J/AJ/156/234 KELT transit false positive catalog for TESS (Collins+, 2018)
The KELT follow-up network and transit false-positive catalog: pre-vetted false
positives for TESS.
Collins K.A., Collins K.I., Pepper J., Labadie-Bartz J., Stassun K.G.,
Gaudi B.S., Bayliss D., Bento J., Colon K.D., Feliz D., James D.,
Johnson M.C., Kuhn R.B., Lund M.B., Penny M.T., Rodriguez J.E., Siverd R.J.,
Stevens D.J., Yao X., Zhou G., Akshay M., Aldi G.F., Ashcraft C.,
Awiphan S., Basturk O., Baker D., Beatty T.G., Benni P., Berlind P., Bruce
Berriman G., Berta-Thompson Z., Bieryla A., Bozza V., Calchi Novati S.,
Calkins M.L., Cann J.M., Ciardi D.R., Clark I.R., Cochran W.D., Cohen D.H.,
Conti D., Crepp J.R., Curtis I.A., D'Ago G., Diazeguigure K.A.,
Dressing C.D., Dubois F., Ellingson E., Ellis T.G., Esquerdo G.A., Evans P.,
Friedli A., Fukui A., Fulton B.J., Gonzales E.J., Good J.C., Gregorio J.,
Gumusayak T., Hancock D.A., Harada C.K., Hart R., Hintz E.G.,
Jang-Condell H., Jeffery E.J., Jensen E.L.N., Jofre E., Joner M.D., Kar A.,
Kasper D.H., Keten B., Kielkopf J.F., Komonjinda S., Kotnik C., Latham D.W.,
Leuquire J., Lewis T.R., Logie L., Lowther S.J., Macqueen P.J., Martin T.J.,
Mawet D., Mcleod K.K., Murawski G., Narita N., Nordhausen J., Oberst T.E.,
Odden C., Panka P.A., Petrucci R., Plavchan P., Quinn S.N., Rau S.,
Reed P.A., Relles H., Renaud J.P., Scarpetta G., Sorber R.L., Spencer A.D.,
Spencer M., Stephens D.C., Stockdale C., Tan T.-G., Trueblood M.,
Trueblood P., Vanaverbeke S., Villanueva S., Warner E.M., West M.L.,
Yalcinkaya S., Yeigh R., Zambelli R.
<Astron. J., 156, 234 (2018)>
=2018AJ....156..234C 2018AJ....156..234C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, bright ; Binaries, eclipsing ; Positional data ;
Stars, distances ; Photometry ; Exoplanets
Keywords: methods: observational - techniques: photometric -
techniques: spectroscopic - techniques: radial velocities
Abstract:
The Kilodegree Extremely Little Telescope (KELT) project has been
conducting a photometric survey of transiting planets orbiting bright
stars for over 10 years. The KELT images have a pixel scale of ∼23"/pixel
very similar to that of NASA's Transiting Exoplanet Survey Satellite
(TESS) - as well as a large point-spread function, and the KELT reduction
pipeline uses a weighted photometric aperture with radius 3'. At this
angular scale, multiple stars are typically blended in the photometric
apertures. In order to identify false positives and confirm transiting
exoplanets, we have assembled a follow-up network (KELT-FUN) to conduct
imaging with spatial resolution, cadence, and photometric precision higher
than the KELT telescopes, as well as spectroscopic observations of the
candidate host stars. The KELT-FUN team has followed-up over 1600 planet
candidates since 2011, resulting in more than 20 planet discoveries.
Excluding ∼450 false alarms of non-astrophysical origin (i.e.,
instrumental noise or systematics), we present an all-sky catalog of
the 1128 bright stars (6<V<13) that show transit-like features in the KELT
light curves, but which were subsequently determined to be astrophysical
false positives (FPs) after photometric and/or spectroscopic follow-up
observations. The KELT-FUN team continues to pursue KELT and other planet
candidates and will eventually follow up certain classes of TESS
candidates. The KELT FP catalog will help minimize the duplication of
follow-up observations by current and future transit surveys such as TESS.
Description:
The Kilodegree Extremely Little Telescope (KELT; Pepper et al.
2003AcA....53..213P 2003AcA....53..213P, 2007PASP..119..923P 2007PASP..119..923P) is a wide-field photometric
transit survey operated by Vanderbilt University, The Ohio State
University, and Lehigh University.
The primary goal of the KELT Follow-up Network (KELT-FUN) is to confirm
and characterize transiting exoplanets orbiting bright stars, but
additional science projects investigating EBs and other variable stars
are also pursued. The members of KELT-FUN are a mix of professional,
student, and highly capable citizen astronomers distributed across the
globe. KELT-FUN started operations in the spring of 2011 when the first
KELT transiting planet candidates were extracted from the KELT data
and vetted by the KELT Science Team.
We present the results of 1128 KELT-FUN false positive (FP) detections
in machine-readable catalog format to help minimize duplicate follow-up
observation efforts by current and future transiting planet wide-field
surveys such as TESS.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 358 1128 False positive catalog
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See also:
J/ApJ/809/77 : Transiting Exoplanet Survey Satellite (TESS) (Sullivan+, 2015)
J/AJ/155/39 : Variability properties of TIC sources with KELT
(Oelkers+, 2018)
J/AJ/156/102 : The TESS Input Catalog and Candidate Target List
(Stassun+, 2018)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- KELT KELT identifier
22- 38 A17 --- 2MASS 2MASS identifier (JHHMMSSss-DDMMSSs)
40- 48 I9 --- TIC [105394/470975994] TESS Input Catalog
identifier
50 I1 --- InCTL [0/1] Object in TESS Candidate Target List?
(1=yes)
52- 62 F11.9 --- Prio [0/0.1242]? Priority from TESS Input Catalog
64- 71 A8 --- FName False positive type name (1)
73 I1 --- FNum [1/9] False positive type number (1)
75- 85 F11.8 h RAhour Right Ascension in decimal hours (J2000)
87- 98 F12.8 deg RAdeg Right Ascension in decimal degrees (J2000)
100-101 I2 h RAh Hour of Right Ascension (J2000)
103-104 I2 min RAm Minute of Right Ascension (J2000)
106-110 F5.2 s RAs Second of Right Ascension (J2000)
112 A1 --- DE- Sign of the Declination (J2000)
113-114 I2 deg DEd Degree of Declination (J2000)
116-117 I2 arcmin DEm Arcminute of Declination (J2000)
119-123 F5.2 arcsec DEs Arcsecond of Declination (J2000)
125-136 F12.8 deg DEdeg Declination in decimal degrees (J2000)
138-147 F10.6 deg GLON Galactic longitude
149-160 F12.8 deg GLAT Galactic latitude
162-173 F12.8 deg ELON Ecliptic longitude
175-186 F12.8 deg ELAT Ecliptic latitude
188-193 F6.3 mag Vmag [5.78/14.315] Apparent V band magnitude
195-205 F11.3 d Tc ? Transit center time in BJDTDB
207-213 F7.5 d e_Tc [0/1.3]? Uncertainty in Tc
215-226 F12.9 d Per [0.1543703/76.1533]? Period of transit
228-240 F13.10 d e_Per [0/16]? Uncertainty in Per
242-253 F12.9 h Dur [0.77/16.68]? Duration of transit
255-261 F7.3 mmag TDepth [0.8/100]? Depth of transit in KELT aperture
263-267 F5.1 km/s RVAmp [5/200]? Binary radial velocity
semi-amplitude
269-271 I3 mmag EBDepth [22/200]? Depth of eclipsing binary
273-274 I2 h RAhNEB ? Nearby eclipsing binary (NEB) Hour of
Right Ascension (J2000)
276-277 I2 min RAmNEB ? NEB Minute of Right Ascension (J2000)
279-283 F5.2 s RAsNEB ? NEB Second of Right Ascension (J2000)
285 A1 --- DE-NEB NEB Sign of the Declination (J2000)
286-287 I2 deg DEdNEB ? NEB Degree of Declination (J2000)
289-290 I2 arcmin DEmNEB ? NEB Arcminute of Declination (J2000)
292-296 F5.2 arcsec DEsNEB ? NEB Arcsecond of Declination (J2000)
298 A1 --- l_DText [~<] Limit flag on DText
299-304 F6.2 arcsec DText [0.14/840]? Readable distance from target
start to NEB
305 A1 --- f_DText [*] Flag on DText (2)
307-312 F6.2 arcsec D [0.14/840]? Distance from target start
to NEB
314 I1 --- f_D [0/1]? Flag on D (1=approximate or limit
flag)
316-321 A6 --- Dir Direction from start to NEB
323-323 A1 --- l_NEBDText [≳] Limit flag on NEBDText
324-328 F5.2 % NEBDText [1/90]? Readable percent depth of NEB
transit
330-333 F4.1 % NEBDepth [1/90]? Percent depth of NEB transit
335 I1 --- f_NEBDepth1 [0/1]? Flag on NEBDepth (1=approximate)
337 I1 --- f_NEBDepth2 [0/1]? Flag on NEBDepth (1=lower limit)
339-348 A10 "Y:M:D" Date Date NEB was observed (3)
350-358 A9 --- Filter Filter(s) used to observe NEB
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Note (1): KELT false positives (FPs) by category/type (Table 3 of this paper):
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Category Type Description Total
---------------------------------------------------------------------
Spectroscopic FPs
SB1 1 Single-lined binary (RV>1km/s) 307
SB2 2 Multi-lined binary 140
RV0 3 No significant RV detected 13
Giant 4 Spectroscopic Giant 29
Photometric FPs
EB1 5 Too deep in follow-up 130
EB2 6 Different primary and secondary depths 25
BEB 7 Blend in follow-up aper. (chromaticity) 90
Variable 8 Variable star caused KELT detection 16
NEB 9 Nearby EB (blend in KELT aperture) 378
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Note (2): Flag as follows:
* = DText may also be equal to 82.8 arcsec.
Note (3): Note that on some occasions an NEB was observed on multiple nights.
The main reason is that additional observations took place prior to the
submission of the results of an earlier observation.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 11-Apr-2019