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264 results for “Stellarator”
Investigating the asymmetry of young stellar outflows: A combined MUSE-X-Shooter study of the Th 28 jet
<h3>This record contains supplementary tables and figures for the article <em>'Investigating the asymmetry of young stellar outflows: A combined MUSE-X-Shooter study of the Th 28 jet' </em>by A. Murphy, E. T. Whelan, F. Bacciotti, D. Coffey, F. Comeron, J. Eisloffel, B. Nisini, S. Antoniucci, J. M. Alcala and T. P. Ray, accepted for publication by Astronomy & Astrophysics.</h3> <p> </p> <p><strong>Abstract: </strong></p> <p>Characterising stellar jet asymmetries is key to providing robust constraints for jet launching models, and hence to understanding the underlying mechanisms of jet launching. This study aims to characterise the asymmetric properties of the bipolar jet from the Classical T Tauri Star Th 28. We combine data from integral field spectroscopy with VLT/MUSE and high-resolution spectra from VLT/X-Shooter to map optical emission line ratios in both jet lobes. We carry out a diagnostic analysis of these ratios to compare the density, electron temperature, and ionisation fraction within both lobes. The mass accretion rate is derived from the emission lines at the source, and compared with the mass outflow rate derived in both lobes using the estimated densities and measured [O I]λ6300 and [S II]λ6731 luminosities. The blue-shifted jet shows a significantly higher electron temperature and moderately higher ionisation fraction than the red-shifted jet. In contrast to previous studies we also estimate higher densities n H in the blue-shifted jet by a factor ∼2. These asymmetries are traced to within 1′′ (160 au) of the source in the line ratio maps. We find Ṁacc = 2.4 × 10^−7 M⊙ yr ^−1 , with an estimated obscuration factor of ∼54 due to grey scattering around the star. Estimated values of Ṁout range between 0.66 – 13.7 × 10^−9 M⊙ yr^−1 in the blue-shifted jet and 5-9 × 10^−9 M⊙ yr^−1 in the red-shifted jet.<em> </em>The emission line maps and diagnostic results suggest that the jet asymmetries originate close to the source and are likely intrinsic to the jet. Furthermore, the combined dataset allows access to a broad array of accretion tracers. This in turn enables a more accurate estimation of the mass accretion rate, revealing Ṁacc higher by a factor > 350 than would otherwise be determined.</p> <p> </p> <p><strong>Summary of supplemental material:</strong></p> <p>Table 1: Emission lines detected in X-shooter observations of the jet. Fluxes are measured from the red-shifted jet lobe.</p> <p>Tables 2 and 3: Mass accretion rates measured from MUSE and X-Shooter observations of Th 28, respectively, assuming an on-source extinction of 2.5 mags.</p> <p>Tables 4 and 5: As in Tables 2 and 3, for an on-source extinction of 1.26 mags.</p> <p>Figures 1-4: Position-velocity maps of detected emission lines from the UV and VIS arms of the X-shooter observations.</p> <p>Figure 5: Accretion luminosities measured from MUSE and X-Shooter data, before and after correction for on-source obscuration. Left and right panels show the corresponding values if the fluxes are corrected for a wavelength-dependent extinction of 2.5 and 1.26 mags, respectively.</p> <div> </div> <div> </div>
Stellar mass and star formation rate within a billion light-years
<p>Tables 1-5 of the paper entitled "Stellar Mass and Star Formation Rate within a Billion Light-Years" are available in machine readable format, together with a ReadMe file in CDS format. The python script loads Table 5 and displays the stellar mass density inferred in a volume of 200 Mpc size. Interactive versions of the six figures shown in Appendix C of the above mentioned article are also available in html format, as generated from a similar script.</p>
The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines
<p>Spectral models of M_ZAMS = 12, 15, 19, 25 Msun progenitors, all epochs.</p>
Stellar
<h1>Stellar (The Manifold Page) Archive</h1> <p>This is an archive of the mathematical research work by <a href="https://www3.math.tu-berlin.de/IfM/Nachrufe/Frank_Lutz/stellar/">Frank H. Lutz</a>. In the current version of this resource, we preserve all triangulations of 2-manifolds and 3-manifolds in <em>mixed lexicographic format</em>. In this version, a new set of simplicial manifolds with small valence (4787 triangulations) has been added.</p> <h3>Major changes</h3> <p>We kept all files as-is, except for keeping an uncompressed copy of the file <code>3_manifolds_10_all.txt.gz</code>, which is now named <code>3_manifolds_10_all.txt</code>. We also added a new file <code>manifolds_lex_d3_deg5_hom.txt</code>, which contains the homology groups (including torsion coefficients) of simplicial manifolds with small valence (4787 triangulations). This file was <strong>not</strong> present in the original archive.</p> <h3>Minor changes</h3> <ul> <li>The syntax of the file <code>manifolds_lex_d3_deg5.txt</code> was fixed to be consistent with the syntax in the order files. This required changing 26 line endings, in which a closing "]" was on a line of its own, to line endings of the form "]]". This change has no bearing on the triangulation as such but it simplifies parsing the format.</li> <li>The syntax of the file <code>2_manifolds.txt</code> was fixed. Two manifolds, <code>manifold_2_15_2_2</code> and <code>manifold_2_15_1_1</code>, were violating the format by being stored without a separating newline. This change has no bearing on the the triangulations as such but it simplifies parsing the format.</li> </ul>
Daset from the paper "Compact object mergers: exploring uncertainties from stellar and binary evolution with SEVN"
<p>This repository contains the dataset produced by the population-synthesis code SEVN for the paper:<br> "Compact object mergers: exploring uncertainties from stellar and binary evolution with SEVN"</p> <p>In this paper, we exploit the SEVN code (publicly available at <a href="https://gitlab.com/sevncodes/sevn">https://gitlab.com/sevncodes/sevn</a>) to analyse the formation and properties of binary compact objects.</p> <p>The repository also includes the initial condistions used as input and the SEVN version used to run the simulations.</p> <p>#Content</p> <p>The repository contains the following folders:</p> <p>- data_from_simulations: the folder contains all the data produced by the simulations and used in the Iorio+22 paper<br> - InitialConditions: the folder contains all the intial conditions (and the code to generate them) that have been used for the Iorio+22 paper<br> - SEVN_iorio22: this folder contains the version of the SEVN code that has been used to run the simulations in the Iorio+22 paper</p> <p>Each folder contains a specific README with additional information</p> <p> </p> <p>#Contatcts</p> <p>giuliano.iorio.astro@gmail.com</p> <p> </p> <p> </p>
Inputs and Outputs for paper The DESC Stellarator Code Suite Part I: Quick and accurate equilibria computations
<p>Contains the DESC and VMEC input and output files used in the paper, as well as the plotting scripts used to create the figures in the paper (Current with the <a href="https://arxiv.org/abs/2203.17173">arxiv Mar 31 2023 version</a>):</p> <p> </p> <p>3D equilibrium codes are vital for stellarator design and operation, and high-accuracy equilibria are also necessary for stability studies. This paper details comparisons of two 3D equilibrium codes, VMEC, which uses a steepest-descent algorithm to reach a minimum-energy plasma state, and DESC, which minimizes the MHD force error in real space directly. Accuracy as measured by final plasma energy and satisfaction of MHD force balance, as well as other metrics, will be presented for each code, along with the computation time. It is shown that DESC is able to achieve more accurate solutions, especially near-axis. DESC's global Fourier-Zernike basis also yields the solution everywhere in the plasma volume, not just on discrete flux surfaces. Further, DESC can compute the same accuracy solution as VMEC in an order of magnitude less time.</p> <p> </p> <p>Updated dataset for better readability 5-5-23</p>
Combined Effects of Rotation and Age Spreads on Extended Main-Sequence Turn Offs - Isochrones and Stellar Tracks
<p>Theoretical isochrones and EEP stellar tracks featured in <a href="https://ui.adsabs.harvard.edu/abs/2019ApJ...887..199G/abstract">Gossage et al. 2019</a> (Combined Effects of Rotation and Age Spreads on Extended Main-Sequence Turn Offs). These 1D stellar evolution models are based on <a href="https://docs.mesastar.org/en/release-r22.11.1/">MESA</a> r7503, and utilize the same physical assumptions as in MIST v1.0 (<a href="https://ui.adsabs.harvard.edu/abs/2016ApJ...823..102C/abstract">Choi et al. 2016</a>).</p> <p>The models are described in <a href="https://ui.adsabs.harvard.edu/abs/2018ApJ...863...67G/abstract">Gossage et al. 2018</a> and <a href="https://ui.adsabs.harvard.edu/abs/2019ApJ...887..199G/abstract">Gossage et al. 2019</a>\(^1\), but salient features include:</p> <ul> <li>Metallicities [Fe/H] = -0.45, -0.30, -0.15, 0.0, 0.15, 0.30, 0.45 (assuming <a href="https://ui.adsabs.harvard.edu/abs/2009ARA%26A..47..481A/abstract">Asplund et al. 2009</a> protosolar abundances \(\rm Z_{\odot}\) = 0.0142).</li> <li>Rotation rates from v/v<sub>crit </sub>= 0.0, 0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8, 0.9 (initiated at ZAMS)</li> <li>Masses from 0.1 to 8 solar masses with spacings of: <ul> <li>\(\rm \Delta M = 0.05 M_{\odot}\) for \(\rm M < 1 M_{\odot}\)</li> <li>\(\rm \Delta M = 0.04 M_{\odot}\) for \(\rm 1 M_{\odot} \leq M < 2 M_{\odot}\)</li> <li>\(\rm \Delta M = 0.2 M_{\odot}\) for \(\rm 2 M_{\odot} \leq M \leq 8 M_{\odot}\)</li> </ul> </li> <li>Models are evolved up to the first thermal pulse.</li> </ul> <p><strong>File name convention:</strong> zip files, e.g., \(\texttt{MIST_v1.0_feh_p0.15_rotating_tracks.zip}\), contain theoretical models at a particular metallcity ([Fe/H] = 0.15 in this case), at all rotation rates and masses. The file \(\texttt{MIST_v1.0_feh_m0.15_rotating_tracks.zip}\) contains models at [Fe/H] = -0.15, and so on. \(\texttt{*_tracks.zip}\) contain EEP stellar track files and \(\texttt{*_isochrones.zip}\) files contain theoretical isochrone files, both in the same format as EEP track and theoretical isochrones found on the <a href="https://waps.cfa.harvard.edu/MIST/index.html">MIST website</a>. Zip files labeled, e.g.,\(\texttt{*_isochrones_FILTERSET.zip}\) contain observable isochrones, with synthetic photometry produced for a particular filter set (as on the <a href="https://waps.cfa.harvard.edu/MIST/model_grids.html">MIST packaged grids</a> site, which contains more information on the filter sets), computed without extinction (\(A_V=0\)). At the moment, filter sets for \(\texttt{UBVRIplus}\) (containing Gaia filters), \(\texttt{HST_WFC3}\), \(\texttt{HST_ACSWF}\), \(\texttt{HST_WFPC2}\), and \(\texttt{CFHTugriz}\) are included, but more can be added upon request\(^2\). </p> <p><strong>Notes:</strong></p> <p>\(^1\) These are the same models as featured in <a href="https://ui.adsabs.harvard.edu/abs/2018ApJ...863...67G/abstract">Gossage et al. 2018</a>, but in that work, [Fe/H] = -0.60 and -0.75 were featured as well and only included models up to v/v<sub>crit </sub>= 0.6. We include these models from <a href="https://ui.adsabs.harvard.edu/abs/2018ApJ...863...67G/abstract">Gossage et al. 2018</a> here as well. Models at [Fe/H] = -0.60 have been extended to v/v<sub>crit </sub>= 0.9, while [Fe/H] = -0.75 only includes up to the original v/v<sub>crit </sub>= 0.6.</p> <p>\(^2\) These tracks and isochrones may be converted into observable tracks and isochrones (w/ gravity darkening effects if desired) via Aaron Dotter's <a href="https://github.com/aarondotter/iso">iso code</a>.</p> <p>\(^3\) Although astroseismic \(\nu_{max}\) and \(\Delta \nu\) are included in the included history files, be aware that these are based on scaling relations reliant on solar values, assuming the Coriolis and centrifugal forces do not play a role. While an OK assumption for the Sun, this is less applicable models with rapid rotation and their values should not be trusted in such regimes.</p>
Spatially resolved mock observations of stellar kinematics: full radiative transfer treatment of the simulated galaxies of the Auriga project
<p>We present realistic mock spectroscopic observations for state-of-the-art hydrodynamical simulations, using high spectral resolution stellar population models (FSPS) and full radiative transfer treatment with SKIRT. The dataset contains IFS-like spectroscopy of the stellar continuum for 10 (of the 30) galaxies in the Auriga Project at z=0. One galaxy at z=0.8 (Au 6) and another at z=3 (Au 29).</p>
Stellar Density Profiles of Dwarf Spheroidal Galaxies - Posterior Distributions
<p>This archive contains samples from the posterior distributions of our 3-plummer, 1-plummer, 3-steeper and 1-steeper fits for 40 dwarf spheroidal galaxies as described in "Stellar Density Profiles of Dwarf Spheroidal Galaxies" (<a href="https://arxiv.org/abs/1910.10134">https://arxiv.org/abs/1910.10134</a>)</p>
All Luminosity Templates Associated with "Classifying Single Stars and Spectroscopic Binaries Using Optical Stellar Templates"
<p>Zip files for the luminosity normalized individual stellar templates, and all combinations of SB2 templates. The templates are in fits format. The first table extension contains the template (wavelength, luminosity, variance, error). These luminosity templates have units of erg /s /angstrom.</p>
Dataset from: Fallback Supernova Assembly of Heavy Binary Neutron Stars and Light Black Hole-Neutron Star Pairs and the Common Stellar Ancestry of GW190425 and GW200115
<p>The results of the simulations shown in "Fallback Supernova Assembly of Heavy Binary Neutron Stars and Light Black Hole-Neutron Star Pairs and the Common Stellar Ancestry of GW190425 and GW200115" (<a href="https://arxiv.org/abs/2106.12381">arXiv:2106.12381</a>).</p> <p>Contents:</p> <ol> <li>Run_Details_COMPAS</li> <li>COMPAS_Output_*.hdf5</li> <li>MESA.zip</li> <li>GADGET.zip</li> </ol> <p>If you use any of these data please kindly include a citation to:<br> Alejandro Vigna-Gómez <em>et al</em> 2021 <em>ApJL</em> <strong>920</strong> L17 <a href="https://iopscience.iop.org/article/10.3847/2041-8213/ac2903">doi:10.3847/2041-8213/ac2903</a></p> <p>If you use the MESA profile or history files please also cite:</p> <p>Aguilera-Dena, D.R., et al., in prep.</p> <p>Additionally, we point the reader towards the following GitHub repositories:<br> 1) <a href="https://github.com/aldobatta/fallback-supernova">aldobatta/fallback-supernova</a><br> 2) <a href="https://github.com/avigna/heavy-BinaryNeutronStars">avigna/heavy-BinaryNeutronStars</a></p>
Stellar Model Isochrone data
<p>Stellar model isochrone data that is downloaded and used by the 'isochrones' python module. Data come from the Dartmouth, Padova, and BASTI stellar model grids.<br /> </p>
A modular set of synthetic spectral energy distributions for young stellar objects - Robitaille (2017) - v1.1
<p>These are the models released with the following publication:</p> <p><em>A modular set of synthetic spectral energy distributions for young stellar objects</em>, Robitaille (2017)</p> <p>A companion repository is available on GitHub:</p> <p>https://github.com/hyperion-rt/paper-2017-sed-models</p> <p>In particular, a notebook is provided, demonstrating how the models here can be used:</p> <p>https://github.com/hyperion-rt/paper-2017-sed-models/blob/master/notebook/using_the_models.ipynb</p> <p><strong>Note:</strong> the files here do not include polarization results, nor do they include the SEDs split by components (e.g. scattered versus direct light). The raw Hyperion output files which contain this information will be made available at a later date, and a link will be provided here.</p> <p>For <strong>announcements</strong> of new versions of these models, you can subscribe to the following mailing list:</p> <p>https://groups.google.com/forum/#!forum/protostars</p> <p>For <strong>questions or issues</strong> using these models, you can open a GitHub issue in the companion repository:</p> <p>https://github.com/hyperion-rt/paper-2017-sed-models/issues/new</p> <p><strong>MacOS X users:</strong> there is a bug in the bundled version of tar in MacOS X that causes issues when expanding some of the largest files here (this results in the <em>flux.fits</em> file being empty). To avoid this, you can use the GNU tar version which can be installed e.g. with Homebrew using <em>brew install gnu-tar</em> then using the <em>gtar</em> command instead of <em>tar</em>.</p>
Empirical Stellar Templates 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>This is the dataset of empirical stellar templates associated with the publication "An Empirical Template Library of Stellar Spectra for a Wide Range of Spectral Classes, Luminosity Classes, and Metallicities Using SDSS BOSS Spectra", which has been accepted for publication in the Astrophysical Journal Supplements. </p>
Photometric Activity Cycles in fast-rotating stars: Revisiting the reality of stellar activity cycle branches
<p>The provided files comprise the tables and Activity cycle fits presented in our manuscript titled "Photometric Activity Cycles in fast-rotating Stars". The files are denoted as Table 1 (main-sequence stars), Table 2 (RS CVn candidates) and a folder containing activity cycle fits for all main-sequence and RSCVn candidates listed in the aforementioned tables. DOI: <a href="https://doi.org/10.1093/mnras/staf754" target="_blank" rel="noopener">10.1093/mnras/staf754</a> </p>
A Possible Mechanism for "Late Phase" in Stellar White-Light Flares
<p>This is the simulation data used for the paper "A Possible Mechanism for 'Late Phase' in Stellar White-Light Flares" that was accepted for publication on ApJ.</p>
Data for section 3.2 of Stellar Population Properties in the Stellar Streams Around SPRC047
<p>Supplementary (input and output) data for Section 3.2 ("<em>Measurement Uncertainties in the Deconvolved Image</em>") of the paper "<em>Stellar Population Properties in the Stellar Streams Around SPRC047</em>", accepted for publication in ApJ and available in <a href="https://arxiv.org/abs/2312.05358" target="_blank" rel="noopener">arXiv:2312.05358.</a> The source code for this project is publicly available <a href="https://gitlab.com/makhlaghi/sprc047-stream-clumps-photometry" target="_blank" rel="noopener">on Gitlab</a> and is archived on<a href="https://archive.softwareheritage.org/swh:1:dir:882514891cdcfc08261409352437bc6b8a836b8b;origin=https://gitlab.com/makhlaghi/sprc047-stream-clumps-photometry;visit=swh:1:snp:11cb02c374d7856028c57fb7312b60531f1be2e6;anchor=swh:1:rev:5d81b833931e58732627c06998c2488e6d2a8fb7" target="_blank" rel="noopener"> SoftwareHeritage</a> for longevity.</p> <p>A brief description of the contents in this repository are given below. Note that because the AWMLE deconvolution code is not yet publicly released, the second two files below are necessary (they are used by the reproducible Makefile of this section <a href="https://gitlab.com/makhlaghi/sprc047-stream-clumps-photometry" target="_blank" rel="noopener">on Gitlab</a>).</p> <ul> <li><a href="../records/10397812/files/sprc047_3.6um-bck.fits?download=1">sprc047_3.6um-bck.fits</a>: Spitzer image of SPRC047.</li> <li><a href="../records/10397812/files/deconvolved-it75.fits?download=1">deconvolved-it75.fits</a>: The deconvolved Spitzer image.</li> <li><a href="../records/10397812/files/deconvolved-simulated.tar.gz?download=1">deconvolved-simulated.tar.gz</a>: 100 realizations of random noise over a point-like source used to estimate the error of the deconvolved measurements.</li> </ul>
PHOENIX Stellar Model Grid for VSPEC
<p>A grid of PHOENIX Stellar Models (Husser et al. 2013) from 0.1 to 20 micron.</p> <p>Teff: [2300, 3900] K</p> <p>Log g: 5.0</p> <p>Metalicity: 0.0</p> <p>Created for VSPEC by Peter Hauschildt</p>
Supplementary material for "Stellar flares" (Living Reviews in Solar Physics)
<p>The file supplementary.tar.gz contains a Jupyter notebook (Figs.ipynb) and supplementary material for recreating Figures 13, 35, 38, and 40 in Kowalski, A.F. (2024), "Stellar flares", <em>Living Reviews in Solar Physics</em> 24, 1 (<a href="10.1007/s41116-024-00039-4">https://doi.org/10.1007/s41116-024-00039-4</a>).</p>
Stellar chromospheric activity database of solar-like stars based on the Ca II H and K lines of LAMOST Low-Resolution Spectroscopic Survey: the bolometric and photospheric calibration
<p>This database contains the stellar chromospheric activity parameters of solar-like stars based on the Ca II H and K lines from the spectra of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). We extract 1,122,495 LRS spectra of solar-like stars from the LAMOST Data Release 8 v2.0 and provide the chromospheric activity parameters $S_{\rm tri}$, $S_{\rm MWO}$, $R_{\rm HK}$ and $R'_{\rm HK}$, as well as their uncertainties in the database. $R_{\rm HK}$ and $R'_{\rm HK}$ are derived from the method in the classic literature (denoted with classic) and the method based on the PHOENIX model (denoted with PHOENIX). These stellar chromospheric activity indexes and their uncertainties, along with the relevant spectroscopic parameters from the LAMOST catalogs, are saved in a CSV-format file (name: CaIIHK_Activity_Indexes_LAMOST_DR8_LRS.csv).</p> <p> </p> <p>Columns in the catalog of the database:</p> <p>obsid - Unique observation identifier of LAMOST LRS spectrum</p> <p>obsdate-Spectral observation date</p> <p>fitsname - FITS file name of LAMOST LRS spectrum</p> <p>snrg - Signal-to-noise ratio in the $g$ band ($\mathrm{S/N}_g$) of LAMOST LRS spectrum</p> <p>snrr - Signal-to-noise ratio in the $r$ band ($\mathrm{S/N}_r$) of LAMOST LRS spectrum</p> <p>teff - Effective temperature ($T_\mathrm{eff}$) derived from the LASP (unit: K)</p> <p>teff_err - Uncertainty of $T_\mathrm{eff}$ derived from the LASP (unit: K)</p> <p>logg - Surface gravity ($\log\,g$) derived from the LASP (unit: dex)</p> <p>logg_err - Uncertainty of $\log\,g$ derived from the LASP (unit: dex)</p> <p>feh - Metallicity ([Fe/H]) derived from the LASP (unit: dex)</p> <p>feh_err - Uncertainty of [Fe/H] derived from the LASP (unit: dex)</p> <p>rv - Radial velocity ($V_r$) derived from the LASP (unit: km/s)</p> <p>rv_err - Uncertainty of $V_r$ derived from the LASP (unit: km/s)</p> <p>ra_obs - Right ascension (RA) of fiber pointing (unit: degree)</p> <p>dec_obs - Declination (DEC) of fiber pointing (unit: degree) </p> <p>gaia_source_id - Source identifier in Gaia DR3 catalog</p> <p>gaia_g_mean_mag - $G$ magnitude in Gaia DR3 catalog</p> <p>S_tri* - $S_{\rm tri}$ index of LAMOST LRS </p> <p>S_tri_err* - Uncertainty of $S_{\rm tri}$ </p> <p>S_MWO* - $S_{\rm MWO}$ </p> <p>S_MWO_err* - Uncertainty of $S_{\rm MWO}$ </p> <p>log_R_HK_classic* - $\log\,R_{\rm HK,classic}$ </p> <p>log_R_HK_classic_err* - Uncertainty of $\log\,R_{\rm HK,classic}$ </p> <p>log_R_p_HK_classic* - $\log\,R'_{\rm HK,classic}$ </p> <p>log_R_p_HK_classic_err* - Uncertainty of $\log\,R'_{\rm HK,classic}$ </p> <p>log_R_HK_PHOENIX* - $\log\,R_{\rm HK,PHOENIX}$ </p> <p>log_R_HK_PHOENIX_err* - Uncertainty of $\log\,R_{\rm HK,PHOENIX}$ </p> <p>log_R_p_HK_PHOENIX* - $\log\,R'_{\rm HK,PHOENIX}$ </p> <p>log_R_p_HK_PHOENIX_err* - Uncertainty of $\log\,R'_{\rm HK,PHOENIX}$ </p> <p>(Note: The columns denoted by an asterisk represent the parameters provided by this database, and the remaining columns are collected from the data release of LAMOST DR8 V2.0. If the values are not available, they will be filled with '-9999' in this database.)</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.