J/AJ/157/218 Transiting planets near the snow line from Kepler (Kawahara+, 2019)
Transiting planets near the snow line from Kepler.
I. Catalog.
Kawahara H., Masuda K.
<Astron. J., 157, 218 (2019)>
=2019AJ....157..218K 2019AJ....157..218K (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Effective temperatures ;
Abundances, [Fe/H] ; Stars, masses ; Stars, diameters ;
Stars, ages ; Exoplanets
Keywords: planets and satellites: detection -
planets and satellites: individual - techniques: photometric
Abstract:
We present a comprehensive catalog of cool (period P≳2 yr) transiting
planet candidates in the 4 yr light curves from the prime Kepler mission.
Most of the candidates show only one or two transits and have largely
been missed in the original Kepler Object of Interest catalog. Our catalog
is based on all known such candidates in the literature, as well as
new candidates from the search in this paper, and provides a resource
to explore the planet population near the snow line of Sun-like stars.
We homogeneously performed pixel-level vetting, stellar characterization
with Gaia parallax and archival/Subaru spectroscopy, and light-curve
modeling to derive planet parameters and to eliminate stellar binaries.
The resulting clean sample consists of 67 planet candidates whose radii
are typically constrained to 5%, in which 23 are newly reported. The
number of Jupiter-sized candidates (29 with radius r>8 R⊕) in
the sample is consistent with the Doppler occurrence. The smaller
candidates are more prevalent (23 with 4<r/R⊕<8, 15 with
r/R⊕<4) and suggest that long-period Neptune-sized planets are
at least as common as the Jupiter-sized ones, although our sample is yet
to be corrected for detection completeness. If the sample is assumed to be
complete, these numbers imply the occurrence rate of 0.39±0.07 planets
with 4<r/R⊕<14 and 2<P/yr<20 per FGK dwarf. The stars hosting
candidates with r>4 R⊕ have systematically higher [Fe/H] than
do the Kepler field stars, providing evidence that giant planet-metallicity
correlation extends to P>2 yr.
Description:
First, we collected archival spectroscopic parameters from the California
Kepler Survey (CKS, Petigura et al. 2017, J/AJ/154/107), the Spectral
Properties of Cool Stars (SPOCS) catalog by Brewer et al. (2016,
J/ApJS/225/32), the Large Sky Area Multi-Object Fiber Spectroscopic
Telescope (LAMOST; Cui et al. 2012RAA....12.1197C 2012RAA....12.1197C; Luo et al. 2015,
Cat. V/146)/LASP stellar parameters (Wu et al. 2014IAUS..306..340W 2014IAUS..306..340W) from
DR4, The Payne (Ting et al. 2019ApJ...879...69T 2019ApJ...879...69T) parameters based on
APOGEE DR14 (Majewski et al. 2017AJ....154...94M 2017AJ....154...94M), and the Kepler input
catalog DR25 (Mathur et al. 2017, J/ApJS/229/30) with spectroscopic
provenance (KIC 6191521 alone, originally from Furlan et al. 2017,
J/AJ/153/71). For these stars, we adopted the literature values of
effective temperature Teff, surface gravity log g, and iron abundance
[Fe/H], with preferences given in this order. For stars without available
archival spectra, we obtained high-resolution spectra using the high
dispersion spectrograph (HDS; Noguchi et al. 2002PASJ...54..855N 2002PASJ...54..855N)
installed on the Subaru 8.2 m telescope. We mainly observed targets
brighter than r-mag=15 and without V-shaped dips. The observations were
performed on UT 2018 July 28, August 5, and September 6 (proposal IDs
S18A-044 and S18B-062, PI: Kawahara) with the standard I2a setup and
2x1 binning without an image rotator.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 132 100 Parameters of the host stars
table3.dat 167 67 Parameters of the systems in the clean sample
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
V/146 : LAMOST DR1 catalogs (Luo+, 2015)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/MNRAS/429/2001 : New transiting planet candidates from Kepler (Huang+, 2013)
J/ApJS/217/31 : Kepler planetary candidates. VI. 4yr Q1-Q16
(Mullally+, 2015)
J/AJ/152/158 : Final Kepler transiting planet search (DR25)
(Twicken+, 2016)
J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+, 2016)
J/AJ/153/71 : Kepler follow-up observation program. I. Imaging
(Furlan+, 2017)
J/AJ/154/107 : California-Kepler Survey (CKS). I. 1305 stars
(Petigura+, 2017)
J/ApJS/229/30 : Revised stellar properties of Q1-17 Kepler targets
(Mathur+, 2017)
J/AJ/155/89 : California-Kepler Survey (CKS). IV. Planets
(Petigura+, 2018)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC [1717722/12454613] Kepler Input Catalog
identifier
10- 11 A2 --- f_KIC Flag on KIC (G1)
13- 16 I4 K Teff [3942/9431] Effective temperature from
isochrone fit
18- 21 I4 K E_Teff [36/1344] Upper uncertainty in Teff
23- 25 I3 K e_Teff [43/796] Lower uncertainty in Teff
27- 31 F5.3 [cm/s2] log(g) [2.71/4.69] Log surface gravity from
isochrone fit
33- 37 F5.3 [cm/s2] E_log(g) [0.01/0.1] Upper uncertainty in log(g)
39- 43 F5.3 [cm/s2] e_log(g) [0.009/0.07] Lower uncertainty in log(g)
45- 49 F5.2 [Sun] [Fe/H] [-0.47/0.2] Metallicity from isochrone fit
51- 54 F4.2 [Sun] E_[Fe/H] [0.02/0.2] Upper uncertainty in [Fe/H]
56- 59 F4.2 [Sun] e_[Fe/H] [0.01/0.2] Lower uncertainty in [Fe/H]
61- 64 F4.2 Msun M* [0.59/2.65] Stellar mass from isochrone fit
66- 69 F4.2 Msun E_M* [0.01/0.3] Upper uncertainty in M*
71- 74 F4.2 Msun e_M* [0.01/0.2] Lower uncertainty in M*
76- 81 F6.3 Rsun R* [0.574/12] Stellar radius from isochrone fit
83- 87 F5.3 Rsun E_R* [0.006/0.6] Upper uncertainty in R*
89- 93 F5.3 Rsun e_R* [0.006/0.6] Lower uncertainty in R*
95- 99 F5.2 [yr] logAge [8.6/10.1] Log stellar age from isochrone fit
101-104 F4.2 [yr] E_logAge [0.02/0.3] Upper uncertainty in logAge
106-109 F4.2 [yr] e_logAge [0.03/0.6] Lower uncertainty in logAge
111-116 A6 --- Source Spectroscopic parameter source (1)
118-121 I4 K D-Teff [4227/8080]? Effective temperature from
Source
123-126 F4.2 [cm/s2] D-log(g) [2.96/4.6]? Log surface gravity from Source
128-132 F5.2 [Sun] D-[Fe/H] [-0.67/0.26]? Metallicity from Source
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Note (1): Source as follows:
HDS = This paper;
CKS = Petigura et al. (2017, J/AJ/154/107);
SPOCS = Brewer et al. (2016, J/ApJS/225/32);
LAMOST = LAMOST DR4 (Wu et al. 2014IAUS..306..340W 2014IAUS..306..340W);
APOGEE = Ting et al. (2018arXiv180401530T 2018arXiv180401530T);
M17 = Mathur et al. (2017, J/ApJS/229/30).
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC [3111510/12454613] Kepler Input Catalog
identifier
10- 12 A3 --- f_KIC Flag on KIC (G1)
14- 17 I4 --- KOI [99/8151]? Kepler Object of Interest identifier
19 A1 --- f_KOI [*] Flag on KOI (1)
21- 24 I4 --- Kepler [150/1475]? Kepler system number
26- 27 A2 --- n_Kepler FP if false positive, nothing if candidate
29- 32 F4.1 mag Kpmag [10.6/15.9] Apparent Kepler band magnitude
34- 37 F4.2 Msun M* [0.59/2.3] Median stellar mass
39- 42 F4.2 Msun E_M* [0.02/0.3] Upper uncertainty in M*
44- 47 F4.2 Msun e_M* [0.01/0.2] Lower uncertainty in M*
49- 53 F5.3 Rsun R* [0.582/3] Median stellar radius
55- 59 F5.3 Rsun E_R* [0.006/0.2] Upper uncertainty in R*
61- 65 F5.3 Rsun e_R* [0.006/0.2] Lower uncertainty in R*
67- 71 F5.2 Rgeo Rp [2.4/14] Median planetary radius
73- 76 F4.2 Rgeo E_Rp [0.08/2.1] Upper uncertainty in Rp
78- 81 F4.2 Rgeo e_Rp [0.06/1] Lower uncertainty in Rp
83- 91 F9.4 d t0 [140.049/1557.302] Median BKJD of mid transit
93- 98 F6.4 d E_t0 [0.0007/0.02] Upper uncertainty in t0
100-105 F6.4 d e_t0 [0.0007/0.02] Lower uncertainty in t0
107-119 E13.7 d P [307.554/8000] Median orbital period
121-128 E8.2 d E_P [0.0005/6000] Upper uncertainty in P
130-137 E8.2 d e_P [0.0005/4000] Lower uncertainty in P
139-142 F4.2 --- b [0.14/0.94] Median impact parameter
144-147 F4.2 --- E_b [0.02/0.3] Upper uncertainty in b
149-152 F4.2 --- e_b [0.02/0.4] Lower uncertainty in b
154-157 F4.2 --- e [0.06/0.92] Median eccentricity
159-162 F4.2 --- E_e [0.02/0.3] Upper uncertainty in e
164-167 F4.2 --- e_e [0.02/0.2] Lower uncertainty in e
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Note (1): Flag as follows:
* = These stars have KOI numbers because of the single and double transiting
events (STEs/DTEs) analyzed here; they are the only transiting planet
candidates.
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Global notes:
Note (G1): Flag as follows:
d = Stars with spectra;
s = Flat-bottomed transits with short ingress/egress; see Section 5.2;
b = Flagged as photometric binary by Berger et al. (2018ApJ...866...99B 2018ApJ...866...99B);
ab = Flagged as AO binary by Berger et al. (2018ApJ...866...99B 2018ApJ...866...99B).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 09-Aug-2019