J/ApJ/813/130 Kepler multiple transiting planet systems (Wang+, 2015)
Influence of stellar multiplicity on planet formation.
IV. Adaptive optics imaging of Kepler stars with multiple transiting planet
candidates.
Wang J., Fischer D.A., Xie J.-W., Ciardi D.R.
<Astrophys. J., 813, 130 (2015)>
=2015ApJ...813..130W 2015ApJ...813..130W (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Photometry, infrared ;
Stars, distances ; Effective temperatures ; Abundances, [Fe/H]
Keywords: methods: observational - planet-star interactions -
planetary systems -
planets and satellites: dynamical evolution and stability -
planets and satellites: formation -
techniques: high angular resolution
Abstract:
The Kepler mission provides a wealth of multiple transiting planet
systems (MTPSs). The formation and evolution of multi-planet systems
are likely to be influenced by companion stars given the abundance of
multiple stellar systems. We study the influence of stellar companions
by measuring the stellar multiplicity rate of MTPSs. We select 138 bright
(KP<13.5) Kepler MTPSs and search for stellar companions with
adaptive optics (AO) imaging data and archival radial velocity data.
We obtain new AO images for 73 MTPSs. Other MTPSs in the sample have
archival AO imaging data from the Kepler Community Follow-up
Observation Program. From these imaging data, we detect 42 stellar
companions around 35 host stars. For stellar separation 1 AU<a<100 AU,
the stellar multiplicity rate is 5.2±5.0% for MTPSs, which is
2.8σ lower than 21.1±2.8% for the control sample, i.e., the
field stars in the solar neighborhood. We identify two origins for the
deficit of stellar companions within 100 AU of MTPSs: (1) a suppressive
planet formation and (2) the disruption of orbital coplanarity due to
stellar companions. To distinguish between the two origins, we compare
the stellar multiplicity rates of MTPSs and single transiting planet
systems (STPSs). However, current data are not sufficient for this
purpose. For 100 AU<a<2000 AU, the stellar multiplicity rates are
comparable for MTPSs (8.0±4.0%), STPSs (6.4±5.8%), and the control
sample (12.5±2.8%).
Description:
The sample of MTPSs remains the same as that in Wang et al. (2014,
J/ApJ/783/4). From the NASA Exoplanet Archive
(http://exoplanetarchive.ipac.caltech.edu), we select Kepler objects
of interest (KOIs) that satisfy the following criteria: (1) disposition
of either Candidate or Confirmed; (2) with at least two planet
candidates; (3) Kepler magnitude (KP) brighter than 13.5. The above
selection criteria resulted in 138 MTPSs in Wang et al. (2014,
J/ApJ/783/4). With the updated Exoplanet Archive, the selection
criteria resulted in 208 MTPSs. In this paper, we focus on the 138 MTPSs
to be consistent with previous work.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 91 169 AO Sensitivity
table2.dat 108 54 Visual Companion Detections with AO Data for
Kepler MTPS
table3.dat 61 91 Stellar Parameters for STPSs
table4.dat 108 44 Visual Companion Detections with AO Data for
Kepler STPS
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/197/8 : Kepler's candidate multiple transiting planets
(Lissauer+, 2011)
J/A+A/546/A10 : Multiplicity in transiting planet-host stars (Lillo-Box+, 2012)
J/AJ/144/42 : Infrared photometry of 90 KOIs (Adams+, 2012)
J/ApJ/783/4 : Properties of Kepler multi-planet candidate systems
(Wang+, 2014)
J/ApJ/790/146 : Planets in Kepler's multi-transiting systems (Fabrycky+, 2014)
J/ApJ/791/35 : Detection of 715 Kepler planet candidates host stars
(Law+, 2014)
J/ApJS/210/19 : Kepler planetary candidates. IV. 22 months (Burke+, 2014)
J/ApJS/211/2 : Revised stellar properties of Q1-16 Kepler targets
(Huber+, 2014)
J/AJ/152/18 : Robo-AO Kepler planetary candidate survey. II. (Baranec+, 2016)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC Kepler Input Catalog identifier (Cat. V/133)
10- 15 A6 --- KOI Kepler Object of Interest number (KNNNNN)
17- 22 F6.3 mag Kpmag Kepler magnitude
24- 29 F6.3 mag imag ? Estimated magnitude in SDSS-i band
31- 36 F6.3 mag Jmag Magnitude in 2MASS J band
38- 43 F6.3 mag Hmag Magnitude in 2MASS H band
45- 50 F6.3 mag Kmag Magnitude in 2MASS K band
52- 54 A3 --- Comp [yes no] Companion within 5"?
56- 59 F4.2 --- Prob ? Isolation probability (1)
61- 65 A5 --- Obs.Inst Instrument used (ARIES,NIRC2,PHARO)
67 A1 --- Obs.Filt [JHK] Filter used for the observation
69- 71 F3.1 mag Delta0.1 Magnitude detection limit at separation 0.1" (2)
73- 75 F3.1 mag Delta0.2 Magnitude detection limit at separation 0.2" (2)
77- 79 F3.1 mag Delta0.5 Magnitude detection limit at separation 0.5" (2)
81- 83 F3.1 mag Delta1.0 Magnitude detection limit at separation 1.0" (2)
85- 87 F3.1 mag Delta2.0 Magnitude detection limit at separation 2.0" (2)
89- 91 F3.1 mag Delta4.0 Magnitude detection limit at separation 4.0" (2)
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Note (1): Isolation probability is the probability of a KOI being isolated
within 2000 AU (i.e., has no stellar companion within 2000 AU) given
the AO and/or RV data and/or dynamical analysis (see Section 3.3). For
stars with detected nearby stellar companions, the physical
association probability can be found in Table 2.
Note (2): Limiting Delta magnitudes are the 5σ limit.
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Byte-by-byte Description of file: table2.dat table4.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- KOI Kepler Object of Interest number (KNNNNN)
8 I1 --- Star [1/3] Number of stars in the system
10- 16 A7 --- Tel Telescope (MMT,Keck,Palomar)
18 A1 --- Filter [JHK] Filter used for the observation
20- 23 F4.2 mag Dmag Differential magnitude in Filter (1)
25- 28 F4.2 arcsec Sep Separation (2)
30- 37 F8.2 AU SepAU Separation, in AU
39- 44 F6.1 pc DistP Distance of primary (3)
46- 51 F6.1 pc E_DistP Upper limit uncertainty in DistP
53- 58 F6.1 pc e_DistP Lower limit uncertainty in DistP
60- 66 F7.1 pc DistS ? Distance of secondary (3)
68- 74 F7.1 pc E_DistS ? Upper limit uncertainty in DistS
76- 82 F7.1 pc e_DistS ? Lower limit uncertainty in DistS
84- 88 F5.1 deg PA Position angle
90 A1 --- l_Prob [>] Limit flag on Prob
91- 94 F4.2 --- Prob Association probability (4)
96-108 A13 --- Ref Reference (5)
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Note (1): Typical Dmag uncertainty is 0.1 mag. The uncertainty is estimated
from the companion injection simulation described in Section 3.3.
Note (2): Typical angular separation uncertainty is 0.05". The uncertainty is
estimated from the companion injection simulation described in
Section 3.3.
Note (3): Distance is estimated based on stellar properties of primary stars
(Huber et al. 2014, J/ApJS/211/2) and color information of secondary
stars (see Section 4.1 in Wang et al. 2015ApJ...806..248W 2015ApJ...806..248W for more
details).
Note (4): Association probability has 10% uncertainty due to statistical error
in simulation.
Note (5): AO images from CFOP are provided by David Ciardi unless otherwise
noted. Other reference as follows:
A12 = Adams et al. (2012, J/AJ/144/42);
C15 = Campante et al. (2015ApJ...799..170C 2015ApJ...799..170C).
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- KOI Kepler Object of Interest number (KNNNNN)
8- 15 I8 --- KIC Kepler Input Catalog identifier (Cat. V/133)
17- 18 I2 h RAh Hour of Right Ascension (J2000)
20- 21 I2 min RAm Minute of Right Ascension (J2000)
23- 27 F5.2 s RAs Second of Right Ascension (J2000)
28 A1 --- DE- Sign of the Declination (J2000)
29- 30 I2 deg DEd Degree of Declination (J2000)
32- 33 I2 arcmin DEm Arcminute of Declination (J2000)
35- 39 F5.2 arcsec DEs Arcsecond of Declination (J2000)
41- 45 F5.2 mag Kpmag Kepler magnitude
47- 50 I4 K Teff Effective temperature
52- 55 F4.2 [cm/s2] log(g) Log surface gravity
57- 61 F5.2 [-] [Fe/H] Metallicity
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History:
From electronic version of the journal
References:
Wang et al. Paper I 2014ApJ...783....4W 2014ApJ...783....4W, Cat. J/ApJ/783/4
Wang et al. Paper II 2014ApJ...791..111W 2014ApJ...791..111W
Wang et al. Paper III 2015ApJ...806..248W 2015ApJ...806..248W
(End) Prepared by Tiphaine Pouvreau [CDS] 12-Oct-2017