Kepler Object of Interest designation as a string. Examples: k1000.01, ... (Note some tables used a KOInnn.n format for the KOI name.) example: K00757.02
Vetting Status derived by the Kepler project. Only 2 categories are currently defined but this may change as more data is received and analyzed. Examples: CANDIDATE, FALSE POSITIVE
Vetting Status derived by NExScI. Currently NExScI flags confirmed planets which are not flagged by the Kepler project. Therefore, 3 categories are currently defined. Examples: CANDIDATE, FALSE POSITIVE, CONFIRMED
Time to first transit (BKJD = BJD-2454833.0). The offset corresponds to 12:00 on Jan 1, 2009 UTC. Note other tables have used an offset value of 2454900, so be careful when comparing entries with earlier data. 120.5159 to 1472.5223
Average interval between transits based on a linear fit to all observed transits. For candidates with only one observed transit, the period is estimated from the duration and knowledge of the stellar radius; values are then rounded to the nearest integer and multiplied by -1. 0.2418 to 129995.7784
The fraction of stellar flux lost (in parts per million) at the minimum of the planetary transit. Transit depths are typically computed from a best-fit model produced by a Mandel-Agol (2002) model fit to a multi-quarter Kepler light curve, assuming a linear orbital ephemeris. 0 to 1541400
Transit duration, first contact to last contact. Contact times are typically computed from a best-fit model produced by a Mandel-Agol (2002) model fit to a multi-quarter Kepler light curve, assuming a linear orbital ephemeris. 0.0520 to 138.5400
The time between first and second contact of the planetary transit. Contact times are typically computed from a best-fit model produced by a Mandel-Agol (2002) model fit to a multi-quarter Kepler light curve, assuming a linear orbital ephemeris. currently all null
The sky-projected distance between the center of the stellar disc and the center of the planet disc at conjunction, normalized by the stellar radius. 0 to 100.8060
The distance between the planet and the star at mid-transit divided by the stellar radius. For the case of zero orbital eccentricity, the distance at mid-transit is the semi-major axis of the planetary orbit. 0.3730 to 79614
Equilibrium surface temperature of planet. The calculation of equilibrium temperature assumes i) thermodynamic equilibrium between the incident stellar flux and the radiated heat from the planet, ii) a Bond albedo (the fraction of total power incident upon the planet scattered back into space) of 0.3, iii) that the planet and star are blackbodies, and iv) that the heat is evenly distributed between the day and night sides of the planet. 25 to 14667
stellar metallicity (dex). The base-10 logarithm of the Fe to H ratio at the surface of the star, normalized by the solar Fe to H ratio. -2.5000 to 0.5600
Provenance of stellar parameters. A flag describing the source of the stellar parameters.
KIC = the parameters are extracted from the Kepler Input Catalog (Brown et al. 2011). Uncertainties of Teff = 200 K, log(g) = 0.3 dex and [Fe/H] = 0.4.
J-K = the star is unclassified in the KIC, J-K has been used to estimate temperature. The host star is assumed to be on the ZAMS with corresponding log(g) based on the Schmidt-Kaler relation.
Solar = the star is unclassified in the KIC, so the host star is assumed to have solar properties.
SME = Spectroscopic parameters derived from SME analysis (Valenti and Piskunov 1996). Stellar parameters are derived based on stellar evolution models.
SPC = Spectroscopic parameters derived from SPC analysis (Buchhave et al. 2012). Stellar parameters are derived based on stellar evolution models.
Pinsonneault = uses a revised Teff scale from Pinsonneault et al. (2012) with [Fe/H] fixed at -0.2. The quantity log(g) is taken from the KIC. Values are then revised by fitting to Yonsei-Yale stellar evolution models (Yi et al. 2001).
Astero = host star properties have been measured by comparison with astroseismologial models. examples: SPC, Solar, SME, null, Pinsonneault, KIC, J-K
bit-map of quarters searched. A bit string indicating which quarters of Kepler data were searched for transit signatures. Reading from left to right, the bits indicate the quarters. A value of one for any bit means that the designated quarter was searched for transits, a value of zero means that quarter was not included in the transit search. 1111111011101110
Limb Darkening Coefficient 1. Up to four coefficients define stellar limb darkening (e.g., Claret 2000). Limb darkening is the variation of specific intensity of the star as a function of μ = cos(θ). θ is the angle between the line-of-sight of an observer and a line perpendicular to the stellar surface at an observed point. 0.1254 to 0.9486
The number of expected transits or partially-observed transits associated with the planet candidate occurring within the searched light curve. This does not include transits that fall completely within data gaps. 0 to 2664
False Positive comment. A description of the reason why an object's disposition has been given as False Positive. The following keywords are short-hand for certain criterion used to determine if a KOI is a False Positive:
APO: "Active Pixel Offset", the pixels showing the transit do not coincide with the target star, indicating that the transit is actually on a background object.
Binary: indicates that the transit event is due to an eclipsing binary, not a planet.
EB: target is an eclipsing binary, or there is an unresolved background binary.
odd-even: the depth of the even numbered transits are statistically different than the depths of the odd numbered transits, this is a sign of a background eclipsing binary.
V-shaped: likely a grazing eclipsing binary.
SB1: target star is a single-lined spectroscopic binary.
SB2: target star is a double-lined spectroscopic binary. all null
The goodness of the transit fit to the data. Within the TCE table this quantity is the chi-squared statistic. Within the KOI table this quantity is the reduced-chi-squared statistic, e.g., divided by the number of degrees of freedom in the fit. currently all null
The Right Ascension (J2000) of the location of the transiting object calculated from the flux-weighted centroids. This result does not reflect the systematics due to crowding which can introduce significant errors in the calculated position. In decimal hours. 18.6570 to 20.1148
The Declination (J2000) of the location of the transiting object calculated from the flux-weighted centroids. This result does not reflect the systematics due to crowding which can introduce significant errors in the calculated position. In degrees. 36.5769 to 52.3382
The RA (J2000) flux-weighted centroid shift. This is the RA of the in-transit flux weighted centroid minus the RA of the out-of-transit flux weighted centroid. -742.4300 to 549.5000
The Dec (J2000) flux-weighted centroid shift. This is the Dec of the in-transit flux weighted centroid minus the Dec of the out-of-transit flux weighted centroid. -417.9000 to 712.5000
The calculated Right Ascension offset of the transiting or eclipsing object from the KIC location of the target star. The accuracy of this calculation degrades when the transit source has significant flux that falls outside the photometric aperture + a halo of pixels around it. -4 to 1.1900
The calculated Declination offset of the transiting or eclipsing object from the KIC location of the target star. The accuracy of this calculation degrades when the transit source has significant flux that falls outside the photometric aperture + a halo of pixels around it. -6 to 5
The angular offset in the RA (J2000) direction between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by simultaneously fitting all quarters. The out-of-transit centroid is subtracted from the difference image centroid. -25.1000 to 45.6800
The angular offset in the Dec (J2000) direction between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by simultaneously fitting all quarters. The out-of-transit centroid is subtracted from the difference image centroid. -75.9000 to 27.5000
The angular offset on the plane of the sky between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by simultaneously fitting all quarters. The out-of-transit centroid is subtracted from the difference image centroid. 0 to 88.6000
The angular offset in the RA (J2000) direction between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by averaging the weighted single-quarter measurements. The out-of-transit centroids are subtracted from the difference image centroids. -11.4290 to 12.6000
The angular offset in the Dec (J2000) direction between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by averaging the weighted single-quarter measurements. The out-of-transit centroids are subtracted from the difference image centroids. -11.8000 to 10.1000
The angular offset on the plane of the sky between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by averaging the weighted single-quarter measurements. The out-of-transit centroids are subtracted from the difference image centroids. 0.0390 to 14.8000
The angular offset in the RA (J2000) direction between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by simultaneously fitting all quarters. The out-of-transit centroid is subtracted from the difference image centroid. -27.8000 to 46.5700
The angular offset in the Dec (J2000) direction between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by simultaneously fitting all quarters. The out-of-transit centroid is subtracted from the difference image centroid. -76.6000 to 34
The angular offset on the plane of the sky between the best-fit PRF centroids from the Out-Of-Transit image and the Difference Image by simultaneously fitting all quarters. The out-of-transit centroid is subtracted from the difference image centroid. 0 to 89.6000
The angular offset in the RA (J2000) direction between the best-fit PRF centroids from the difference image and the Kepler Input Catalog position by averaging the weighted single-quarter measurements. The KIC position is subtracted from the difference image centroids. -11.3460 to 10.9000
he angular offset in the Dec (J2000) direction between the best-fit PRF centroids from the difference image and the Kepler Input Catalog position by averaging the weighted single-quarter measurements. The KIC position is subtracted from the difference image centroids. -12.3000 to 10.7000
The angular offset in the plane of the sky between the best-fit PRF centroids from the difference image and the Kepler Input Catalog position by averaging the weighted single-quarter measurements. The KIC position is subtracted from the difference image centroids. 0.0410 to 14.7000
Delivery Vetting Status (active or done). After a period of activity, the classification of the KOI table will change from ACTIVE to DONE when all dispositions are judged as final and all model parameters have been updated appropriately. This will typically occur after a new delivery of TCEs to the archive based on a longer data baseline. active,done
Link to the DR25 Data Validation Report (DVR) File if available. Note the Kepler Data Release 25 Data Validation process produces several files for stars with at least one Threshold-crossing event (TCE). One TCE is defined as three transit-like signals detected with a consistent period. If a TCE was detected for the input target, links will appear to the following files: A single-page summary PDF file for each TCE (DVS), an extensive multi-page PDF report (DVR). The DV time series files in FITS format can be found in the same directories.
Not Transit-Like: A KOI whose light curve is not consistent with that of a transiting planet. This includes, but is not limited to, instrumental artifacts, non-eclipsing variable stars, and spurious (very low SNR) detections. (1=true, 0=false) 0 to 1
Significant Secondary: A KOI that is observed to have a significant secondary event, indicating that the transit-like event is most likely caused by an eclipsing binary. However, self-luminous, hot Jupiters with a visible secondary eclipse will also have this flag set to true (1) with a disposition of PC. 0 to 1
Centroid Offset: The source of the transit-like signal is from a nearby star, as observed by measuring the centroid location of the image both in and out of transit. (1=true, 0=false) 0 to 1
Ephemeris Match Indicates Contamination: The KOI shares the same period and epoch as another object and is judged to be the result of flux contamination in the aperture or electronic crosstalk. (1=true, 0=false) 0 to 1
Planetary fit type. Possible values include LS (Least Squares fit), MCMC (Markov Chain Monte Carlo fit), DV (Data Validation pipeline fit), and none (fit is not provided, only orbital period, transit epoch and transit duration are reported)
The disposition score has a value between 0 and 1. Values close to one indicate high confidence in the disposition of a KOI as a Planetary Candidate. Values close to zero indicate high confidence in the disposition of a KOI as a False Positive. 0 to 1