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.
5
datasets available to search
ShareScore release 0.9.0
Dataset results
5 results for “stellar atmospheres”
WP2: Photochemical model of planetary atmospheres driven by high-energy stellar irradiation
<p>Modeling results of irradiated planetary atmospheres (Locci et al. 2021, <em>Extreme Ultraviolet and X-ray Driven Photochemistry of Gaseous Exoplanets</em>, PSJ, submitted). See <em>Introduction</em> and <em>Readme_Reference_model</em> for more details.</p>
Output Dataset from "Stellar Atmospheric Parameters From Gaia BP/RP Spectra using Uncertain Neural Networks"
<p>Output dataset of stellar parameters and associated uncertainties derived by the machine learning approach, as decribed in <a href="https://doi.org/10.1093/mnras/stae1303" target="_blank" rel="noopener"><em>"Stellar Atmospheric Parameters From Gaia BP/RP Spectra using Uncertain Neural Networks", Fallows & Sanders</em> (</a><em><a href="https://doi.org/10.1093/mnras/stae1303" target="_blank" rel="noopener">2024)</a>. </em></p> <p>Included parameters: [Fe/H] (fe_h), effective temperature (teff), surface gravity (logg), [C/Fe] (c_fe), [N/Fe] (n_fe), and [a/M] (a_m). Gaia DR3 source ids are included for matching purposes, alongside Gaia bp_rp_excess_factor and ruwe metrics for quality filtering.</p> <p><em>We include predictions for only Gaia objects with radial velocity measurements ('output_0.0_360.0_v2.txt'), and for all* Gaia objects with XP spectra ('gaiaFull_output_0.0_360.0.zip'). Note our full catalogue has a total size of 30.9GB once uncompressed.</em></p> <p> </p> <p><em>* Not truly all objects with XP spectra; stars with spurious or unreliable measurements in our requred inputs (Gaia, 2MASS, WISE) have been removed.</em></p>
The data for Time-dependent Stellar Flare Models of Deep Atmospheric Heating
<p>This repository contains model output (within two .tar.gz files) and a pdf document (analysis_tools_mdwarfradyngrid-v1.0.pdf) that explains the contents and use. The models are described in Kowalski, A.F., Allred, J.C., & Carlsson, M. <em>Time-dependent Stellar Flare Models of Deep Atmospheric Heating, </em>published 2024 July 5 in <em>The Astrophysical Journal</em> Volume 969, Number 2 (DOI: <a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad4148">10.3847/1538-4357/ad4148</a>).</p> <p>The Jupyter notebook demo, radyn_xtools_Demo.ipynb is included in the PyPI package installation that is described in analysis_tools_mdwarfradyngrid-1.0.pdf.</p>
Data Products for "The Upper Atmosphere of Uranus from Stellar Occultations II: Revised Temperatures in the Upper Stratosphere and Lower Thermosphere"
<p>From the README file:</p> <p>Organization of data products connected to Saunders et al. (2023, PSJ) and Saunders et al. (2024, PSJ).</p> <p>/forward_modeling_results.csv -- Anderson-Darling test values and critical values for each comparison between Voyager 2 profiles and observed stellar occultation light curves. Voyager 2 profiles were forward modeled into stellar occultation light curves to enable a direct comparison to observed, Earth-based stellar occultation profiles using the Anderson-Darling test of normality. Critical values are provided. See Section 3 of Saunders+23 and Section 2 of Saunders+24.</p> <p>/original_occultation_profiles/ -- Previously published atmospheric profiles from Earth-based stellar occultations. Data were extracted using a data extraction software on published papers. The citation for each data source is provided below. <br>/original_occultation_profiles/1977* -- Elliot et al. (1979)<br>/original_occultation_profiles/1981* -- French et al. (1983)<br>/original_occultation_profiles/1982-04* -- Sicardy et al. (1985)<br>/original_occultation_profiles/1982-05* -- French et al. (1987)<br>/original_occultation_profiles/1983* -- Elliot et al. (1987)</p> <p>/reprocessed_occultation_profiles/ -- All atmospheric profiles resulting from reprocessing the 26 occultation profiles.<br>/reprocessed_occultation_profiles/profiles/ -- Only the atmospheric profiles.<br>/reprocessed_occultation_profiles/profiles/* -- Each individual profile, in original vertical resolution. Columns: radius [km] (from center of Uranus), temperature [k], pressure [microbar], number density [m^-3], refractivity, scale_height [km] (pressure scale height H = kT/mg), y [km] (close-approach distance of the line connecting the viewer and the occulted star to the center of Uranus, see Saunders+23 for description). Units are provided in column headers.<br>/reprocessed_occultation_profiles/errors/ -- Only the errors for the atmospheric profiles.<br>/reprocessed_occultation_profiles/errors/* -- 1-sigma srrors for each individual profile.</p> <p>/atmospheric_models/ -- One-dimensional atmospheric model products. See Section 5 of Saunders+24.<br>/atmospheric_models/model_parameters/model_constants -- Values of constants used in the models. See Table 3 of Saunders+24.<br>/atmospheric_models/model_parameters/model_parameters -- Values and uncertainties of model parameters. See Table 3 of Saunders+24.<br>/atmospheric_models/model_profiles/* -- Profiles for the 9 models provided in Appendix C of Saunders+24. "Average" profiles are fit to the average of the 26 reprocessed stellar occultations; "cool" profiles are fit to the lower bound of the reprocessed occultations; "warm" profiles are fit to the upper bound of the reprocessed occultations. "Best-fit" profiles are the best fit model results; "lower" profiles are the lower bound of the family of generated profiles, meant to serve as a range of uncertainty; "upper" profiles are the upper bound. See Table 3 and Appendix C in Saunders+24 for more information. Units are provided in column headers.</p> <p> </p>
Chemical species in Titan's upper atmosphere observed by Cassini/UVIS stellar occultations
<p>The archive files contain the line-of-sight abundances and local densities of CH<sub>4</sub>, C<sub>2</sub>H<sub>2</sub>, C<sub>2</sub>H<sub>4</sub>, C<sub>2</sub>H<sub>6</sub>, C<sub>4</sub>H<sub>2</sub>, C<sub>6</sub>H<sub>6</sub>, HCN, HC<sub>3</sub>N, and haze particles in Titan's upper atmosphere retrieved using Cassini/UVIS stellar occultation observations during 18 Titan flybys. These results are shown in Figures 5-10 of the manuscript listed below.</p> <p>Fan, S., Zhao, D., Li, C., Shemansky, D. E., Liang, M. -C., and Yung, Y. L. (2022) Seasonal Variations of Chemical Species in Titan’s Upper Atmosphere. <em>The Planetary Science Journal.</em></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.