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283 results for “orbital data”
Spectral reflectance data of Mercury's surface collected by the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument during orbital observations of the NASA MESSENGER mission between 2011 and 2015 resampled to a [55399 × 396] tabular data format.
<p>MASCS is a three sensor point spectrometer with a spectral coverage from 200 nm to 1450 nm.<br> Single spectra are resamples in to steps to a format useful for our ML application : a datacube with ~400 spectral channel covering the whole surface of Mercury.<br> The final dataset has dimension [N×M] where N is the number of grid cells (360 × 180 = 64, 800) and M is the number of spectral features (396).<br> Due to the incomplete coverage and data filtering, some grid cells are empty.<br> After removing these empty cells, the size of the dataset is [55399 × 396].</p> <p>This specific product is stored as a gzip compressed json, where each element is a grid cell.<br> We are in the process to publish a complete pipeline to produce this product from RAW data on https://github.com/epn-ml/MESSENGER-Mercury-Surface-Cassification-Unsupervised_DLR/ .</p> <p>Spectral reflectance data of Mercury’s surface collected by the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument during orbital observations of the NASA MESSENGER mission between 2011 and 2015.<br> MASCS is a three sensor point spectrometer with a spectral coverage from 200 nm to 1450 nm.<br> Single spectra are resamples in to steps to a format useful for our ML application : a datacube with ~400 spectral channel covering the whole surface of Mercury.<br> The final dataset has dimension [N×M] where N is the number of grid cells (360 × 180 = 64, 800) and M is the number of spectral features (396).<br> Due to the incomplete coverage and data filtering, some grid cells are empty.<br> After removing these empty cells, the size of the dataset is [55399 × 396].</p> <p>0. Pre-filtering<br> We used the most recent dataset that had large-scale photometric corrections and thus was almost free from observation geometry effects.<br> However, extreme geometry are still present and are typically associated with high noise and some residual instrumental effects.<br> Based on our empirical tests, we filtered out observations with an emission/incidence angle ≥80∘.<br> We also calculated the median value per wavelength and per cell grid when constructing the global hyperspectral data cube and filtered out observations falling under the 2nd percentile and above 99.9th percentile to clean some residual geometry effects.<br> With this approach we create an effective noise filter while retaining enough observations to be able to analyse the entirety of the surface of the planet.</p> <p>1. Spectral resmpling<br> Unprocessed MASCS spectra could have 512 or 256 channes, depending on binning.<br> We resampled the data in the spectral dimension to a common wavelength range from 260 nm to 1052 nm with a 4 nm resolution (2 nm spectral sampling), resulting in 396 spectral channels.<br> This approach slightly oversamples the original 4.77 nm spectral resolution and removes some points from the original 200-1050 nm range.<br> The resulting data matrix is expressed in tabular form, with each row representing a single grid cell or pixel on the surface.<br> The elements of each row are the spectral reflectance values from the VIS instrument at 396 (resampled) wavelengths.</p> <p>2. Spatial resmpling<br> The whole dataset of ∼ 5 million spectra is resampled to a planet-wide rectangular grid of 1×1deg in the latitudinal band between ± 80.<br> The cell longitudinal size varies between ∼ 40 km at the equator to a minimum of ∼ 10 km at ±80∘.<br> Thus, the area spanned by each grid cell depends on the latitude. However, the same is true for the acquisition process, where higher spatial resolution is reached near the equator and lower resolution at the poles.</p>
Data for: Terahertz orbital angular momentum modes with flexible twisted hollow core antiresonant fiber
<p>Supporting data for the published work on "Terahertz orbital angular momentum modes with flexible twisted hollow core antiresonant fiber". The data here reported are all the necessary data to reproduce the figures in the paper both measurements an simulations (except for the analytical results, which are obtained directly from the formulas included in the paper). The Info file describes each file, how they have been obtained and what they have been used for. </p>
Data for Entanglement of Orbital Angular Momentum in Non-Sequential Double Ionization
<p>Data for publication “Entanglement of Orbital Angular Momentum in Non-Sequential Double Ionization”, available at https://arxiv.org/abs/2111.10148. A readme.txt file is included with the data.</p> <p><strong>Authors</strong></p> <p>Andrew S. Maxwell, Lars Bojer Madsen, Maciej Lewenstein</p> <p><strong>Abstract</strong></p> <p>We address orbital angular momentum (OAM) entanglement in ultrafast processes. In the strongly correlated process of non-sequential double ionization (NSDI) we demonstrate robust photoelectron entanglement. In contrast to commonly considered continuous variable entanglement measures, the discrete OAM allows for a simpler interpretation, computation, and measurement of entanglement. The logarithmic negativity reveals that the entanglement is robust to incoherent effects and an entanglement witness is used to minimize the number of measurements to detect the entanglement, while both quantities can be directly related to coherence terms between OAM channels. We quantify the entanglement for a large range of targets and field parameters to find the most entangled photoelectron pairs. This methodology provides a general way to use OAM to quantify and measure entanglement that is well-suited to attosecond processes, and we show can be exploited to enhance imaging capabilities through correlated measurements, or could be used for generation of OAM-entangled electrons.</p>
Data for "Hot-carrier transfer across a nanoparticle-molecule junction: The importance of orbital hybridization and level alignment"
<p>This upload includes the data presented and analyzed in the article "Hot-carrier transfer across a nanoparticle-molecule junction: The importance of orbital hybridization and level alignment" by Jakub Fojt, Tuomas P. Rossi, Mikael Kuisma, and Paul Erhart.</p> <p>The codes for reproducing the data are provided at <a href="https://doi.org/10.5281/zenodo.7118376">doi:10.5281/zenodo.7118376</a>.</p> <p>See <em>README.md</em> in <em>data.zip</em> for a detailed description.</p>
Mars orbital image (HiRISE) labeled data set
<p>This data set contains 3820 landmarks that were extracted from 168 HiRISE images. The landmarks were detected in HiRISE browse images. For each landmark, we cropped a square bounding box the included the full extent of the landmark plus a 30-pixel margin to left, right, top, and bottom. Each cropped image was then resized to 227x227 pixels.</p> <p><strong>Contents</strong>:</p> <ul> <li>map-proj/: Directory containing individual cropped landmark images</li> <li>labels-map-proj.txt: Class labels (ids) for each landmark image</li> <li>landmark_mp.py: Python dictionary that maps class ids to semantic names</li> </ul> <p><strong>Attribution</strong>:</p> <p>If you use this data set in your own work, please cite this DOI: 10.5281/zenodo.1048301</p> <p>Please also cite this paper, which provides additional details about the data set.</p> <p>Kiri L. Wagstaff, You Lu, Alice Stanboli, Kevin Grimes, Thamme Gowda, and Jordan Padams. "Deep Mars: CNN Classification of Mars Imagery for the PDS Imaging Atlas." <em>Proceedings of the Thirtieth Annual Conference on Innovative Applications of Artificial Intelligence</em>, 2018.</p> <p> </p>
"Hydration of a clay-rich unit on Mars, comparison of orbital data to rover data" supplementary data
<p>MCMC results from individual DAN measurements from sols 1814 to 3069 used in this work with material classifications from Figure 11.</p>
Data used to evaluate ORBITS: Optimal Repair-Based Inconsistency-Tolerant Semantics
<p>This dataset provides the input files that were used in the evaluation of the ORBITS system (Optimal Repair-Based Inconsistency-Tolerant Semantics, <a href="https://github.com/bourgaux/orbits">https://github.com/bourgaux/orbits</a>). A detailed description is available in a technical report on arXiv (<a href="https://arxiv.org/abs/2202.07980">https://arxiv.org/abs/2202.07980</a>).</p> <p><strong>Content:</strong></p> <p>Folders <em>cqapri_benchmark</em>, <em>food_inspection_benchmark</em>, and <em>physicians_benchmark</em> contain JSON files of conflict graphs and candidate queries and their causes.<br> These files are named using the following pattern: files of candidate answers and their causes are named <database>_<query>_answers_causes.json, and conflict graphs are named <database>_conflictGraph_<priority relation>.json where <priority relation> says whether the priority relation is score-structured (prio_score) or not (prio_non_score) and the probability (p<proba>) or number of scores (n<number>) used to build the priority relation.</p> <p>Folder <em>original_datasets_and_queries</em> contains the Food Inspection and Physicians datasets used to generate files from <em>food_inspection_benchmark</em> and <em>physicians_benchmark</em>.<br> Files from <em>cqapri_benchmark</em> have been generated from the CQAPri benchmark available at <a href="https://lahdak.lri.fr/CQAPri/CQAPri.php">https://lahdak.lri.fr/CQAPri/CQAPri.php</a>.<br> In all cases, we use ProvSQL (<a href="https://github.com/PierreSenellart/provsql">https://github.com/PierreSenellart/provsql</a>) to build conflict graphs and causes from the datasets.</p>
Experimental data and scripts used for the paper "Imperfect symmetry of real annular combustors: beating thermoacoustic modes and heteroclinic orbits"
<p>The folder contains the experimental data, the scripts an the instructions to generate the figures of the paper.</p>
Data for the article "Tuning Spin-Orbit Torques Across the Phase Transition in VO2/NiFe Heterostructure"
<p>Data for the article "Tuning Spin-Orbit Torques Across the Phase Transition in VO2/NiFe Heterostructure" (<a href="https://onlinelibrary.wiley.com/doi/full/10.1002/adfm.202111555">https://onlinelibrary.wiley.com/doi/full/10.1002/adfm.202111555</a> and <a href="http://arxiv.org/abs/2201.12984">http://arxiv.org/abs/2201.12984</a>)</p>
A Survey of Electron Conics at Jupiter Utilizing the JADE-E Data During Science Orbits 01, 03-30
<p>This dataset provides Figure 1 from the AGU <em>JGR: Space Physics</em> article of the same name as a PNG image. It also includes text files with the data to reproduce Figures 2-13 in the same AGU <em>JGR:Space Physics</em> article.</p> <p><strong>Key Points:</strong></p> <ol> <li>We surveyed the JADE-E data for science orbits 01, 03-30 and found upward, downward, and bidirectional electron conics 2.5% of the time</li> <li>We observed all electron conics to occur most often at altitudes of 0.3-0.4 R<sub>J</sub> and local times of 15-16h</li> <li>We observed all electron conic types to have energies greater than 0.7 keV below an altitude of 0.5 R<sub>J</sub> and over the main auroral region</li> </ol> <p><strong>Abstract</strong></p> <p>We present a survey of electron conics over Jupiter’s high latitude regions utilizing 22.6 hours of data from the Jovian Auroral Distribution Experiment electron (JADE-E) instrument aboard NASA’s Juno spacecraft during science orbits 01 and 03-30. We observed electron conics for about 2.5% of this time and characterized them into three types based on their direction of motion along Jupiter’s magnetic field lines: upward, downward, and bidirectional. We observed the upward electron conics most often and at energies of 0.057-80.1 keV, while we observed the downward electron conics least often and at energies of 0.073-1.2 keV. We observed bidirectional electron conics mostly around the same times and places as the upward electron conics having energies of 0.081-49.6 keV. We observed all electron conic types to occur mostly at altitudes 0.3-0.4 R<sub>J</sub> and local times 15-16h. Furthermore, we observed all electron conic types to have energies greater than 0.7 keV below an altitude of 0.5 R<sub>J</sub> and over the main auroral region.</p> <p> </p>
Compositional maps of the lunar polar regions derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter data
<p>Compositional maps of the lunar polar regions derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter data as described in Lemelin et al. (2022). </p> <p>This folder includes different GeoTIFF files described and shown in Lemelin et al. (2022). The files are projected in Polar Stereographic Projection, at a spatial resolution of 1000 m/pixel. A version of each of the following file is given for the north and south polar region (50-90 N/S).</p> <p>- Gridded and interpolated Spectral Profiler reflectance mosaics scaled to the LOLA dataset at 1064 nm<br> - Data counts used in the gridded and interpolated Spectral Profiler reflectance mosaics scaled to the LOLA dataset at 1064 nm<br> - Spectral Profiler FeO mosaics <br> - Spectral Profiler OMAT mosaics <br> - Spectral Profiler plagioclase mosaics <br> - Spectral Profiler olivine mosaics <br> - Spectral Profiler low-calcium pyroxene mosaics<br> - Spectral Profiler high-calcium pyroxene mosaics <br> - Nanophase iron mosaics <br> - Correlation coefficient mosaics</p>
Data associated with "The Role of Magma Oceans in Maintaining Surface Water on Rocky Planets Orbiting M-Dwarfs"
<p>The data included here involves all simulations outlined in the manuscript "The Role of Magma Oceans in Maintaining Surface Water on Rocky Planets Orbiting M-Dwarfs", submitted to MNRAS. Files are divided between models with and without a basal magma ocean, as well as different host stars, different magma ocean saturation limits, and different fringe/sensitivity analysis checks. Files are further sub-divided based on our studied parameter space: each is for a single orbital distance within the habitable zone, and a single initial water inventory. "MO_only" files correspond to the concurrent surface magma ocean/runaway greenhouse phase, while "combined_MO_cycling" files correspond to the deep-water cycling period.</p>
Data for "Opposing changes in Indian Summer Monsoon Rainfall variability produced by orbital and anthropogenic forcing"
<p>The dataset for the CAM5 and LBM experiments is presented in the manuscript titled "Opposing changes in Indian summer monsoon rainfall variability produced by orbital and anthropogenic forcing. And the proxy data for the paper.</p>
Data supporting "Universality of Free Fall Shown by Orbital Motion of a Pulsar in a Stellar Triple System"
<p>This is a collection of data supporting the research paper "Orbital Motion of a Pulsar in a Stellar Triple System Shows Universality of Free Fall".</p> <p>The main data content (the ".tim" file) is a set of pulse arrival times, the primary input to the fitting process, in tempo2 format. These times are annotated with post-fit residuals and derivatives with respect to fit parameters using the tempo2 format's per-TOA flags.</p> <p>Additional files include the data that went into several figures, plus the above converted to CSV format - but note that the CSV format does not record the pulse arrival times with sufficient precision to permit fitting. Derivative and uncertainty information may permit reanalysis of the systematics.</p>
CESM1.2 simulation data for "CO2 and orbitally driven oxygen isotope variability in the Early Eocene"
<p>CESM1.2 simulation data for the Early Eocene. These are atmosphere and land climatology files for simulations at both 3x and 6x pre-industrial CO2 levels, as well as 4 separate orbits. The climatology was averaged over the last 100 years of each simulation.</p>
Data for: Higher water loss on Earth-like exoplanets in eccentric orbits
<p>The climate of a terrestrial exoplanet is controlled by the type of host star, the orbital configuration and the characteristics of the atmosphere and the surface. Many rocky exoplanets have higher eccentricities than those in the Solar System, and about 18% of planets with masses < 10 M⊕ have 𝑒 > 0.1. Underexplored are the implications of such high eccentricities on the atmosphere, climate, and potential habitability on such planets. We use WACCM6, a state-of-the-art fully-coupled Earth-system model, to simulate the climates of two Earth-like planets; one in a circular orbit (𝑒 = 0), and one in an eccentric orbit (𝑒 = 0.4). We quantify the effects of eccentricity on the atmospheric water abundance and loss given the importance of liquid water for habitability. The asymmetric temperature response in the eccentric orbit results in a water vapour mixing ratio in the stratosphere (> 20 ppmv) that is approximately five times greater than that for circular orbit (∼ 4 ppmv). This leads to a ∼ 3 time increase in the atmospheric hydrogen loss rate and a corresponding ∼ 3 times decrease in the ocean loss timescale. Thus, highly-eccentric Earth-like exoplanets can still retain their oceans over the lifetime of the system. Using the Planetary Spectrum Generator, we simulate the idealised transmission spectra for both cases. We find that the water absorption features are stronger at all wavelengths for the 𝑒 = 0.4 spectrum than for the circular case. Hence, highly-eccentric Earth-like exoplanets may be prime targets for future transmission spectroscopy observations to confirm, or otherwise, the presence of atmospheric water vapour.</p>
Data for AJ paper: Mass ratio of single-line spectroscopic binaries with visual orbits using Bayesian inference and suitable priors
<p>Data and plots for paper "Mass ratio of single-line spectroscopic binaries with visual orbits using Bayesian inference and suitable priors" accepted for publication in The Astronomical Journal.</p>
Data for: Higher water loss on Earth-like exoplanets in eccentric orbits
Open the record for dataset details and reuse information.
Open data of Control of damping in perpendicularly magnetized thin films using spin-orbit torques
<p>Open access data set for manuscript "Control of damping in perpendicularly magnetized thin films using spin-orbit torques" published in Physical Review B, <strong>101</strong>, 224401 (2020)</p>
Nanomechanical topological insulators with an auxiliary orbital degree of freedom - source data
<p>This data set contains the source data and the matlab scripts applied to obtain the results published in "Nanomechanical topological insulators with an auxiliary orbital degree of freedom". For details of the experimental procedure please refer to the main text of the article, as well as the supplementary information. </p>
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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.