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 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 (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)
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 2014AJ....148...78D);
H14 = Horch et al. (2014ApJ...795...60H 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 2014ApJ...783....4W, Cat. J/ApJ/783/4
Wang et al. Paper II 2014ApJ...791..111W 2014ApJ...791..111W
Wang et al. Paper IV 2015ApJ...813..130W 2015ApJ...813..130W
(End) Prepared by Tiphaine Pouvreau [CDS] 15-Sep-2017