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304 results for “Planets”
Dataset for "Radiation environment at the surface and subsurface of the Moon: Model development and validation" publication in Journal of Geophysical Research: Planets
<p>data set used for plots in manuscript "Radiation environment at the surface and subsurface of the Moon: Model development and validation" submitted to GRL</p>
FIG. 2. — Souzalopesmyia polleti n in Souzalopesmyia Albuquerque, 1951 (Diptera: Muscidae): new species from South America with an updated phylogeny based on morphological evidence, in Touroult J. (ed.), "Our Planet Reviewed" 2015 large-scale biotic survey in Mitaraka, French Guiana.
FIG. 2. — Souzalopesmyia polleti n. sp.: A-D, ♂: sternite 5, dorsal view (A); epandrium, cercal plate and surstyli, dorsal view (B); epandrium, cercal plate and surstyli, lateral view (C); hypandrium and associated structures, lateral view (D); E-H, ♀: ovipositor, dorsal view (E); ovipositor, ventral view (F); spermatheca (G). Scale bars: 0.5 mm.
A close-in giant planet escapes engulfment by its star
<p>Data for Nature article 'A close-in giant planet escapes engulfment by its star'.</p> <p>Included in this repository are:</p> <p>TESS oscillation spectra of host star -- tess_oscillation_spectra.zip<br> CHFT ESPaDOnS spectropolarimetry of host star and control red giant -- espadons_polarimetric_spectra.zip<br> Least squares deconvolution profiles of spectropolarimetry data -- lsd_profiles.zip<br> Markov chain Monte Carlo chains for radial velocity fitting -- mcmc.zip<br> Inlists for MESA binary simulations -- mesa_binary.zip<br> Keck/HIRES radial velocity measurements of host star and control red giant -- rv.zip<br> Keck/HIRES S_HK indices of host star and control red giant -- s_hk.zip<br> Measurements and model of host star spectral energy distribution -- sed.zip<br> Hipparcos, ASAS-SN, and TESS light curves for host star -- other_photometry.zip</p>
The energetic particle environment of a GJ 436 b-like planet
<p>This data set corresponds to the simulation data presented in the article "The energetic particle environment of a GJ 436b-like planet" (Rodgers-Lee, et al., MNRAS, 2023). Details of the stellar wind and cosmic ray models used for the simulations are available in the article.</p> <p>Each data file consists of the temperature, pressure and heights in the exoplanet atmosphere at a given orbital distance from the star (shown in Fig.3 of Rodgers-Lee et al. 2023). The number density, n(z), of the exoplanet atmosphere can be calculated from the temperature and pressure. Further details relating to the temperature pressure profiles are given in Section 2.3 of Rodgers-Lee et al. (2023). The last two but one columns in the data files are the ionisation rates for molecular hydrogen from Galactic cosmic rays and stellar energetic particles (shown in Fig.4 of Rodgers-Lee et al. 2023). The last column is the assumed planetary effective temperature.</p> <p>The data is given for a number of different orbital distances between 0.01 - 0.2au. File names are formatted as "zenodo_GJ436_manysp_solar_aX_tp.dat" where "X" corresponds to 100 x orbital distance in au (e.g. "a1" corresponds to a=0.01au) considered. The first line describes the data in the file. The second line gives the column headings and units.</p>
Monteux et al., JGR Planets, 2023. Data Repository
<p>Source material to obtain the figures from the article entitled : Conditions for segregation of a crystal-rich layer within a convective magma ocean (JGR Planets 2023).</p> <p>The data that support the findings of this study were obtained using the commercial software COMSOL Multiphysics (version 5.4). COMSOL Multiphysics® is a simulation platform that provides fully coupled multiphysics and single-physics modelling capabilities. COMSOL Multiphysics (version 5.4) has been previously validated for two phase flow applications (Qaddah et al, 2019, Qaddah et al., 2020). To compute our simulations we used the Heat Transfer (www.comsol.com/heat-transfer-module) and Computational Flow Dynamics (www.comsol.com/cfd-module) modules in addition to the main Multiphysics platform (www.comsol.com/comsol-multiphysics). All the parameters used in our simulation are listed and described in the manuscript. The open source software used for data visualisation was Xmgrace (https://plasma-gate.weizmann.ac.il/Grace/). </p> <p>The software used for this study is the commercial software COMSOL Multiphysics (version 5.4) previously validated for two phase flow applications (Qaddah et al., 2019, Qaddah et al., 2020). User manual can be downloaded here:<br> https://doc.comsol.com/5.4/doc/com.comsol.help.cfd/CFDModuleUsersGuide.pdf. <br> A trial version of COMSOL Multiphysics may be requested (see www.comsol.com).<br> <br> More details can be found on the following COMSOL webpages:<br> - On the Foundations of the General Heat Transfer Equation:<br> https://doc.comsol.com/6.1/docserver/#!/com.comsol.help.heat/heat_ug_theory.07.002.html</p> <p>- Theory for Heat Transfer in Fluids :<br> https://doc.comsol.com/6.1/docserver/#!/com.comsol.help.heat/heat_ug_theory.07.008.html</p> <p>- The Euler–Euler Model Equations and in particular how incompressibility is handled:<br> https://doc.comsol.com/6.1/docserver/#!/com.comsol.help.cfd/cfd_ug_fluidflow_multi.09.153.html</p> <p>- The Boussinesq Approximation:<br> https://doc.comsol.com/6.1/docserver/#!/com.comsol.help.cfd/cfd_ug_fluidflow_noniso.07.20.html</p> <p> </p>
Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations
<p>This data set consists of 1D radiative-convective equilibrium boundary conditions for Jupiter-like giant planets, computed using coolTLUSTY and a recently updated set of molecular absorption cross sections. Models span internal temperatures of 80 - 450 K, and surface gravities of log10(g / [cm/s^2]) = 1.8 - 3.6. The planet is irradiated by a black body star at a distance of 5.2AU with effective temperature of 5777K with the zenith angle factor (accounting for an average incident angle) being FACFLX=0.5 or 0.67. The models assume a composition of 3.16x solar abundance, and allow the formation of ammonia clouds at low temperatures with characteristic sizes of 1 or 3 micron. More numerical details on the treatments of irradiation and clouds can be found in "Jupiter Atmospheric Models and Outer Boundary Conditions for Giant Planet Evolutionary Calculations", arXiv number TBA.</p> <p>See README.txt for a description of data formats.</p>
A Unified Treatment of Kepler Occurrence to Trace Planet Evolution: Supplemental Data
<p>Here we present supplementary data underlying the paper "A Unified Treatment of Kepler Occurrence to Trace Planet Evolution I: Methodology." Included are:</p> <ul> <li>Planet catalogs; filenames "dr25_X_PCs_B20_ruwe.csv"</li> <li>Completeness contours; filenames "out0819_X_slog_insol__.fits.gz"</li> <li>Observed planet KDEs; filenames "out0827_X_sboot_1000__avg.npy"</li> </ul>
Orbital Stability of Circumstellar Planets in Binary Systems
<p>Tar archives of simulations for circumstellar planets orbiting a range of host binary stars, where the archives are delineated by the mutual inclination in the filename. Each file in the archive has the assumed mass ratio, mu, and binary eccentricity, e_bin, in the file name as a tuple (mu,e_bin). Tools in python to manipulate and plot the data are provided through a GitHub repository, https://github.com/saturnaxis/ThreeBody_Stability. Inside each file contains a comma delimited text file, where the columns are the initial semimajor axis ratio, the initial phase of the planet, the maximum planetary eccentricity attained over the simulation time, the minimum planetary eccentricity attained over the simulation time, and the collision/escape time. Collisions are defined as collisions with either star, where the escape is when the radial distance of the planet exceeds 200 AU.</p>
CCSM3 simulation data for tidally locked planets
<p>This data set includes simulation results of atmosphere, ocean and sea ice on tidally locked planets, using the model CCSM3.</p>
Data from: Modeling phylogenetic biome shifts on a planet with a past
<p>The spatial distribution of biomes has changed considerably over deep time, so the geographical opportunity for an evolutionary lineage to shift into a new biome may depend on how the availability and connectivity of biomes has varied temporally. To better understand how lineages shift between biomes in space and time, we developed a phylogenetic biome shift model in which each lineage shifts between biomes and disperses between regions at rates that depend on the lineage's biome affinity and location relative to the spatiotemporal distribution of biomes at any given time. To study the behavior of the biome shift model in an empirical setting, we developed a literature-based representation of paleobiome structure for three mesic forest biomes, six regions, and eight time strata, ranging from the Late Cretaceous (100 Ma) through the present. We then fitted the model to a time-calibrated phylogeny of 119 <em>Viburnum</em> species to compare how the results responded to various realistic or unrealistic assumptions about paleobiome structure. Ancestral biome estimates that account for paleobiome dynamics reconstructed a warm temperate (or tropical) origin of <em>Viburnum</em>, which is consistent with previous fossil-based estimates of ancestral biomes. Imposing unrealistic paleobiome distributions led to ancestral biome estimates that eliminated support for tropical origins, and instead inflated support for cold temperate ancestry throughout the warmer Paleocene and Eocene. The biome shift model we describe is applicable to the study of evolutionary systems beyond <em>Viburnum</em>, and the core mechanisms of our model are extensible to the design of richer phylogenetic models of historical biogeography and/or lineage diversification. We conclude that biome shift models that account for dynamic geographical opportunities are important for inferring ancestral biomes that are compatible with our understanding of Earth history.</p>
Processed data of grasshoppers, butterflies and moths for analyses of species trend models for the regional WWF Living Planet Index for Belgium
<p>This archive contains pre-processed datasets used for the analysis of species occupancy models, the results of which were used in the calculation of multi-species indices as part of the regional WWF Living Planet Index for Belgium.</p> <p>The datasets are csv files (comma separated and . as decimal mark). </p> <p>For each species group (moths, butterflies and grasshoppers), the following files are available:</p> <ul> <li>a species list (files with 'species' in the name)</li> <li>an observations list (files with 'observations' in the name - for butterfly or moth species with two distinct flight periods, also a file with the data for the second generation is available)</li> </ul> <p>For one species, <em>Fabriciana adippe</em>, separate files are available with corrected data.</p> <p>The species list files contain the following variables:</p> <ul> <li>species_id (unique species id)</li> <li>scientific_name (accepted scientific name according to the GBIF taxonomic backbone)</li> <li>species_name_NL (Dutch species name)</li> <li>species_name_FR (French species name)</li> <li>season_start (n-th day of the year that marks the beginning of the first -and possibly only- generation)</li> <li>season_end (n-th day of the year that marks the end of the first -and possibly only- generation)</li> </ul> <p>The observations files contain the following variables:</p> <ul> <li>species_id (a unique identifier)</li> <li>year (year of observation)</li> <li>month (month of observation)</li> <li>day (day of observation)</li> <li>julian_day (n-th day of the year)</li> <li>site_id (unique identifier for the 1 km x 1km EEA 1 km x 1 km reference grid square <a href="https://www.eea.europa.eu/data-and-maps/data/eea-reference-grids-2">https://www.eea.europa.eu/data-and-maps/data/eea-reference-grids-2</a>)</li> <li>source (name of data provider)</li> <li>count (max number of sightings for the species for that day and site</li> </ul>
Spectral data used in the paper "Intense Zonal Wind in the Martian Mesosphere During the 2018 Planet-Encircling Dust Event Observed by Ground-based IR Heterodyne Spectroscopy"
<p>This data contains the spectral data used in the paper "Intense Zonal Wind in the Martian Mesosphere During the 2018 Planet-Encircling Dust Event Observed by Ground-based IR Heterodyne Spectroscopy". </p> <p>"MILAHI_2018PEDE_Spectral_Data" is the spectral data and you can find the detailed information of the data in "README".</p> <p> </p> <p> </p>
The Rotating Planet
<p>Second place in the 2023 IAU OAE Astrophotography Contest, category Time-lapses of rotation of Big Dipper or Southern Cross: The Rotating Planet, by Jianfeng Dai.</p> <p>A cosmic journey unfolds across continents in this time-lapse video which takes second place in the category of Time-lapses of rotation of Big Dipper or Southern Cross. The video captures both iconic constellations from diverse corners of the world. Starting in China, the Big Dipper graces the night sky, a steadfast guide embedded in cultural narratives. Its luminance marks the beginning of this celestial odyssey. The two pointer stars on the end of the Big Dipper point to the North Star (Polaris) which appears to remain stationary as the sky rotates. From Nepal’s lofty peaks, the Big Dipper’s familiarity persists, a reliable fixture in the shifting panorama of the rotating planet. Moving to Chile, the Southern Cross adorns the firmament, emblematic of the southern skies. Frames from Chile showcase this constellation accompanied by the Milky Way Galaxy. In Namibia, a telescope from the H.E.S.S. Observatory appears in the video. Later, nestled beneath sheltering trees, the Big Dipper persists in its celestial prominence, appearing against a canvas of stars. Using varied techniques — fisheye lenses, static cameras, and Earth's movement-tracking — each frame unveils the Cross’s grandeur against diverse landscapes. These sequences — marked by star trails and Earth’s rotation—highlight the enduring presence of the Big Dipper and Southern Cross, bridging cultures and celestial beauty across hemispheres.</p> <p><strong>Credit</strong>: Jianfeng Dai/IAU OAE (<a href="https://creativecommons.org/licenses/by/4.0/legalcode">CC BY 4.0</a>)</p>
Planet Earth at night
3d model of the planet earth at night, you can turn off the clouds layer. Source: Objaverse 1.0 / Sketchfab
Complete Data and Results for "Four-of-a-kind? Comprehensive atmospheric characterisation of the HR~8799 planets with VLTI/GRAVITY"
<p><strong>Four-of-a-kind? Comprehensive atmospheric characterisation of the HR~8799 planets with VLTI/GRAVITY</strong></p> <p>We explored the atmospheres of the HR 8799 system of directly imaged planets using petitRADTRANS atmospheric retrievals. This required reprocessing existing data, preparing new observations from VLTI/GRAVITY and combining additional archival spectroscopic and photometric datasets. We ran 95 retrievals across the four planets, and include here the full set of outputs from the sampling process, as well as synthesised results for each retrieval. Finally, we also include templates for running these retrievals.</p> <p>This data, together with the results of the retrievals and templates for running similar emission spectra retrievals are included in this Zenodo archive. Additional README files are included throughout the archive in order to explain file structures, units, and to provide original references where necessary. An archived repository of the petitRADTRANS code can be found at <span><a href="https://doi.org/10.5281/zenodo.10892021">https://doi.org/10.5281/zenodo.10892021</a>,</span> while the up-to-date repository is available at <span><a href="https://gitlab.com/mauricemolli/petitRADTRANS">https://gitlab.com/mauricemolli/petitRADTRANS</a>.</span></p>
Dataset for Dichotomic core solidification caused by nonideally-mixing effects in rocky planets
<p>All data involved in the manuscript.</p>
Figures referring to the paper "Radii, masses, and transit-timing variations of the three-planet system orbiting the naked-eye star TOI-396" (Bonfanti et al.) accepted for publication in A&A on 20/11/2024
<p>Fig. A.1: ttv_pla1_2.pdf</p> <p>TTV amplitudes obtained for TOI-396 b (black markers) and TOI-396 c (red markers). This is a superposition of the first two panels of Figure 4 in the paper emphasising the anti-correlation pattern.</p> <p> </p> <p>Fig. A.2: lcGLS*.pdf</p> <p>First column: Generalised Lomb-Scargle periodograms of TESS Sector 3 (lcGLS_3.pdf), 4 (lcGLS_4RawFluxrm.pdf), 30 (lcGLS_30RawFlux.pdf), and 31 (lcGLS_31RawFlux.pdf) raw photometry. Second column: Generalised Lomb-Scargle periodograms of the residuals (lcGLSRaw_3noSine.pdf, lcGLSRaw_4noSinerm.pdf, lcGLSRaw_30noSine.pdf, lcGLSRaw_31noSine.pdf) after removing the best fitting sinusoidal signals at the most significant frequency identified in the periodograms of the corresponding TESS time series. The long dashed red line marks the FAP at 0.1\%. Significant peaks are detected in the 6---8 day range, which we attribute to the presence of active regions co-rotating with the star.</p>
Age Dependence of the Occurrence and Architecture of Ultra-Short-Period Planet Systems (public data release)
<p>This file includes key data and column definitions for generating figures in the manuscript. The data were collected and processed from publicly available datasets, including Kepler DR25 and the planetary systems table (https://exoplanetarchive.ipac.caltech.edu/), LAMOST DR9 (https://www.lamost.org/), Gaia DR3 (https://gea.esac.esa.int/archive/), and The California-Kepler Survey (https://california-planet-search.github.io/cks-website/). Additional data required for the manuscript can also be obtained from these publicly available datasets.</p>
Opacities for atoms and molecules relevant to the spectra of hot rocky planets
<p>This dataset contains opacities for atoms and molecules that are relevant to the sector of hot rocky planets, such as magma ocean planets, post-giant impact atmospheres, or planets in ultra-short period orbits. These species can arise above a magma ocean with a composition specific to the continental crust or bulk silicate earth. We do not include opacities for major species that are not specific to hot rocky planet atmospheres, such as water, methane, carbon dioxide, ammonia, etc., as these can be found elsewhere, for example in datasets related to brown dwarf and hot Jupiter atmospheres. </p> <p>Most of the species included in this dataset can be seen in the attached plot, hot_spectra.pdf, which shows a secondary eclipse model of a lava planet and the contributions of individual species to this spectrum. The references for the line lists used to generate these opacities can be found in the file reference_table.pdf.</p> <p>Each *.zip file contains a set of 1060 opacity layers in ASCII format, each identified with the temperature and pressure it corresponds to. Each layer file contains a header showing the layer number, the temperature (in K), and pressure (in mbar). The data consists of to columns: wavelength in microns and opacity in cm<sup>2</sup>/molecule. The wavelength grid goes from 0.4 to 50 microns. A list of all the layers calculated for each molecule is given in the file layer_list.</p> <p><em>Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center.</em></p>
Plankton Planet Pilot Project rDNA 18S V9 OTU tables
<p>This repository contains the rDNA 18S V9 OTU table, its rarefied version, and the related contextual data from Plankton Planet Pilot Project.</p> <p>In the file <strong>P2_TO_18SV9_otu_table.tsv.gz</strong>, each OTU, one per row, is described by the following fields: <strong>amplicon</strong> = identifier of the representative (most abundant) sequence of the swarm; <strong>total</strong> = total number of reads in the entire dataset; <strong>cloud</strong> = number of unique sequences constituting the OTU; <strong>length</strong> = length of the representative sequence; <strong>spread</strong> = number of samples in which the OTU has been found; <strong>quality</strong> = minimum expected error observed for the representative sequence, divided by sequence length; <strong>sequence</strong> = nucleic acid sequence of the representative sequence; <strong>identity</strong> = percentage of identity of the representative sequence to the closest reference sequence from PR2_V9 (https://doi.org/10.5281/zenodo.3768951); <strong>references</strong> = best hit reference sequence(s); <strong>taxonomy</strong> = taxonomic path assigned to the representative sequence; <strong>taxogroup</strong> = high-taxonomic level assignation of the representative barcode; <strong>chloroplast</strong> = <em>yes</em>: presence of permanent chloroplast / <em>no</em>: absence of permanent chloroplast / <em>NA</em>: undetermined; <strong>symb_small</strong> = <em>parasite</em>: the species is a parasite / <em>commensal</em>: the species is a commensal / <em>mutualist</em>: the species is a mutualist symbiont, most often a microalgal taxa involved in photosymbiosis / <em>no</em>: the species is not involved in a symbiosis as small partner / <em>NA</em>: undetermined; <strong>symbiont_host</strong> = <em>photo</em>: the host species relies on a mutualistic microalgal photosymbiont to survive (obligatory photosymbiosis) / <em>photo_falc</em>: same as photo, but facultative relationship / <em>photo_klep</em>: the host species maintains chloroplasts from microalgal prey(s) to survive / <em>photo_klep_falc</em>: same as <em>photo_klep</em>, but facultative / <em>Nfix</em> = the host species must interact with a mutualistic symbiont providing N2 fixation to survive / <em>Nfix_falc</em> = same as Nfix, but facultative / <em>no</em>: the species is not involved in any mutualistic symbioses; <em>NA</em>: undetermined; <strong>silicification</strong> = <em>yes</em>: the species has a silicified skeleton / <em>no</em>: it does not / <em>NA</em>: undetermined; <strong>calcification</strong> = <em>yes</em>: the species has a calcified skeleton / <em>no</em>: it does not / <em>NA</em>: undetermined; <strong>strontification</strong> = <em>yes</em>: the species has a skeleton made of strontium / <em>no</em>: it does not / <em>NA</em>: undetermined; <strong>PPXXX</strong> = number of reads in each of the 214 Plankton Planet samples; <strong>TARA_XXXXXXXXXX</strong> = number of reads in each of the 386 <em>Tara</em> Oceans samples.</p> <p>The file <strong>P2_TO_18SV9_otu_table_raref_313539.tsv.gz</strong> contains the same fields but with number of reads (total and per sample) obtained after random subsampling (313,539 reads per sample).</p> <p>In the file <strong>P2_TO_18SV9_context.tsv.gz</strong>, each sample is described by the following fields: <strong>sample</strong> = identifier of the sample; <strong>lower_size_fraction</strong> = lower limit of the size fraction in µm; <strong>upper_size_fraction</strong> = lower limit of the size fraction in µm; <strong>event_date</strong> = date (year-month-day); <strong>event_latitude</strong> = geographic position (latitude in DD); <strong>event_longitude</strong> = geographic position (longitude in DD); <strong>depth</strong> = depth in meters; <strong>temperature</strong> = sea water temperature in °C</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.