J/MNRAS/426/91 Kepler stars with infrared excess (Kennedy+, 2012)
Confusion limited surveys: using WISE to quantify the rarity of warm dust
around Kepler stars.
Kennedy G.M., Wyatt M.C.
<Mon. Not. R. Astron. Soc., 426, 91-107 (2012)>
=2012MNRAS.426...91K 2012MNRAS.426...91K
ADC_Keywords: Stars, double and multiple ; Planets ; Effective temperatures ;
Photometry, infrared
Keywords: planets and satellites: formation - circumstellar matter -
stars: individual: HIP 13642 - stars: individual: KIC 7345479 -
planetary systems
Abstract:
We describe a search for infrared excess emission from dusty
circumstellar material around 180000 stars observed by the Kepler and
Wide-field Infrared Survey Explorer missions. This study is motivated
by (i) the potential to find bright warm discs around planet host
stars, (ii) a need to characterize the distribution of rare warm discs
and (iii) the possible identification of candidates for discovering
transiting dust concentrations. We find about 8000 stars that have
excess emission, mostly at 12um.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 58 271 The 271 Kepler stars with WISE 3-4 excesses
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/199/24 : The first three quarters of Kepler mission (Tenenbaum+, 2012)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC KIC Identifier (Cat. V/133)
10- 14 F5.2 mag kepmag Predicted Kepler Kp magnitude
16- 21 I6 --- Quarters Quarters target was observed in (up to 6)
23- 26 I4 K Teff Fitted effective temperature
28- 31 F4.1 --- RW3 ?=- WISE W3 (11.6µm) flux excess (1)
33- 36 F4.1 --- XW3 [4/]?=- W3 excess significance (1)
38- 42 F5.1 --- RW4 ?=- WISE W4 (22.1µm) flux excess (1)
44- 46 F3.1 --- XW4 [4/]?=- W4 excess significance (1)
48- 58 A11 --- Notes The single KOI 5KOI NNN) and T12 for potential
planet hosts from Tenebaum et al., 2012,
Cat. J/ApJS/199/24
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Note (1): The flux excess R(B) in a band B is defined by R(B)=F(B)/Fp(B),
ratio of the observed to the predicted flux in the band. The excess
significance X(B) is defined by X(B)=F(B)-Fp(B)/σ, where σ
is the combined uncertainty sqrt(σ2+σp2).
Only sources with excess significance >4 are included.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Apr-2013