J/ApJ/783/4 Properties of Kepler multi-planet candidate systems (Wang+, 2014)
Influence of stellar multiplicity on planet formation. I. Evidence of suppressed
planet formation due to stellar companions within 20 AU and validation of four
planets from the Kepler multiple planet candidates.
Wang J., Xie J.-W., Barclay T., Fischer D.A.
<Astrophys. J., 783, 4 (2014)>
=2014ApJ...783....4W 2014ApJ...783....4W (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Stars, masses ;
Effective temperatures ; Abundances, [Fe/H] ; Stars, diameters
Keywords: astronomical databases: miscellaneous - methods: numerical -
methods: observational - methods: statistical - planetary systems -
planets and satellites: formation - techniques: radial velocities
Abstract:
The planet occurrence rate for multiple stars is important in two
aspects. First, almost half of stellar systems in the solar
neighborhood are multiple systems. Second, the comparison of the
planet occurrence rate for multiple stars to that for single stars
sheds light on the influence of stellar multiplicity on planet
formation and evolution. We developed a method of distinguishing
planet occurrence rates for single and multiple stars. From a sample
of 138 bright (KP<13.5) Kepler multi-planet candidate systems, we
compared the stellar multiplicity rate of these planet host stars to
that of field stars. Using dynamical stability analyses and archival
Doppler measurements, we find that the stellar multiplicity rate of
planet host stars is significantly lower than field stars for
semimajor axes less than 20AU, suggesting that planet formation and
evolution are suppressed by the presence of a close-in companion star
at these separations. The influence of stellar multiplicity at larger
separations is uncertain because of search incompleteness due to a
limited Doppler observation time baseline and a lack of
high-resolution imaging observation. We calculated the planet
confidence for the sample of multi-planet candidates and find that the
planet confidences for KOI 82.01, KOI 115.01, KOI 282.01, and KOI
1781.02 are higher than 99.7% and thus validate the planetary nature
of these four planet candidates. This sample of bright Kepler
multi-planet candidates with refined stellar and orbital parameters,
planet confidence estimation, and nearby stellar companion
identification offers a well-characterized sample for future
theoretical and observational study.
Description:
Our sample consists of bright host stars with multi-planet transiting
systems from Kepler. Out of 5779 Kepler Objects of Interest
(http://exoplanetarchive.ipac.caltech.edu/), we selected all the
systems with a Kepler magnitude (KP) brighter than 13.5mag and with
at least two planet candidates. The sample includes 343 planet
candidates (see Table3) in 138 multi-planet candidate systems (see
Table2) from the Kepler mission. For these systems, we used archival
data from Kepler to characterize their stellar (see Table2) and
orbital properties (see Table3). We used UKIRT images to calculate
brightness contrast curves and to detect stellar companions around
planet candidate host stars (see Table4).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 162 138 Stellar parameters
table3.dat 220 344 Orbital parameters
table4.dat 28 234 Visual companion detections with UKIRT images
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
V/136 : Teff and metallicities for Tycho-2 stars (Ammons+, 2006)
J/ApJS/210/19 : Kepler planetary candidates. IV. 22 months (Burke+, 2014)
J/ApJS/208/22 : Transit timing variation for 12 planetary pairs (Xie, 2013)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/ApJ/771/107 : Spectroscopy of faint KOI stars (Everett+, 2013)
J/ApJ/770/90 : Candidate planets in the habitable zones (Gaidos, 2013)
J/ApJ/770/69 : Kepler planet candidates radii (Petigura+, 2013)
J/ApJ/767/95 : Stellar parameters of smallest KIC stars (Dressing+, 2013)
J/MNRAS/421/2342 : Kepler systems transit timing observations (Steffen+, 2012)
J/ApJS/199/30 : Temperature scale for KIC stars (Pinsonneault+, 2012)
J/ApJ/753/90 : Stellar parameters of K5 and later type Kepler stars
(Mann+, 2012)
J/ApJS/197/8 : Kepler's candidate multiple transiting planets
(Lissauer+, 2011)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
http://exoplanetarchive.ipac.caltech.edu/ : NASA Exoplanet Archive
http://surveys.roe.ac.uk/wsa/ : WFCAM Science Archive
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- --- [K]
2- 6 I5 --- KOI [5/4288] Kepler Object of Interest
identifier (1)
8 A1 --- f_KOI [d] Flag on KOI (d=star with missing Teff) (2)
10- 17 I8 --- KIC [1871056/12785320] Kepler Input Catalog
identifier (1)
19- 28 F10.6 deg RAdeg Right Ascension in decimal degrees (J2000) (1)
30- 38 F9.6 deg DEdeg Declination in decimal degrees (J2000) (1)
40- 44 F5.2 mag Kpmag [8.7/13.5] Kepler magnitude (1)
46- 49 I4 K Teff [3900/8229] Effective temperature (1)
51- 54 F4.2 [cm/s2] logg [1.87/4.75]? Log surface gravity (1)
56- 60 F5.2 [-] [Fe/H] [-1.15/0.55]? Metallicity (1)
62- 65 I4 K DTeff [3936/8232] Derived effective temperature
67- 69 I3 K E_DTeff [37/525] Upper limit uncertainty in DTeff
71- 73 I3 K e_DTeff [37/555] Lower limit uncertainty in DTeff
75- 78 F4.2 [cm/s2] Dlogg [3.5/4.75] Derived log surface gravity
80- 83 F4.2 [cm/s2] E_Dlogg [0/0.45] Upper limit uncertainty in Dlogg
85- 88 F4.2 [cm/s2] e_Dlogg [0/0.6] Lower limit uncertainty in Dlogg
90- 94 F5.2 [-] D[Fe/H] [-1.15/0.55] Derived metallicity
96- 99 F4.2 [-] E_D[Fe/H] [0.06/0.6] Upper limit uncertainty in D[Fe/H]
101-104 F4.2 [-] e_D[Fe/H] [0.29/0.56] Lower limit uncertainty in D[Fe/H]
106-109 F4.2 Msun Mass [0.58/2.15] Derived mass
111-114 F4.2 Msun E_Mass [0/1] Upper limit uncertainty in Mass
116-119 F4.2 Msun e_Mass [0/0.4] Lower limit uncertainty in Mass
121-124 F4.2 Rsun Rad [0.5/4.2] Derived radius
126-129 F4.2 Rsun E_Rad [0/1.8] Upper limit uncertainty in Rad
131-134 F4.2 Rsun e_Rad [0/1.15] Lower limit uncertainty in Rad
136-140 F5.2 Lsun Lum [0/43] Derived luminosity
142-146 F5.2 Lsun E_Lum [0/27] Upper limit uncertainty in Lum
148-152 F5.2 Lsun e_Lum [0/18] Lower limit uncertainty in Lum
154-157 F4.2 g/cm3 rho [0/5] Derived density
159-162 F4.2 g/cm3 e_rho [0/2.25] Uncertainty in rho
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Note (1): From NASA Exoplanet Archive
(http://exoplanetarchive.ipac.caltech.edu/).
Note (2):
d = Star has a missing Teff. These Teff values are estimated based on
g-r and g-i values (Pinsonneault et al. 2012, cat. J/ApJS/199/30), the
adopted Teff is the average of the results. There are three exceptions,
values of Teff for K03158 and K0368 are adopted from Ammons et al. 2006
(cat. V/136) and Teff for K04021 is based on the infrared flux method in
Pinsonneault et al. 2012 (cat. J/ApJS/199/30).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- --- [K]
2- 9 F8.2 --- KOI [5.01/4288.02] Kepler Object of Interest
identifier
11 A1 -- f_KOI [b] Flag on KOI (b=high planet confidence) (1)
13- 20 I8 --- KIC [1871056/12785320] Kepler Input Catalog identifier
22- 29 F8.4 d T0 [122.9/481.3] Time of minimum
31- 39 F9.5 d Per [0.8/296.7] Period
41- 47 F7.5 d E_Per [0/0.15] Upper limit uncertainty in Per
49- 55 F7.5 d e_Per [0/0.5] Lower limit uncertainty in Per
57- 60 F4.2 --- b [0/2.77] Impact parameter
62- 65 F4.2 --- E_b [0/4.2] Upper limit uncertainty in b
67- 70 F4.2 --- e_b [0/1.3] Lower limit uncertainty in b
72- 76 F5.3 --- Rp/R* [0.003/0.09] Ratio of planetary to stellar radii
78- 82 F5.3 --- E_Rp/R* [0/0.04] Upper limit uncertainty in Rp/R*
84- 88 F5.3 --- e_Rp/R* [0/0.05] Lower limit uncertainty in Rp/R*
90- 93 F4.2 --- e [0/0.9] Eccentricity
95- 98 F4.2 --- E_e [0/0.7] Upper limit uncertainty in e
100-103 F4.2 --- e_e [0/0.8] Lower limit uncertainty in e
105-108 F4.2 rad omega [0/6.3] Argument of periastron ω
110-113 F4.2 rad E_omega [0/6.3] Upper limit uncertainty in omega
115-118 F4.2 rad e_omega [0/6.3] Lower limit uncertainty in omega
120-124 F5.2 Rgeo Rp [0.3/18.7] Planetary radius in Earth radii
126-129 F4.2 Rgeo e_Rp [0.04/6.5] Uncertainty in Rp
131-135 F5.2 deg i [39.7/90] Inclination
137-141 F5.2 deg E_i [0/27.7] Upper limit uncertainty in i
143-147 F5.2 deg e_i [0/19] Lower limit uncertainty in i
149-153 F5.1 --- a/R* [1.3/141.8] Ratio of the separation to stellar
radius
155-158 F4.1 --- E_a/R* [0/84.8] Upper limit uncertainty in a/R*
160-163 F4.1 --- e_a/R* [0/52.3] Lower limit uncertainty in a/R*
165-169 F5.3 AU a [0/1] Planet-star separation
171-175 F5.3 AU e_a [0/0.08] Uncertainty in a
177-180 I4 K T [239/2648] Planet temperature
182-185 I4 K e_T [7/2228] Uncertainty in T
187-190 I4 ppm Depth [12/9267] Light curve depth (parts per million)
192-194 I3 ppm e_Depth [1/128] Uncertainty in Depth
196-199 F4.1 h Dur [1/21.2] Depth duration
201-204 F4.1 --- Signi [0/37.2] Significance of pixel centroid offset (2)
206 A1 --- f_Signi [b] Flag on Signi (b=high planet confidence) (3)
208-212 F5.3 --- p1 [0/1] Planet confidence before considering the
existence of other candidates in the same
system (4)
214-218 F5.3 --- p2 [0.1/1] Planet confidence after (augmented planet
confidence for a multi-planet system) (4)
220 A1 --- f_p2 [b] Flag on p2 (b=high planet confidence) (3)
--------------------------------------------------------------------------------
Note (1): b=A planet candidate with higher than 0.997 planet confidence.
Note (2): Between in- and out-of-transit.
Note (3): b=A planet candidate with significant pixel centroid offset
(>3σ) and with higher than 0.997 planet confidence.
Note (4): Considering the planetary likelihood boost in Lissauer et al.
(2012ApJ...750..112L 2012ApJ...750..112L).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- --- [K]
2- 6 I5 --- KOI [5/4288] Kepler Object of Interest identifier
8- 10 F3.1 mag DKpmag [0.1/8.2]? Differential Kepler magnitude (of a
possible contaminating object)
12- 15 F4.1 arcsec Sep [2.2/21.9]? Separation
17- 22 F6.1 --- Signi [5/3379.6]? Significance in σ unit
24- 28 F5.1 deg PA [0.6/354.7]? Position angle
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History:
From electronic version of the journal
References:
Wang et al. Paper II 2014ApJ...791..111W 2014ApJ...791..111W
Wang et al. Paper III 2015ApJ...806..248W 2015ApJ...806..248W
Wang et al. Paper IV 2015ApJ...813..130W 2015ApJ...813..130W
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 19-May-2016