J/AJ/150/133 Stellar noise for 4529 Kepler solar-type dwarfs (Gilliland+, 2015)
Kepler mission stellar and instrument noise properties revisited.
Gilliland R.L., Chaplin W.J., Jenkins J.M., Ramsey L.W., Smith J.C.
<Astron. J., 150, 133 (2015)>
=2015AJ....150..133G 2015AJ....150..133G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, dwarfs
Keywords: methods: observational - stars: activity - stars: late-type -
stars: statistics - techniques: photometric
Abstract:
An earlier study of the Kepler Mission noise properties on timescales
of primary relevance to detection of exoplanet transits found that
higher than expected noise followed, to a large extent, from the stars
rather than instrument or data analysis performance. The earlier study
over the first six quarters of Kepler data is extended to the full
four years ultimately comprising the mission. Efforts to improve the
pipeline data analysis have been successful in reducing noise levels
modestly as evidenced by smaller values derived from the current data
products. The new analyses of noise properties on transit timescales
show significant changes in the component attributed to instrument and
data analysis, with essentially no change in the inferred stellar
noise. We also extend the analyses to timescales of several days,
instead of several hours to better sample stellar noise that follows
from magnetic activity. On the longer timescale there is a shift in
stellar noise for solar-type stars to smaller values in comparison to
solar values.
Description:
The NASA Kepler Mission has left an indelible imprint on the research
of exoplanet and stellar properties for a large number of stars
(∼150000), over four years.
Our earlier study (Gilliland et al., 2011ApJS..197....6G 2011ApJS..197....6G; Paper I)
provided a discussion about the Kepler Mission noise properties. The
earlier study over the first six quarters of Kepler data is extended
to the full four years ultimately comprising the mission.
A total of 4529 stars (see Table3) brighter than Kp=12.5 met the
selection criteria for solar-type dwarfs as detailed in Paper I
(Gilliland et al., 2011ApJS..197....6G 2011ApJS..197....6G).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 45 4529 Standard and long timescale Combined Differential
Photometric Precision (CDPP) values
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/217/31 : Kepler planetary candidates. VI. 4yr Q1-Q16 (Mullally+, 2015)
J/ApJS/217/16 : Kepler planetary candidates. V. 3yr Q1-Q12 (Rowe+, 2015)
J/ApJS/210/19 : Kepler planetary candidates. IV. 22 months (Burke+, 2014)
J/AJ/147/45 : Kepler. IV. Eclipse times for close binaries (Conroy+, 2014)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/AJ/142/160 : Kepler Mission. II. eclipsing binaries (Slawson+, 2011)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/ApJ/728/117 : Transit timing observations from Kepler. I. (Ford+, 2011)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC Identifier in Kepler Input Catalog (1)
10- 15 F6.3 mag Kpmag [6.9/12.5] Kepler magnitude
17- 22 F6.2 ppm CDPP [10.7/999.99] Noise on standard 6.5 hours Combined
Differential Photometric Precision (CDPP) analog
(in parts per million)
24- 29 F6.2 ppm Noise* Noise at 6.5 hours intrinsic to stars (2)
31- 37 F7.2 ppm RNoise Noise at 3.25 days CDPP in raw data (x12) (3)
39- 45 F7.2 ppm CNoise Noise at 3.25 days CDPP in calibrated data
(x12) (3)
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Note (1): A total of 4529 stars brighter than Kpmag=12.5 met the selection
criteria for solar-type dwarfs as detailed in Paper I (Gilliland et al.,
2011ApJS..197....6G 2011ApJS..197....6G).
Note (2): The standard timescale values for our CDPP analog and inferred
intrinsic stellar noise are discussed in Section 3.
Note (3): As summarized in Figure 7. The longer timescale CDPP values
corresponding to analysis of both raw and calibrated time series are
discussed in Section 4.
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History:
From electronic version of the journal
References:
Gilliland et al., Paper I, 2011ApJS..197....6G 2011ApJS..197....6G
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 05-Nov-2015