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264 results for “Stellarator”
Pickled stellar photospheres (MARCS, Castelli & Kurucz) for Oracle
<p>These are just pickled photospheres from Castelli & Kurucz (2004) and MARCS (2011) for use with Oracle.</p>
Bayesian analysis of resolved stellar spectra: application to MMT/Hectochelle observations of the Draco dwarf spheroidal
<p>supplementary data products, including all sky-subtracted spectra from individual targets, as well as random draws from posterior PDFs for model parameters (see enclosed README file)</p>
Stellar model grid data for isochrones Python package
<p>These are the data files that get downloaded by the "isochrones" Python package. "mist.tgz" and "dartmouth.tgz" contain stellar model grid data for the MIST and Dartmouth stellar models (http://waps.cfa.harvard.edu/MIST/ and http://stellar.dartmouth.edu/models/). "dartmouth.tri" is the precomputed Delaunay triangulation for the Dartmouth models (the MIST models are too big to use the triangulation-based interpolation method).</p> <p>***Note***</p> <p>For the dartmouth grids here, this zenodo repository should now be used: https://zenodo.org/record/1002927.</p>
All Spectra Associated with "An Empirical Template Library of Stellar Spectra for a Wide Range of Spectral Classes, Luminosity Classes, and Metallicities Using SDSS BOSS Spectra"
<p>Zip files of all the individual SDSS BOSS spectra. They are sorted by metallicity, luminosity class and spectral type, where each zip file contains all the original SDSS spectra to be co-added into each template. The fits files are in the following format: The primary HDU contains comments about the right ascension, declination and other useful object information. The first table extension contains the spectrum information (wavelength, flux, inverse variance, etc.) The second table extension contains other parameter information (object type, flags, and more). </p> <p> </p>
The young massive SMC cluster NGC 330 seen by MUSE. III. Stellar parameters and rotational velocities - diagnostic plots
<p>This Zenodo repository hosts additional diagnostic plots for the article "<em>The young massive SMC cluster NGC 330 seen by MUSE. III. Stellar parameters and rotational velocities</em>" by Bodensteiner et al. 2023. It provides three diagnostic figures for each of the 282 stars in the sample described in the paper. Three example figures are given for one star (#654) in the Figures 2, 3, and 4 in the paper.</p> <p>Here, we provide a .zip archive with three additional figures for all other stars that are similar to the ones in the paper:</p> <ol> <li>the <strong>spectroscopic fit</strong> ("<em>id###_spec.pdf</em>"): Each panel, one for each of the six diagnostic spectral regions, shows the combined spectrum (black) and the best-fitting tlusty model (red). Grayed-out regions are only shown for comparison but were not included in the fit, which may vary from star to star.</li> <li>the <strong>photometric fit</strong> ("<em>id###_phot.pdf</em>"): The top panel shows a comparison between the observed HST fluxes (black crosses) and the flux (colored circles) computed from the best-fit model (gray line) by convolution with the HST filters (colored lines). The bottom panel gives residuals.</li> <li>the <strong>combined fit results</strong> ("<em>correlationplot_comb_id###.pdf</em>"): The diagonal gives the χ2-distribution as a function of each parameter and the panels below show 2-dimensional χ2 -maps. The red line marks the 95% confidence level.</li> </ol> <p>The star ids (###) correspond to the ones provided in Table 1 (also available at the CDS).</p>
AGN and stellar spectra used to produce model molecular emission lines
<p><span>Aiming to investigate the effects of stellar and AGN radiation fields to the excitation of molecular gas, we present an analysis of model CO, H</span><span><sub>2</sub>O, and OH<sup>+</sup> emission lines produced with the application of these radiation fields using MOLPOP-CEP. We find that the ratios of CO(J<sub>upp</sub>) = 11, 12, 13, 14, 15) to CO(J<sub>upp</sub>) = 1, 2, 3, 4, 5, 6, 7, 8) obtained with the application of AGN radiation are larger than the ones produced by applying stellar radiation. Similarly, some H<sub>2</sub>O and </span><span>OH<sup>+</sup> ratios obtained with AGN radiation are found to be higher than the corresponding ratios produced by applying stellar radiation field, making the line ratios a diagnostic tool to disentangle AGN from star formation. In all cases, we find that the ratios vary as a function of the molecular gas density and the scale of the radiation field, the larger the scale of the radiation field is the stronger the excitation of the molecular transitions. Also, the effect of the radiation fields is found to be dependent on the molecular gas density, indicating that the effect of the radiation fields is regulated by the physical properties that are intrinsic to the molecular gas. Thus, due to the dependency of the line ratios on the scale of the radiation fields and the effect of the radiation fields on the molecular gas density, we conclude that it is not sufficient to use a single line ratio to claim the presence of AGN contribution to the molecular gas excitation.</span></p>
Measuring the conditional luminosity and stellar mass functions of galaxies by combining the DESI LS DR9, SV3 and Y1 data
Open the record for dataset details and reuse information.
Data for paper "An asymptotic Grad-Shafranov equation for quasisymmetric stellarators"
Open the record for dataset details and reuse information.
The data and notebook for "Predicting the Slowing of Stellar Differential Rotation by Instability-Driven Turbulence"
<p>The data and Jupyter notebook for "Predicting the Slowing of Stellar Differential Rotation by Instability-Driven Turbulence."</p> <p><br><strong>Fig_6_code_implementation.ipynb</strong></p> <p>This notebook presents implementation of our closure model in python to predict turbulent transport for all $(r, \mathrm{Pr})$ in Fig. 6(a).</p> <p><br><strong>GSF_r_Pr_scan__Shear_eq_3.h5</strong></p> <p>This file contains data output from the $(r, \mathrm{Pr})$-scan of the closure model, obtained using "Fig_6_code_implementation.ipynb". The h5 data file can be simply read using the following lines of code:</p> <p><br><code>import h5py</code><br><code>hf=h5py.File('~/GSF_r_Pr_scan__Shear_eq_3.h5', 'r')</code><br><code>ux_uy = hf['ux_uy/ux_uy/ux_uy'][()]</code><br><code>ux_th = hf['ux_th/ux_th/ux_th'][()]</code></p> <p><code>Pr_exp = np.linspace(0.02, 7, 28)</code><br><code>Pr_array = 10**(-Pr_exp) #These are the values of Pr for which the transport is computed.</code></p> <p><code>r_exp = np.linspace(0.02, 5, 20)</code><br><code>r_array = 10**(-r_exp) #These are the values of r for which the transport is computed.</code><br><br></p> <p> </p> <blockquote> <p>Authors:</p> <p><strong>B. Tripathi<br></strong>Department of Physics, University of Wisconsin--Madison, Madison, Wisconsin 53706, USA<br>ORCID : 0000-0002-4723-2170<br>Email : btripathi@wisc.edu</p> <p><strong>A.J. Barker</strong><br>Department of Applied Mathematics, School of Mathematics, University of Leeds, Leeds LS2 9JT, UK<strong><br></strong>ORCID : 0000-0003-4397-7332<br>Email : A.J.Barker@leeds.ac.uk</p> <p><strong>A.E. Fraser<br></strong>Department of Applied Mathematics, University of Colorado, Boulder, Colorado 80309, USA<br>Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA<br>Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, Colorado 80309, USA<br>ORCID : 0000-0003-4323-2082</p> <p><strong>P.W. Terry<br></strong>Department of Physics, University of Wisconsin--Madison, Madison, Wisconsin 53706, USA<br>ORCID : 0000-0002-4981-9637</p> <p><strong>E.G. Zweibel<br></strong>Department of Physics, University of Wisconsin--Madison, Madison, Wisconsin 53706, USA<br>Department of Astronomy, University of Wisconsin--Madison, Madison, Wisconsin 53706, USA<br>ORCID : 0000-0003-4821-713X</p> </blockquote>
Supporting data for "A method for non-linear inversion of the stellar structure applied to gravity-mode pulsators"
<p>These are the inlist and run_star_extras required to reproduce the stellar and asteroseismic models presented in 'A method for non-linear inversion of the stellar structure applied to gravity-mode pulsators', run with MESA r22.05.1.</p>
Supplementary material for "Stellar flare morphology with TESS across the main sequence"
<p>Online material for the paper titled "Stellar flare morphology with TESS across the main sequence". The dataset includes the manually flagged TESS light curves used to train the <em>flatwrm2</em> flare detection algorithm (<a href="https://github.com/vidakris/flatwrm2" target="_blank" rel="noopener">https://github.com/vidakris/flatwrm2</a>), the final manually vetted flare catalog, the extracted flare profiles, and Jupyter notebooks demonstrating how the data can be used.</p> <h2>Files</h2> <ul> <li><strong>flatwrm2_training_set.tar.gz</strong>: TESS 2-min cadence light curves used to train <em>flatwrm2</em> for flare detection. All files contain three columns, time in TBJD, PDCSAP flux, and a 1/0 flag for flare/not flare. Files are sorted into three directories:<br> <ul> <li>active_stars: Selected active stars up to sector 40 for the original training set of <em>flatwrm2</em>, 208 light curves.</li> <li>random_sample: Random stars up to sector 40 for the original training set of <em>flatwrm2</em>, 8000 light curves. Only a small fraction of them is flaring.</li> <li>new_selection: New selection of stars up to sector 69, 4631 light curves. It includes flaring and non-flaring stars, and also known astrophysical false positives (e.g., RR Lyrae stars). See Sect. 2.2 of the paper for details.</li> </ul> </li> <li><strong>Table2_flaring_star_catalog.csv</strong>: Catalog of flaring stars (Table 2 in the paper)</li> <li><strong>Table3_flare_catalog.csv</strong>: TESS flare catalog, including only the correctly extracted flares, with the same length as TESS_flare_shapes.dat (Table 3 in the paper)</li> <li><strong>Table3_flare_catalog_not_extracted.csv</strong>: Continuation of the TESS flare catalog, including only the incorrectly extracted flares (Table 3 in the paper). As most calculated parameters are probably erroneous, only the flare peak times are reported.</li> <li><strong>TESS_flare_shapes.dat</strong>: Scaled and interpolated TESS flare shapes, one flare profile for each entry in Table3_flare_catalog.csv</li> <li><strong>TESS_original_flare_shapes_time.dat</strong>: Times for the scaled, but not interpolated flares</li> <li><strong>TESS_original_flare_shapes_flux.dat</strong>: Fluxes for the scaled, but not interpolated flares</li> <li><strong>Table6_solar_flare_catalog.csv</strong>: Solar flare parameters from SDO/EVE (Table 6 in the paper). <em>Note:</em> the SDO/EVE data products have a version number in the URL. We used version 7 for the analysis, but it can change after major updates in the SDO data processing pipeline. Please change the URL accordingly, if you have issues accessing the data (e.g., 007 --> 008).</li> <li><strong>solar_flare_shapes.dat</strong>: Scaled and interpolated solar flare profiles from SDO/EVE, one flare profile for each entry in Table6_solar_flare_catalog.csv</li> <li><strong>01_Loading_data.ipynb</strong>: A Jupyter notebook demonstrating how the above datasets can be used</li> <li><strong>02_Sampling_flare_shapes.ipynb</strong>: A Jupyter notebook demonstrating how flare shapes can be sampled (Sect. 4.2 in the paper)</li> <li><strong>03_Locating_similar_flares.ipynb</strong>: A Jupyter notebook demonstrating how flares similar to an input shape can be located in the catalog (Sect. 4.3 in the paper)</li> </ul>
Table A.3: New stellar multiple systems proposed
Open the record for dataset details and reuse information.
The Demographics of Giant Exoplanets and Brown Dwarfs in Wide Stellar Binaries
<p>While numerous exoplanets have now been uncovered in stellar binaries, the impact of companion stars on planet formation and evolution is still not understood. In this talk, I will present results of population trends seen among the known sample of planets in wide multiple star systems, which allows us to investigate the effects of stellar binarity on the resulting planetary architectures. In particular, observations of stars hosting close-in giant planets and brown dwarfs find an excess of binary companions on few hundred AU separations, and different planet demographics for these systems, suggesting that such binaries may provide favourable conditions for the formation of the observed inner companions. I will show results from simulations of self-gravitating protoplanetary disks adapted to binary-star environments, which show that certain binary configurations may trigger gravitational fragmentation and lead to the formation of giant planets in otherwise-stable disks.</p>
Stellar triples on the edge
<p>This is a basic reproduction package for the paper "Stellar triples on the edge -- Comprehensive overview of the evolution of destabilised triples leading to stellar and binary exotica" by Toonen et al. 2021. It aims to provide the most important data products to check and reproduce the main results of the paper. </p>
CODEX multiplexed imaging cell datasets used for using STELLAR to transfer cell type annotations to other tissues and donors
<p>We performed CODEX (co-detection by indexing) multiplexed imaging on 24 sections of the human intestine from 3 donors (B004, B005, B006) using a panel of 47 oligonucleotide-barcoded antibodies. We also performed CODEX imaging on both human tonsil and Barrett's esophagus (BE) using a panel of 57 oligonucleotide-barcoded antibodies. Subsequently images underwent standard CODEX image processing (tile stitching, drift compensation, cycle concatenation, background subtraction, deconvolution, and determination of best focal plane), single cell segmentation, and column marker z-normalization by tissue. Output of this process were dataframes of 870,000 cells and 220,000 cells respectively with fluorescence values quantified from each marker.</p>
Stellar Archaeology with the NOT
<p>Stellar archaeology seeks to use information gathered from old, metal-poor stars (pop II stars) in the Milky Way and its satellites to place constraints on the first generation of stars to form in the Universe (pop III stars), which we can no longer directly observe. I will present the results of two observing campaigns carried out with the NOT (and other similar sized telescopes). The first project aims to determine the binary nature of a sample of chemically peculiar metal-poor stars. When using the abundance pattern of metal-poor stars to investigate nucleosynthesis channels in the early Universe, it is vital to verify that the abundances reflect the star's birth cloud and have not been altered by mass transfer from a binary companion. To this end, we monitored a sample of 63 stars over eight years with the NOT collecting over 900 FIES spectra. Resulting in binary frequencies being determined for three types of chemically peculiar stars; CEMP-s, CEMP-no, and r-process enhanced stars. The second campaign is part of the R-Process Alliance (RPA) which seeks to constrain the nature and astrophysical site of the rapid neutron-capture process. The first phase of this project focuses on increasing the sample of metal-poor stars exhibiting large enhancement in r-process elements for which detailed abundances can be derived. </p>
Evolutionary tracks accompanying Stellar Evolution in Real Time II (1/4)
<p>Evolutionary tracks generated with MESA accompanying the project ``Stellar Evolution in Real Time II: R Hydrae and an Open-Source Grid of >3000 Seismic TP-AGB Models Computed with MESA'' ApJ, 2024</p> <p>Due to data volume, this is one of four Zenodo repositories associated to this project. The full list of related dataset DOIs is:</p> <ul> <li>https://doi.org/10.5281/zenodo.11280179</li> <li>https://doi.org/10.5281/zenodo.11282597</li> <li>https://doi.org/10.5281/zenodo.11353933</li> <li>https://doi.org/10.5281/zenodo.11357395</li> </ul> <p><strong>Details on archive files:</strong></p> <p>All phase 1 and phase 2 evolutionary tracks are contained in the files</p> <p>ZAMS_to_TCHeB_y-fixed.tar.gz<br>TCHeB_to_AGB_y-fixed.tar.gz<br>ZAMS_to_TCHeB_y-varied.tar.gz<br>TCHeB_to_AGB_y-varied.tar.gz</p> <p>sorted by whether a varied or static helium assumption was used.</p> <p>To use the smallest number of separate Zenodo listings possible, not all data are grouped in the same way.</p> <p>The tar.gz archive files labeled with a string of the form "AGB_to_end_M1.XX_y-fixed.tar.gz" include all models having a mass beginning with 1 (1.00, 1.10, 1.20, etc) and adopting the fixed helium assumption.</p> <p>Archive files labeled in the form "AGB_to_end_M1.XX_y-varied.tar.gz" include the same, but using the helium-varied assumption. </p> <p>Archive files labeled with a string of the form "AGB_to_end_M3.10_all.tar.gz" include both the fixed-helium and varied-helium tracks for all masses that start with 3 (3.00, 3.10, 3.20, etc).</p> <p> </p> <p><strong>Details on files unpacked from archives:</strong></p> <div>Every unpacked file has a name of the form </div> <div> </div> <div>history_m4.90_z0.0060_y0.261_eta0.01_yi-on_seismic_p3.data</div> <div> </div> <div>Anything that starts with "history" and ends with ".data" is an evolutionary track. Tracks that have "_p3" are the third phase: AGB to end (or failure of the model) and these files are large.</div> <div> </div> <div>Tracks that have "_p1" are the evolution from the zero-age main sequence (ZAMS) to the terminal age core helium burning (TCHeB). Tracks that have "_p2" evolve from TACHeB to the onset of the asymptotic giant branch (AGB).<br><br>In the file name, the two-decimal number after m, four-decimal number after z and 3-decimal number after y encode the evolutionary track's initial mass, initial metallicity (Z) and initial helium abundance (Y), respectively. In cases where there is no y value provided, the helium abundance is fixed as described in the paper. </div> <div> </div> <div>When the file name contains "yi-on" in the name, it means the helium-varied assumption was used. When the file contains "seismic" (should only be the case for p3's), it means the GYRE calculations are included in the output. </div>
Dataset from: Electron root optimisation for stellarator reactor designs
<p>In this work, we propose a method of optimising stellarator devices to favour the presence of an electron root solution of the radial electric field. Such a solution can help avoid heavy impurity accumulation, improve neoclassical thermal ion confinement and helium ash exhaust, and possibly reduce turbulence. This study shows that an optimisation for such a root is possible in quasi-isodynamic stellarators. Examples are shown for both vacuum and finite plasma pressure configurations.</p>
Evolutionary tracks accompanying Stellar Evolution in Real Time II (4/4)
<p>Evolutionary tracks generated with MESA accompanying the project <br>``Stellar Evolution in Real Time II: R Hydrae and an Open-Source Grid of >3000 Seismic TP-AGB Models Computed with MESA'' ApJ 2024</p> <div> <div> <div> <p>Due to data volume, this is one of four Zenodo repositories associated to this project. The full list of related dataset DOIs is:</p> <ul> <li>https://doi.org/10.5281/zenodo.11280179</li> <li>https://doi.org/10.5281/zenodo.11282597</li> <li>https://doi.org/10.5281/zenodo.11353933</li> <li>https://doi.org/10.5281/zenodo.11357395</li> </ul> <p><strong>Details on archive files:</strong></p> <p>All phase 1 and phase 2 evolutionary tracks are contained in the files</p> <p>ZAMS_to_TCHeB_y-fixed.tar.gz<br>TCHeB_to_AGB_y-fixed.tar.gz<br>ZAMS_to_TCHeB_y-varied.tar.gz<br>TCHeB_to_AGB_y-varied.tar.gz</p> <p>sorted by whether a varied or static helium assumption was used.</p> <p>To use the smallest number of separate Zenodo listings possible, not all data are grouped in the same way.</p> <p>The tar.gz archive files labeled with a string of the form "AGB_to_end_M1.XX_y-fixed.tar.gz" include all models having a mass beginning with 1 (1.00, 1.10, 1.20, etc) and adopting the fixed helium assumption.</p> <p>Archive files labeled in the form "AGB_to_end_M1.XX_y-varied.tar.gz" include the same, but using the helium-varied assumption. </p> <p>Archive files labeled with a string of the form "AGB_to_end_M3.10_all.tar.gz" include both the fixed-helium and varied-helium tracks for all masses that start with 3 (3.00, 3.10, 3.20, etc).</p> <p> </p> <p><strong>Details on files unpacked from archives:</strong></p> <div>Every unpacked file has a name of the form </div> <div> </div> <div>history_m4.90_z0.0060_y0.261_eta0.01_yi-on_seismic_p3.data</div> <div> </div> <div>Anything that starts with "history" and ends with ".data" is an evolutionary track. Tracks that have "_p3" are the third phase: AGB to end (or failure of the model) and these files are large.</div> <div> </div> <div>Tracks that have "_p1" are the evolution from the zero-age main sequence (ZAMS) to the terminal age core helium burning (TCHeB). Tracks that have "_p2" evolve from TACHeB to the onset of the asymptotic giant branch (AGB).<br><br>In the file name, the two-decimal number after m, four-decimal number after z and 3-decimal number after y encode the evolutionary track's initial mass, initial metallicity (Z) and initial helium abundance (Y), respectively. In cases where there is no y value provided, the helium abundance is fixed as described in the paper. </div> <div> </div> <div>When the file name contains "yi-on" in the name, it means the helium-varied assumption was used. When the file contains "seismic" (should only be the case for p3's), it means the GYRE calculations are included in the output. </div> </div> <p> </p> </div> <p> </p> </div>
Evolutionary tracks accompanying Stellar Evolution in Real Time II (3/4)
<p>Evolutionary tracks generated with MESA accompanying the project <br>``Stellar Evolution in Real Time II: R Hydrae and an Open-Source Grid of >3000 Seismic TP-AGB Models Computed with MESA'' ApJ 2024</p> <div> <div> <p>Due to data volume, this is one of four Zenodo repositories associated to this project. The full list of related dataset DOIs is:</p> <ul> <li>https://doi.org/10.5281/zenodo.11280179</li> <li>https://doi.org/10.5281/zenodo.11282597</li> <li>https://doi.org/10.5281/zenodo.11353933</li> <li>https://doi.org/10.5281/zenodo.11357395</li> </ul> <p><strong>Details on archive files:</strong></p> <p>All phase 1 and phase 2 evolutionary tracks are contained in the files</p> <p>ZAMS_to_TCHeB_y-fixed.tar.gz<br>TCHeB_to_AGB_y-fixed.tar.gz<br>ZAMS_to_TCHeB_y-varied.tar.gz<br>TCHeB_to_AGB_y-varied.tar.gz</p> <p>sorted by whether a varied or static helium assumption was used.</p> <p>To use the smallest number of separate Zenodo listings possible, not all data are grouped in the same way.</p> <p>The tar.gz archive files labeled with a string of the form "AGB_to_end_M1.XX_y-fixed.tar.gz" include all models having a mass beginning with 1 (1.00, 1.10, 1.20, etc) and adopting the fixed helium assumption.</p> <p>Archive files labeled in the form "AGB_to_end_M1.XX_y-varied.tar.gz" include the same, but using the helium-varied assumption. </p> <p>Archive files labeled with a string of the form "AGB_to_end_M3.10_all.tar.gz" include both the fixed-helium and varied-helium tracks for all masses that start with 3 (3.00, 3.10, 3.20, etc).</p> <p> </p> <p><strong>Details on files unpacked from archives:</strong></p> <div>Every unpacked file has a name of the form </div> <div> </div> <div>history_m4.90_z0.0060_y0.261_eta0.01_yi-on_seismic_p3.data</div> <div> </div> <div>Anything that starts with "history" and ends with ".data" is an evolutionary track. Tracks that have "_p3" are the third phase: AGB to end (or failure of the model) and these files are large.</div> <div> </div> <div>Tracks that have "_p1" are the evolution from the zero-age main sequence (ZAMS) to the terminal age core helium burning (TCHeB). Tracks that have "_p2" evolve from TACHeB to the onset of the asymptotic giant branch (AGB).<br><br>In the file name, the two-decimal number after m, four-decimal number after z and 3-decimal number after y encode the evolutionary track's initial mass, initial metallicity (Z) and initial helium abundance (Y), respectively. In cases where there is no y value provided, the helium abundance is fixed as described in the paper. </div> <div> </div> <div>When the file name contains "yi-on" in the name, it means the helium-varied assumption was used. When the file contains "seismic" (should only be the case for p3's), it means the GYRE calculations are included in the output. </div> </div> <p> </p> </div>
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.