J/ApJS/204/24 Kepler planetary candidates. III. (Batalha+, 2013)
Planetary candidates observed by Kepler.
III. Analysis of the first 16 months of data.
Batalha N.M., Rowe J.F., Bryson S.T., Barclay T., Burke C.J.,
Caldwell D.A., Christiansen J.L., Mullally F., Thompson S.E., Brown T.M.,
Dupree A.K., Fabrycky D.C., Ford E.B., Fortney J.J., Gilliland R.L.,
Isaacson H., Latham D.W., Marcy G.W., Quinn S.N., Ragozzine D., Shporer A.,
Borucki W.J., Ciardi D.R., Gautier III T.N., Haas M.R., Jenkins J.M.,
Koch D.G., Lissauer J.J., Rapin W., Basri G.S., Boss A.P., Buchhave L.A.,
Carter J.A., Charbonneau D., Christensen-Dalsgaard J., Clarke B.D.,
Cochran W.D., Demory B.-O., Desert J.-M., Devore E., Doyle L.R.,
Esquerdo G.A., Everett M., Fressin F., Geary J.C., Girouard F.R., Gould A.,
Hall J.R., Holman M.J., Howard A.W., Howell S.B., Ibrahim K.A.,
Kinemuchi K., Kjeldsen H., Klaus T.C., Li J., Lucas P.W., Meibom S.,
Morris R.L., Prsa A., Quintana E., Sanderfer D.T., Sasselov D.,
Seader S.E., Smith J.C., Steffen J.H., Still M., Stumpe M.C., Tarter J.C.,
Tenenbaum P., Torres G., Twicken J.D., Uddin K., Van Cleve J.,
Walkowicz L., Welsh W.F.
<Astrophys. J. Suppl. Ser., 204, 24 (2013)>
=2013ApJS..204...24B 2013ApJS..204...24B
ADC_Keywords: Stars, double and multiple ; Planets ; Surveys ; Stars, dwarfs ;
Stars, diameters ; Stars, masses ; Effective temperatures
Keywords: catalogs - eclipses - planetary systems - space vehicles -
techniques: photometric
Abstract:
New transiting planet candidates are identified in 16 months (2009
May-2010 September) of data from the Kepler spacecraft. Nearly 5000
periodic transit-like signals are vetted against astrophysical and
instrumental false positives yielding 1108 viable new planet
candidates, bringing the total count up to over 2300. Improved vetting
metrics are employed, contributing to higher catalog reliability. Most
notable is the noise-weighted robust averaging of multi-quarter
photo-center offsets derived from difference image analysis that
identifies likely background eclipsing binaries. Twenty-two months of
photometry are used for the purpose of characterizing each of the
candidates. Ephemerides (transit epoch, T0, and orbital period, P)
are tabulated as well as the products of light curve modeling: reduced
radius (RP/R*), reduced semimajor axis (d/R*), and impact
parameter (b).
Description:
The data employed for transit identification were acquired between
2009 May 13 00:15 UTC and 2010 Sep 22 19:03 UTC (Q1-Q6). Over
190000 stars were observed at some time during this period.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 30 95 KOIs (old and new) noted as V-shaped
table3.dat 84 932 Host star characteristics
table4.dat 139 1108 Planet candidate characteristics: light curve
modeling
table5.dat 101 1108 Planet candidate characteristics and vetting metrics
table8.dat 75 24 *Planet candidates with 185K<Teq<303K
table9.dat 195 2338 Cumulative planet candidate catalog
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Note on table8.dat: Planet candidates in and near the habitable zone; plotted
in Figure 10.
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJ/728/117 : Kepler planetary candidates. I. (Borucki+, 2011)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/ApJ/736/L25 : Habitability of Kepler planet candidates (Kaltenegger+, 2011)
J/ApJ/738/170 : False positive probabilities for KOI (Morton+, 2011)
J/AJ/142/19 : Speckle observations of KOI (Howell+, 2011)
J/ApJS/197/2 : Transit timing observations from Kepler. I. (Ford+, 2011)
J/ApJS/199/24 : The first three quarters of Kepler mission (Tenenbaum+, 2012)
J/ApJS/199/30 : Effective temperature scale for KIC stars (Pinsonneault+, 2012)
J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 2012)
http://archive.stsci.edu/kepler/ : MAST Kepler home page
http://exoplanetarchive.ipac.caltech.edu/ : NASA exoplanet archive
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOI [51.01/2639.02] KOI identifier
9- 18 F10.2 d Per [-201292/498.39] Period (G2)
20- 23 F4.2 --- Rp/R* [0.02/0.66] Reduced planet radius
25- 30 F6.3 --- Grazing [-1.208/99.886] 1-b-RP/R* (1)
--------------------------------------------------------------------------------
Note (1): The complement of the impact parameter, b, minus the reduced
planet radius, RP/R*. This diagnostic serves as an indication of a
grazing, or V-shaped, transit. This value is negative if the purported
planet is not fully blocking the stellar disk at mid-transit. The closer
this number is to -2x(RP/R*), the more severely it is grazing.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- KOI [5/2841] Kepler Object of Interest number
6- 14 I9 --- KIC [1725016/12505654] Kepler Input Catalog Id
16- 22 F7.3 mag Kpmag [7.837/16.22] Kepler magnitude
24- 29 F6.1 10-6 CDPP [12.2/594.5] Combined 6hr Differential
Photometric Precision; parts per million (1)
31- 39 F9.5 h RAhour Right Ascension in decimal hours (J2000)
41- 48 F8.4 deg DEdeg Declination in decimal degrees (J2000)
50- 54 I5 K Teff [3240/9355] Stellar effective temperature
56- 60 F5.2 [cm/s2] log(g) [1.87/4.83] Log of stellar surface gravity
62- 67 F6.2 Rsun R* [0.45/19.16] Stellar radius R*
69- 73 F5.2 Msun M* [0.45/2.25] Stellar mass derived from log(g)
and R*
75 I1 --- n_Teff [0/3]? Method to derive stellar parameters (G3)
79- 84 I06 --- Obs [000000/111211] Six integers indicating
which quarters the star was observed (3)
--------------------------------------------------------------------------------
Note (1): RMS of Quarters 1 through 6 CDPP value in units of parts per million.
Note (3): Concatenation of six integers, one for each of the six quarters
of spacecraft data; zero indicates the star was not observed that
quarter; one indicates the star was observed. For example, a value of
000111 indicates the star was observed in quarters 4, 5, and 6 but not
in quarters 1, 2, or 3. Stars located on CCD Module 3 during Q4 have
an integer value of 2 for the fourth integer.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOI [5.02/2841.01] Kepler Object of Interest id
9- 15 F7.4 h Dur [0.3/33.6] Transit duration, first contact
to last contact
17- 21 I5 10-6 Depth [20/21002] Transit depth at center of transit;
part per million
23- 27 F5.1 --- SNR [5/450] Total SNR of all transits detected (1)
29- 37 F9.5 d t0 Time of a transit center; BJD-2454900 (G2)
39- 47 F9.5 d e_t0 ?=-99 Uncertainty in t0
49- 61 F13.7 d Per [-1548/346] Average interval between
transits, negative if estimation (G2)
63- 73 F11.7 d e_Per ?=-99 Uncertainty in Per
75- 84 F10.6 --- d/R* ?=-99 Ratio of planet-star separation to stellar
radius (3)
86- 95 F10.6 --- e_d/R* ?=-99 Uncertainty in d/R*
97-103 F7.5 --- r/R* Ratio of planet radius to stellar radius
105-113 F9.5 --- e_r/R* ?=-99 Uncertainty in r/R*
115-123 F9.5 --- b ?=-99 Impact parameter of transit (4)
125-133 F9.5 --- e_b ?=-99 Uncertainty in b
135-139 F5.2 --- Chi [0.39/17.45] Goodness of fit metric
--------------------------------------------------------------------------------
Note (1): SNR of the phase folded transit signal computed from modeling of
Quarter 1 through Quarter 8 data. detection pipeline using
Quarter 1 - Quarter 8 data.
Note (3): To first order, this parameter is equivalent to the ratio of the
planet-star separation (at the time of transit) to the stellar radius.
In the case of a zero eccentricity orbit, it is equivalent to the
reduced semi-major axis, a/R*.
Note (4): Note that there is a strong co-variance between b and d/R*.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOI [5.02/2841.01] Kepler Object of Interest id (G1)
9- 21 F13.7 d Per [-1548/346] Average interval between transits (G2)
23- 27 F5.2 Rgeo Rp [0.3/58.1] Planetary radius in Earth radii
(=6378km) (5)
29- 35 F7.3 AU a [0.01/0.99]?=-99 Semi-major axis of orbit (6)
37- 40 I4 K Teq [187/3866]?=-99 Equilibrium temperature of
planet (7)
42- 47 F6.2 --- O/E1 [0/28.5]?=-99 Ratio of odd to even numbered
transit depths derived from light curve modeling
49- 54 F6.2 --- O/E2 [0/6.46]?=-99 Ratio of odd to even numbered
transit depths reported by Data Validation
pipeline
56- 61 F6.2 --- Occ ?=-99 Relative flux level at phase=0.5 divided
by noise
63- 68 F6.2 arcsec dra ?=-99 Source position in RA relative to target (8)
70- 75 F6.2 arcsec e_dra ?=-99 Uncertainty in dra
77- 82 F6.2 arcsec ddec [-15/11]?=-99 Source position in DEC
relative to target (8)
84- 89 F6.2 arcsec e_ddec ?=-99 Uncertainty in ddec
91- 95 F5.1 --- Dist [0/51.5]?=-99 Distance to source position divided
by noise
97-101 F5.1 --- MES [0/170]?=-99 Multiple Event Statistic; MES (9)
--------------------------------------------------------------------------------
Note (5): Product of r/R* and the stellar radius given in Table 1.
Note (6): Based on Newton's generalization of Kepler's third law and the
stellar mass in Table 1.
Note (7): See main text for discussion.
Note (8): Offset is transit source position minus target star position.
Note (9): Reported by the pre-release SOC 7.0 TPS pipeline run on Q1-Q6 data;
MES is the detection statistic akin to a total SNR of the phase-folded
transit but constructed using the matched filter correlation
statistics over phase and period.
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOI [119.02/2841.01] KOI identifier
9- 15 F7.3 d Per [34/346] Average interval between transits
17- 21 F5.2 Rgeo Rp [1/21] Planetary radius Rp in Earth radii
23- 25 I3 K Teq [187/300] Equilibrium temperature
27- 29 F3.1 --- O/E1 [0/2.6] Ratio of odd to even numbered transit
depths derived from light curve modeling
31- 35 F5.1 --- Offset [0.6/3.2]?=-99 Distance to source position
divided by noise
37- 41 F5.1 --- MES [7/20.2]?=-99 Multiple Event Statistic
43- 47 F5.1 --- S/N [7.1/209.8] Total SNR of all transits detected
49- 52 I4 K Teff1 Stellar effective temperature (1)
54- 57 F4.2 [cm/s2] logg1 Log of stellar surface gravity (1)
59- 61 F3.1 Rsun R*1 Stellar radius (1)
63- 66 I4 K Teff2 Stellar effective temperature (2)
68- 71 F4.2 [cm/s2] logg2 Log of stellar surface gravity (2)
73- 75 F3.1 Rsun R*2 Stellar radius (2)
--------------------------------------------------------------------------------
Note (1): Original values from the Kepler Input Catalog are displayed here
unless spectroscopic stellar parameters are available.
Note (2): Values reproduced from Table 3. Here, Kepler Input Catalog values are
updated using the Yonsei-Yale evolutionary tracks as described in
Section 5.2.
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Byte-by-byte Description of file: table9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOI [1.01/2841.01] Kepler Object of Interest id (G1)
9- 16 I8 --- KIC Kepler Input Catalog Identifier
18- 23 F6.3 mag Kpmag [7.8/16.5] Kepler magnitude
25- 33 F9.5 d t0 Time of a transit center; BJD-2454900 (G2)
35- 43 F9.5 d e_t0 ?=-99 Uncertainty in t0
45- 59 F15.7 d Per Average interval between transits (G2)
61- 71 F11.7 d e_Per ?=-99 Uncertainty in Per
73- 77 F5.2 Rgeo Rp [0.34/90.5] Planetary radius in Earth
radii=6378km (3)
79- 85 F7.3 AU a ?=-99 Semi-major axis of orbit (4)
87- 90 I4 K Teq ?=-99 Equilibrium temperature of planet (5)
92- 98 F7.4 h Dur Transit duration, first contact to last contact
100-104 I5 10-6 Depth [20/86080] Transit depth at center of transit;
part per million
106-115 F10.6 --- d/R* ?=-99 Ratio of planet-star separation to stellar
radius (6)
117-126 F10.6 --- e_d/R* ?=-99 Uncertainty in d/R*
128-134 F7.5 --- r/R* Ratio of planet radius to stellar radius
136-144 F9.5 --- e_r/R* ?=-99 Uncertainty in r/R*
146-154 F9.5 --- b ?=-99 Impact parameter of transit (7)
156-164 F9.5 --- e_b ?=-99 Uncertainty in b
166-171 F6.1 --- SNR Total SNR of all transits detected (8)
173-177 F5.2 --- Chi Goodness of fit metric
179-182 I4 K Teff Stellar effective temperature
184-187 F4.2 [cm/s2] log(g) Log of stellar surface gravity
189-193 F5.2 Rsun R* Stellar radius
195 I1 --- n_Teff [0/3] Method to derive stellar parameters (G3)
--------------------------------------------------------------------------------
Note (3): Product of r/R* and the stellar radius given in Table 1.
Note (4): Based on Newton's generalization of Kepler's third law and the
stellar mass in Table 1.
Note (5): See main text for discussion.
Note (6): To first order, this parameter is equivalent to the ratio of the
planet-star separation (at the time of transit) to the stellar radius.
In the case of a zero eccentricity orbit, it is equivalent to the
reduced semi-major axis, a/R*.
Note (7): Note that there is a strong co-variance between b and a/R*.
Note (8): SNR of the phase folded transit signal computed from modeling of
Quarter 1 through Quarter 8 data.
--------------------------------------------------------------------------------
Global notes:
Note (G1): In all columns, zero denotes a value smaller than
the recorded precision.
Note (G2): Period based on a linear fit to all observed transits. For
candidates with only one observed transit, the period is estimated
from the duration and knowledge of the stellar radius; values are then
rounded to the nearest integer and multiplied by -1.
Note (G3): Method as follows:
0 = Teff,log(g), and R* are derived using KIC J-K color and linear
interpolation of luminosity class V stellar properties of
Schmidt-Kaler (1982, Landolt-Bornstein New Series, Group 6, Vol. 2b,
Stars and Star Clusters, ed. K. Schaifers & H.-H. Voigt (Berlin:
Springer), 1).
1 = KIC Teff and log(g) are used as initial values for a parameter search
of Yonsei-Yale stellar evolution models yielding Teff, log(g), and R*.
2 = Teff, log(g), and R* are derived using SPC spectral synthesis and
interpolation of the Yale-Yonsei evolutionary tracks.
3 = Teff, log(g), and R* are derived using SME spectral synthesis and
interpolation of the Yale-Yonsei evolutionary tracks.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Borucki et al. Paper I. 2011ApJ...728..117B 2011ApJ...728..117B Cat. J/ApJ/728/117
Borucki et al. Paper II. 2011ApJ...736...19B 2011ApJ...736...19B Cat. J/ApJ/736/19
Burke et al. Paper IV. 2014ApJS..210...19B 2014ApJS..210...19B Cat. J/ApJS/210/19
Rowe et al. Paper V. 2015ApJS..217...16R 2015ApJS..217...16R Cat. J/ApJS/217/16
Mullally et al. Paper VI. 2015ApJS..217...31M 2015ApJS..217...31M Cat. J/ApJS/217/31
Coughlin et al. Paper VII. 2016ApJS..224...12C 2016ApJS..224...12C Cat. J/ApJS/224/12
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 13-Mar-2013