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Dataset results
18 results for “stellar populations”
Data for The UNCOVER Survey: A First-Look HST+JWST Catalog of Galaxy Redshifts and Stellar Populations Properties Spanning 0.2 ≲ z ≲ 15
<p>The recent UNCOVER survey with the James Webb Space Telescope (JWST) exploits the nearby cluster Abell 2744 to create the deepest view of our universe to date by leveraging strong gravitational lensing. In this work, we perform photometric fitting of more than 50,000 robustly detected sources out to z ~ 15. We show the redshift evolution of stellar ages, star formation rates, and rest-frame colors across the full range of 0.2 < z < 15. The galaxy properties are inferred using the Prospector Bayesian inference framework using informative Prospector-beta priors on masses and star formation histories to produce joint redshift and stellar populations posteriors, and additionally lensing magnification is performed on-the-fly to ensure consistency with the scale-dependent priors. We show that this approach produces excellent photometric redshifts with NMAD ~ 0.03, of a similar quality to the established photometric redshift code EAzY. In line with the open-source scientific objective of the Treasury survey, we publicly release the stellar populations catalog with this paper, derived from the photometric catalog adapting aperture sizes based on source profiles. This release includes posterior moments, maximum-likelihood spectra, star-formation histories, and full posterior distributions, offering a rich data set to explore the processes governing galaxy formation and evolution over a parameter space now accessible by JWST.</p>
X-rays across the galaxy population: The distribution of AGN accretion rates as a function of stellar mass and redshift
<p>We provide measurements of the probability distribution function of specific black hole accretion rates within a sample of galaxies of a given stellar mass and redshift, <span class="math-tex">\(p(\log \lambda_{sBHAR} | M_*,z)\)</span>. Measurements are provided for all galaxies, star-forming galaxies and quiescent galaxies. We also provide estimates of the AGN duty cycle, <span class="math-tex">\(f(\lambda_{sBHAR} >0.01)\)</span> i.e. the fraction of galaxies with an AGN above a given limit in specific accretion rate, based on the probability distribution functions. Full details are provided in Aird et al. (2018, MNRAS, 474, 1225); please cite this publication if you use these measurements. </p>
RCSED - A Value-Added Reference Catalog of Spectral Energy Distributions of 800,299 Galaxies in 11 Ultraviolet, Optical, and Near-Infrared Bands: Morphologies, Colors, Ionized Gas and Stellar Populations Properties
<p>We present RCSED, the value-added Reference Catalog of Spectral Energy Distributions of galaxies, which contains homogenized spectrophotometric data for 800,299 low and intermediate redshift galaxies (0.007 < z < 0.6) selected from the Sloan Digital Sky Survey spectroscopic sample. Accessible from the Virtual Observatory (VO) and complemented with detailed information on galaxy properties obtained with the state-of-the-art data analysis, RCSED enables direct studies of galaxy formation and evolution during the last 5 Gyr. We provide tabulated color transformations for galaxies of different morphologies and luminosities and analytic expressions for the red sequence shape in different colors. RCSED comprises integrated k-corrected photometry in up-to 11 ultraviolet, optical, and near-infrared bands published by the GALEX, SDSS, and UKIDSS wide-field imaging surveys; results of the stellar population fitting of SDSS spectra including best-fitting templates, velocity dispersions, parameterized star formation histories, and stellar metallicities computed for instantaneous starburst and exponentially declining star formation models; parametric and non-parametric emission line fluxes and profiles; and gas phase metallicities. We link RCSED to the Galaxy Zoo morphological classification and galaxy bulge+disk decomposition results by Simard et al. We construct the color-magnitude, Faber-Jackson, mass-metallicity relations, compare them with the literature and discuss systematic errors of galaxy properties presented in our catalog. RCSED is accessible from the project web-site and via VO simple spectrum access and table access services using VO compliant applications. We describe several SQL query examples against the database. Finally, we briefly discuss existing and future scientific applications of RCSED and prospectives for the catalog extension to higher redshifts and different wavelengths.</p>
Magellan/M2FS Spectroscopy of Galaxy Clusters: Stellar Population Model and Application to Abell 267
<p>supplementary data products, including all sky-subtracted spectra from individual galaxies, as well as random draws from posterior PDFs for model parameters (see included README file)</p>
Dataset from: Rapid stellar and binary population synthesis with COMPAS
<p>This data set is used to produce Figure 16 of the COMPAS Paper (<a href="https://arxiv.org/abs/2109.10352">Team COMPAS et al. 2021</a>).</p> <p>The file contains the output of 10,000,000 binaries evolved using COMPAS v02.21.00, using adaptive importance sampling (STROOPWAFEL) , sampling from a metallicity uniform in <span class="math-tex">\(\log(Z) \in [10^{-4},0.03]\)</span>. More details can be found in the `Run_Details` group.</p> <p>*****************************<br> Contents<br> *****************************</p> <ol> <li>COMPAS simulation output:<br> The hdf5 file Includes necessary information about the simulated binaries in the following groups:<br> <br> <strong>BSE_Double_Compact_Objects<br> BSE_Common_Envelopes<br> BSE_RLOF<br> BSE_Supernovae<br> BSE_System_Parameters<br> Run_</strong><strong>Details</strong><br> <br> We point the reader to the documentation at <a href="https://compas.science/docs">https://compas.science/docs</a>, for information and instructions regarding the contained data.<br> </li> <li><strong>Rate Data</strong><br> The hdf5 file contains 1 groups with BBH merger rate data for every BBH with an inspiral time that is smaller than the age of the Universe. This group contains a dataset "DCOmask" which can be used to point from the "DoubleCompactObjects" to the data contained in the respective rates datasets.<br> <br> We include the rates for one realization of the metallicity-dependent SFRD as discussed in the manuscript.<br> The metallicity-dependent SFRD used is the phenomenological metallicity-dependent SFRD as described in Neijssel et al. 2019, this contained in:<br> <strong>'Rates_mu00.035_muz-0.23_alpha0.0_sigma00.39_sigmaz0.0'</strong></li> </ol> <p>*****************************</p> <p>The rates were calculated by running ```FastCosmicIntegration.py``` from COMPAS's post-processing tools.<br> For a more detailed explanation of the workings of COMPAS's post-processing tools, please the docs <a href="https://compas.science/docs">https://compas.science/docs</a></p>
Stellar Population Spectra from Bruzual & Charlot (2003)
<p>Models from <a href="http://adsabs.harvard.edu/abs/2003MNRAS.344.1000B">Bruzual & Charlot (2003; MNRAS; 344; 1000)</a>. Data was downloaded from <a href="http://www2.iap.fr/users/charlot/bc2003/">http://www2.iap.fr/users/charlot/bc2003/</a></p> <ul> <li> <p>SSP_Spectra_BC2003_highResolution_imfChabrier.hdf5</p> <ul> <li> <p><a href="http://adsabs.harvard.edu/abs/2001ApJ...554.1274C">Chabrier IMF</a></p> </li> <li> <p>High resolution spectra</p> </li> </ul> </li> <li> <p>SSP_Spectra_BC2003_highResolution_imfSalpeter.hdf5</p> <ul> <li> <p><a href="http://adsabs.harvard.edu/abs/1955ApJ...121..161S">Salpeter IMF</a></p> </li> <li> <p>High resolution spectra</p> </li> </ul> </li> <li> <p>SSP_Spectra_BC2003_lowResolution_imfChabrier.hdf5</p> <ul> <li> <p><a href="http://adsabs.harvard.edu/abs/2001ApJ...554.1274C">Chabrier IMF</a></p> </li> <li> <p>Low resolution spectra</p> </li> </ul> </li> <li> <p>SSP_Spectra_BC2003_lowResolution_imfSalpeter.hdf5</p> <ul> <li> <p><a href="http://adsabs.harvard.edu/abs/1955ApJ...121..161S">Salpeter IMF</a></p> </li> <li> <p>Low resolution spectra</p> </li> </ul> </li> </ul>
Stellar Population Spectra from BPASS v2.0
<p>The BPASS models of <a href="http://adsabs.harvard.edu/abs/2012MNRAS.419..479E">Eldridge & Stanway (2012, MNRAS, 419, 479)</a>; <a href="http://adsabs.harvard.edu/abs/2011MNRAS.414.3501E">Eldridge, Langer & Tout (2011, MNRAS, 414, 3501)</a>; <a href="http://adsabs.harvard.edu/abs/2009MNRAS.400.1019E">Eldridge & Stanway (2009, MNRAS, 400, 1019)</a>; <a href="http://adsabs.harvard.edu/abs/2008MNRAS.384.1109E">Eldridge, Izzard & Tout (2008, MNRAS, 384, 1109)</a>. Data was downloaded from <a href="http://flexiblelearning.auckland.ac.nz/bpass/2/files/">http://flexiblelearning.auckland.ac.nz/bpass/2/files/</a>.</p> <ul> <li> <p>SSP_Spectra_BPASS_binary.hdf5</p> <ul> <li> <p>Canonical BPASS IMF</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.0 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASS_single.hdf5</p> <ul> <li> <p>Canonical BPASS IMF</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Use v2.0 of BPASS</p> </li> </ul> </li> </ul>
Stellar Population Spectra from BPASS v2.2.1
<p>The BPASS models of <a href="https://ui.adsabs.harvard.edu/abs/2017PASA...34...58E">Eldridge, Stanway et al. (2017)</a> and <a href="https://ui.adsabs.harvard.edu/abs/2018MNRAS.479...75S">Stanway & Eldridge et al. (2018)</a>. Data was downloaded from <a href="https://drive.google.com/drive/folders/1BS2w9hpdaJeul6-YtZum--F4gxWIPYXl?usp=sharing">https://drive.google.com/drive/folders/1BS2w9hpdaJeul6-YtZum--F4gxWIPYXl?usp=sharing</a>.</p> <ul> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf100_100.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.00 from 0.5M<sub>☉</sub> to 100M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf100_300.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.00 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf135_100.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 100M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf135_300.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf135all_100.hdf5</p> <ul> <li> <p>Power law IMF (α=-2.35 from 0.1M<sub>☉</sub> to 100M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf170_100.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.70 from 0.5M<sub>☉</sub> to 100M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf170_300.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.70 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf_chab100.hdf5</p> <ul> <li> <p>Chabrier IMF (α=-2.00; maximum mass 100M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_bin-imf_chab300.hdf5</p> <ul> <li> <p>Chabrier IMF (α=-2.00; maximum mass 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf100_100.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.00 from 0.5M<sub>☉</sub> to 100M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf100_300.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.00 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf135_100.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 100M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf135_300.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf135all_100.hdf5</p> <ul> <li> <p>Power law IMF (α=-2.35 from 0.1M<sub>☉</sub> to 100M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf170_100.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.70 from 0.5M<sub>☉</sub> to 100M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf170_300.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.70 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf_chab100.hdf5</p> <ul> <li> <p>Chabrier IMF (α=-2.00; maximum mass 100M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.2.1_sin-imf_chab300.hdf5</p> <ul> <li> <p>Chabrier IMF (α=-2.00; maximum mass 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>Uses v2.2.1 of BPASS</p> </li> </ul> </li> </ul>
Stellar Population Spectra from Conroy et al. (2010)
<p>Models from <a href="http://adsabs.harvard.edu/abs/2010ascl.soft10043C">Conroy & Gunn (2010; ascl:1010.043)</a>.</p> <ul> <li> <p>SSP_Spectra_Conroy-et-al_v2.5_imfChabrier.hdf5</p> <ul> <li> <p>Computed with v2.5 of FSPS</p> </li> <li> <p><a href="http://adsabs.harvard.edu/abs/2001ApJ...554.1274C">Chabrier IMF</a></p> </li> </ul> </li> <li> <p>SSP_Spectra_Conroy-et-al_v2.5_imfKroupa.hdf5</p> <ul> <li> <p>Computed with v2.5 of FSPS</p> </li> <li> <p><a href="http://adsabs.harvard.edu/abs/2001MNRAS.322..231K">Kroupa IMF</a></p> </li> </ul> </li> <li> <p>SSP_Spectra_Conroy-et-al_v2.5_imfSalpeter.hdf5</p> <ul> <li> <p>Computed with v2.5 of FSPS</p> </li> <li> <p><a href="http://adsabs.harvard.edu/abs/1955ApJ...121..161S">Salpeter IMF</a></p> </li> </ul> </li> </ul>
Stellar Population Spectra from Maraston et al. (2005)
<p>Models from <a href="http://adsabs.harvard.edu/abs/2005MNRAS.362..799M">Maraston (2005, MNRAS, 362, 799)</a>; <a href="http://adsabs.harvard.edu/abs/1998MNRAS.300..872M">Maraston (1998, MNRAS, 300, 872)</a>. Data downloaded from <a href="http://web.archive.org/web/20220121155147/http://www.icg.port.ac.uk/~maraston/Claudia's_Stellar_Population_Model.html">http://web.archive.org/web/20220121155147/http://www.icg.port.ac.uk/~maraston/Claudia's_Stellar_Population_Model.html</a>.</p> <ul> <li> <p>SSP_Spectra_Maraston_hbMorphologyRed_imfKroupa.hdf5</p> <ul> <li> <p><a href="http://adsabs.harvard.edu/abs/2001MNRAS.322..231K">Kroupa IMF</a></p> </li> <li> <p>“Red” horizontal branch morphology</p> </li> </ul> </li> <li> <p>SSP_Spectra_Maraston_hbMorphologyRed_imfSalpeter.hdf5</p> <ul> <li> <p><a href="http://adsabs.harvard.edu/abs/1955ApJ...121..161S">Salpeter IMF</a></p> </li> <li> <p>“Red” horizontal branch morphology</p> </li> </ul> </li> <li> <p>SSP_Spectra_Maraston_hbMorphologyBlue_imfKroupa.hdf5</p> <ul> <li> <p><a href="http://adsabs.harvard.edu/abs/2001MNRAS.322..231K">Kroupa IMF</a></p> </li> <li> <p>“Blue” horizontal branch morphology</p> </li> </ul> </li> <li> <p>SSP_Spectra_Maraston_hbMorphologyBlue_imfSalpeter.hdf5</p> <ul> <li> <p><a href="http://adsabs.harvard.edu/abs/1955ApJ...121..161S">Salpeter IMF</a></p> </li> <li> <p>“Blue” horizontal branch morphology</p> </li> </ul> </li> </ul>
Stellar Population Spectra from Venkatesan et al. (2003)
<p>Simple stellar population spectra from <a href="http://adsabs.harvard.edu/abs/2003ApJ...584..621V">Venkatesan et al. (2003; ApJ; 584; 621)</a> in the Galacticus format. Two models are provided. Both assume a <a href="http://adsabs.harvard.edu/abs/1955ApJ...121..161S">Salpeter IMF</a>, one from 10-140M<sub>☉</sub> and the other from 1-100M<sub>☉</sub>.</p> <p> </p>
Stellar Population Spectra from BPASS v2.3
<p>The BPASS models of <a href="https://ui.adsabs.harvard.edu/abs/2017PASA...34...58E">Eldridge, Stanway et al. (2017)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2018MNRAS.479...75S">Stanway & Eldridge et al. (2018)</a> and <a href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.5329B">Byrne et al. (2022, MNRAS, 512, 5329)</a>. Data was downloaded from <a href="https://livewarwickac.sharepoint.com/sites/Physics-BinaryPopulationandSpectralSynthesisBPASS/Shared%20Documents/Forms/AllItems.aspx?id=%2Fsites%2FPhysics%2DBinaryPopulationandSpectralSynthesisBPASS%2FShared%20Documents%2FPaper%20Data%20Packages%2FByrne23&p=true&ga=1">here</a>.</p> <ul> <li> <p>SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha-02.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=-0.2</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha+00.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=+0.0</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha+02.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=+0.2</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha+04.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=+0.4</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_sin-imf135_300-alpha+06.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Does not include binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=+0.6</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha-02.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=-0.2</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha+00.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=+0.0</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha+02.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=+0.2</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha+04.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=+0.4</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> <li> <p>SSP_Spectra_BPASSv2.3_bin-imf135_300-alpha+06.hdf5</p> <ul> <li> <p>Broken power law IMF (α=-1.30 from 0.1M<sub>☉</sub>-0.5M<sub>☉</sub>, α=-2.35 from 0.5M<sub>☉</sub> to 300M<sub>☉</sub>)</p> </li> <li> <p>Includes binary stars</p> </li> <li> <p>α-alement enhancement of Δlog₁₀(α/Fe)=+0.6</p> </li> <li> <p>Uses v2.3 of BPASS</p> </li> </ul> </li> </ul>
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>
DirtyGrid: 3D dust radiative transfer modeling of spectral energy distributions of dusty stellar populations
<p>Output global SEDs of a large grid of 3D stellar+dust radiative transfer models spanning the range of star formation and dust contents of regions of galaxies.</p> <p>Paper describing the DirtyGrid is Law, Gordo, & Misset (2018, ApJ, submitted)</p> <p>Code to make to access this data at: https://github.com/karllark/pydirtygrid</p>
On the Observability of Individual Population III Stars and Their Stellar-mass Black Hole Accretion Disks through Cluster Caustic Transits
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018ApJS..234...41W/abstract">On the Observability of Individual Population III Stars and Their Stellar-mass Black Hole Accretion Disks through Cluster Caustic Transits</a></p>
oceanus: Populations of stellar streams in deforming MW--LMC systems - I
<p>We publish o<em>ceanus,</em> the t = 0 Gyr simulation snapshots of all 16,384 streams in each MW--LMC potential used in<em> </em>Brooks, R. A. N et al. (2024)<em>.</em> The first part of the archived data includes:</p> <ul> <li><strong>rigid-mw-woutmotion-nolmc.hdf5</strong> - dataset for the stream population generated in the "Rigid MW without motion (no LMC)" potential.</li> <li><strong>rigid-mw-wmotion-nolmc.hdf5</strong> - dataset for the stream population generated in the "Rigid MW + motion (no LMC)" potential.</li> <li><strong>rigidmono-wlmc.hdf5 </strong>- dataset for the stream population generated in the "Rigid Monopole & LMC" potential.</li> <li><strong>evolmono-wlmc.hdf5</strong> - dataset for the stream population generated in the "Evolving Monopole & LMC" potential.</li> </ul> <p>Each stream contains 20,000 particles with 3-D Galactocentric positions and velocities, plus progenitor information on its initial conditions, mass and scale radius. We do not include summary statistic values. The functions to calculate stream summary statistics will be shared upon reasonable request. This dataset can be used to explore the effect of the LMC and the MW halo response on MW streams.</p> <p>The basis function expansion MW--LMC potentials can be found and installed using instruction at:<em> </em><a href="https://github.com/sophialilleengen/mwlmc" target="_blank" rel="noopener">https://github.com/sophialilleengen/mwlmc</a>.</p>
oceanus: Populations of stellar streams in deforming MW--LMC systems - II
<p>We publish o<em>ceanus,</em> the t = 0 Gyr simulation snapshots of all 16,384 streams in each MW--LMC potential used in Brooks, R. A. N et al. (2024)<em>.</em> The second part of the archived data includes:</p> <ul> <li><strong>monodipole-wlmc.hdf5 </strong>- dataset for the stream population generated in the "Monopole + Dipole & LMC" potential.</li> <li><strong>monoquad-wlmc.hdf5 </strong>- dataset for the stream population generated in the "Monopole + Quadrupole & LMC" potential.</li> <li><strong>monodipolequad-wlmc.hdf5 </strong>- dataset for the stream population generated in the "Monopole + Dipole + Quadrupole & LMC" potential.</li> <li><strong>fullexp-nolmc.hdf5 </strong>- dataset for the stream population generated in the "ull Expansion & LMC" potential.</li> <li><strong>fullexp-wlmc.hdf5 </strong>- dataset for the stream population generated in the "ull Expansion (no LMC)" potential.</li> </ul> <p>Each stream contains 20,000 particles with 3-D Galactocentric positions and velocities, plus progenitor information on its initial conditions, mass and scale radius. We do not include summary statistic values. The functions to calculate stream summary statistics will be shared upon reasonable request. This dataset can be used to explore the effect of the LMC and the MW halo response on MW streams.</p> <p>The basis function expansion MW--LMC potentials can be found and installed using instruction at: <a href="https://github.com/sophialilleengen/mwlmc" target="_blank" rel="noopener">https://github.com/sophialilleengen/mwlmc</a>.</p>
The catalogue of "MaNGA DynPop - II. Global stellar population, gradients, and star-formation histories from integral-field spectroscopy of 10K galaxies: link with galaxy rotation, shape, and total-density gradients"
<p><strong>NOTE: Three parameters related to dust extinction ("delta_Map", "Fred_tot_Map", "Fred_gal_Map") in v1 catalogue are incorrectly saved, we have updated the catalogue in <a href="https://zenodo.org/records/15742825">https://zenodo.org/records/15742825</a> .</strong></p> <p> </p> <p>This catalogue is related to the paper "<strong>MaNGA DynPop - II. Global stellar population, gradients, and star-formation histories from integral-field spectroscopy of 10K galaxies: link with galaxy rotation, shape, and total-density gradients</strong>" by <strong>Lu et al. </strong><a href="https://ui.adsabs.harvard.edu/abs/2023MNRAS.tmp.2611L/abstract">https://ui.adsabs.harvard.edu/abs/2023MNRAS.tmp.2611L/abstract</a>. In this paper, we analyze the stellar population properties and star formation histories for over 10,000 MaNGA galaxies.</p> <p>Below are the descriptions of the files: </p> <ul> <li><strong>DynPop2_SPSFH_v1.hdf5 </strong>A HDF5 file containing the catalogue.</li> <li><strong>HDF5_reading_script.py</strong> A Python script to read the catalogue from the HDF5 file.</li> <li><strong>SP_catalog_explanation.pdf</strong> The data explanations for the catalogue, also see Table B1 in the paper. </li> </ul>
ScienceDex guides
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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)
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DANDI Archive for NWB datasets
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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.