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**Resource Description:**

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to this table's
resource, see Information on resource 'Lunar craters (demo)'

This table has an **associated publication**. If you use data from it,
it may be appropriate to reference
2009LPI....40.1532L
(ADS BibTeX entry for the publication) either
in addition to or instead of the service reference.

To cite the **table as such**, we suggest the following
BibTeX entry:

@MISC{vo:lunar_crater_database_epn_core, year=2015, title={Lunar craters (demo)}, author={François Andrieu}, url={http://voparis-cdpp.obspm.fr/tableinfo/lunar_crater_database.epn_core}, howpublished={{VO} resource provided by the {PADC} {TAP} Server on voparis-cdpp.obspm.fr} }

Sorted by DB column index. [Sort alphabetically]

Name | Table Head | Description | Unit | UCD |
---|---|---|---|---|

granule_uid | Granule_uid | Internal table row index Unique ID in data service, also in v2. Can be alphanumeric. | N/A | meta.id |

granule_gid | Granule_gid | Common to granules of same type (e.g. same map projection, or geometry data products). Can be alphanumeric. | N/A | meta.id |

obs_id | Obs_id | Associates granules derived from the same data (e.g. various representations/processing levels). Can be alphanumeric, may be the ID of original observation. | N/A | meta.id |

dataproduct_type | Dataproduct_type | The high-level organization of the data product, from enumerated list (e.g., 'im' for image, sp for spectrum) [Note et_prod] | N/A | meta.code.class |

target_name | Target_name | Standard IAU name of target (from a list related to target class), case sensitive | N/A | meta.id;src |

target_class | Target_class | Type of target, from enumerated list | N/A | meta.code.class;src |

time_min | Time_min | Acquisition start time (in JD) | d | time.start |

time_max | Time_max | Acquisition stop time (in JD) | d | time.end |

time_sampling_step_min | Time_sampling_step_min | Sampling time for measurements of dynamical phenomena, lower limit. | s | time.interval;stat.min |

time_sampling_step_max | Time_sampling_step_max | Sampling time for measurements of dynamical phenomena, upper limit | s | time.interval;stat.max |

time_exp_min | Time_exp_min | Integration time of the measurement, lower limit. | s | time.duration;obs.exposure;stat.min |

time_exp_max | Time_exp_max | Integration time of the measurement, upper limit | s | time.duration;obs.exposure;stat.max |

spectral_range_min | Spectral_range_min | Spectral range (frequency), lower limit. | Hz | em.freq;stat.min |

spectral_range_max | Spectral_range_max | Spectral range (frequency), upper limit | Hz | em.freq;stat.max |

spectral_sampling_step_min | Spectral_sampling_step_min | spectral sampling step, lower limit. | Hz | em.freq.step;stat.min |

spectral_sampling_step_max | Spectral_sampling_step_max | spectral sampling step, upper limit | Hz | em.freq.step;stat.max |

spectral_resolution_min | Spectral_resolution_min | Sectral resolution, lower limit. | Hz | spect.resolution;stat.min |

spectral_resolution_max | Spectral_resolution_max | Sectral resolution, upper limit | Hz | spect.resolution;stat.max |

c1min | C1min | Longitude on body, lower limit. | deg | pos.bodyrc.long;stat.min |

c1max | C1max | Longitude on body, upper limit | deg | pos.bodyrc.long;stat.max |

c2min | C2min | Latitude on body, lower limit. | deg | pos.bodyrc.lat;stat.min |

c2max | C2max | Latitude on body, upper limit | deg | pos.bodyrc.lat;stat.max |

c3min | C3min | Height over defined null, lower limit. | m | pos.bodyrc.alt;stat.min |

c3max | C3max | Height over defined null, upper limit | m | pos.bodyrc.alt;stat.max |

s_region | S_region | ObsCore-like footprint, valid for celestial, spherical, or body-fixed frames. | N/A | phys.outline;obs.field |

c1_resol_min | C1_resol_min | Resolution in the first coordinate, lower limit. | deg | pos.resolution;stat.min |

c1_resol_max | C1_resol_max | Resolution in the first coordinate, upper limit | deg | pos.resolution;stat.max |

c2_resol_min | C2_resol_min | Resolution in the second coordinate, lower limit. | deg | pos.resolution;stat.min |

c2_resol_max | C2_resol_max | Resolution in the second coordinate, upper limit | deg | pos.resolution;stat.max |

c3_resol_min | C3_resol_min | Resolution in the third coordinate, lower limit. | m | pos.resolution;stat.min |

c3_resol_max | C3_resol_max | Resolution in the third coordinate, upper limit | m | pos.resolution;stat.max |

spatial_frame_type | Spatial_frame_type | Flavor of coordinate system, defines the nature of coordinates. From enumerated list | N/A | meta.code.class;pos.frame |

incidence_min | Incidence_min | Incidence angle (solar zenithal angle) during data acquisition, lower limit. | deg | pos.posAng;stat.min |

incidence_max | Incidence_max | Incidence angle (solar zenithal angle) during data acquisition, upper limit | deg | pos.posAng;stat.max |

emergence_min | Emergence_min | Emergence angle during data acquisition, lower limit. | deg | pos.posAng;stat.min |

emergence_max | Emergence_max | Emergence angle during data acquisition, upper limit | deg | pos.posAng;stat.max |

phase_min | Phase_min | Phase angle during data acquisition, lower limit. | deg | pos.phaseAng;stat.min |

phase_max | Phase_max | Phase angle during data acquisition, upper limit | deg | pos.phaseAng;stat.max |

instrument_host_name | Instrument_host_name | Standard name of the observatory or spacecraft. | N/A | meta.id;instr.obsty |

instrument_name | Instrument_name | Standard name of instrument | N/A | meta.id;instr |

measurement_type | Measurement_type | UCD(s) defining the data, with multiple entries separated by hash (#) characters. | N/A | meta.ucd |

processing_level | Processing_level | CODMAC calibration level; see the et_cal note http://dc.g-vo.org/tableinfo/titan.epn_core#note-et_cal for what values are defined here. [Note et_cal] | N/A | meta.code;obs.calib |

creation_date | Creation_date | Date of first entry of this granule | N/A | time.creation |

modification_date | Modification_date | Date of last modification (used to handle mirroring) | N/A | time.update |

release_date | Release_date | Start of public access period | N/A | time.release |

service_title | Service_title | Title of resource (an acronym really, will be used to handle multiservice results) | N/A | meta.title |

publisher | Publisher | A short string identifying the entity running the data service used. | N/A | meta.ref |

bib_reference | Bib_reference | Bibcode preferred if available (does that include link?), doi, or other biblio id, URL | N/A | meta.bib |

feature_name | Feature_name | Secondary name (can be standard name of region of interest). | N/A | meta.id;pos |

Diameter | Diameter | Diameter of the crater | km | phys.size.diameter |

Longitude | Longitude | Longitude of the crater from -180 to 180 eastward | deg | pos.bodyrc.lon |

Apparent_diameter | Apparent_diameter | Apparent diameter [km], measured at the pre-impact surface level, according to Pike (1977b). | km | phys.size.diameter |

Tcd_high | Transient_cavity_diameter_simple | Transient cavity diameter [km], for simple craters (smaller than 15 km) equation Dtc=0.84D from Melosh (1989, p. 129) is applied, for complex craters larger than 15 km equation 9 from Croft (1985) is applied. | km | phys.size.diameter |

Tcd_low | Transient_cavity_diameter_complex | Transient cavity diameter [km] for complex craters. Equation 5 from Kring (1995) is applied with the assumption that transient cavity radius of complex and simple craters are the same. (0 means that value can not be calculated for simple craters, i.e. smaller than 15 km in diameter.) | km | phys.size.diameter |

Citation_for_first_mention | Citation_for_first_mention | Citation for first mention, citation for nomenclature (see the References worksheet) from Chuck Wood database | N/A | meta.bib |

Floor_diameter | Floor_diameter | Floor diameter [km], calculated based on Hörz et al. (1991, table 4.1, pp. 66; Pike 1977). (0 means that basin is too big to be able to use the equation accurately for craters smaller than 20 and larger than 125 km in diameter.) | km | phys.size.diameter |

Measured_rim_to_floor_depth | Measured_rim_to_floor_depth | Measured rim to floor depth, mainly from Arthur (1974) with additional data from Pike (1976). When both values were available, Arthur s data was used. | km | phys.size |

Rim_to_floor_depth | Rim_to_floor_depth | Rim to floor depth [km], calculated based on Pike 1977a. (0 means that basin is too big to be able to use the equation accurately for craters smaller than 15 km and larger than 275 km in diameter.) | km | phys.size |

Apparent_depth | Apparent_depth | Apparent depth [km], measured at the pre-impact surface level, according to Pike (1977b). | km | phys.size |

Transient_cavity_depth | Transient_cavity_depth | Transient cavity depth [km] equal to 1/3 of transient cavity diameter Stöffler et al. (2006). | km | phys.size |

Interior_volume | Interior_volume | Interior volume [km^3], calculated based on Hörz et al. (1991, table 4.1, pp. 66; Croft 1978). (0 means that value can not be calculated accurately for craters smaller than 13 and larger than 150 km in diameter.) | km**3 | phys.volume |

Rim_height | Rim_height | Rim height [km], calculated based on Hörz et al. (1991, table 4.1, pp. 66; Pike 1977a). (0 means that basin is too big to be able to use the equation accurately for craters smaller than 15 km and larger than 375 km in diameter.) | km | phys.size |

Rim_flank_width | Rim_flank_width | Rim flank width [km], calculated based on Hörz et al. (1991, table 4.1, pp. 66; Pike 1977). (0 means that basin is too big to be able to use the equation efficiently.) | km | phys.size |

Measured_height_of_central_peak | Measured_height_of_central_peak | Measured central peak height, from Wood 1973 (The actual central peak heights are available at: http://www.lpod.org/cwm/DataStuff/CP-heights.html). | km | phys.size |

Height_of_central_peak | Height_of_central_peak | Height of central peak [km], calculated based on Hörz et al. (1991, table 4.1, pp. 66; Hale and Grieve (1982)). (0 means that value cannot be calculated accurately for craters smaller than 17 km and larger than 51 km in diameter.) | km | phys.size |

Diameter_of_central_peak | Diameter_of_central_peak | Diameter of central peak [km], calculated based on Hörz et al. (1991, table 4.1, pp. 66; Hale and Head (1979)). (0 means that value cannot be calculated accurately for craters smaller than 17 km and larger than 175 km in diameter.) | km | phys.size.diameter |

Basal_area_of_central_peak | Basal_area_of_central_peak | Basal area of central peak [km^2], calculated based on Hörz et al. (1991, table 4.1, pp. 66; Hale and Grieve (1982)). (0 means that value cannot be calculated accurately for craters smaller than 17 km and larger than 136 km in diameter.) | km**2 | phys.area |

Maximum_diameter_of_ejecta_blocks_1 | Maximum_diameter_of_ejecta_blocks_1 | Maximum diameter of ejecta blocks [km] - coefficient 2, calculated from Hörz et al. (1991, table 4.3, pp. 72; based on Moore (1971)). (0 means that value cannot be calculated accurately for craters smaller than 0.1 and larger than 98 km in diameter.) | km | phys.size.diameter |

Maximum_diameter_of_ejecta_blocks_2 | Maximum_diameter_of_ejecta_blocks_2 | Maximum diameter of ejecta blocks [km] - coefficient 1, calculated from Hörz et al. (1991, table 4.3, pp. 72; based on Moore (1971)). (0 means that value cannot be calculated accurately for craters smaller than 0.1 and larger than 98 km in diameter.) | km | phys.size.diameter |

Thickness_of_ejecta_in_the_distance_equal_to_one_radius | Thickness_of_ejecta_in_the_distance_equal_to_one_radius | Thickness of ejecta in the distance equal to one radius [m] - ejecta on the rim, for simple craters equation 4 from Kring (1995), for complex craters (D>15000 m) calculated based on equation from McGetchin et al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) suggest that values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equation to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | m | phys.size |

Thickness_of_ejecta_in_the_distance_equal_to_two_radii | Thickness_of_ejecta_in_the_distance_equal_to_two_radii | Thickness of ejecta in the distance equal to two radii [m], for simple craters equation 4 from Kring (1995), for complex craters (D>15000 m) calculated based on equation from McGetchin et al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) suggest that values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equation to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | m | phys.size |

Thickness_of_ejecta_in_the_distance_equal_to_three_radii | Thickness_of_ejecta_in_the_distance_equal_to_three_radii | Thickness of ejecta in the distance equal to three radii [m], for simple craters equation 4 from Kring (1995), for complex craters (D>15000 m) calculated based on equation from McGetchin et al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) suggest that values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equation to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | m | phys.size |

Thickness_of_ejecta_in_the_distance_equal_to_four_radii | Thickness_of_ejecta_in_the_distance_equal_to_four_radii | Thickness of ejecta in the distance equal to four radii [m], for simple craters equation 4 from Kring (1995), for complex craters (D>15000 m) calculated based on equation from McGetchin et al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) suggest that values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equation to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | m | phys.size |

Thickness_of_ejecta_in_the_distance_equal_to_five_radii | Thickness_of_ejecta_in_the_distance_equal_to_five_radii | Thickness of ejecta in the distance equal to five radii [m], for simple craters equation 4 from Kring (1995), for complex craters (D>15000 m) calculated based on equation from McGetchin et al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) suggest that values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equation to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | m | phys.size |

Thickness_of_ejecta_in_the_distance_of_10km_outside_the_rim_1 | Thickness_of_ejecta_in_the_distance_of_10km_outside_the_rim_1 | Thickness of ejecta in the distance of 10,000 m outside the rim [m], for simple craters equation 4 from Kring (1995), for complex craters (D>15000 m) calculated based on equation from McGetchin al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) suggest that values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equation to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | m | phys.size |

Thickness_of_ejecta_in_the_distance_of_10km_outside_the_rim_2 | Thickness_of_ejecta_in_the_distance_of_10km_outside_the_rim_2 | Thickness of ejecta in the distance of 10,000 m outside the rim [m], calculated based on equation no 9 from Pike (1974), values for large multiring basins can be ambiguous. | m | phys.size |

Thickness_of_ejecta_in_the_distance_of_10km_outside_the_rim_3 | Thickness_of_ejecta_in_the_distance_of_10km_outside_the_rim_3 | Thickness of ejecta in the distance of 10,000 m outside the rim [m], calculated based on equation no 10 from Pike (1974), values for large multiring basins can be ambiguous. | m | phys.size |

Thickness_of_ejecta_in_the_distance_of_10km_outside_the_rim_4 | Thickness_of_ejecta_in_the_distance_of_10km_outside_the_rim_4 | Thickness of ejecta in the distance of 10,000 m outside the rim [m], calculated based on equation no 12 from Pike (1974), values for large multiring basins can be ambiguous. | m | phys.size.radius |

Radial_distance_of_continuous_ejecta_1 | Radial_distance_of_continuous_ejecta_1 | Radial distance of continuous ejecta [km] from the center of the crater, calculated based on Moore et al. (1974). (0 means that value cannot be calculated accurately for craters smaller than 0.65 km or larger than 218 km in diameter.) | km | phys.size.radius |

Radial_distance_of_continuous_ejecta_2 | Radial_distance_of_continuous_ejecta_2 | Radial distance of continuous ejecta [km], calculated after Hörz et al. (1991, table 4.3, pp. 72, based on Fig. 8 in Oberbeck et al. (1974)). (0 means that value cannot be calculated accurately for craters smaller than 0.56 km or larger than 1340 km in diameter.) | km | phys.size.radius |

Radius_of_ejecta_blanket_thicker_than_10_m | Radius_of_ejecta_blanket_thicker_than_10_m | Radius of ejecta blanket thicker than 10 m [km], equation no 9 from Pike (1974), values for large multiring basins can be ambiguous. | km | phys.size.radius |

Radius_of_ejecta_blanket_thicker_than_10_m_minimum | Radius_of_ejecta_blanket_thicker_than_10_m_minimum | Radius of ejecta of thicker than 10 m [km] (minimum estimate), for simple craters equation 4 from Kring (1995), for complex craters (D>15000 m) calculated based on equation from McGetchin et al. (1973). Minimum and maximum exponents are from Kring (1995), based on McGetchin et al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equations to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | km | phys.size.radius |

Radius_of_ejecta_blanket_thicker_than_10_m_best_estimate | Radius_of_ejecta_blanket_thicker_than_10_m_best_estimate | Radius of ejecta of thicker than 10 m [km] (best estimate), for simple craters equation 4 from Kring (1995), for complex craters (D>15) calculated based on equation from McGetchin et al. (1973). Minimum and maximum exponents are from Kring (1995), based on McGetchin et al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equations to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | km | phys.size.radius |

Radius_of_ejecta_blanket_thicker_than_10_m_maximum | Radius_of_ejecta_blanket_thicker_than_10_m_maximum | Radius of ejecta of thicker than 10 m [km] (maximum estimate), for simple craters equation 4 from Kring (1995), for complex craters (D>15) calculated based on equation from McGetchin et al. (1973). Minimum and maximum exponents are from Kring (1995), based on McGetchin et al. (1973). Equation used for complex craters was used in the original paper to calculate ejecta thickness of large basins like Imbrium in the Apollo landing sites, other authors (Hörz et al. 1991) values for large multiring basins can be ambiguous. Pike (1974) suggested 3 other equations to calculate thickness of ejecta blankets on the Moon that vary significantly (also calculated in this database). Because the equations are not calibrated in the reliable way, it is very hard to evaluate their precision. Usually the distance of continuous ejecta is assumed to be equal to distance of 2 or 3 radii (from crater center). | km | phys.size.radius |

Radius_of_radar_bright_halo | Radius_of_radar_bright_halo | Radius (from the center of the crater) of radar-bright halos (at 70 cm wavelength) emplaced ballistically around craters [km], from Eq. 8 in Ghent et al. (2010). Equation based on craters approximately D=5...130 km. | km | phys.size.radius |

Measured_radius_of_radar_bright_halo | Measured_radius_of_radar_bright_halo | Measured radius (from the center of the crater) of radar-bright halos (at 70 cm wavelength) emplaced ballistically around craters [km], from Table 1 in Ghent et al. (2010). | km | phys.size.radius |

Radius_of_radar_dark_halo | Radius_of_radar_dark_halo | Radius of radar-dark halos (at 70 cm wavelength) around craters [km], measured from the center of the crater. Based on data from Table 1 in Ghent et al. (2010), excluding Sinus Iridum and Orientale (too few data points in such large diameters). Thus, the craters range D=5.6…191 km. The equation is derived by plotting the data and fitting a power function in Excel. | km | phys.size.radius |

Measured_radius_of_radar_dark_halo | Measured_radius_of_radar_dark_halo | Measured radius of radar-dark halos (at 70 cm wavelength) around craters [km], measured from the center of the crater. Taken from Table 1 in Ghent et al. (2010). | km | phys.size.radius |

Depth_of_excavation_1 | Depth_of_excavation_1 | Depth of excavation [km] based on updated Fig. 22 (transient cavity) from Cintala and Grieve (1998). Reliable for craters larger than approx. 50 km | km | phys.size |

Depth_of_excavation_2 | Depth_of_excavation_2 | Depth of excavation [km] 1/10 transient cavity diameter Stöffler et al. (2006) | km | phys.size |

Depth_of_melting_1 | Depth_of_melting_1 | Depth of melting [km] based on updated Fig. 22 (transient cavity) from Cintala and Grieve (1998). Reliable for craters larger than approx. 50 km | km | phys.size |

Depth_of_melting_2 | Depth_of_melting_2 | Depth of melting [km] based on Fig. 23 (transient cavity) from Cintala and Grieve (1998). Reliable for craters between approximately 1 km and 400 km. Assumes a chondritic projectile hitting an anothosite target at 20 km/s. | km | phys.size |

Melt_volume | Melt_volume | Melt volume [km^3] calculated for chondritic projectile impacting anorthosite target at 20 km/s, based on equation 8 and Table 2 from Cintala and Grieve (1998). | km**3 | phys.volume |

Melt_volume_45deg_on_basalt | Melt_volume_45deg_on_basalt | Melt volume [km^3] calculated for a 45 degree impact on a basaltic target, using Eq. 12 and Table 1 from Abramov et al. (2012). | km**3 | phys.volume |

Melt_volume_45deg_on_anorthosite | Melt_volume_45deg_on_anorthosite | Melt volume [km^3] calculated for a 45 degree impact on an anorthositic target, using Eq. 12 and Table 1 from Abramov et al. (2012). | km**3 | phys.volume |

Age | Age | Age (Wilhelms, 1987; Wilhelms, personal communication, 2008; Wilhelms and Byrne, 2009). Note that there are discrepancies between the different sources. In most cases the most recent data has been used, see the remarks. | N/A | time.age |

Age_class | Age_class | Age class (1 Pre-Nectarian, 2 Nectarian, 3 Lower Imbrian, 4 Upper Imbrian, 5 Eratosthenian, 6 Copernican) (Wilhelms, 1987; Wilhelms, personal communication, 2008; Wilhelms and Byrne, 2009) | N/A | meta.code.class |

Remarks | Remarks | Remarks (Wilhelms, 1987; Wilhelms, personal communication, 2008; Wilhelms and Byrne, 2009); Also included are the unapproved names and the former names of recently renamed craters, as well as if the crater is a small crater in Apollo or Lunokhod-1 landing sites. | N/A | meta.note |

Age_source | Age_source | Age - source (Wilhelms, 1987 table: 1, map only: 2; personal communication, 2008: PC; Wilhelms and Byrne, 2009: WandB09). Note that most of the ages from PC are incorporated in WandB09. | N/A | meta.bib |

Age_other_sources | Age_other_sources | Age - other sources | N/A | meta.bib |

Basin_age_group | Basin_age_group | Basin age group (higher number - younger) (Wilhelms, 1987) | N/A | meta.code.class |

Approval | Approval | Approval year or date in the official IAU-USGS database (Gazetteer of Planetary Nomenclature) | N/A | time |

OMAT_range | OMAT_range | The range of optical maturity parameter (OMAT) using Kaguya (SELENE) Multiband Imager (MI) data, from Supplement Table 1 in Ohtake et al. 2009. | N/A | arith.factor |

Province | Province | Geological province: PKT = Procellarum KREEP Terrane, SPA = South Pole - Aitken (Terrane?), or highlands (Feldspathic Highlands Terrane?), from Supplement Table 1 in Ohtake et al. 2009. | N/A | meta |

Peak_degradation | Peak_degradation | Central peak degradation, 1 = freshest, 4 = most degraded. From Table 1 in Donaldson Hanna et al. 2014 (they refer to Baker et al. 2012, which was not available for the database). | N/A | obs |

Rays | Rays | Are ejecta rays observable in visual imagery or not. Combined from a number of sources, verified and appended by T. Öhman. Original sources: Elger 1895; Grier et al. 2001; McEwen et al. 1997; Morota and Furumoto 2003; C. Wood s Moon Wiki (https://the-moon.wikispaces.com/Ray+craters) | N/A | meta.code.class |

Columns that are parts of indices are marked like this.

VO nerds may sometimes need VOResource XML for this table.

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