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J/ApJ/790/31     Transit times and durations of three KOIs     (Nesvorny+, 2014)

Photo-dynamical analysis of three Kepler Objects of Interest with significant transit timing variations. Nesvorny D., Kipping D., Terrell D., Feroz F. <Astrophys. J., 790, 31 (2014)> =2014ApJ...790...31N (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Ephemerides Keywords: planets and satellites: detection - planets and satellites: dynamical evolution and stability - planets and satellites: individual: (KOI-227, KOI-319, KOI-884) Abstract: KOI-227, KOI-319 and KOI-884 are identified here as (at least) two planet systems. For KOI-319 and KOI-884, the observed Transit Timing Variations (TTVs) of the inner transiting planet are used to detect an outer non-transiting planet. The outer planet in KOI-884 is ≃2.6 Jupiter masses and has the orbital period just narrow of the 3:1 resonance with the inner planet (orbital period ratio 2.93). The distribution of parameters inferred from KOI-319.01's TTVs is bimodal with either a ≃1.6 Neptune-mass (MN) planet wide of the 5:3 resonance (period 80.1 days) or a ≃1 Saturn-mass planet wide of the 7:3 resonance (period 109.2 days). The radial velocity measurements can be used in this case to determine which of these parameter modes is correct. KOI-227.01's TTVs with large ≃10 hr amplitude can be obtained for planetary-mass companions in various major resonances. Based on the Bayesian evidence, the current TTV data favor the outer 2:1 resonance with a companion mass ≃1.5 MN, but this solution implies a very large density of KOI-227.01. The inner and outer 3:2 resonance solutions with sub-Neptune-mass companions are physically more plausible, but will need to be verified. Description: Briefly, our analysis consists of two steps. In the first step, we fit a transit model to the Kepler photometry. This gives us time, duration, and other basic parameters of each transit, and their relative uncertainties. In the second step, we attempt to model the inferred transit times and durations as being caused by the gravitational interaction with a planetary, stellar or lunar companion. Note that we do not require that the companion itself to be transiting, although cases with multiple transiting bodies can be accommodated as well (e.g., Kipping et al. 2014ApJ...784...28K). This two-step method is a useful alternative to a general photo-dynamical method, where a N-body integration scheme is used to directly fit the Kepler photometry (e.g., Carter et al. 2012Sci...337..556C). The main advantage of the general method is that it fits for a smaller number of parameters and more directly links computed uncertainties to the photometry. The main advantage of the two-step method is its transparency, which makes it easier to understand of how different dynamical parameters relate to the measured properties of transits. Objects: ---------------------------------------------------------- RA (ICRS) DE Designation(s) ---------------------------------------------------------- 18 57 24.49 +41 31 09.1 KOI-227 = KIC 6185476 19 20 28.20 +44 52 22.5 KOI-319 = KIC 8684730 19 14 34.21 +43 02 21.5 KOI-884 = KIC 7434875 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 92 134 Transit times and durations of KOI-227.01, KOI-319.01 and KOI-884.02
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/ApJS/197/2 : Transit timing observations from Kepler. I. (Ford+, 2011) J/ApJ/821/47 : KOI transit probabilities of multi-planet syst. (Brakensiek+, 2016) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 10 A10 --- ID Kepler identifier (KOI-227.01, KOI-319.01, KOI-884.02) 12- 14 I3 --- Cycle Cycle 16- 33 F18.12 d tau Modified Julian Date of mid-transit 35- 50 F16.14 d e_tau Error in tau 52- 70 F19.17 d T Transit duration 72- 92 F21.19 d e_T Error in T
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 17-Mar-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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