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.
587
datasets available to search
ShareScore release 0.7.1
Dataset results
587 results for “Asteroid”
Early Partial Melting and Formation of Na-rich Asteroidal Crust from the Albite-rich Achondrite Erg Atouila 001
<p>This is the research data related to the manuscript titled: Early Partial Melting and Formation of Na-rich Asteroidal Crust from the Albite-rich Achondrite Erg Atouila 001,<strong> </strong>including the the petrological and elemental mapping images, and the supplementary materials of the manuscript.</p>
The metre-scale roughness of asteroid (101955) Bennu from the OSIRIS-REx Laser Altimeter: Processed OLA v21 pointclouds for RMS deviation (L = 0.2 m to L = 20.0 m) [Dataset]
<p>Pointclouds:</p> <ul> <li>Pointcloud (.pcd) files for OLA RMS deviation calculation with fields: <br> <ul> <li>'Location': node points (XYZ points on Bennu's surface)</li> <li>'Intensity': height delta between the node and a neighbouring point at distance L from the node. 'Height' is defined as height above an orthogonally regressed plane fit to points within 2L of the node. </li> </ul> </li> </ul> <p> Tables:</p> <ul> <li>2020_06_bt_final_ma.xlsx: <ul> <li>Crater catalog from Bierhaus et al (2022)</li> </ul> </li> <li>bierhaus2023_craters_gt5m_lt80m_olav21_roi_flags.xlsx: <ul> <li>Subset of catalog from Bierhaus et al. (2022) with craters between 5 m - 80 m diameter used for interior-exterior roughness ratio in Bierhaus et al. (2023) and Rossmann et al. (2024).</li> </ul> </li> </ul> <p> </p>
Effects of embryo energy, egg size and larval food supply on the development of asteroid echinoderms
Organisms have limited resources available to invest in reproduction, causing a tradeoff between the number and size of offspring. One consequence of this tradeoff is the evolution of disparate egg sizes and, by extension, developmental modes. In particular, echinoid echinoderms (sea urchins and sand dollars) have been widely used to experimentally manipulate how changes in egg size affect development. Here we test the generality of the echinoid results by 1) using laser ablations of blastomeres to experimentally reduce embryo energy in the asteroid echinoderms (sea stars), Pisaster ochraceus and Asterias forbesi and 2) comparing naturally produced, variably-sized eggs (1.7 fold volume difference between large and small eggs) in A. forbesi. In P. ochraceus and A. forbesi there were no significant differences between juveniles from both experimentally reduced embryos and naturally produced eggs of variable size. However, in both embryo reduction and egg size variation experiments, simultaneous reductions in larval food had a significant and large effect on larval and juvenile development. These results indicate that 1) food levels are more important than embryo energy or egg size in determining larval and juvenile quality in sea stars and 2) the relative importance of embryo energy or egg size to fundamental life history parameters (time-to and size-at metamorphosis), does not appear to be consistent within echinoderms.
Data and scripts for manuscript "Full-field modeling of heat transfer in asteroid regolith 2: Effects of porosity"
<p>Includes summary spreadsheet, solution files (zipped) in vtk format, and scripts. Vtk filenames are the same as those listed in the tables in the supplement to the JGR:Planets paper. </p>
Data for paper entitled "Effect of iron content on the thermal conductivity of orthopyroxene with implications for the thermal evolution of S-type asteroids and the thermal structure of the Moon"
<p>This data include all the plat data in the paper "<strong>Effect of iron content on the thermal conductivity of orthopyroxene with implications for the thermal evolution of S-type asteroids and the thermal structure of the Moon"</strong></p>
Evidence for asteroid scattering and distal solar system solids from meteorite paleomagnetism
<p>Alternating field demagentisation data for the Tagish Lake meteorite, published in 'Evidence for asteroid scatting and distal solars system solids from meteorite paleomagnetism' (2020) <em>The Astrophysical Journal</em>, <strong>892</strong>, 126</p>
Distribution of encounters of individual asteroid pairs
<p>The figures present the results for each new asteroid pair. The first subfigure of each panel shows the time distribution of encounters between clones of asteroids. The legend describes the parameters of the primary component for each pair and the cut-off parameters of the considered encounters. The second subplot demonstrates the distribution of encounters in terms of Hill sphere radii and escape velocities, and gives the information of how close the registered encounters were. </p>
BC430 Asteroid Ephemerides
<p>We used the new observational error model to recalculate the orbits of the 300 large asteroids that appeared in the JPL DE405 planetary ephemeris due to their potential perturbations of the orbits of the major planets (Standish 1998). These newly recalculated epoch state vectors were then integrated over the timespan 1800–2200, with mutual perturbations modeled using the best available published and estimated masses of the 300 asteroids. The resulting BC430 asteroid ephemeris are presented here.</p>
Update on the 53Mn-53Cr ages of dolomite in the Ivuna CI chondrite and asteroid Ryugu sample
<p>Table S1: XRD data of synthetic carbonates</p> <p>Table S2: Checmical composition of synthetic carbonates</p> <p>Table S3: SIMS data of synthetic carbonates and San Carlos olivine</p> <p>Table S4: SIMS data of Ivuna H2 dolomite</p> <p> </p>
Experimental and analytical methods for thermal infrared spectroscopy of complex dust coatings in a simulated asteroid environment
<p>The spectral and thermophysical effects of thin-continuous, macro-discontinuous, and micro-discontinuous dust cover are not understood and require relevant laboratory analyses to be deconvolved in an orbital setting. We have constructed a custom environment chamber that enables the controlled deposition of size-regulated dust particles in coatings with varying continuity and thickness. TIR spectra of coated substrates acquired in a simulated asteroid environment (SAE) are used to investigate the extent to which dust coatings of different thicknesses and arrangements contribute to orbital spectral signatures of airless body surfaces. </p> <p>TIR (5-50 𝜇m) spectra of each sample are acquired under SAE conditions using the Planetary and Asteroid Regolith Spectroscopy Environmental Chamber (PARSEC) at Stony Brook University. PARSEC is designed to measure samples under environmental conditions typical of airless bodies. The chamber houses a sample wheel with six sample cups and a calibration target coated with Nextel black. There is also a black body target under the wheel. All sample cup and black body targets can be individually heated and rotated into position from outside of the chamber. Temperature is controlled through two Eurotherm Mini8 Loop Controllers and managed on an in-lab computer with the Eurotherm iTools interface. Samples are illuminated at 55° incidence by a quartz halogen lamp connected to a Bentham 610 power source. Surrounding the sample wheel is a cold shield actively cooled by the input of liquid nitrogen into an internal dewar to reach temperatures < 150 K. Pressure in the chamber is controlled by a Pfeiffer HiCube turbo vacuum pump to reach 10<sup>-6</sup> mbar. In line with the vacuum chamber is a pressure regulated tank of N<sub>2</sub> used for purging and ambient pressure measurements. The PARSEC chamber is connected to a Nicolet 6700 FTIR spectrometer equipped with a Cesium Iodide (CsI) beamsplitter and a deuterated L-alanine doped triglycine sulfate (DLaTGS) detector with a CsI window. The spectrometer is actively purged with air scrubbed of CO<sub>2</sub> and water vapor and sealed at the interface with PARSEC. A total of 256 scans from 2,200 to 400 cm<sup>-1</sup> are integrated for a 10-minute measurement period, using a spectral sampling of 2 cm<sup>-1</sup>. During each experimental session, all samples and the black body are measured under SAE conditions. Calibration measurements of the blackbody target at 70 and 100°C are acquired, then the integrated sample cup heaters and solar lamp are adjusted to achieve the desired sample brightness temperature of 80°C. Samples are allowed to reach temperature under the lamp for more than 45 minutes until the spectral maximum stabilizes and the calculated brightness temperature at the CF is within ~10 K of the target 353 K. This procedure is repeated for all samples while ensuring the chamber temperature remains stable under 150 K through continued addition of liquid nitrogen. The Radiance-to-emissivity conversion method used determines the maximum brightness temperature between 500 and 1700 cm-1 and divides the radiance by a Planck function of the same temperature. This assures the maximum brightness temperature is the kinetic temperature of the same, and its emissivity is unity at the frequency of this maximum. This dataset includes 15 different samples acquired under SAE and ambient pressure/temperature conditions. These samples range in layer thickness and continuity and are intended to test and demonstrate the range of the coating process.</p>
Carbonate record of temporal change in oxygen fugacity and gaseous species in asteroid Ryugu
<p>Supplementary Table 1. Carbon- and oxygen-isotope data of carbonates obtained with SIMS.</p> <p>Supplementary Table 2. Chemical compositions of carbonates measured with EDS.</p> <p> </p>
FIG.3 in Deep-Sea asteroids (Echinodermata; Asteroidea) from the Galician Bank (North Atlantic Ocean)
FIG.3. Hymenaster giboryi (124131-B79): a. Abactinal general view. Scale bar: 2.5 mm. b. Anus. Spine's wreath. Scale bar: 2.5 mm. c. Actinal general view. Adambulacral plates and furrow spines. Scale bar: 2.5 mm. d. Adambulacral spines detail. Scale bar: 2.5 mm. Map. World distribution area of some species of the genus Hymenaster (see legend).
FIG.2 in Deep-Sea asteroids (Echinodermata; Asteroidea) from the Galician Bank (North Atlantic Ocean)
FIG.2. Circeaster americanus (178094-B35): a. Abactinal general view. Scale bar: 20 mm. b. Abactinal plates detail. Scale bar: 2.5 mm. c. Marginal fringe. Arrow: Inferomarginal plates. Scale bar: 10 mm. d. Actinal view (plates arrangement). Pedicellariae detail. Oral plates. Adambulacral plates and furrow spines. Scale bar: 10 mm. Map. World distribution area of species: Circeaster americanus (see legend).
Short-term gluCOCOrticoid in Adult STEROID-sensitive Nephrotic Syndrome: The COCO-ASTEROID Study
ClinicalTrials.gov study NCT07151456. IPD Sharing: NO. Countries: 1. Publications: 7.
A Study To Evaluate the Effect of Rosuvastatin On Intravascular Ultrasound-Derived Coronary Atheroma Burden (ASTEROID)
ClinicalTrials.gov study NCT00240318. IPD Sharing: Not stated. Countries: 8. Publications: 1.
Data from: Echinoderm phylogeny including Xyloplax, a progenetic asteroid
Open the record for dataset details and reuse information.
Effects of embryo energy, egg size and larval food supply on the development of asteroid echinoderms
Open the record for dataset details and reuse information.
Data from: Analysis of four-band WISE observations of asteroids
Open the record for dataset details and reuse information.
Ultra-wideband SAR Tomography on asteroids : FDBP and Compressive Sensing datasets
<p>Our knowledge of the internal structure of asteroids is currently indirect and relies on inferences from remote sensing observations of surfaces. However, it is fundamental for understanding small bodies’ history and for planetary defense missions. Radar observation of asteroids is the most mature technique available to characterize their inner structure, and Synthetic Aperture Radar Tomography (TomoSAR) allows 3D imaging by extending the synthetic aperture principle in the elevation direction. However, as the geometry of observation of small asteroids is complex, and TomoSAR studies have always been performed in the Earth observation geometry, TomoSAR results in a small body geometry must be simulated to assess the methods’ performances. Different tomography algorithms can be adopted, depending on the characteristics of the problem. While the Frequency Domain Back Projection (FDBP) is based on the correction of the Fourier transform of the received signal by an <em>ad-hoc</em> function built from the geometry of study, it can only retrieve the true position of the scatterers when applied along with ray-tracing methods, which are unreliable in the case of rough asteroid surfaces. Meanwhile, the Compressive Sensing (CS) is based on the compressive sampling theory, which relies on the hypothesis that few scatterers lie in the same direction from the subsurface. The CS can be used to retrieve the position of the scatterers, but its application in the small body geometry is questioned. Thus, both performances of the FDBP and the CS in a small body geometry are demonstrated, and the quality of the reconstruction is analyzed.</p>
Fig. 3 in New articulated asteroids (Echinodermata, Asteroidea) and ophiuroids (Echinodermata, Ophiuroidea) from the Late Jurassic (Volgian / Tithonian) of central Spitsbergen
Fig. 3. Savignaster septentrionalis Rousseau & Gale sp. nov. A–B. Holotype PMO 218.000. A. Complete arm and associated interradial area showing chevron ossicles. B. Drawing of holotype showing main morphological features. C. Paratype PMO 217.976, partial arm preserved up to the tip. D. Paratype PMO 217.977, partial arm specimen with elongated, narrow ambulacrals set at nearly right-angle to the arm axis. E. Paratype PMO 217.978, a near complete arm with associated adambulacral spines. F. Paratype PMO 218.008, close-up view of fan-shaped trellis-like adambulacral spines articulated to the lateral margin of the adambulacral. Abbreviations: abact = abactinal ossicle; adamb = adambulacral; amb = ambulacral; cho = chevron ossicle.
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.