J/ApJ/750/113 Kepler TTVs. II. Confirmed multiplanet systems (Ford+, 2012)
Transit timing observations from Kepler.
II. Confirmation of two multiplanet systems via a non-parametric
correlation analysis.
Ford E.B., Fabrycky D.C., Steffen J.H., Carter J.A., Fressin F.,
Holman M.J., Lissauer J.J., Moorhead A.V., Morehead R.C., Ragozzine D.,
Rowe J.F., Welsh W.F., Allen C., Batalha N.M., Borucki W.J., Bryson S.T.,
Buchhave L.A., Burke C.J., Caldwell D.A., Charbonneau D., Clarke B.D.,
Cochran W.D., Desert J.-M., Endl M., Everett M.E., Fischer D.A.,
Gautier III T.N., Gilliland R.L., Jenkins J.M., Haas M.R., Horch E.,
Howell S.B., Ibrahim K.A., Isaacson H., Koch D.G., Latham D.W., Li J.,
Lucas P., MacQueen P.J., Marcy G.W., McCauliff S., Mullally F.R.,
Quinn S.N., Quintana E., Shporer A., Still M., Tenenbaum P., Thompson S.E.,
Torres G., Twicken J.D., Wohler B., (the Kepler Science Team)
<Astrophys. J., 750, 113 (2012)>
=2012ApJ...750..113F 2012ApJ...750..113F
ADC_Keywords: Stars, double and multiple ; Planets
Keywords: planetary systems - planets and satellites: detection -
planets and satellites: dynamical evolution and stability -
stars: individual (KIC 3231341, KIC 11512246, KOI-168, KOI-1102,
Kepler-23, Kepler-24) - techniques: miscellaneous
Abstract:
We present a new method for confirming transiting planets based on the
combination of transit timing variations (TTVs) and dynamical
stability. Correlated TTVs provide evidence that the pair of bodies is
in the same physical system. Orbital stability provides upper limits
for the masses of the transiting companions that are in the planetary
regime. This paper describes a non-parametric technique for
quantifying the statistical significance of TTVs based on the
correlation of two TTV data sets. We apply this method to an analysis
of the TTVs of two stars with multiple transiting planet candidates
identified by Kepler. We confirm four transiting planets in two
multiple-planet systems based on their TTVs and the constraints
imposed by dynamical stability. An additional three candidates in
these same systems are not confirmed as planets, but are likely to be
validated as real planets once further observations and analyses are
possible. If all were confirmed, these systems would be near 4:6:9 and
2:4:6:9 period commensurabilities. Our results demonstrate that TTVs
provide a powerful tool for confirming transiting planets, including
low-mass planets and planets around faint stars for which Doppler
follow-up is not practical with existing facilities. Continued Kepler
observations will dramatically improve the constraints on the planet
masses and orbits and provide sensitivity for detecting additional
non-transiting planets. If Kepler observations were extended to eight
years, then a similar analysis could likely confirm systems with
multiple closely spaced, small transiting planets in or near the
habitable zone of solar-type stars.
Description:
In this paper, we analyze Kepler observations of two stars taken from
Q0 (2009 May 13) through the end of Q6 (2010 September 22).
The Kepler Follow-up Observation Program (FOP) has obtained
high-resolution spectra of KOI host stars from the 10m Keck I
Observatory, the 3m Shane Telescope at Lick Observatory, 2.7m Harlan
J. Smith Telescope at McDonald Observatory, or the 1.5m Tillinghast
Reflector at Fred Lawrence Whipple Observatory (FLWO).
The Kepler mission follow-up observing program includes speckle
observations obtained at the WIYN 3.5m telescope located on Kitt Peak.
Classical imaging systems provide complementary observations with a
wider field of view. In particular, the Lick Observatory 1m Nickel
Telescope took an I-band image of Kepler-23 with a pixel scale of
0.368"/pixel and seeing of ∼1.5". For Kepler-24, the 2m Faulkes
Telescope North (FTN) provides SDSS-r' band images with a pixel scale
of 0.304"/pixel in the default 2x2 pixel binning mode, and a typical
seeing of ∼1.2".
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 78 7 Key properties of planets and planet candidates
table2.dat 35 361 Transit times for Kepler transiting
planet candidates during Q0-6
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/208/16 : Kepler transit timing observations. VIII. (Mazeh+, 2013)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/A+A/556/A150 : SWEETCat I. Stellar parameters for host stars (Santos+, 2013)
J/A+A/555/A58 : New Kepler planetary candidates (Ofir+, 2013)
J/A+A/552/A119 : Planet-star and moon-planet interaction (Saur+, 2013)
J/ApJ/750/114 : Kepler TTVs. IV. 4 multiple-planet systems (Fabrycky+, 2012)
J/MNRAS/421/2342 : Kepler systems transit timing observations (Steffen+, 2012)
J/MNRAS/420/L23 : Non-resonant Kepler planetary systems (Veras+, 2012)
J/ApJS/199/30 : KIC stars effective temperature scale (Pinsonneault+, 2012)
J/ApJS/199/24 : The first three quarters of Kepler mission (Tenenbaum+, 2012)
J/PASP/124/1279 : Q3 Kepler's combined photometry (Christiansen+, 2012)
J/A+A/529/A89 : Kepler satellite variability study (Debosscher+, 2011)
J/ApJS/197/8 : Kepler's cand. multiple transiting planets (Lissauer+, 2011)
J/ApJS/197/2 : Transit timing observations from Kepler. I. (Ford+, 2011)
J/ApJ/742/L19 : Kepler hot rocky planetary candidates (Miguel+, 2011)
J/ApJ/738/170 : False positive Kepler planet candidates (Morton+, 2011)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
http://archive.stsci.edu/kepler : MAST Kepler
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOI [168.01/1102.04] KOI designation
9- 18 A10 --- AName Kepler designation
20- 26 F7.4 d Epoch Epoch of transit (BJD-2454900)
28- 34 F7.4 d Per [4.2/19] Period
36- 39 F4.2 h Tdur [2.4/6.2] Transit duration
41- 43 F3.1 Rgeo Rp [1.7/3.2] Planet radius (1)
45- 49 F5.3 AU a [0.05/0.2] Semi-major axis (1)
51- 53 I3 --- nTT [23/103] Number of transit times measured in Q0-6
55- 60 F6.4 d sTT [0.009/0.05] Median timing uncertainty (σTT)
62- 67 F6.4 d rms [0.01/0.06]
69- 74 F6.4 d MAD [0.009/0.03] Median absolute deviation from
linear ephemeris measured during Q0-6
76- 78 F3.1 Mjup Mpm [0.8/2.7]? Planetary maximum mass (Mp,max) (2)
--------------------------------------------------------------------------------
Note (1): Updated to reflect stellar properties and dilution from Table 3.
Note (2): Based on assumption of dynamical stability and stellar mass from
Table 3 (Kepler-23: M*=1.11+0.09-0.12;
Kepler-24: M*=1.03+0.11-0.14).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOI Kepler Object of interest identifier (1)
9- 11 I3 --- n [0/115] Transit number
13- 20 F8.4 d tn Barycentric Julian date of transit (BJD-2454900) (2)
22- 28 F7.4 d TTV [-0.32/0.14] Transit Timing Variation
30- 35 F6.4 d e_TTV [0.007/0.09] The 1σ uncertainty in TTV
--------------------------------------------------------------------------------
Note (1):
168.01 = Kepler-23c
168.03 = Kepler-23b
1102.01 = Kepler-24c
1102.02 = Kepler-24b
Note (2): Best-fit linear ephemerides
168.01: tn = 66.292554 + n * 10.742052
168.02: tn = 80.565492 + n * 15.274994
168.03: tn = 71.302255 + n * 7.1072785
1102.01: tn = 70.585989 + n * 12.333487
1102.02: tn = 73.568866 + n * 8.1452511
1102.03: tn = 77.751210 + n * 18.998137
1102.04: tn = 70.071210 + n * 4.2442814
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Ford et al. Paper I. 2011ApJS..197....2F 2011ApJS..197....2F Cat. J/ApJS/197/2
Steffen et al. Paper III. 2012MNRAS.421.2342S 2012MNRAS.421.2342S Cat. J/MNRAS/421/2342
Fabrycky et al. Paper IV. 2012ApJ...750..114F 2012ApJ...750..114F Cat. J/ApJ/750/114
Ford et al. Paper V. 2012ApJ...756..185F 2012ApJ...756..185F
Steffen et al. Paper VI. 2012ApJ...756..186S 2012ApJ...756..186S
Steffen et al. Paper VII. 2013MNRAS.428.1077S 2013MNRAS.428.1077S
Mazeh et al. Paper VIII. 2013ApJS..208...16M 2013ApJS..208...16M Cat. J/ApJS/208/16
Holczer et al. Paper IX. 2016ApJS..225....9H 2016ApJS..225....9H Cat. J/ApJS/225/9
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 06-Dec-2013