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587 results for “Asteroid”
Dataset for paper "Target selection for Near-Earth Asteroids in-orbit sample collection missions"
<p>This dataset can be used to reproduce the results of the paper titled "Target selection for Near-Earth Asteroids in-orbit sample collection missions."</p> <p>The "results" folder contains the data to reproduce the maps and the rankings of the target asteroids.</p> <p>The "trajectories" folder contains the propagation of the sample trajectories used to obtain the grids.</p>
Dataset for paper "Ejecta cloud distributions for the statistical analysis of impact cratering events onto asteroids' surfaces: a sensitivity analysis"
<p>Dataset for the paper "Ejecta cloud distributions for the statistical analysis of impact cratering events onto asteroids' surfaces: a sensitivity analysis" published in Icarus.</p>
Spherical harmonic models of the shape of asteroid (1) Ceres [JPL SPC]
<p>This archive contains two spherical harmonic models of the shape of asteroid (1) Ceres, truncated at different maximum spherical harmonic degrees. The highest resolution model has a maximum spherical harmonic degree of 1023, which was generated from an ICQ shape model with Q=1024.</p> <p>The data used to generate these models are from a JPL stereo photoclinometric shape model based on Dawn framing camera images, as found in the file <code>CERES_SPC181019_1024.ICQ</code> on <a href="https://sbnarchive.psi.edu/pds3/dawn/fc/DWNCSPC_4_01/DATA/ICQ/">NASA's PDS website</a>. The vertices were first converted from Cartesian to spherical coordinates, from which a regular gridline registered netcdf file was created using the <a href="https://www.generic-mapping-tools.org/">generic-mapping-tools</a> function <code>surface</code> with a tension of 0.6 and with a grid spacing of 0.087890625 degrees. This file was then read into the <a href="https://shtools.github.io/SHTOOLS/index.html">pyshtools</a> software and expanded into spherical harmonics using the function <code>SHCoeffs.expand()</code>. The spherical harmonic functions were chosen to be "4pi" normalized and to exclude the Condon-Shortley phase factor of (-1)<sup>m</sup>. The units of the coefficients are meters.</p> <p>The two files in this archive are</p> <ul> <li>Ceres_JPL_SPC_shape_1023.sh.gz</li> <li>Ceres_JPL_SPC_shape_719.sh.gz</li> </ul> <p>The numbers 1023 and 719 in the filename refer to the maximum spherical harmonic degree of file, which corresponds to effective spatial resolutions of ~11.4 and 8 pixels per degree, respectively. The files are stored in the binary "bshc" format as described in the pyshtools documentation and are furthermore compressed using gzip. The lower resolution model was generated by truncating the spherical harmonic coefficients of the highest resolution model.</p>
Spherical harmonic models of the shape of asteroid (4) Vesta [DLR SPG]
<p>This archive contains four spherical harmonic models of the shape of asteroid 4 Vesta, truncated at different maximum spherical harmonic degrees. The highest resolution model has a maximum spherical harmonic degree of 5759, which was generated from a shape model sampled at 64 pixels per degree.</p> <p>The data used to generate these models are from a DLR stereo photogrammetric shape model based on Dawn high altitude mapping orbit framing camera images, as found in the file <code>VE_HAMO_G_00N_330E_EQU_DTM.IMG</code> on <a href="https://sbnarchive.psi.edu/pds3/dawn/fc/DWNVSPG_2/DATA/">NASA's PDS website</a>. This image file was first converted to netcdf format using the <a href="https://www.generic-mapping-tools.org/">generic-mapping-tools</a> function <code>xyz2grd</code>, and it was then converted to a gridline registration using the function <code>grdsample</code>. The grid was then shifted such that the frist column corresponded to 0 E longitude using the function <code>grdedit</code>, and the resulting netcdf file was read into the <a href="https://shtools.github.io/SHTOOLS/index.html">pyshtools</a> software and expanded into spherical harmonics using the function <code>SHCoeffs.expand()</code>. The spherical harmonic functions were chosen to be "4pi" normalized and to exclude the Condon-Shortley phase factor of (-1)<sup>m</sup>. The units of the coefficients are meters.</p> <p>The four files in this archive are</p> <ul> <li>Vesta_DLR_SPG_shape_5759.bshc.gz</li> <li>Vesta_DLR_SPG_shape_2879.bshc.gz</li> <li>Vesta_DLR_SPG_shape_1439.bshc.gz</li> <li>Vesta_DLR_SPG_shape_719.bshc.gz</li> </ul> <p>The numbers 5759, 2879, 1439, and 719 in the filename refer to the maximum spherical harmonic degree of file, which corresponds to effective spatial resolutions of 64, 32, 16, and 8 pixels per degree, respectively. The files are stored in the binary "bshc" format as described in the pyshtools documentation and are furthermore compressed using gzip. The lower resolution models were generated by truncating the spherical harmonic coefficients of the highest resolution model.</p>
Spherical harmonic models of the shape of asteroid (1) Ceres [DLR SPG]
<p>This archive contains four spherical harmonic models of the shape of asteroid (1) Ceres, truncated at different maximum spherical harmonic degrees. The highest resolution model has a maximum spherical harmonic degree of 5399, which was generated from a shape model sampled at 60 pixels per degree.</p> <p>The data used to generate these models are from a DLR stereo photogrammetric shape model based on Dawn high altitude mapping orbit framing camera images, as found in the file <a href="https://sbnarchive.psi.edu/pds3/dawn/fc/DWNCHSPG_2/DATA/"><code>CE_HAMO_G_00N_180E_EQU_DTM.IMG</code></a> on <a href="https://sbnarchive.psi.edu/pds3/dawn/fc/DWNCHSPG_2/DATA/">NASA's PDS website</a>. This image file was first converted to netcdf format using the <a href="https://www.generic-mapping-tools.org/">generic-mapping-tools</a> function <code>xyz2grd</code>, it was then converted to a gridline registration using the function <code>grdsample</code>, and the resulting netcdf file was read into the <a href="https://shtools.github.io/SHTOOLS/index.html">pyshtools</a> software and expanded into spherical harmonics using the function <code>SHCoeffs.expand()</code>. The spherical harmonic functions were chosen to be "4pi" normalized and to exclude the Condon-Shortley phase factor of (-1)<sup>m</sup>. The units of the coefficients are meters.</p> <p>The four files in this archive are</p> <ul> <li>Ceres_DLR_SPG_shape_5399.bshc.gz</li> <li>Ceres_DLR_SPG_shape_2879.bshc.gz</li> <li>Ceres_DLR_SPG_shape_1439.bshc.gz</li> <li>Ceres_DLR_SPG_shape_719.bshc.gz</li> </ul> <p>The numbers 5399, 2879, 1439, and 719 in the filename refer to the maximum spherical harmonic degree of file, which corresponds to effective spatial resolutions of 60, 32, 16, and 8 pixels per degree, respectively. The files are stored in the binary "bshc" format as described in the pyshtools documentation and are furthermore compressed using gzip. The lower resolution models were generated by truncating the spherical harmonic coefficients of the highest resolution model.</p>
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> <p>*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.</p> <p>**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.</p> <p>*** 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.</p> <p>**** 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.</p> <p>***** 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.</p> <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>
Spherical harmonic models of the shape of asteroid (16) Psyche
<p>This archive contains spherical harmonic models of the shape of asteroid (16) Psyche.</p> <p><strong>Psyche-Shepard2017.sh</strong></p> <p>This is a degree and order 29 spherical harmonic model of the shape of Psyche that was constructed from the shape model of Shepard et al. (2017). The spherical harmonic coefficients were obtained from a least squares inversion that made use of the vertex coordinates from the file <code>psyche.v.final.mod.mod</code>. The least squares inversion was performed using the pyshtools routine <code>SHCoeffs.from_least_squares()</code> and tests show that the power spectrum is stable for maximum degrees up to, and including, 29. The coefficients are in meters and should be used with 4-pi normalized spherical harmonic functions.</p> <p><strong>Psyche-Shepard2021.sh</strong></p> <p>This is a degree and order 10 spherical harmonic model of the shape of Psyche that was constructed from the shape model of Shepard et al. (2021). The spherical harmonic coefficients were obtained from a least squares inversion that made use of the vertex coordinates from the file <code>psyche.vertex.obj</code>. The least squares inversion was performed using the pyshtools routine <code>SHCoeffs.from_least_squares()</code>, and tests show that the power spectrum decreases dramatically for maximum spherical harmonic degrees beyond 10. The coefficients are in meters and should be used with 4-pi normalized spherical harmonic functions.</p>
The bearing capacity of asteroid (65803) Didymos estimated from boulder tracks
<p>This material constitutes the source data and codes used for the the computations and plots of the paper 'The bearing capacity of asteroid (65803) Didymos estimated from boulder tracks' by Bigot, Lombardo et al. This article has been published in Nature Communications on 30 July, 2024.</p> <p>The folder "Source Data" contains an Excel document that provides the raw data used to make the figures and supplementary figures. </p> <p>The folder "Codes" contains the Matlab codes used for the computations of the results, including comments on the figures produced by each code. It also contains a .mat file that consitutes the topographic data of Didymos from Barnouin et al. (2024), used in the code 'TopographyDidymos.m'.</p> <p>The folder "Images" contains the three DART images (DRACO) and the Moon image from LROC used in this article.</p> <p> </p>
Data for Dodds et al., The direction of core solidification in asteroids: implications for dynamo generation
<p>Numerical dataset for the data presented in Dodds et al., The direction of core solidification in asteroids: implications for dynamo generation, manuscript submitted to Icarus journal.</p>
Size, Mass and Density of Asteroids (SiMDA)
<p>This data set contains 'best' values for the bulk density, the size (volume-equivalent diameter) and the mass of 428 small bodies (mainly asteroids) of our Solar System.</p>
Fig. 7 in New articulated asteroids (Echinodermata, Asteroidea) and ophiuroids (Echinodermata, Ophiuroidea) from the Late Jurassic (Volgian / Tithonian) of central Spitsbergen
Fig. 7. Ophioculina hoybergia Rousseau & Thuy gen. et sp. nov., paratypes. A–B. Paratype PMO 218.001c. A. Nearly complete specimen (outlined) preserving five arms and the ventral side of the disc, on a concretion slab with an accumulation of specimens. B. Detail view of arm section. C. Paratype PMO 218.048. Articulated ventral disc preserving good details of the oral plates, the second oral tentacle pores and the rows of papillae bordering the genital slit. D–E. Paratype PMO 218.010b. D. Articulated specimen preserving the basal portion of five arms and showing details of the dorsal disc. E. Detail view of arm section. Abbreviations: aos = adoral shield; lap = lateral arm plate; os = oral shield; rs = radial shield; sart = spine articulation; tp = tentacle pore; vap = ventral arm plate; 2otp = second oral tentacle pore.
Fig. 4 in New articulated asteroids (Echinodermata, Asteroidea) and ophiuroids (Echinodermata, Ophiuroidea) from the Late Jurassic (Volgian / Tithonian) of central Spitsbergen
Fig. 4. Ophiogaleus sp. PMO 217.899a. A. Specimen preserving the ventral side of the disc area, two nearly complete arms and proximal area of a third arm. B. Detail view of the disc area. C. Drawing detail of the area shown in B. D. Detail view of a proximal section of arm. Abbreviations: abgp = abradial genital plate; adgp = adradial genital plate; ds = disc spine; lopa = lateral oral papillae; op = oral plate; sart = spine articulation; v = vertebra.
Fig. 6 in New articulated asteroids (Echinodermata, Asteroidea) and ophiuroids (Echinodermata, Ophiuroidea) from the Late Jurassic (Volgian / Tithonian) of central Spitsbergen
Fig. 6. Ophioculina hoybergia Rousseau & Thuy gen. et sp. nov., holotype PMO 217.930. A. Specimen preserving the ventral side of about half of the disc area and the proximal section of three arms. B. Drawing detail of the oral region, from D. C. Detail view of the base of an arm showing the arm comb. D. Detail view of the oral region. Abbreviations: abgp = abradial genital plate; adgp = adradial genital plate; aopa = apical oral papilla; as = arm spine; gpa = genital papilla; lap = lateral arm plate; lopa = lateral oral papilla; op = oral plate; os = oral shield; v = vertebra; 2opa = papilla of the second oral tentacle pore.
Fig. 2 in New articulated asteroids (Echinodermata, Asteroidea) and ophiuroids (Echinodermata, Ophiuroidea) from the Late Jurassic (Volgian / Tithonian) of central Spitsbergen
Fig. 2. Polarasterias janusensis Rousseau & Gale gen. et sp. nov. A–C. Holotype PMO 218.011a. A. Nearly complete specimen preserved in a cut-through fashion. B. Drawing detail from ambulacral groove showing ambulacrals, adambulacrals, adambulacral spines and scattered valves of forcipulate pedicellariae. C. Portion of arm illustrated in B, basal pieces of straight pedicellariae visible in cross section. D. Paratype PMO 217.982, oral region in actinal view. E. Paratype PMO 217.936, Arm tip showing terminal ossicle. F–G. Paratype PMO 218.069. F. Obliquely compressed radius showing adambulacrals, marginals, and columns of abactinal ossicles. G. Drawing detail from F. Abbreviations: abact = abactinal ossicle; adamb sp = adambulacral spine; adamb = adambulacral; amb = ambulacral; im = inferomarginal; ped bp = basal piece of pedicellariae; sm = superomarginal; sp = spine.
Fig. 5 in New articulated asteroids (Echinodermata, Asteroidea) and ophiuroids (Echinodermata, Ophiuroidea) from the Late Jurassic (Volgian / Tithonian) of central Spitsbergen
Fig. 5. Ophiogaleus sp. A–E. PMO 218.060, specimen preserving the ventral side of the disc area and the base of all five arms. The specimen has been split through a horizontal plane and is visible as part (A) and counterpart (B). Photographs in A and B by H.A. Nakrem. C. Drawing detail of the oral and interradial area. D. Detail view of proximal arm segments with articulated spines. E. Detail view of distal arm segment. F. PMO 218.053a, partly disarticulated arm portion composed of three median segments showing details of the ventral side of the arms. Abbreviations: abgp = abradial genital plate; adgp = adradial genital plate; as = arm spine; cs = arm in cross section; dp = dental plate; ds = disc spine; lap = lateral arm plate; op = oral plate; rs = radial shield; vap = ventral arm plate.
Fig. 1. A in New articulated asteroids (Echinodermata, Asteroidea) and ophiuroids (Echinodermata, Ophiuroidea) from the Late Jurassic (Volgian / Tithonian) of central Spitsbergen
Fig. 1. A. Simplified geological map of the study area in Sassenfjorden, central Spitsbergen, with location of the Janusfjellet (1), Konusdalen (2) and Knorringfjellet (3) collection sites. Redrawn and adapted from Dallmann et al. (2001) by H.A. Nakrem, used with permission. B. Chrono- and lithostratigraphic correlation for the Late Jurassic-Earliest Cretaceous interval of central Spistbergen. The Slottsmøya Member is indicated by a star. Modified with permission from Dalseg et al. (2016). C. Janusfjellet locality, 78°20′35.4″ N, 15°49′85.2″ E, surface outcrop. D. Konusdalen locality, 78°19′97.1″ N, 15°52′15.5″ E, in situ layer. E. Knorringfjellet locality, N 78° 18' 04.4" E 16° 16' 02.0", surface outcrop.
Data from: Deep learning-assisted near-Earth asteroid tracking in astronomical images
<p>This repository is the data release of our paper <em>Deep learning-assisted near-Earth asteroid tracking in astronomical images</em>. There are two categories in this repository:</p> <ul> <li>Simulated training dataset for training the star segmentation network. </li> </ul> <p>The dataset consists of two folders: image (grayscale images) and mask (binary images). The size of each image is 256*256.</p> <ul> <li>Example data for testing asteroid tracking algorithm.<br><br></li> </ul> <p>If you find this work useful, please cite our paper:</p> <div> <div>@article{du2024ASR,</div> <div>title = {Deep learning-assisted near-Earth asteroid tracking in astronomical images},</div> <div>journal = {Advances in Space Research},</div> <div>volume = {73},</div> <div>number = {10},</div> <div>pages = {5349-5362},</div> <div>year = {2024},</div> <div>issn = {0273-1177},</div> <div>doi = {https://doi.org/10.1016/j.asr.2024.02.048},</div> <div>url = {https://www.sciencedirect.com/science/article/pii/S0273117724001911},</div> <div>author = {Zhenhong Du and Hai Jiang and Xu Yang and Hao-Wen Cheng and Jing Liu},</div> <div>keywords = {Near-Earth asteroid, Deep learning, Convolutional neural network, Faint object extraction, Moving object linking},</div> <div>}</div> </div>
Mechanical properties of rubble pile asteroids (Dimorphos, Itokawa, Ryugu, and Bennu) through surface boulder morphological analysis
<p>This material constitutes the dataset used for the computation of the results of the paper Mechanical properties of rubble pile asteroids (Dimorphos, Itokawa, Ryugu, and Bennu) through surface boulder morphological analysis by Robin & al. </p> <p>The folders "Bennu", "Dimorphos", "Itokawa" and "Ryugu" contains the raw images from PDS used for this study as well as the images with the outlined boulders made with segmentanygrains (https://github.com/zsylvester/segmenteverygrain), and the associated morphological descriptor values. The folder "ExtremeCases" contains the raw and outlined images for extreme roundness cases.</p> <p>This material also contains the main figures of the paper as well as the code to remake most the figures.</p> <p>Last version of this manuscript has been submitted to Nature Communications on May 14th, 2024 and accepted on May 17th, 2024.</p> <p><strong>Abstract</strong>: </p> <table> <tbody> <tr> <td>Planetary defense efforts rely on estimates of the mechanical properties of asteroids, which are difficult to constrain accurately from Earth. The mechanical properties of asteroid material are also important in the interpretation of the Double Asteroid Redirection Test (DART) impact. Here we perform a detailed morphological analysis of the surface boulders on Dimorphos using images, the primary data set available from the DART mission. We estimate the bulk angle of internal friction of the boulders to be 32.7 ± 2.5° from our measurements of the roundness of the 34 best-resolved boulders ranging in size from 1.67 to 6.64 m. The elongated nature of the boulders around the DART impact site implies that they were likely formed through impact processing. Finally, we find striking similarities in the morphology of the boulders on Dimorphos with those on other rubble pile asteroids (Itokawa, Ryugu and Bennu). This leads to very similar internal friction angles across the four bodies and suggests that a common formation mechanism has shaped the boulders. Our results provide key inputs for understanding the DART impact and for improving our knowledge about the physical properties, the formation and the evolution of both near-Earth rubble-pile and binary asteroids.</td> </tr> <tr></tr> </tbody> </table>
Gaia DR3 asteroid reflectance spectra: L-type families, memberships and ages
<p>The Gaia Data Release 3 (DR3) contains reflectance spectra at visible wavelengths for 60,518 asteroids over the range between 374-1034 nm, representing a large sample that is well suited to studies of asteroid families.</p> <p>We wanted to assess the potential of Gaia spectra in identifying asteroid family members. Here, we focus on two L-type families, namely Tirela/Klumpkea and Watsonia. These families are known for their connection to Barbarian asteroids, which are potentially abundant in calcium-aluminum rich inclusions (CAIs).</p> <p>The method we developed to establish family memberships is based (1) on a color taxonomy specifically built on Gaia data and (2) on the similarity of spectra of candidate members with the template spectrum of a specific family.</p> <p>Our work demonstrates the advantage of combining the classical hierarchical clustering method (HCM) approach to spectral properties obtained by Gaia for the study of asteroid families. Future data releases are expected to further expand the capabilities in this domain.</p> <p>The memberships for the Tirela/Klumpkea and Watsonia families are reported here. The columns report, from left to right: the identifier of the asteroid, the absolute magnitude, the proper elements (semi-major axis, eccentricity and sine of the inclination, taken from AFP, Novaković et al., 2022), NEOWISE albedo (Masiero et al., 2011) and spectral type from our color taxonomy. For the objects that are not directly classified into the S and L classes, their most probable spectral type is also reported. </p>
Maps of thermal inertia, dielectric constant and brightness temperature of asteroid (16) Psyche derived from ALMA data
<p>These data and results are in support of the findings by Cambioni, S., de Kleer, K. and Shepard, M. in their paper "The Heterogeneous Surface of Asteroid (16) Psyche", Journal of Geophysical Research: Planets, link: https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/2021JE007091. </p> <p>If using any of this material, please cite the above article as doi: 10.1029/2021JE007091</p> <p> </p>
ScienceDex guides
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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.