J/MNRAS/429/2001 New transiting planet candidates from Kepler (Huang+, 2013)
150 new transiting planet candidates from Kepler Q1-Q6 data.
Huang X., Bakos G.A., Hartman J.D.
<Mon. Not. R. Astron. Soc., 429, 2001-2018 (2013)>
=2013MNRAS.429.2001H 2013MNRAS.429.2001H
ADC_Keywords: Stars, double and multiple ; Planets
Keywords: planets and satellites: detection - planetary systems
Abstract:
We have performed an extensive search for planet candidates in the
publicly available Kepler long cadence data from quarters Q1 through
Q6. The search method consists of initial de-trending of the data,
applying the trend filtering algorithm, searching for transit signals
with the Box Least Squares fitting method in three frequency domains,
visual inspection of the potential transit candidates and an in-depth
analysis of the shortlisted candidates. In this paper we present 150
new periodic planet candidates and seven single transit events, 72 of
which are in multiple systems. The periods of these planet candidates
vary from ∼0.17 to ∼440d. 124 of the planet candidates have radii
smaller than 3R{earth}. We recover 82.5 per cent of the Batalha et
al. (2012, Cat. J/ApJS/204/24). Kepler Objects of Interest (KOI)
catalogue. We also report 40 newly identified false positives -
systems that look like transiting planets, but are probably due to
blended eclipsing binaries. Our search improves the statistics in the
short-period and small-planet radii parameter ranges.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 106 2321 Detection report of KOIs
table3.dat 89 40 *False positive (FP) list
table4.dat 50 137 Stellar parameter table
table5.dat 156 157 Planet candidates table
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Note on table3.dat: We only report the FPs not in the Kepler FP catalogue here.
We do not report FPs in single transit events. These FPs are all identified
by examining the centroids. We refer to the text for a detailed description
of the method.
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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/ApJS/199/24 : The first three quarters of Kepler mission (Tenenbaum+, 2012)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/A+A/555/A58 : New Kepler planetary candidates (Ofir+, 2013)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 --- KOI KOI (Kepler Object of Interest) planet number
9- 16 I8 --- KIC KIC star number (Cat. V/133)
18- 31 F14.6 d PerK Kepler period
33- 44 F12.7 d Per ? Period from BLS analysis (1)
46- 56 F11.6 d EpK Kepler epoch (BJD-2454000)
57- 68 F12.7 d Ep ? Epoch (BJD-2454000)
69 A1 --- l_Dip Limit flag on Dip
70- 77 E8.4 mag Dip ?=- Dip magnitude from BLS analysis (1)
80- 87 E8.3 --- Q ?=- Dimensionless parameter representing the
transit duration. Defined as Tdur/P (1)
89- 95 F7.3 --- SNR ? Signal-to-noise ratio measured in the BLS
spectrum
96-102 F7.3 --- DSP ? Dip significance
103-106 A4 --- Com Comments (2)
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Note (1): We compare the parameters of KOIs with the Batalha et al. 2012
(J/ApJS/204/24) catalogue. The period, epoch, dip and q are taken from
our box least-square fitting (BLS) analysis instead of modelling the
candidates.
Note (2): Comments as follows:
sod = (short of data): KOIs do not have sufficient length of LC data to
fulfil the requirement of TFA. They are not selected for our reanalysis.
wp = (wrong period): KOIs recovered with a wrong period. For some planet
candidates, the harmonics of the KOI period (or other periods due to the
imperfect correction of the light curve) show higher SNR and DSP in the
BLS analysis. The SNR and DSP values reported here correspond to the
detected signal instead of the KOI period. In other cases, frequencies
not related to the signal are detected, the true signal is recovered in
visual inspection, we fill the SNR and DSP with '-'.
snd = (single transit, no detection): KOIs with a single transit, and all the
reported BLS peaks, are under our selection limits.
ld = (low DSP): KOIs with lower DSP than our selection limits, therefore not
recovered in our selection process.
lr = (large radius): KOIs with transit dip larger than 0.04, therefore not
selected for analysis.
ls = (low SNR): KOIs with lower SNR than our selection limits, therefore not
recovered in our selection process.
nd = (no detection): KOIs for which the first five BLS peaks are under our
selection limits, and the correct period is not one of the first
five BLS peaks.
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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- 8 I8 --- KIC KIC star number
9 A1 --- n_KIC [c] there are visible companion(s) in the
2MASS image stamp within 20x20arcsec2
11- 16 F6.3 d PerK Kepler period
18- 19 I2 h RAh Right ascension (J2000)
21- 22 I2 min RAm Right ascension (J2000)
24- 29 F6.3 s RAs Right ascension (J2000)
31 A1 --- DE- Declination sign (J2000)
32- 33 I2 deg DEd Declination (J2000)
35- 36 I2 arcmin DEm Declination (J2000)
38- 42 F5.2 arcsec DEs Declination (J2000)
44- 53 F10.5 d Epoch Epoch (BJD-2454000)
56- 65 F10.6 d Per Period
67- 73 F7.4 pix Xdisp ? Displacement along X (1)
75- 82 F8.5 pix Ydisp ? Displacement along Y (1)
84- 89 F6.2 --- SNR Signal-to-noise ratio measured in the BLS
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Note (1): The flux centroid displacement amplitude is computed from the phase
folded centroids. The x and y directions are listed separately. We do not
list a displacement when the shift is not detected.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC KIC star number
9 A1 --- n_KIC [d] Note on limb darkening coefficient (1)
10- 15 F6.3 mag Kpmag Kepler magnitude
17- 20 I4 K Teff ?=- Effective temperature
22- 26 F5.3 [cm/s2] logg ? Surface gravity
28- 33 F6.3 [Sun] [Fe/H] ? Metallicity
35- 40 F6.3 Rsun R* ? Stellar radius
42- 45 F4.2 --- ua Quadratic limb darkening parameter a
47- 50 F4.2 --- ub Quadratic limb darkening parameter b
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Note (1): d: The limb darkening coefficient is obtained from the estimated
stellar properties based on the J, H and K magnitudes.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC KIC star number
9 A1 --- n_KIC [b] indicates more than one set of values for
this star
11- 21 F11.6 d Epoch Epoch (BJD-2454000)
23- 28 F6.3 10-3d e_Epoch rms uncertainty on Epoch
30- 42 F13.8 d Per Period
43- 50 F8.5 10-4d e_Per ? rms uncertainty on Per
52- 60 F9.6 Rgeo Rp ? Planet radius in Earth radius unit
62- 69 F8.6 10-3 Rp/R* Fractional planet radius
71- 74 F4.2 Rgeo e_Rp rms uncertainty on radius
76- 81 F6.4 --- b [0/1]? Impact parameter
83- 88 F6.4 --- e_b [0/1]? rms uncertainty on b
91- 97 F7.3 d-1 zeta/R* Inverse of half transit duration (=2/Tdur)
99-104 F6.4 d-1 e_zeta/R* rms uncertainty on zeta/R*
108-115 F8.4 --- SNR ? Signal-to-noise ratio measured in the BLS
117-123 F7.4 --- DSP ? Dip significance
125-130 F6.3 --- chi2 χ2 value
132-156 A25 --- Com Comments (1)
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Note (1): Comments:
KOINNN = Stars already identified as KOIs. The candidates presented here are
transit signals that have not previously been detected in these
systems.
O12 = Planet candidates also identified by Ofir & Dreizler 2012
(J/A+A/555/A58).
T12 = Planet candidates classified as potential transit candidates by
Tenenbaum et al. 2012, Cat. J/ApJS/199/24.
If noted as T12t, the same signal is identified as a different set of
parameters by Tenenbaum et al., 2012, Cat. J/ApJS/199/24.
wp = The signal is selected by a different period originally and then
corrected by visual inspection. The SNR and DSP reported here
correspond to the period we report here instead of the selected period
PH = Planet candidates classified as potential transit candidates by
PlanetHunters. If noted as PHt, the transit feature is identified by
PlanetHunters but they did not report a period for comparison. These
information can be accessed through http://www.planethunters.org.
blend = Systems may be blended by nearby stars. There exists a visible
companion(s) within 20arcsec2 in a 2MASS image stamp centred on
the target star.
Lintott = Lintott et al., 2012, preprint (1202.6007)
Schwamb:2012 = Schwamb et al., 2012ApJ...754..129S 2012ApJ...754..129S
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 26-Mar-2014