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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 (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:
FileName Lrecl Records Explanations
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
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
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)
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.
Byte-by-byte Description of file: table2.dat table4.dat
Bytes Format Units Label Explanations
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)
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 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).
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
History: From electronic version of the journal References: Wang et al. Paper I 2014ApJ...783....4W, Cat. J/ApJ/783/4 Wang et al. Paper II 2014ApJ...791..111W Wang et al. Paper III 2015ApJ...806..248W
(End) Prepared by Tiphaine Pouvreau [CDS] 12-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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