Find research datasets worth reusing
Search datasets from major research repositories and use ShareScore to quickly assess how well each record supports discovery, access, and reuse.
1,880
datasets available to search
ShareScore release 0.9.0
Dataset results
1,880 results for “MAR”
DoMars16k: A Diverse Dataset for Weakly Supervised Geomorphologic Analysis on Mars
<p>The dataset contains 16150 samples extracted from 163 CTX images. Each sample depicts one of fifteen Martian surface landforms. One CTX image contributed with at least three and at most 1247 patches to the creation of the dataset. The dataset is subdivided into training, test, and validation sets, which contain seventy, ten, and twenty percent of the samples. The sets are mutually exclusive. Each sample has a size of 200 x 200 px or roughly 1.2km x 1.2km.</p> <p><strong>Contents</strong></p> <ul> <li>data.zip contains the dataset separated into training, validation, and test sets. </li> <li>models.zip contains pre-trained neural networks.</li> </ul> <p><strong>Classes</strong></p> <ul> <li><strong>Aeolian Bedforms</strong> <ul> <li>Aeolian Curved (ael)</li> <li>Aeolian Straight (aec)</li> </ul> </li> <li><strong>Topographic Landforms</strong> <ul> <li>Cliff (cli)</li> <li>Ridge (rid)</li> <li>Channel (fsf)</li> <li>Mounds (sfe)</li> </ul> </li> <li><strong>Slope Feature Landforms</strong> <ul> <li>Gullies (fsg)</li> <li>Slope Streaks (fse)</li> <li>Mass Wasting (fss)</li> </ul> </li> <li><strong>Impact Landforms</strong> <ul> <li>Crater (cra)</li> <li>Crater Field (sfx)</li> </ul> </li> <li><strong>Basic Terrain Landforms</strong> <ul> <li>Mixed Terrain (mix)</li> <li>Rough Terrain (rou)</li> <li>Smooth Terrain (smo)</li> <li>Textured Terrain (tex)</li> </ul> </li> </ul> <p><strong>Code</strong></p> <p>Python code to train, evaluate, and apply deep neural networks to Martian surface data is available at GitHub: <a href="https://github.com/thowilh/geomars">https://github.com/thowilh/geomars</a></p> <p><strong>Attribution</strong></p> <p>If you find this work useful please consider citing:</p> <p>Wilhelm, T.; Geis, M.; Püttschneider, J.; Sievernich, T.; Weber, T.; Wohlfarth, K.; Wöhler, C. DoMars16k: A Diverse Dataset for Weakly Supervised Geomorphologic Analysis on Mars. Remote Sens. 2020, 12, 3981.</p> <pre><code>@article{wilhelm2020domars16k, doi = {10.3390/rs12233981}, url = {https://doi.org/10.3390/rs12233981}, year = {2020}, month = dec, publisher = {{MDPI} {AG}}, volume = {12}, number = {23}, pages = {3981}, author = {Thorsten Wilhelm and Melina Geis and Jens P\"{u}ttschneider and Timo Sievernich and Tobias Weber and Kay Wohlfarth and Christian W\"{o}hler}, title = {{DoMars}16k: A Diverse Dataset for Weakly Supervised Geomorphologic Analysis on Mars}, journal = {Remote Sensing} }</code></pre> <p> </p>
Electron density and altitude of the main ionospheric peak of Mars as observed by Mars Express instruments. Archived data for the paper "Seasonal and geographical variability of the Martian ionosphere from Mars Express observations", submitted to JGR-Planets
<p>This repository contains archived data for the manuscript "Seasonal and geographical variability of the Martian ionosphere from Mars Express observations", published in Journal of Geophysical Research-Planets. Details about the methods to generate the data can be found in the paper.</p> <p>5 data files plus 2 readme text files are included.</p> <p>The file MEx_ionpeak.dat (described in the readme file README_ionpeak.txt) contains the peak electron densities and peak altitudes resulting from 34539 observations. Each record includes 14 columns. The content of each column is:</p> <p>Column 1: Instrument providing the observation (MARSIS or MaRS)<br> Column 2: Mars Year at which the observation was obtained (from MY27 to MY33)<br> Column 3: Solar Longitude (Ls) of the observation (unit: degrees)<br> Column 4: Latitude of the observation (unit: degrees)<br> Column 5: Longitude of the observation (unit: degrees)<br> Column 6: Solar Zenith Angle (SZA) of the observation (unit: degrees)<br> Column 7: F10.7 solar proxy index at 1 Astronomic Unit (unit: solar flux units)<br> Column 8: Peak electron density measured by the instrument (unit: cm-3)<br> Column 9: Peak electron density at the subsolar point, i.e., corrected for the SZA variation (unit: cm-3)<br> Column 10: Peak electron density at the subsolar point and at F10.7 (1AU)=100, i.e., corrected for the SZA and the solar radiation output variations (unit: cm-3)<br> Column 11: Peak electron density at the subsolar point, at F10.7 (1AU)=100 and corrected for the seasonal variation (unit: cm-3)<br> Column 12: Peak altitude measured by the instrument (unit: km)<br> Column 13: Peak altitude at the subsolar point, i.e. corrected for the SZA variation (unit: km)<br> Column 14: Peak altitude at the subsolar point and corrected for the seasonal variation (unit: km)</p> <p> </p> <p>The files eprofiles_MaRS.dat, eprofiles_MARSIS_prof1.dat, eprofiles_MARSIS_prof2.dat and eprofiles_MARSIS_prof3.dat contain 4 electron density profiles. They are described in the file README_eprofiles.txt. Each file includes 2 columns, the first one being the altitude (unit: km) and the second one the electron density (unit: cm-3).</p> <p> </p> <p>Contact: Francisco Gonzalez-Galindo, ggalindo@iaa.es<br> </p>
Repository: The Distribution of Frosts on Mars: Links to Present-Day Gully Activity
<p>This repository contains:</p> <p>1. Global calculated CO2 frost point temperatures (Kelvin) calculated at 1 ppd every 10 Ls using surface pressure from the online version of the Mars Climate Database<br> (http://www-mars.lmd.jussieu.fr/mcd_python/)<br> CO2 Frost Points</p> <p><br> 2. Local Solar Time and Season of THEMIS CO2 Frost Detections at gully locations<br> corr_gully_detections_filenames_meta</p> <p>3. Calculated CO2 frost amounts (kg/m^2) at 30S, 40S, 50S and 60S on pole-facing slopes<br> Frost Amounts</p> <p>4. Calculated CO2 frost amounts (kg/m^2) varying with lower material thermal inertia, slope azimuth, top material thermal inertia, top material thickness and surface albedo<br> Frost Sensitivity</p> <p>5. Predicted H2O frost lifetimes (hours)<br> H2OFrost_Stability</p> <p>6. Global THEMIS CO2 Frost Detections from Mars Year (MY) 26<br> MY26_THEMIS_CO2_Frost_Detections</p> <p>7. THEMIS CO2 Frost Detections at gully locations (Harrison et al. 2015) from MYs 26 - 35<br> MY26_35_THEMIS_GULLY_CO2_Frost_Detections</p> <p>8. H2O frost temperatures (Kelvin) at the Opportunity rover site<br> Opportunity_H2OFrost</p> <p>9. CO2 Frost detections made by Piqueux et al. (2016) using Mars Climate Sounder data<br> Piqueux et al (2016) MCS CO2 Frost Detections</p> <p>10. TES-derived data<br> a) TES_MY26_H2OFrost_Temp_Map<br> b) TES_MY26_H2OFrost_Temp_Seasonal</p> <p>11. The seasonal variation of the CO2 frost point (Kelvin) at the Viking Lander sites<br> Viking_Lander_Data</p>
Kittel et al. (2021), The Cryosphere : MAR and ESMs data
<p>Outputs used in:</p> <p><em>Kittel, C., Amory, C., Agosta, C., Jourdain, N. C., Hofer, S., Delhasse, A., Doutreloup, S., Huot, P.-V., Lang, C., Fichefet, T., and Fettweis, X.: Diverging future surface mass balance between the Antarctic ice shelves and grounded ice sheet, The Cryosphere https://doi.org/10.5194/tc-2020-291,2021.</em></p> <ul> <li>MAR outputs with yearly values of SMB and components over the Antarctic ice sheet (1980--2100)</li> <li>Grid file used in MAR simulations</li> <li>ESM and GCM yearly near-surface temperature over 1960--2100 (as downloaded from the ESGF nodes)</li> </ul> <p><br> Associated daily datasets:<br> MAR(ACCESS1.3): 10.5281/zenodo.4525735<br> MAR(NorESM1-M): 10.5281/zenodo.4528998<br> MAR(CESM2): 10.5281/zenodo.4529002<br> MAR(CNRM-CM6-1): 10.5281/zenodo.4529004<br> <br> <br> If you need other variables or output frequencies from MAR, write me (c2kittel@gmail.com) and I will be glad to help you. I will also be happy to share the scripts I have developed to analyse the outputs and make the figures in this paper if needed. Please cite the paper if you use these MAR outputs.<br> <br> Data usage notice:</p> <p>If you use any of these results, please acknowledge the work of the people involved in producing them. Acknowledgements should have language similar to the below that contained both informations related to MAR and CMIP5/6. In order to document MAR scientific impact and enable ongoing support of the model, users are likely encouraged to contact C. Kittel to add their works in the list of MAR-related publications. </p> <p>"We thank C. Kittel and the MAR team which make available the model outputs, as well agencies (F.R.S - FNRS, CÉCI, and the Walloon Region) that provided computational resources for MAR simulations. We acknowledge the World Climate Research Programme, which, through it's Working Group on Coupled Modelling, coordinated and promoted CMIP5 and CMIP6. We thank the climate modeling groups for producing and making available their model output, the Earth System Grid Federation (ESGF) for archiving the CMIP data and providing access, and the multiple funding agencies who support CMIP5 and CMIP6 and ESGF. "</p> <p>You should also refer to and cite the following paper:</p> <p>Kittel, C., Amory, C., Agosta, C., Jourdain, N. C., Hofer, S., Delhasse, A., Doutreloup, S., Huot, P.-V., Lang, C., Fichefet, T., and Fettweis, X.: Diverging future surface mass balance between the Antarctic ice shelves and grounded ice sheet, The Cryosphere Discuss. [preprint], https://doi.org/10.5194/tc-2020-291, accepted, 2020.</p>
Chemistry of the Surface of Mars
<p>Concentration of 11 major elements at the surface of Mars (SiO2, TiO2, Al2O3, FeO,MnO,MgO, CaO, Na2O, K2O, P2O5 and Cr23O3) following the approach presented in the following article :</p> <p>Baratoux, D., H. Samuel, C. Michaut, M. J. Toplis, M. Monnereau,<br /> M. Wieczorek, R. Garcia, and<br /> K. Kurita (2014), Petrological constraints on the density of the Martian crust, <em>J. Geophys. Res. Planets, 119, </em>1707-1727, doi:10.1002/2014JE004642. </p>
Retrograde Motion of Mars
<p>Winner in the 2023 IAU OAE Astrophotography Contest, category Still images with smartphones-mobile devices: Retrograde Motion of Mars, by Rob Kerby Guevarra.</p> <p>This image captures the celestial waltz of Mars as it demonstrates its intriguing retrograde motion against the background of fixed stars. This event, when Mars appears to backtrack in its orbit, arises from the different speeds at which Earth and Mars orbit the Sun. Earth’s faster movement occasionally positions it ahead of Mars, creating the illusion of the Red Planet moving in reverse from our perspective. This retrograde motion occurs when Mars is on the other side of the sky from the Sun, when it is said to be in opposition. Following Mars from 14 August 2022 to 5 April 2023, this smartphone image stands as a testament to perseverance and precision in the tranquil setting of Bataan, Philippines. Enduring unpredictable weather and ever-shifting celestial alignments, the photographer meticulously captured each shot at regular intervals of five to eight days. The process involved aligning 35 distinct images of Mars, taken without any external lens or telescope, alongside a stacked background image composed of 54 frames lasting 15 seconds each, portraying the starry expanse. Fusing these images involved precisely aligning them and cropping Mars in order to centre its position, revealing its retrograde movement against the backdrop of stars. This intricate process, blending the images seamlessly into the background by masking, highlights the planet’s unique motion. In the lower right corner, the Pleiades star cluster is visible.</p> <p>Credit: Rob Kerby Guevarra/IAU OAE (<a href="https://creativecommons.org/licenses/by/4.0/legalcode">CC BY 4.0</a>)</p>
Characterization and morphometry of prone and affected watersheds by hydro-geomorphological processes in the Serra do Mar Mountain Range, southeastern Brazil: foundation for planning and mitigation actions.
<p>Data: shapefile, tables, and kmz files. </p> <ol> <li>SHAPEFILES</li> </ol> <p>- Dataset with watersheds mapped in the Serra do Mar Paulista Region in the follow cities:</p> <ul> <li>Ubatuba (Abbvr. WU)</li> <li>Caraguatatuba (Abbvr. WC)</li> <li>São Sebastião (Abbvr. WSS)</li> <li>Bertioga (Abbvr. WB)</li> <li>Santos (Abbvr. WS)</li> <li>Praia Grande (Abbvr. WPG)</li> <li>Cubatão (Abbvr. WCUB)</li> <li>São Vicente (Abbvr. WSV)</li> <li>Itanhaém (Abbvr. WITA)</li> <li>Peruíbe (Abbvr. WPERU)</li> <li>Iguape (Abbvr. WIGUA)</li> <li>Itariri (Abbvr. WITR)</li> <li>Pedro de Toledo (Abbvr. WPDT)</li> <li>Iporanga (Abbvr. WIPORA)</li> <li>Apiaí (Abbvr. WAPI)</li> <li>Itaoca Abbvr. WITAO)</li> </ul> <p>- Each shapefile contain information about altitude (min., max, and mean), area (km²), and length (km). </p> <p>- Debris-flow Inventory shapefile.</p> <p> 2. TABLES</p> <ul> <li>Tables for the watersheds mapped in each cities also contain information about the morphometric parameters (melton ratio, basin relief, and relief ratio).</li> <li>Debris-flow inventory information. </li> </ul> <p> </p>
AMPERE GRD & IRD Data (2013-Mar)
<p>2013-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2012-Mar)
<p>2012-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2011-Mar)
<p>2011-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2020-Mar)
<p>2020-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
Detection of detached ice-fragments at polar scarps of Mars
<p>This dataset includes the detections of the detached ice-fragments from 19 polar steep scarps of Mars. The results were detected by a deep learning model, and were saved in shapefile form. </p>
AMPERE GRD & IRD Data (2019-Mar)
<p>2019-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2018-Mar)
<p>2018-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2017-Mar)
<p>2017-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2016-Mar)
<p>2016-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2015-Mar)
<p>2015-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2014-Mar)
<p>2014-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2023-Mar)
<p>2023-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
AMPERE GRD & IRD Data (2024-Mar)
<p>2024-Mar AMPERE GRD and IRD data.</p><p>AMPERE IRD files contain hemispheric delta-B observations in global coordinates (geographic and AACGM). Data are blocked into 10-minute 'chunks' at 2-minute resolution for use in the fitting algorithm. Measurements flagged 'bad' in the earlier processing are removed prior to entry in IRD.</p><p>AMPERE GRD files contain hemispheric delta-B and Birkeland current fits at 2-minute resolution.</p>
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.