; Ford et al. 2012; Steffen et al. 2012).”
• EXTRACTING PLANET MASS AND ECCENTRICITY FROM TTV DATA (2012, methodology): “This feature has been noted before and has been used to help confirm some Kepler planets (Steffen et al. 2012).”
• TRANSIT TIMING OBSERVATIONS FROM KEPLER. IX. CATALOG OF THE FULL LONG-CADENCE DATA SET (2016, methodology): “Therefore, it can be useful to perform a systematic TTV search of all KOIs, as was done by Ford et al. (2011, 2012b) and Steffen et al. (2012a) at the early stages of the mission.”
• FALSE POSITIVE PROBABILITIES FOR ALL KEPLER OBJECTS OF INTEREST: 1284 NEWLY VALIDATED PLANETS AND 428 LIKELY FALSE POSITIVES (2016, background): “…10027 6 California Institute of Technology, Pasadena, CA 91125, USA 7 Hubble Fellow ing variations (TTVs) in multi-planet systems (e.g., Ford et al. 2012; Steffen et al. 2012; Fabrycky et al. 2012; Steffen et al. 2013; Jontof-Hutter et al. 2015), but this still leaves the vast majority of…”
• PLANETARY CANDIDATES OBSERVED BY KEPLER IV: PLANET SAMPLE FROM Q1–Q8 (22 MONTHS) (2013, background): “…binary signals (e.g., Torres et al. 2011; Morton & Johnson 2011; Fressin et al. 2011; Borucki et al. 2012; Wang et al. 2013; Barclay et al. 2013), and transit time variations (e.g., Holman et al. 2010; Lissauer et al. 2011a; Fabrycky et al. 2012a; Ford et al. 2012; Steffen et al. 2012; Xie 2013).”
• Transit timing observations from Kepler - VII. Confirmation of 27 planets in 13 multiplanet systems via transit timing variations and orbital stability (2012, methodology): “…(Lissauer et al. 2011a), Kepler 18 (Cochran et al. 2011), and Kepler 36 (Carter et al. 2012)), 21 planets in 10 multiplanet systems have been confirmed by these new methods that we apply again here (Kepler systems 23 through 32, Fabrycky et al. (2012a); Ford et al. (2012a); Steffen et al. (2012a)).”
• One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c (2015, background): “…and PASTIS analyses of the probability of false positive scenarios (Torres et al. 2010b; Díaz et al. 2014), high resolution photometry to search for close companions (e.g. Everett et al. 2015; Lillo-Box et al. 2012, 2014; Law et al. 2014) or TTVs (e.g. Steffen et al. 2012; Nesvorný et al. 2014).”
• LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS (2015, unknown): “These are Kepler-10c (Fressin et al. 2011), Kepler11b (Lissauer et al. 2011), Kepler-14b (Buchhave et al. 2011), Kepler-18b,c (Cochran et al. 2011), Kepler19b Ballard et al. (2011), Kepler-20b,c Gautier et al. (2012), Kepler-22b (Borucki et al. 2012), Kepler25b,c (Steffen et al. 2012), Kepler-26c (S”
• DENSITIES AND ECCENTRICITIES OF 139 KEPLER PLANETS FROM TRANSIT TIME VARIATIONS (2013, background): “If these transit time variations (TTVs) can be detected, they can be used to characterize planets (Agol et al. 2005; Holman & Murray 2005; Steffen et al. 2013, 2012; Fabrycky et al. 2012; Nesvornỳ et al. 2012; Lithwick et al. 2012; Xie 2013).”
• FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY (2013, unknown): “We note that four unevolved hosts in our sample are confirmed planetary systems that until now had no available asteroseismic constraints: Kepler-4 (Borucki et al. 2010b), Kepler-14 (Buchhave et al. 2011), Kepler-23 (Ford et al. 2012), and Kepler-25 (Steffen et al. 2012a).”
• THE OCCURRENCE RATE OF SMALL PLANETS AROUND SMALL STARS (2013, methodology): “…for KOIs 248.01, 248.02, 886.01, and 886.02 (Kepler-49b, 49c, 54b, and 54c) from Steffen et al. (2012a), KOIs 250.01 and 250.02 (Kepler-26b and 26c) from Steffen et al. (2012b), KOIs 952.01 and 952.02 (Kepler-32b and 32c) from Fabrycky et al. (2012a), and KOIs 898.01 and 898.03 from Xie (2012).”
• VALIDATION OF KEPLER'S MULTIPLE PLANET CANDIDATES. III. LIGHT CURVE ANALYSIS AND ANNOUNCEMENT OF HUNDREDS OF NEW MULTI-PLANET SYSTEMS (2014, background): “…have also been confirmed from radial velocity (RV) detection (Marcy et al. 2013; Gautier et al. 2012), transit timing variations (Ford et al. 2011; Steffen et al. 2012), and planet validation techniques such as BLENDER (Torres et al. 2011; Fressin et al. 2012) and now through multiplicity boost…”
• TRANSIT TIMING OBSERVATIONS FROM KEPLER. VIII. CATALOG OF TRANSIT TIMING MEASUREMENTS OF THE FIRST TWELVE QUARTERS (2013, background): “It is interesting to compare the analysis of F11, F12, and Steffen et al. (2012b, 2013) on the one hand and the present results on the other hand, and see how doubling the time span can change our assessment (A color version of this figure is available in the online journal.) of the nature of the…”
• Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, unknown): “…−0.112 6.35 +1.05 −1.05 464.73 +14.88 −15.28 Kepler-109 Marcy et al. (2014) 244 4349452 6270± 79 -0.04±0.10 1.159+0.040−0.051 1.297 +0.015 −0.015 0.745 +0.009 −0.010 4.275 +0.007 −0.008 2.406 +0.126 −0.128 3.45 +0.81 −0.72 247.49 +7.96 −7.96 Kepler-25 Steffen et al. (2012) 245 8478994 5417±…”