J/ApJS/208/22 Transit timing variation for 12 planetary pairs (Xie, 2013)
Transit timing variation of near-resonance planetary pairs: confirmation of 12
multiple-planet systems.
Xie J.-W.
<Astrophys. J. Suppl. Ser., 208, 22 (2013)>
=2013ApJS..208...22X 2013ApJS..208...22X
ADC_Keywords: Planets ; Stars, double and multiple ; Photometry
Keywords: planetary systems - planets and satellites: detection -
planets and satellites: dynamical evolution and stability
Abstract:
We extract transit timing variation (TTV) signals for 12 pairs of
transiting planet candidates that are near first-order mean motion
resonances (MMR), using publicly available Kepler light curves
(Q0-Q14). These pairs show significant sinusoidal TTVs with
theoretically predicted periods, which demonstrate these planet
candidates are orbiting and interacting in the same system. Although
individual masses cannot be accurately extracted based only on TTVs
because of the well-known degeneracy between mass and eccentricity,
TTV phases and amplitudes can still place upper limits on the masses
of the candidates, confirming their planetary nature. Furthermore, the
mass ratios of these planet pairs can be relatively tightly
constrained using these TTVs. The planetary pair in KOI 880 seems to
have particularly high mass and density ratios, which might indicate
very different internal compositions of these two planets. Some of
these newly confirmed planets are also near MMR with other candidates
in the system, forming unique resonance chains (e.g., KOI 500).
Description:
The data used in this paper are the long cadence (LC), "corrected"
light curves (PDC) of KOIs from Kepler Q0 to Q14, which are available
at the Multi-mission Archive at STScI (MAST).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 42 1806 Transit time measurements of 12 pairs of KOIs
table2.dat 98 12 Results of transit timing variation (TTV) analyses
for 12 pairs of planets
table3.dat 133 12 Key properties of planets and stars of the 12 systems
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/MNRAS/421/2342 : Kepler systems transit timing observations (Steffen+, 2012)
J/ApJS/197/8 : Kepler candidate multiple transiting planets (Lissauer+, 2011)
J/ApJS/197/2 : Transit timing observations from Kepler. I. (Ford+, 2011)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/ApJ/728/117 : Kepler planetary candidates. I. (Borucki+, 2011)
J/AJ/142/19 : Speckle observations of KOI (Howell+, 2011)
http://archive.stsci.edu/kepler/ : MAST Kepler home page
http://exoplanetarchive.ipac.caltech.edu/ : NASA exoplanet archive
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [KOI]
5- 11 F7.2 --- KOI [148.01/2038.02] Kepler object of interest number
13- 15 I3 --- Ntr [24/208] Number of transits
17- 19 I3 --- n [-6/260] Transit sequence identifier
21- 32 F12.7 d t Barycentric Julian Date of transit time;
BJD-2454900
34- 42 F9.7 d e_t [0.001/0.08] Uncertainty in t
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOI [148.01/2038.01] KOI name for the inner candidate
9- 15 F7.2 --- KOI' [148.02/2038.02] KOI name for the outer candidate
17 I1 --- j [2/4] j index
19- 24 F6.3 --- Delta [-0.03/0.04] Proximity Δ to resonance (see
equation (2)): 1+Δ=P'/P.(j-1)/j
26- 31 F6.1 d Pj [191/1009] TTV period (Pj=P'/j|Δ|)
33- 38 F6.4 d Attv [0.002/0.04] TTV amplitude for the inner candidate
40- 45 F6.4 d e_Attv Attv uncertainty
47- 52 F6.4 d A'ttv [0.001/0.05] TTV amplitude for the outer candidate
54- 59 F6.4 d e_A'ttv A'ttv uncertainty
61- 65 F5.1 deg phi [-46/93] TTV phase φ for the inner candidate
67- 70 F4.1 deg e_phi phi uncertainty
72- 76 F5.1 deg phi' [112/321] TTV phase for the outer candidate
78- 81 F4.1 deg e_phi' phi' uncertainty
83 A1 --- l_FAP1 Limit flag on FAP1
84- 90 E7.2 --- FAP1 [9e-05/0.0002] 1st set of false alarm probability
(FAP) analysis (1)
92 A1 --- l_FAP2 Limit flag on FAP1
93- 98 E6.2 --- FAP2 [0.0005/0.009] 2nd set of FAP analysis (1)
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Note (1): The first set of FAP analysis, i.e., FAP1, is based on the
Lomb-Scargle (LS) periodogram (Scargle 1982ApJ...263..835S 1982ApJ...263..835S;
Zechmeister & Kurster 2009A&A...496..577Z 2009A&A...496..577Z). The second set of FAP
analysis, i.e., FAP2, is based on refitting 104 sets of random
permutations of the original TTV data using the procedure mentioned in
Section 3.1 but with the LM fitting algorithm. See section 3.2 for
further explanations.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 --- KOI [148.01/2038.01] KOI id for the inner candidate
9- 15 F7.2 --- KOI' [148.02/2038.02] KOI id for the outer candidate
17- 22 F6.3 d P [4/27] Orbital period of the inner candidate (2)
24- 29 F6.3 d P' [9/52] Orbital period of the outer candidate (2)
31- 34 F4.2 Rgeo R [1.9/4] Radius of the inner candidate
36- 39 F4.2 Rgeo e_R R uncertainty (3)
41- 44 F4.2 Rgeo R' [1.5/5.4] Radius of the outer candidate
46- 49 F4.2 Rgeo e_R' R' uncertainty (3)
51- 54 F4.1 Mgeo Mnom [5/92] Nominal mass of the inner candidate (4)
56- 60 F5.1 Mgeo B_Mnom Upper limit for Mnom (4)
62- 65 F4.1 Mgeo b_Mnom Lower limit fo Mnom (4)
67- 70 F4.1 Mgeo M'nom [4/34] Nominal mass of the outer candidate (4)
72- 75 F4.1 Mgeo B_M'nom Upper limit for M'nom (4)
77- 80 F4.1 Mgeo b_M'nom Lower limit for M'nom (4)
82- 87 F6.1 Mgeo Mmax [30/7664] Inner candidate maximum mass (5)
89- 93 F5.1 Mgeo M'max [8/676] Maximum mass of the outer candidate (5)
95- 98 F4.2 Msun M* [0.5/1.1] Stellar mass derived from log.g and R*
100-103 F4.2 Msun E_M* Positive error on M*
105-108 F4.2 Msun e_M* Negative error on M*
110-113 F4.2 [cm/s2] logg [4.1/4.8] Surface gravity (6)
115-118 F4.2 [cm/s2] e_logg logg uncertainty (6)
120-123 F4.2 Rsun R* [0.5/1.5] Stellar radius (6)
125-128 F4.2 Rsun e_R* R* uncertainty (6)
130-133 F4.2 --- xi [0.7/1.2] Normalized transits duration ratio (7)
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Note (2): Uncertainties are all less than 10-3 days.
Note (3): Error bars reflect the uncertainties of the transit light-curve
fittings (i.e., Rp/R*) and stellar radii.
Note (4): Derived from Equation (8). Error bars reflect the uncertainties of the
Transit Time Variation (TTV) amplitudes and stellar masses.
Note (5): Obtained from Monte Carlo simulations as described in Section 3.3.
Note (6): For KOI = 829, 1589, and 2038, stellar parameters are adopted from
Everett et al. (2013ApJ...771..107E 2013ApJ...771..107E); otherwise, they are adopted from
the NASA exoplanet archive (http://exoplanetarchive.ipac.caltech.edu).
Note (7): Normalized transits duration ratio, ξ=(Tdur/T'dur)(P'/P)1/3
(Fabrycky et al. 2012arXiv1202.6328F 2012arXiv1202.6328F).
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History:
From electronic version of the journal
References:
Lithwick et al. 2012ApJ...761..122L 2012ApJ...761..122L
Xie J.-W. Paper II. 2014ApJS..210...25X 2014ApJS..210...25X Cat. J/ApJS/210/25
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 29-Oct-2013