Find research datasets worth reusing

opencc-by-4.0Feb 2024View details →

Supplementary Data for Wueller et al. (2024): Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration

Supplementary Data for Wueller et al. (2024): Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration Data contains the georeferenced map plate of our geologic map that can be used in any geoinformation system (GIS). If you use these data, please cite BOTH the Planetary Science Journal publication and the Zenodo dataset. Wueller, L., Iqbal, W., Frueh, T., van der Bogert, C. H., & Hiesinger, H. (2024). Geologic history of the Amundsen crater region near the Lunar South Pole: Basis for future exploration. The Planetary Science Journal, 5(6), 147. <a href="https://iopscience.iop.org/article/10.3847/PSJ/ad2c04">https://iopscience.iop.org/article/10.3847/PSJ/ad2c04</a> Wueller, L., Iqbal, W., Frueh, T., van der Bogert, C. H., & Hiesinger, H. (2024). Supplementary Data for Wueller et al. (2024): Geologic history of the Amundsen crater region near the Lunar South Pole: Basis for future exploration. Zenodo Dataset. <a href="https://doi.org/10.5281/zenodo.10693820" target="_blank" rel="noopener">https://doi.org/10.5281/zenodo.10693820</a> ----------------------------------------------------------------------------------------------------------------------------------------- Mapping Scale is 1:100,000 Print Scale is 1:1,000,000 ----------------------------------------------------------------------------------------------------------------------------------------- For further questions contact lwueller@uni-muenster.de Lukas Wueller, Institut für Planetologie, Universität Münster, Germany, June 2024

opencc-by-4.0Mar 2024View details →

Tycho Region Database of impact craters >=21 meters on the Moon.

This dataset presents the results of an innovative AI-driven lunar crater mapping project, focused exclusively on the Tycho region of the Moon at 21m/px (see Version V2 for the global catalog at 100m/px) , marking the first comprehensive application of artificial intelligence to detect, classify, and map lunar craters. Created through extensive work over a two-year period, this dataset leverages YOLOLens, a state-of-the-art deep learning model specifically optimized for high-resolution crater detection. YOLOLens, an innovative variant of the YOLO architecture, has been fine-tuned to handle the unique challenges of lunar surface imagery, delivering unparalleled accuracy in crater identification and localization. Detailed information on the model architecture and methodology can be found in relevant publications on: <ol> <li>La Grassa, Riccardo, et al. "YOLOLens: A deep learning model based on super-resolution to enhance the crater detection of the planetary surfaces." Remote Sensing 15.5 (2023): 1171,  https://doi.org/10.3390/rs15051171.</li> <li>La Grassa, R, et al. "LU5M812TGT: An AI-Powered global database of impact craters ≥0.4 km on the Moon", ISPRS Journal of Photogrammetry and Remote Sensing, 2025, ISSN 0924-2716, https://doi.org/10.1016/j.isprsjprs.2024.11.010. </li> </ol> The dataset preparation process involved rigorous steps in preprocessing and post-processing to enhance the quality and usability of the data. Preprocessing techniques were employed to reduce noise and enhance contrast within the complex lunar landscape, while post-processing was used to refine the accuracy of crater boundaries and dimensions detected by the model. This approach facilitated a high-confidence dataset that stands as a valuable resource for the astronomical and AI research communities. The area analyzed in this dataset is defined by the following coordinates: longitude [-21.0000000001998046, 44.9997999998701630] and latitude [-50.9998000002697722, 39.0000000003997229]. This dataset, which includes over 6.8 million craters at a resolution of 21m/px, is a valuable resource for both astrophysicists and AI researchers. It provides precisely labeled crater data, including coordinates, dimensions, and classifications, serving as an essential benchmark for comparative analyses, model validation, and advancements in lunar and planetary science. Notably, the global catalog created using the WAC imagery at 100m/px resolution is available in version V2 of this repository. This global dataset complements the Tycho region-specific data by offering a broader perspective on lunar crater distribution. *********************************************************************🌕🌖🌗🌘🌑🌒🌓🌔🌕 ********************************************************************** Release of a Tycho area at 21m/px of craters catalog  with more than 6.8 million craters. <ul> <li>File source csv</li> <li>Header: Longitude, Latitude, Diameter_w, Diameter_h, Confidence.</li> <li>The coordinates are absolute in the range of [-180, +180] of Longitude and [-90, +90] of Latitude. </li> <li>Diameters (km)</li> </ul>

Martian crater ages and crater counting - Does the impact flux of small and large asteroids varied through time on Mars, the Earth and the Moon?

<ul> <li>The SM_mars_crater_dating.xlsx table contains all the information used to date the 49 martian impact craters considered in this study (< 600 Ma). </li> </ul> <ol> <li>CRATER ID </li> <li>CRATER NAME</li> <li>DIAM KM </li> <li>LAT </li> <li>LONG </li> <li>DEPTH RIM KM </li> <li>DEPTH SURF KM </li> <li>DEPTH FLOOR KM </li> <li>NUMBER LAYER</li> <li>MORPHO EJECTA </li> <li>PRESERVATION </li> <li>COUNT AREA KM2: counting area from ejecta banket mapping </li> <li>COUNT AREA ASCI* KM2: counting area after removal of surfaces contaminated by secondary craters </li> <li>THRESHOLD AREA KM2: minimum size of Voronoi polygon area below which all associated detected craters are considered of secondary origin</li> <li>NB SEC: number of secondary craters dentified by ASCI </li> <li>PERCENT SEC</li> <li>NB CRAT 100M: total number of craters > 100 m detected by the CDA** on the CTX global mosaic*** over the counting area</li> <li>NB PRIM 100M: number of craters identified as primaries by ASCI</li> <li>TURNOFF DIAM KM: minimum crater diameter used to fit the crater-size frequency distribution (CSFD) with an isochron</li> <li>NB CRAT FIT: number of craters used to fit the CSFD with an isochron</li> <li>AGE GA: model age based on Hartmann (2005) chronology model**** and Michael et al. (2016) fitting technique*****</li> <li>AGE MAX GA</li> <li>AGE MIN GA</li> <li>N(1): equivalent number of accumulated craters >1km per km2</li> <li>N(1) MAX</li> <li>N(1) MIN</li> </ol> *ASCI: Automatic Secondary Crater Identification: A. Lagain, K. Servis, G. K. Benedix, C. Norman, S. Anderson, P. A. Bland, Model Age Derivation of Large Martian Impact Craters, Using Automatic Crater Counting Methods, Earth and Space Science 8 (2) (2021). doi:10.1029/2020EA001598. **CDA: Crater Detection Algorithm: G. K. Benedix, A. Lagain, K. Chai, S. Meka, S. Anderson, C. Norman, P. A. Bland, J. Paxman, M. C. Towner, T. Tan, Deriving Surface Ages on Mars Using Automated Crater Counting, Earth and Space Science 7 (3) (2020). doi:10.1029/2019EA001005. *** CTX global mosaic: Context Camera global mosaic: J. L. Dickson, L. A. Kerber, C. I. Fassett, B. L. Ehlmann, A Global, Blended CTX Mosaic of Mars with Vectorized Seam Mapping: A New Mosaicking Pipeline Using Principles of Non-Destructive Image Editing, in: Lunar and Planetary Science Conference (2018), p. 2480. **** W. K. Hartmann, Martian cratering 8: Isochron refinement and the chronology of Mars, Icarus 174 (2) (2005) 294–320. doi:10.1016/j.icarus.2004.11.023. ***** G. G. Michael, T. Kneissl, A. Neesemann, Planetary surface dating from crater size-frequency distribution measurements: Poisson timing analysis, Icarus 277 (2016) 279–285. doi:10.1016/j.icarus.2016.05.019. <ul> <li>The crater_counting.csv table contains the location and size of impact craters used to derive the ages of the 49 craters younger than 600 Ma old presented in this study. </li> </ul>

Unit Map and Dips/Strikes of Sakarya Vallis, Gale Crater, Mars

This dataset comprises the unit map derived from 3D analysis of Sakarya Vallis in Gale crater, Mars. The units are named Package 1–7. These packages have been extrapolated from morpho-stratigraphic analysis of a HiRISE scene in PRo3D. They have been further extrapolated using underlying image data. Included here is a shapefile representing the marker bed (Milliken et al. 2010) in Gale crater. The "CDD" refers to the Central Debris Deposit, identified by Hughes (2021). The structural data represents dip measurements along the boundaries of these packages within the feature; the "sub-package" data represent layering within the packages. For more on how dip is calculated in PRo3D, see https://pro3d.space/. Finally, the profiles mark the locations where topographic profiles were extracted for constructing cross-sections, as discussed in the thesis Persaud (2022). These data are intended to be displayed with the HiRISE ORI (https://doi.org/10.5281/zenodo.5808371) and CTX ORI mosaic (https://doi.org/10.5281/zenodo.5808357) over Sakarya Vallis, and over the basemap over the northwest of Aeolis Mons (https://doi.org/10.5281/zenodo.5808381). Format: SHP, SHX, DBF, PRJ, QPJ Projection: Equidistant cylindrical Datum: Spheroid (r = 3396.190 km) N.B. the PROJ4 format of the project is "+proj=eqc +lat_ts=0 +lat_0=0 +lon_0=0 +x_0=0 +y_0=0 +a=3396190 +b=3396190 +units=m +no_defs"

Multi-Resolution Basemap of Northwest Aeolis Mons, Gale Crater, Mars

This multi-resolution, multi-spectral basemap comprises HiRISE, CTX, MOC-NA, and CRISM imagery over the northwest of Aeolis Mons in Gale crater, Mars, to complement the HiRISE and CTX data over Sakarya Vallis (Persaud 2021, https://doi.org/10.5281/zenodo.5808371; Persaud et al. 2021, https://doi.org/10.5281/zenodo.5808357). All of the products have been georeferenced to the CTX ORI mosaic (Persaud et al. 2021) and/or each other using QGIS and GDAL; their IDs, resolutions, and sources prior to this alignment are listed below. The greyimage ORIs produced in this work were generated using the Ames Stereo Pipeline. The other HiRISE ORI were selected based on the data used by the USGS to make the MSL orthophoto mosaic (Calef III and Parker 2016, https://astrogeology.usgs.gov/search/map/Mars/MarsScienceLaboratory/Mosaics/MSL_Gale_Orthophoto_Mosaic_10m_v3). The four CRISM images were processed using the CRISM Analysis Tool (CAT) in ENVI (Morgan et al. 2009) following the workflow described in Campbell and Muller (2017), adapted from Seelos (2009). Four RGB products were assembled from one CRISM image over Sakarya Vallis using the spectral library from Viviano-Beck et al. (2014); the band assignments are listed below. Format: GeoTiff Projection: Equidistant cylindrical Datum: Spheroid (r = 3396.190 km) HiRISE (0.25 m/px) <ul> <li>ESP_012340_1750_RED, this work</li> <li>PSP_009149_1750_RED, this work</li> <li>ESP_018854_1755_RED, this work</li> <li>ESP_019698_1750_RED, U. Arizona</li> <li>ESP_012551_1750_RED, U. Arizona</li> <li>ESP_024300_1755_RED, U. Arizona</li> <li>PSP_001488_1750_RED, U. Arizona</li> <li>PSP_009650_1755_RED, U. Arizona</li> </ul> HiRISE RGB (0.50 m/px): <ul> <li>ESP_061750_1750_RGB, U. Arizona (mosaicked in this work, "Mont Mercou")</li> <li>ESP_069031_1750_MRGB, U. Arizona (mosaicked in this work, "Mont Mercou")</li> <li>PSP_009149_1750_MRGB, U. Arizona (mosaicked in this work, "Mont Mercou")</li> <li>ESP_029034_1750_MRGB, U. Arizona</li> </ul> MOC-NA (NASA/JPL/MSSS): <ul> <li>S2200845 (2.2 m/px)</li> <li>R1100953 (6.75 m/px)</li> </ul> CRISM, FRT000095ee (18 m/px): <ul> <li>Hydrated mineralogy <ul> <li>Red: SINDEX2</li> <li>Green: BD2100_2</li> <li>Blue: BD1900_2</li> </ul> </li> <li>Hydrated sulphates (1) <ul> <li>Red: SINDEX2</li> <li>Green: BD1900R2</li> <li>Blue: HCPINDEX3</li> </ul> </li> <li>Mafics <ul> <li>Red: LCPINDEX3</li> <li>Green: HCPINDEX3</li> <li>Blue: OLINDEX3</li> </ul> </li> <li>Hydrated sulphates (2): SINDEX2</li> </ul>

Co-registered U. Arizona HiRISE DTM and ORI over Sakarya Vallis, Gale Crater, Mars

Local digital terrain model (DTM) and orthorectified image (ORI) of Sakarya Vallis, west of Aeolis Mons in Gale crater, Mars. The DTM was originally processed by the University of Arizona (DTEEC_006855_1750_007501_1750_A01, https://www.uahirise.org/dtm/dtm.php?ID=PSP_006855_1750); this product is co-registered to CTX DTMs which were themselves co-registered to HRSC DTMs (Persaud et al. 2021, https://doi.org/10.5281/zenodo.5808357) using Ames Stereo Pipeline. The ORI was processed using Ames Stereo Pipeline and adjusted with GDAL. Format: GeoTiff Projection: Equidistant cylindrical Datum: Spheroid (r = 3396.190 km) Bit depth: Float32 DTM grid-spacing: 1 m/pixel ORI resolution: 0.25 m/pixel Stereo pairs (from University of Arizona): PSP_006855_1750_RED, PSP_007501_1750_RED <ul> </ul> Image ID of the ORI: PSP_007501_1750_RED

CTX DTM and ORI Mosaics over Sakarya Vallis, Gale Crater, Mars

Local digital terrain model (DTM) and orthorectified image (ORI) mosaics over Sakarya Vallis, west of Aeolis Mons in Gale crater, Mars. The two constituent DTMs were processed using the CASP-GO suite described in Tao et al. (2018); the ORIs were processed using Ames Stereo Pipeline. The DTMs were then co-registered to an HRSC DTM mosaic (Persaud et al. 2021, https://doi.org/10.5281/zenodo.5808354) and each other using Ames Stereo Pipeline, and then cropped and mosaicked. Format: GeoTiff Projection: Equidistant cylindrical Datum: Spheroid (r = 3396.190 km) Bit depth: Float32 DTM grid-spacing: 18 m/pixel ORI resolution: 6 m/pixel Stereo pairs (from Grindrod and Davis, 2018): <ul> <li>P04_002675_1746_XI_05S222W, B21_017786_1746_XN_05S222W</li> <li>D02_027834_1748_XN_05S222W, G04_019698_1747_XI_05S222W</li> </ul> Image IDs of the ORIs: P04_002675_1746_XI_05S222W, D02_027834_1748_XN_05S222W

30-m HRSC DTM Mosaic of Gale Crater, Mars

Digital terrain model (DTM) mosaic of Gale crater, Mars, processed from High-Resolution Stereo Camera (HRSC) stereo images using the modification of DLR-VICAR described by Kim and Muller (2009). Format: GeoTiff Projection: Equidistant cylindrical Datum: Spheroid (r = 3396.190 km) Bit depth: Float32 Grid-spacing: 30 m/pixel Terrain reference: 200-m MOLA and HRSC blended global DTM (Fergason et al. 2018) HRSC source images: H1938_0000, H1927_0000, and H1916_0000

opencc-by-4.0Sep 2024View details →

Images and Crater Data for "Crater Detection Dependence on Resolution, Incidence Angle, Emission Angle, and Phase Angle"

Images are from the LROC-NAC and have been cartographically controlled to each other and the Apollo 11 landing site as described in Supporting Information Text S1.  Images are cropped so that the cover ±0.025° from the landing site when coordinates have three significant figures.  The images are provided as .png files with .pgw ("PNG World").  The images are at 1 mpp (contain a "1mpp" string in the file name), 2.5 mpp (contain a 2p5mpp" string in the file name), and 6.25 mpp (contain a "6p25mpp" string in the file name).  Additionally, the three e > 10° images are included as unprojected .cub files; these files omit the "l2" (map projected, Level-2 data) string and any "l4" (mosaicked) string from the file name, but they instead include "trim" to indicate the image has been trimmed from its full extent to the area of interest. Crater data are formatted as .csv (comma-separated values) files and are one file per image per researcher.  File names have the exact same name as the image file that was used to map crater data, with two differences:  The initials of the author are appended, and the file extension is "csv" instead of "png".  The files do not have headers, but they are formatted such that the first column is latitude (decimal degrees north), second column is longitude (decimal degrees east), and diameter (kilometers).  Crater data are entirely in one .zip file.

opencc-by-4.0Jun 2020View details →

Depths of Pluto's and Charon's Impact Craters

Tab-Separated Values (TSV) files of crater depth data for Pluto and Charon, as published in supplemental material for the publication, "Depths of Pluto’s and Charon’s craters, and their simple-to-complex transition," by S.J. Robbins et al. (2020), doi: 10.1016/j.icarus.2020.113902).  The first row in both files describes what is contained in that column.  Calculations were carried out to machine's precision and are not reliable past about 2–3 significant figures.

opencc-by-4.0Apr 2020View details →

Morpho-stratigraphic map of Jezero crater landing area

The rover Perseverance of the Mars2020 mission will depart to Mars in July 2020 and land on Mars in February 2021. Its landing site, Jezero crater, has been selected due to the presence of two fan deltas, inlet and outlet valleys and a huge number of aqueous landforms (fluvial and lacustrine sediments). This morpho-stratigraphic map has been produced from orbital visible imagery and its interpretations take into account the orbital facies (layers, massive, etc.) and their stratigraphic relationships, the texture and albedo of terrains, without taking into account mineralogical data. The area studied here is centered around the landing area comprising the east of the fan delta and the west of the crater floor. The map has been done at 1:10,000 scale.

opencc-by-4.0Sep 2023View details →

Updated database of craters on Mars with pitted impact deposits

This point-based database (provided in two formats: as a ESRI shapefile set and simple .csv) currently contains 309 craters on Mars that possess “crater-related pitted materials” (CRPM), which are consistent with impact deposits described in detail in Tornabene et al. (2007; 2012). The Tornabene et al. (2012) publication is the original source of the initial database of 204 craters, which was based on a survey by the Mars Reconnaissance Orbiter (MRO) over a period of late 2006 to early 2012. MRO continues to image the surface and its craters, as such the database has since grown from 204 to 309 entries to date. Despite this growth, the general characteristics of the crater population remains generally consistent with what is described in Tornabene et al. (2012) (e.g., size range, latitudinal and elevation distribution, etc.). When present, these pitted impact deposits represent the upper most surface of the crater-fill with the pits potentially representing top-down views of so-called degassing pipes observed only in eroded cross-sections at some terrestrial impact structures such as the Ries in Germany (e.g., Caudill et al., 2021). Therefore, the craters that contain pits and preserve them well are themselves amongst the very best-preserved and often youngest craters of their size-class on Mars. Indeed, some of these craters are observed to have far-reaching (10s to 100s of crater radii) thermal / secondary crater rays (e.g., Tornabene et al. 2006), which is considered to be a feature associated with only the best-preserved and youthful craters on planets/moons with solid surfaces. These craters have enabled us to place further constraints on the scaling of crater depth as a function of diameter for complex craters on Mars (Tornabene et al. 2018) and may even help us to ultimately determine where the only samples we have of Mars — the Martain Meteorites — come from. See README rtf file for further details on the database.   Versions 8.21.2025: 4th version - deleted 3 additional duplicates (Lunae, Oudemans and Toro) total entries is now 309 8.20.2025b: 3rd version upload - fixed 1 duplicate (312 entries), caught some additional updates with respect to new official crater names, and CTX image IDs. 8.20.2025: 2nd version with an increase to 313 entries with some updates to preservation ratings, image IDs, etc. 5.3.2023: 1st version uploaded with 300 entries   Main references (*original/source  database): *Tornabene, L.L., Osinski, G.R., McEwen, A.S., Boyce, J.M., Bray, V.J., Caudill, C.M., Grant, J.A., Hamilton, C.W., Mattson, S. and Mouginis-Mark, P.J., 2012. Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process. Icarus, 220(2), pp.348-368. https://doi.org/10.1016/j.icarus.2012.05.022 Tornabene, L.L., McEwen, A.S., Osinski, G.R., Mouginis-Mark, P.J., Boyce, J.M., Williams, R.M.E., Wray, J.J. and Grant, J.A., 2007. Impact melting and the role of subsurface volatiles: Implications for the formation of valley networks and phyllosilicate-rich lithologies on early Mars. In International Conf. on Mars VII. Lunar Planet. Sci. Inst. Contri (Vol. 1353), Abstract# 3288. Other references: Tornabene, L.L., Moersch, J.E., McSween Jr, H.Y., McEwen, A.S., Piatek, J.L., Milam, K.A. and Christensen, P.R., 2006. Identification of large (2–10 km) rayed craters on Mars in THEMIS thermal infrared images: Implications for possible Martian meteorite source regions. Journal of Geophysical Research: Planets, 111(E10). Boyce, J.M., Wilson, L., Mouginis-Mark, P.J., Hamilton, C.W. and Tornabene, L.L., 2012. Origin of small pits in martian impact craters. Icarus, 221(1), pp.262-275. Denevi, B.W., Blewett, D.T., Buczkowski, D.L., Capaccioni, F., Capria, M.T., De Sanctis, M.C., Garry, W.B., Gaskell, R.W., Le Corre, L., Li, J.Y. and Marchi, S., 2012. Pitted terrain on Vesta and implications for the presence of volatiles. Science, 338(6104), pp.246-249. Sizemore, H.G., Platz, T., Schorghofer, N., Prettyman, T.H., De Sanctis, M.C., Crown, D.A., Schmedemann, N., Neesemann, A., Kneissl, T., Marchi, S. and Schenk, P.M., 2017. Pitted terrains on (1) Ceres and implications for shallow subsurface volatile distribution. Geophysical Research Letters, 44(13), pp.6570-6578. Tornabene, L.L., Watters, W.A., Osinski, G.R., Boyce, J.M., Harrison, T.N., Ling, V. and McEwen, A.S., 2018. A depth versus diameter scaling relationship for the best-preserved melt-bearing complex craters on Mars. Icarus, 299, pp.68-83. Caudill, C., Osinski, G.R., Greenberger, R.N., Tornabene, L.L., Longstaffe, F.J., Flemming, R.L. and Ehlmann, B.L., 2021. Origin of the degassing pipes at the Ries impact structure and implications for impact‐induced alteration on Mars and other planetary bodies. Meteoritics & Planetary Science, 56(2), pp.404-422. Michalik, T., Matz, K.D., Schröder, S.E., Jaumann, R., Stephan, K., Krohn, K., Preusker, F., Raymond, C.A., Russell, C.T. and Otto, K.A., 2021. The unique spectral and geomorphological characteristics of pitted impact deposits associated with Marcia crater on Vesta. Icarus, 369, p.114633.

opencc-by-4.0Dec 2023View details →

Spectral Units for Tsiolkovskiy crater (Moon, Far side)

Spectral Units derived from the Moon Mineralogy Mapper (M3) data for the lunar far side Tsiolkovskiy crater.

opencc-by-4.0Feb 2024View details →

Data for "Multi-band Spectropolarimetric Image Data of Lunar Maria, Pyroclastics, Fresh Craters, and Swirl Materials"

This data repository contains the georeferenced spectropolarimetric data analyzed in the following article: Wöhler, C., Arnaut, M., Bhatt, M., 2024. Multi-band Spectropolarimetry of Lunar Maria, Pyroclastics, Fresh Craters, and Swirl Material. Astronomical Journal, accepted for publication. The data products are available in separate .zip archives in GEOTIFF and BSQ format. Each .zip archive contains data from eight different observations: <table> <tbody> <tr> <td>Dataset</td> <td>Date</td> <td>UT time</td> <td>Phase angle</td> </tr> <tr> <td>20221114_WOP</td> <td>Nov 14th, 2022</td> <td>05:20</td> <td>64°</td> </tr> <tr> <td>20221216_WOP</td> <td>Dec 16th, 2022</td> <td>04:10</td> <td>88°</td> </tr> <tr> <td>20230225_AT</td> <td>Feb 25th, 2023</td> <td>19:20</td> <td>108°</td> </tr> <tr> <td>20230227_AT</td> <td>Feb 27th, 2023</td> <td>21:44</td> <td>85°</td> </tr> <tr> <td>20230228_AT</td> <td>Feb 28th, 2023</td> <td>19:33</td> <td>74°</td> </tr> <tr> <td>20230302_MV</td> <td>Mar 2nd, 2023</td> <td>19:03</td> <td>52°</td> </tr> <tr> <td>20230302_AT</td> <td>Mar 2nd, 2023</td> <td>19:10</td> <td>52°</td> </tr> <tr> <td>20230402_AT</td> <td>Apr 2nd, 2023</td> <td>20:03</td> <td>38°</td> </tr> </tbody> </table>   Data products of spectropolarimetric image analysis in GEOTIFF and BSQ format ============================================================================= Prefix 1: Date of data acquisition (YYYYMMDD) Prefix 2: Area (WOP: Western Oceanus Procellarum; MV: Mare Vaporum; AT: Atlas) F    : image intensity (5 bands) [DN] P    : degree of linear polarization (DoLP) (5 bands) W    : angle of linear polarization (AoLP) (5 bands) [degrees] GS   : relative grain size (5 bands) logGS: logarithm of relative grain size (5 bands) UE   : across-band Umov exponent (1 band) UEres: residual of across-band Umov exponent (1 band) PCAP : scores on the first three principal components derived from the DoLP (3 bands)  PCAW : scores on the first three principal components derived from the AoLP (3 bands) CIM  : cluster index map (1 band) The longitude ranges of the maps are as follows: WOP: Longitude=[-70 -35], Latitude=[2 33] MV : Longitude=[-13 12], Latitude=[-2 17] AT : Longitude=[35 60], Latitude=[40 55] All maps are in simple cylindrical projection with a resolution of 30 pixels per degree. The CIM maps are provided in uint8 numerical format. All other maps are provided in single-precision (32-bit) floating point numerical format. The BSQ files are in binary format without header. Matlab example: BSQ=multibandread('20230302_AT_P__Latitude_35_60__Latitude_35_60.bsq',[750 750 5],'single',0,'bsq','ieee-le');

opencc-by-4.0Nov 2024View details →

Air/Snow temperature vertical profiles at different nodes of the 'Crater Lake' CALM site in Deception Island, Antarctica (2012-2023)

Air or seasonal snow temperature data were collected at different heights above the ground between 2012 and 2023 using an array of temperature micro-loggers (iButton models by Maxim) mounted on vertical wooden masts. These measurements were conducted at various nodes within the 100x100 m 'Crater Lake' CALM site (A16) grid of the PERMATHERMAL network, managed by the University of Alcalá, Madrid, Spain, to monitor active layer thickness in Deception Island, South Shetland Islands, Antarctica. In 2012, nine arrays were installed at nodes with relative coordinates (00,00), (00,05), (00,10), (05,00), (05,05), (05,10), (10,00), (10,05), and (10,10). Measurements were taken at heights of 2.5, 5, 10, 15, 20, 25, 30, and 40 cm above the ground surface using DS1921G iButton loggers, which recorded air/snow temperatures every 4 hours. This experiment, referred to as 'Mini', was active until early 2021. Between 2017 and 2023, four arrays were installed at nodes (00,010), (05,05), (06,00), and (10,00). These arrays measured air/snow temperatures at heights of 2.5, 5, 10, 20, 30, 40, 50, 60, 70, 80, 90, 100, 120, 140, and 160 cm above the ground surface using DS1922L iButton loggers, which recorded temperatures every 3 hours. Three of the arrays of this experiment, referred to as 'HR', has also been discontinued in early 2021, althought one of them was active until early 2024.

opencc-by-4.0Mar 2022View details →

Supplemental data from: "From lake to river: Documenting an environmental transition across the Jura/Knockfarril Hill members boundary in the Glen Torridon region of Gale crater (Mars)."

This document, uploaded on the FAIR repository Zenodo, contains large data tables pertaining to the Supplementary Online Material of the above-mentioned article. These tables contain the complete list of individual MAHLI and ChemCam targets investigated, detailed laminae measurements and complete ChemCam compositional data.

opencc-by-4.0Mar 2022View details →

Supporting Material for "Automatic Mapping of Small Lunar Impact Craters Using LROC NAC Images"

The supporting material for 'Automatic Mapping of Small Lunar Impact Craters Using LROC NAC'. This File contains: <ul> <li>Supporting Material (.pdf);</li> <li>List of True Positive detections (.csv);</li> <li>List of all ground truth and CDA detections (.csv);</li> <li>Folder (.zip) with images of the evaluation sites (.pdf); and</li> <li>Folder (.zip) with training image tiles (.png and .txt).</li> </ul> Refer to Supporting Material (.pdf) for file name and header information.

opencc-by-4.0May 2020View details →

Data accompanying: Impacts into a porous graphite: an investigation on crater formation and ejecta distribution

Reconstructed X-ray tomographies and python analysis scripts for the publication "Impacts into a porous graphite:  an investigation on crater formation and ejecta distribution"   Uses the spam python toolkit, which can probably be replaced by scipy.ndimage.center_of_mass if needed.