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J/ApJ/806/248       AO imaging of KOIs with gas giant planets      (Wang+, 2015)

Influence of stellar multiplicity on planet formation. III. Adaptive optics imaging of Kepler stars with gas giant planets. Wang J., Fischer D.A., Horch E.P., Xie J.-W. <Astrophys. J., 806, 248 (2015)> =2015ApJ...806..248W (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Effective temperatures ; Stars, distances ; Photometry, ugriz ; Photometry, infrared Keywords: methods: observational - methods: statistical - planetary systems - planets and satellites: formation - planet-star interactions - techniques: high angular resolution Abstract: As hundreds of gas giant planets have been discovered, we study how these planets form and evolve in different stellar environments, specifically in multiple stellar systems. In such systems, stellar companions may have a profound influence on gas giant planet formation and evolution via several dynamical effects such as truncation and perturbation. We select 84 Kepler Objects of Interest (KOIs) with gas giant planet candidates. We obtain high-angular resolution images using telescopes with adaptive optics (AO) systems. Together with the AO data, we use archival radial velocity data and dynamical analysis to constrain the presence of stellar companions. We detect 59 stellar companions around 40 KOIs for which we develop methods of testing their physical association. These methods are based on color information and galactic stellar population statistics. We find evidence of suppressive planet formation within 20 AU by comparing stellar multiplicity. The stellar multiplicity rate (MR) for planet host stars is 0-0+5% within 20 AU. In comparison, the stellar MR is 18%±2% for the control sample, i.e., field stars in the solar neighborhood. The stellar MR for planet host stars is 34%±8% for separations between 20 and 200 AU, which is higher than the control sample at 12%±2%. Beyond 200 AU, stellar MRs are comparable between planet host stars and the control sample. We discuss the implications of the results on gas giant planet formation and evolution. Description: From the NASA Exoplanet Archive (, we select Kepler Objects of Interest (KOIs) that satisfy the following criteria: (1) disposition of either Candidate or Confirmed, (2) stellar effective temperature (Teff) lower than 6500 K, (3) stellar surface gravity (log g) higher than 4.0, (4) Kepler magnitude (KP) brighter than 14th mag, (5) with at least one gas giant planet (3.8 R{earth}=<RP=<22.0 R{earth}). In total, we select 84 KOIs with 97 gas giant planets. Stellar and orbital parameters for these KOIs are given in Table 1. The median distance of these KOIs is 580 pc. There are 27 multi-planet systems among 84 KOIs. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 143 97 RV and AO Data for 97 KOIs table2.dat 92 103 Visual Companion Detections with AO Data
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/AJ/144/42 : Infrared photometry of 90 KOIs (Adams+, 2012) J/A+A/566/A103 : Kepler planet host candidates imaging (Lillo-Box+, 2014) J/ApJ/783/4 : Properties of Kepler multi-planet candidate systems (Wang+, 2014) J/ApJ/791/35 : Detection of 715 Kepler planet candidates host stars (Law+, 2014) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 9 A9 --- KOI Kepler Object of Interest identifier (K0NNNN.NN) 11- 18 I8 --- KIC [3323887/12735740] Kepler Input Catalog number 20- 29 F10.6 deg RAdeg Right Ascension in decimal degrees (J2000) 31- 39 F9.6 deg DEdeg Declination in decimal degrees (J2000) 41- 46 F6.3 mag Kpmag Kepler magnitude 48- 54 F7.2 K Teff Stellar effective temperature 56- 60 F5.3 [cm/s2] logg Stellar surface gravity 62- 67 F6.1 pc Dist Distance 69 I1 --- Npl [1/6] Number of planet 71- 75 F5.2 Rgeo Rpl Planet radius 77- 80 F4.2 Rgeo e_Rpl Uncertainty in Rpl 82- 91 F10.6 d Per Orbital period 93-104 F12.6 d Tstart ? Start time in MJD 106-117 F12.6 d Tend ? End time in MJD 119-121 I3 --- Nrv [5/104]? Number of radial velocity measurements 123-133 A11 --- Tel Telescope name 135-137 A3 --- Band Band(s) used in the observation (J,K,JK,JHK,rz) 139-143 A5 --- Work [check-] KOI with AO image taken through this work
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 A6 --- KOI Kepler Object of Interest identifier (K0NNNN) 7 A1 --- n_KOI [*] Note on KOI (1) 9- 11 F3.1 mag Dmag Differential magnitude in Band 13 A1 --- Band [rizJHK] Band of the magnitude 15- 18 F4.2 arcsec Sep Companion separation 20- 25 F6.1 AU Sepa ? Companion separation in AU 27- 31 F5.1 pc DistP ? Distance of primary 33- 37 F5.1 pc E_DistP ? Upper limit uncertainty in DistP 39- 43 F5.1 pc e_DistP ? Lower limit uncertainty in DistP 45- 50 F6.1 pc DistS ? Distance of secondary 52- 58 F7.1 pc E_DistS ? Upper limit uncertainty in DistS 60- 65 F6.1 pc e_DistS ? Lower limit uncertainty in DistS 67- 71 F5.1 --- Signi ? Detection significance in σ unit 73- 77 F5.1 deg PA ? Position angle 79- 82 F4.2 --- Prob ? Probability of association 84- 92 A9 --- Ref Reference code (2)
Note (1): Note as follows: * = This KOI has stellar companions that are not detected by our detection pipeline. Note (2): Reference as follows: A12 = Adams et al. (2012, J/AJ/144/42); D14 = Dressing et al. (2014AJ....148...78D); H14 = Horch et al. (2014ApJ...795...60H); L14 = Law et al. (2014, J/ApJ/791/35); LB14 = Lillo-Box et al. (2014, J/A+A/566/A103); CFOP = Kepler Community Follow-up Observing Program.
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 IV 2015ApJ...813..130W
(End) Prepared by Tiphaine Pouvreau [CDS] 15-Sep-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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