J/AJ/142/19 Speckle observations of KOI (Howell+, 2011)
Speckle camera observations for the NASA Kepler mission follow-up program.
Howell S.B., Everett M.E., Sherry W., Horch E., Ciardi D.R.
<Astron. J., 142, 19 (2011)>
=2011AJ....142...19H 2011AJ....142...19H
ADC_Keywords: Stars, double and multiple ; Planets ; Magnitudes
Keywords: instrumentation: high angular resolution -
planets and satellites: general - techniques: photometric
Abstract:
We present the first results from a speckle imaging survey of stars
classified as candidate exoplanet host stars discovered by the Kepler
mission. We use speckle imaging to search for faint companions or
closely aligned background stars that could contribute flux to the
Kepler light curves of their brighter neighbors. Background stars are
expected to contribute significantly to the pool of false positive
candidate transiting exoplanets discovered by the Kepler mission,
especially in the case that the faint neighbors are eclipsing binary
stars. Here, we describe our Kepler follow-up observing program, the
speckle imaging camera used, our data reduction, and astrometric and
photometric performance. Kepler stars range from R=8 to 16 and our
observations attempt to provide background non-detection limits 5-6mag
fainter and binary separations of ∼0.05-2.0-arcsec. We present data
describing the relative brightness, separation, and position angles
for secondary sources, as well as relative plate limits for
non-detection of faint nearby stars around each of 156 target stars.
Faint neighbors were found near 10 of the stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 57 338 Kepler speckle targets lacking detectable secondaries
table2.dat 68 35 Kepler speckle targets with detected secondaries
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- KOI Kepler object identifier
5 A1 --- f_KOI [b] False positives (1)
7- 14 I8 --- KIC Kepler identification (Cat. V/133)
16- 20 F5.2 mag Kpmag Kepler magnitude
22- 31 A10 "YYYY/MM/DD" ObsDate UT date of the observation
33- 37 A5 ms t.int Integration time
39- 40 I2 --- Nco Number of coadds
42- 44 I3 nm lambda Central wavelength of filter
46- 47 A2 --- Class [S SD] Classification: S (single star)
or SD (suspected double)
49- 52 F4.2 mag Dmag ? Maximum magnitude difference from primary
54- 57 F4.2 arcsec See Seeing
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Note (1): KOIs 77,78,79 are now known to be false positives.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- KOI Kepler object identifier
5 A1 --- f_KOI [abc] Flag on KOI (1)
7- 14 I8 --- KIC Kepler identification
16- 20 F5.2 mag Kpmag Kepler magnitude
22- 31 A10 "YYYY/MM/DD" ObsDate UT date of the observation
33- 34 I2 ms t.int Integration time
36 I1 --- Nco Number of coadds
38- 40 I3 nm lambda Central wavelength of filter
42- 46 F5.3 arcsec rho ?=- Separation
48- 53 F6.2 deg PA ?=- Position angle
55- 58 F4.2 mag Dmag ?=- Magnitude difference
60- 63 F4.2 mag DmagM ?=- Maximum magnitude difference
65- 68 F4.2 arcsec See Seeing
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Note (1): Notes as follows:
a = Secondary lies outside the slightly different field of view in
this camera
b = Quadrant is ambiguous in our observations
c = Quadrant is ambiguous in our observations. Tycho measurements lists
the PA as 208-deg with a separation consistent with our value
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 21-Sep-2012