You may now search on any column in the mission database. Select the field you wish to search on and type in the qualification. NOTE that if you choose a field in BOTH the form and in the User Option field, then you may not get results or the result you expect.
In the table below is a list of all the column names available for search. Where reasonable a range or set of valid values is listed. Additional useful notes are included. If you click on the field name, a more detailed description of the data will be found. The column label is used in the search forms and search results. The column name needs to be specified for GET requests.
| Column Name | Column Label | Data Type | Valid Values | Notes | UCDs |
|---|---|---|---|---|---|
| kic_kepler_id | Kepler_ID | long | range: 482,249 to 13,160,229 | Unique Kepler ID. Also used in Kepler Target Catalog and in naming data files. Note there are 6,569,466 entries in the KIC_CT joined table | ID_MAIN |
| kic_tmid | 2MASS_ID | long | range: 79221107 to 1316970448 | 2MASS catalog ID | ID_CATALOG |
| kic_degree_ra | RA_(J2000) | double | range: 279.14 to 302.32 degrees | Right Ascension (J2000) in decimal degrees. All but roughly 36,000 photometric standards, are within the Kepler FOV. | POS_EQ_RA_MAIN |
| kic_dec | Dec_(J2000) | double | range: 36.3 to 52.82 degrees | Declination (J2000) in decimal degrees. All but roughly 36,000 photometric standards, are within the Kepler FOV. | POS_EQ_DEC_MAIN |
| kic_pmra | RA_PM | float | range: -8.36 to 8.04 arcsec/yr | RA proper motion | POS_PM |
| kic_pmdec | Dec_PM | float | range: -7.2 to 8.848 arcsec/yr | Dec proper motion | POS_PM |
| kic_umag | U_Mag | float | range: 10.23 to 20.96 | U-band magnitude accurate to 0.04 magnitude | PHOT_MAG_U |
| kic_gmag | G_Mag | float | range: 2.87 to 24.40 | G-band magnitude | PHOT_MAG_G |
| kic_rmag | R_Mag | float | range: 2.895 to 24.99 | R-band magnitude | PHOT_MAG_M |
| kic_imag | I_Mag | float | range: 5.66 to 25.18 | I-band magnitude | PHOT_MAG_I |
| kic_zmag | Z_Mag | float | range: 5.31 to 19.42 | Z-band magnitude accurate to 0.03 magnitude | PHOT_MAG_Z |
| kic_gredmag | GRed_Mag | float | range: 8.52 to 19.13 | GRed-band magnitude | PHOT_MAG_UNDEF |
| kic_d51mag | D51_Mag | float | range: 7.02 to 19.85 | D51-band magnitude | PHOT_MAG_UNDEF |
| kic_jmag | J_Mag | float | range: 0.001 to 19.87 | 2MASS J-band magnitude | PHOT_MAG_J |
| kic_hmag | H_Mag | float | range: 0.0001 to 20.52 | 2MASS H-band magnitude | PHOT_MAG_H |
| kic_kmag | K_Mag | float | range: 0.001 to 18.59 | 2MASS K-band magnitude | PHOT_MAG_K |
| kic_kepmag | Kepler_Mag | float | range: 2.98 to 24.99 | Kepler-band magnitude | PHOT_MAG_UNDEF |
| kic_scpid | SCP_ID | long | range: 79224823 to 1305757552 | SCP processing ID | |
| kic_altid | Alt_ID | long | range: -1244299 to 1065212930 | ID from alternate source catalog (see Alt ID Source entry) | ID_CATALOG |
| kic_altsource | Alt_ID_Source | long | 0 - null, 1 - Hipparcos catalog ID, 2 - Tycho2 ID, 3 - UCAC2 ID, 4 - General Catalog of Var. Stars ID, 5 - Lepine proper motion catalog star. altid>0 is 2MASS ID, altid< 0 is a pseudo-id generated by SCP processing, 6 - altid contains 2MASS ID coming from Astroseiseismology catalog, 11 - NED ID, 12 - Extended 2MASS ID, 13 - FIRST ID, 14 - NVSS catalog ID, 15 - VLBA catalog ID, 16 - CHANDRA catalog ID | Source catalog that was used for deriving stellar parameters. | ID_CATALOG |
| kic_galaxy | Star/Gal_ID | long | 0 = USNO-B values 0 to 5 (i.e., a galaxy), 1 = values 6 to 11 (i.e., a star). The values 0 - 11 were a measure of the similarity between a given image to a stellar point spread function. 0 is quite dissimilar, 11 means quite similar. | Star/galaxy indicator based on the USNO-B star/galaxy estimator. | ID_GROUP |
| kic_blend | Isolated/Blend_ID | long | Not yet (and may never be) determined. All values are null. | Isolated/blended indicator | ID_GROUP |
| kic_variable | Var._ID | long | 0 - constant, 1 - variable | Constant/variable indicator based on data from the General Catalog of Variable Stars. (Additional catalogs will be used in future versions.) | ID_GROUP |
| kic_teff | Teff | long | range: 3105 to 19337 degrees K | Derived Effective Temperature accurate to 200 K | PHYS_TEMP_EFFEC |
| kic_logg | Log_G | float | range: -0.43 to 6.16 | Derived Log10 surface gravity accurate to 0.5 dex | PHYS_GRAVITY_SURFACE |
| kic_feh | Metallicity | float | range: -2.62 to 0.62 | Derived Log10 Fe/H metallicity accurate to 0.5 dex. | PHYS_ABUND_[FE/H] |
| kic_ebminusv | E(B-V) | float | range: 0.001 to 0.521 | Derived Excess B-V reddening accurate to 0.1 magnitude | PHOT_COLOR_EXCESS |
| kic_av | A_V | float | range: 0.003 to 1.62 | Derived A-V extinction | PHOT_EXTINCTION |
| kic_radius | Radius | float | range: 0.097 to 316.30 | Estimated Stellar Radius (solar = 1.0) | PHYS_SIZE_RADIUS |
| kic_cq | Kepmag_Source | char | SCP, NOCAL, 2MASS, UNCAL, PHOTO, TYBV SCP - SCP values for sdssg and sdssr were used to compute KEPMAG using equation below . The error for KEPMAG is roughly 0.03 mag., NOCAL - No calibration to optical mag. possible, used for entries from non-optical catalogs. KEPMAG field is null. , 2MASS - Objects found only in 2MASS Catalog with no optical counterpart, KEPMAG is null, UNCAL - KEPMAG copied from a single color of the parent catalog, uncertainty could be 1.0 mag or higher, PHOTO - parent catalog contained a red and blue mag. obtained from Photographic photometry. Values used to compute KEPMAG on the basis of: sdssg=blue sdssr=red color=sdssg-sdssr if (color<=0.8) kepmag = 0.8*sdssr + 0.2*sdssg else kepmag = 0.9*sdssr+0.1*sdssg, internal photographic errors have errors of 0.2 mag suggest KEPMAG errors of 0.03 mag, TYBV - parent catalog is Tycho-2 and this gives B and V magnitudes. KEPMAG value computed from sdssg=0.54*b+0.46*v-0.07 sdssr=-0.44*b+1.44*v+0.12 using same transformation as above to calc. KEPMAG. Errors same as for TYCHO-2 catalog. | Source of Kepler-band magnitude. | |
| kic_pq | Photometry_Qual | long | range: Integer from 0 to 8 which is the count of non-null entries in USNO-B1.0 (O,E,J,F,N), UCAC-2 (R), TYcho-2 (B,V). In general the more colors the more likely the star is real. For NOCAL and 2MASS entries, this value = 0. Stars with low values (e.g., < 3) may not be real and should be verified by other means. | Photometry quality indicator. | |
| kic_aq | Astrophysics_Qual | long | range: currently 0 to 6 which is the count of all non-null entries in Teff, logG, FeH, AV, E(B-V), and Radius. | Astrophysics quality indicator. Placeholder for SCP values not yet determined. | |
| kic_catkey | Catalog_key | long | range: 310909 to 12958343 | Unique integer key to CATKEY database table (not currently available). | |
| kic_scpkey | Scp_Key | long | range: 262005541 to 1305757193 | Unique integer key to SCPKEY database table (not currently available). | |
| kic_parallax | Parallax | float | range: -0.0297 to 0.04 arcsec | Parallax in arcsec | POS_PARLX |
| kic_glon | Gal_Lon | float | range: 67.75 to 84.88 degrees | Galactic Longitude | POS_GAL_LON |
| kic_glat | Gal_Lat | float | range: 5.17 to 21.82 degrees | Galactic Latitude | POS_GAL_LAT |
| kic_pmtotal | Total_PM | float | range: 0.0 to 9.46 arcsec/yr | Total proper motion accurate to 20 mas/yr | POS_PM |
| kic_grcolor | G-R_color | float | range: -10.31 to 10.43 | G-R color | |
| kic_jkcolor | J-K_color | float | range: -7.44 to 8.21 | J-K color | |
| kic_gkcolor | G-K_color | float | range: -6.67 to 14.85 | G-K color | |
| kic_ra | RA_hours_(J2000) | float | range: 18.61 to 20.15 hours | Right Ascension (J2000) in decimal hours | POS_EQ_RA |
| kct_sky_group_id_value | Skygroup_ID | long | range: 1 - 84 | An integer value from 1 to 84 describing the module/channel where the target falls. It's equivalent to the channel number during season 2. The sky group is an integer that groups stars together on the sky depending on which channel they fall on (or near) during season 2. Due to slight asymmetries in the CCD array layout, positions are not perfectly maintainted upon seasonal rotation of the spacecraft. Therefore, there are objects that fall off silicon during season 2 but are on silicon in subsequent seasons. This is especially problematic for Module 13 due to the center gap. Such stars are assigned the sky group corresponding to the other stars that fall on the same channel during other seasons. | |
| kct_crowding_value | Crowding value | float | range: 0.0 to 1.0 | The crowding metric is a number between 0 and 1 that specifies the fraction of flux (in the optimal photometric aperture) due to the target star with respect to the total flux from all sources (background flux primarily including that from neighboring stars) in the same aperture. The metric is simulated using a complete end-to-end model of the instrument. It is derived from stellar magnitudes taken from the Kepler Input Catalog. A value of 0.5 means half the light through the aperture is due to the target. | |
| kct_channel_season_0_value | Channel_0 | long | range: 1 to 84 | Integer channel number for season 0. There are 21 modules, each with 4 outputs for a total of 84 channels. CHANNEL is an integer ranging from 1 to 84 that uniquely specifies the MODULE/OUTPUT pair. An object can have a non-zero channel number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_module_season_0_value | Module_0 | long | 2-4,6-20,22-24 | Integer module number for season 0. A module refers to a pair of CCDs that share a field flattener and are read out simultaneously by the detector electronics. There are 21 modules on the focal plane. MODULE is an integer from the set [2-4,6-20,22-24]. An object can have a non-zero module number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_output_season_0_value | Output_0 | long | range 1 to 4 | Each module has four output channels (two per CCD). Each output is read out by a unique analog signal chain (e.g. amplifier). OUTPUT is an integer ranging from 1 to 4. An object can have a non-zero output number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_row_season_0_value | Row_0 | long | range -225 to 1094 | Row number for season 0 with values ranging from -225 to 1094. Each channel has 1132 columns and 1070 rows. There are 1024 science rows enumerated as rows 20 through 1043. Collateral data is enumerated as rows 0 through 19 and 1044 through 1069. Values outside 0 through 1069 are enumerated in order to provide information about how far off a target is from the CCD channel. | |
| kct_column_season_0_value | Column_0 | long | range -201 to 1111 | Column number for season 0 defined like the Row values. Each channel has 1132 columns. There are 1100 science channels described as columns 12 - 1111. Collateral values range from 0-11 and 1112-1131. Other values ranging from -201 to -1 describe how far a target is from the CCD channel. | |
| kct_channel_season_1_value | Channel_1 | long | range: 1 to 84 | Integer channel number for season 1. There are 21 modules, each with 4 outputs for a total of 84 channels. CHANNEL is an integer ranging from 1 to 84 that uniquely specifies the MODULE/OUTPUT pair. An object can have a non-zero channel number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_module_season_1_value | Module_1 | long | 2-4,6-20,22-24 | Integer module number for season 1. A module refers to a pair of CCDs that share a field flattener and are read out simultaneously by the detector electronics. There are 21 modules on the focal plane. MODULE is an integer from the set [2-4,6-20,22-24]. An object can have a non-zero module number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_output_season_1_value | Output_1 | long | range 1 to 4 | Each module has four output channels (two per CCD). Each output is read out by a unique analog signal chain (e.g. amplifier). OUTPUT is an integer ranging from 1 to 4. An object can have a non-zero output number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_row_season_1_value | Row_1 | long | range -225 to 1094 | Row number for season 1 with values ranging from -225 to 1094. Each channel has 1132 columns and 1070 rows. There are 1024 science rows enumerated as rows 20 through 1043. Collateral data is enumerated as rows 0 through 19 and 1044 through 1069. Values outside 0 through 1069 are enumerated in order to provide information about how far off a target is from the CCD channel. | |
| kct_column_season_1_value | Column_1 | long | range -201 to 1111 | Column number for season 1 defined like the Row values. Each channel has 1132 columns. There are 1100 science channels described as columns 12 - 1111. Collateral values range from 0-11 and 1112-1131. Other values ranging from -201 to -1 describe how far a target is from the CCD channel. | |
| kct_channel_season_2_value | Channel_2 | long | range: 1 to 84 | Integer channel number for season 2. There are 21 modules, each with 4 outputs for a total of 84 channels. CHANNEL is an integer ranging from 1 to 84 that uniquely specifies the MODULE/OUTPUT pair. An object can have a non-zero channel number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_module_season_2_value | Module_2 | long | 2-4,6-20,22-24 | Integer module number for season 2. A module refers to a pair of CCDs that share a field flattener and are read out simultaneously by the detector electronics. There are 21 modules on the focal plane. MODULE is an integer from the set [2-4,6-20,22-24]. An object can have a non-zero module number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_output_season_2_value | Output_2 | long | range 1 to 4 | Each module has four output channels (two per CCD). Each output is read out by a unique analog signal chain (e.g. amplifier). OUTPUT is an integer ranging from 1 to 4. An object can have a non-zero output number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_row_season_2_value | Row_2 | long | range -225 to 1094 | Row number for season 2 with values ranging from -225 to 1094. Each channel has 1132 columns and 1070 rows. There are 1024 science rows enumerated as rows 20 through 1043. Collateral data is enumerated as rows 0 through 19 and 1044 through 1069. Values outside 0 through 1069 are enumerated in order to provide information about how far off a target is from the CCD channel. | |
| kct_column_season_2_value | Column_2 | long | range -201 to 1111 | Column number for season 2 defined like the Row values. Each channel has 1132 columns. There are 1100 science channels described as columns 12 - 1111. Collateral values range from 0-11 and 1112-1131. Other values ranging from -201 to -1 describe how far a target is from the CCD channel. | |
| kct_channel_season_3_value | Channel_3 | long | range: 1 to 84 | Integer channel number for season 3. There are 21 modules, each with 4 outputs for a total of 84 channels. CHANNEL is an integer ranging from 1 to 84 that uniquely specifies the MODULE/OUTPUT pair. An object can have a non-zero channel number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_module_season_3_value | Module_3 | long | 2-4,6-20,22-24 | Integer module number for season 3. A module refers to a pair of CCDs that share a field flattener and are read out simultaneously by the detector electronics. There are 21 modules on the focal plane. MODULE is an integer from the set [2-4,6-20,22-24]. An object can have a non-zero module number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_output_season_3_value | Output_3 | long | range 1 to 4 | Each module has four output channels (two per CCD). Each output is read out by a unique analog signal chain (e.g. amplifier). OUTPUT is an integer ranging from 1 to 4. An object can have a non-zero output number if it is off, but near, a CCD. Such cases can be identified by examining the expected ROW and COLUMN values for a specified season. | |
| kct_row_season_3_value | Row_3 | long | range -225 to 1094 | Row number for season 3 with values ranging from -225 to 1094. Each channel has 1132 columns and 1070 rows. There are 1024 science rows enumerated as rows 20 through 1043. Collateral data is enumerated as rows 0 through 19 and 1044 through 1069. Values outside 0 through 1069 are enumerated in order to provide information about how far off a target is from the CCD channel. | |
| kct_column_season_3_value | Column_3 | long | range -201 to 1111 | Column number for season 3 defined like the Row values. Each channel has 1132 columns. There are 1100 science channels described as columns 12 - 1111. Collateral values range from 0-11 and 1112-1131. Other values ranging from -201 to -1 describe how far a target is from the CCD channel. | |
| kct_distance_0 | Edge_Distance_0 | long | range 1 to 511 | The shortest distance to the detector edge for season 0. | |
| kct_distance_1 | Edge_Distance_1 | long | range 1 to 511 and null | The shortest distance to the detector edge for season 1. | |
| kct_distance_2 | Edge_Distance_2 | long | range 1 to 511 and null | The shortest distance to the detector edge for season 2. | |
| kct_distance_3 | Edge_Distance_3 | long | range 1 to 511 and null | The shortest distance to the detector edge for season 3. | |
| kct_num_season_onCCD | Seasons_on_CCD | long | range 1 to 4 and null (note: roughly 30% of the targets were included because they are near the edge) | Number of seasons a target is on the detector | |
| kct_contamination | Contamination | float | range 0 - 1 | Measure of light contamination defined as 1 - crowding_value |