This table is available for ADQL queries and through the TAP endpoint.
Resource Description:
For a list of all services and tables belonging 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 alphabetically. [Sort by DB column index]
Name | Table Head | Description | Unit | UCD |
---|---|---|---|---|
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 |
Age_other_sources | Age_other_sources | Age - other sources | N/A | meta.bib |
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 |
Apparent_depth | Apparent_depth | Apparent depth [km], measured at the pre-impact surface level, according to Pike (1977b). | km | phys.size |
Apparent_diameter | Apparent_diameter | Apparent diameter [km], measured at the pre-impact surface level, according to Pike (1977b). | km | phys.size.diameter |
Approval | Approval | Approval year or date in the official IAU-USGS database (Gazetteer of Planetary Nomenclature) | N/A | time |
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 |
Basin_age_group | Basin_age_group | Basin age group (higher number - younger) (Wilhelms, 1987) | N/A | meta.code.class |
bib_reference | Bib_reference | Bibcode preferred if available (does that include link?), doi, or other biblio id, URL | N/A | meta.bib |
c1_resol_max | C1_resol_max | Resolution in the first coordinate, upper limit | deg | pos.resolution;stat.max |
c1_resol_min | C1_resol_min | Resolution in the first coordinate, lower limit. | deg | pos.resolution;stat.min |
c1max | C1max | Longitude on body, upper limit | deg | pos.bodyrc.long;stat.max |
c1min | C1min | Longitude on body, lower limit. | deg | pos.bodyrc.long;stat.min |
c2_resol_max | C2_resol_max | Resolution in the second 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 |
c2max | C2max | Latitude on body, upper limit | deg | pos.bodyrc.lat;stat.max |
c2min | C2min | Latitude on body, lower limit. | deg | pos.bodyrc.lat;stat.min |
c3_resol_max | C3_resol_max | Resolution in the third coordinate, upper limit | m | pos.resolution;stat.max |
c3_resol_min | C3_resol_min | Resolution in the third coordinate, lower limit. | m | pos.resolution;stat.min |
c3max | C3max | Height over defined null, upper limit | m | pos.bodyrc.alt;stat.max |
c3min | C3min | Height over defined null, lower limit. | m | pos.bodyrc.alt;stat.min |
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 |
creation_date | Creation_date | Date of first entry of this granule | N/A | time.creation |
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 |
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 |
Diameter | Diameter | Diameter of the crater | km | phys.size.diameter |
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 |
emergence_max | Emergence_max | Emergence 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 |
feature_name | Feature_name | Secondary name (can be standard name of region of interest). | N/A | meta.id;pos |
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 |
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 |
granule_uid | Granule_uid | Internal table row index Unique ID in data service, also in v2. Can be alphanumeric. | N/A | meta.id |
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 |
incidence_max | Incidence_max | Incidence angle (solar zenithal angle) during data acquisition, upper limit | deg | pos.posAng;stat.max |
incidence_min | Incidence_min | Incidence angle (solar zenithal angle) during data acquisition, lower limit. | deg | pos.posAng;stat.min |
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 |
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 |
Longitude | Longitude | Longitude of the crater from -180 to 180 eastward | deg | pos.bodyrc.lon |
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 |
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 |
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 |
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 |
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 |
measurement_type | Measurement_type | UCD(s) defining the data, with multiple entries separated by hash (#) characters. | N/A | meta.ucd |
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_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 |
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 |
modification_date | Modification_date | Date of last modification (used to handle mirroring) | N/A | time.update |
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 |
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 |
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 |
phase_max | Phase_max | Phase angle during data acquisition, upper limit | deg | pos.phaseAng;stat.max |
phase_min | Phase_min | Phase angle during data acquisition, lower limit. | deg | pos.phaseAng;stat.min |
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 |
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 |
publisher | Publisher | A short string identifying the entity running the data service used. | N/A | meta.ref |
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_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_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_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 |
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 |
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 |
release_date | Release_date | Start of public access period | N/A | time.release |
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 |
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 |
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_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 |
s_region | S_region | ObsCore-like footprint, valid for celestial, spherical, or body-fixed frames. | N/A | phys.outline;obs.field |
service_title | Service_title | Title of resource (an acronym really, will be used to handle multiservice results) | N/A | meta.title |
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 |
spectral_range_max | Spectral_range_max | Spectral range (frequency), upper limit | Hz | em.freq;stat.max |
spectral_range_min | Spectral_range_min | Spectral range (frequency), lower limit. | Hz | em.freq;stat.min |
spectral_resolution_max | Spectral_resolution_max | Sectral resolution, upper limit | Hz | spect.resolution;stat.max |
spectral_resolution_min | Spectral_resolution_min | Sectral resolution, lower limit. | Hz | spect.resolution;stat.min |
spectral_sampling_step_max | Spectral_sampling_step_max | spectral sampling step, upper limit | Hz | em.freq.step;stat.max |
spectral_sampling_step_min | Spectral_sampling_step_min | spectral sampling step, lower limit. | Hz | em.freq.step;stat.min |
target_class | Target_class | Type of target, from enumerated list | N/A | meta.code.class;src |
target_name | Target_name | Standard IAU name of target (from a list related to target class), case sensitive | N/A | meta.id;src |
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 |
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_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_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_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_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_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 |
time_exp_max | Time_exp_max | Integration time of the measurement, upper limit | s | time.duration;obs.exposure;stat.max |
time_exp_min | Time_exp_min | Integration time of the measurement, lower limit. | s | time.duration;obs.exposure;stat.min |
time_max | Time_max | Acquisition stop time (in JD) | d | time.end |
time_min | Time_min | Acquisition start time (in JD) | d | time.start |
time_sampling_step_max | Time_sampling_step_max | Sampling time for measurements of dynamical phenomena, upper limit | s | time.interval;stat.max |
time_sampling_step_min | Time_sampling_step_min | Sampling time for measurements of dynamical phenomena, lower limit. | s | time.interval;stat.min |
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 |
Columns that are parts of indices are marked like this.
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