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6 results for “Stellar ages”
Data and Code for: 'Stellar Models are Reliable at Low Metallicity: An Asteroseismic Age for the Ancient Very Metal-Poor Star KIC 8144907', Huber et al. 2024.
<p>Data and code to reproduce plots for the paper '<em>Stellar Models are Reliable at Low Metallicity: An Asteroseismic Age for the Ancient Very Metal-Poor Star KIC 8144907'</em>, Huber et al. 2024.</p> <p>Descriptions of the enclosed data files are as follows:</p> <div> <ul> <li>Freqs_best_fit.dat: Best-fitting GARSTEC model frequencies (Figure 3, right)</li> <li>KIC10006158_spec.txt: Reduced and normalized HDS spectrum of KIC10006158 (Figure 1)</li> <li>KIC8144907_ps.txt: Power spectrum of the Kepler light curve of KIC8144907 (Figure 3, left)</li> <li>KIC8144907_spec.txt: Reduced and normalized HDS spectrum of KIC8144907 (Figure 1)</li> <li>apokasc2.tsv: APOKASC sample from Pinsonneault+ 2014 (Figure 2)</li> <li>dwarfs.csv: Asteroseismic sample from Serenelli+ 2017 (Figure 2) </li> <li>freqs.csv: Data in Table 1</li> <li>hosts.tsv: Asteroseismic ages from Silva Aguirre+ 2015 (Figure 4) </li> <li>legacy-t1.tsv: Asteroseismic ages from Silva Aguirre+ 2017 (Figure 4) </li> <li>legacy-t2.tsv: Asteroseismic ages from Silva Aguirre+ 2017 (Figure 4) </li> <li>li-2020.csv: Asteroseismic ages from Li+ 2020 (Figure 4) </li> <li>matsuno.txt: Asteroseismic sample from Matsuno+ 2021 (Figure 2) </li> </ul> </div>
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>
Data for the paper "Uncovering the birth of the Milky Way through accurate stellar ages with Gaia", accepted in Nature Astronomy
<p>Data files used in the paper that contain information that is not available in public catalogues, and that is necessary to produce the figures.</p> <p>The extended dataset consists of: i) (<strong>a</strong> and <strong>b</strong> panels of figure 1): two tables directly retrieved from the Gaia archive as described in Methods, supplemented by extinction information on a star-by-star basis; the code used to interpolate the 3-D extinction maps by Lallement et al. (2018) can be retrieved from \url{https://github.com/edober/dust_maps_3d}. ii) (<strong>c</strong> and <strong>d</strong> panels of Figure 1, Figure 2 and panel <strong>a </strong>of Figure 3): two tables with the derived solution CMDs. Two files with the necessary data to define the boxes used to select stars in the blue and red sequences of the halo CMD are also included. iii) (panel <strong>b</strong> of Figure 3): necessary tables with the age, metallicity and velocity data for the main progenitor and accreted satellite for realisation g15784 of the MaGICC program (Brook et al. 2012). The complete information on the final timestep of that simulation, together with scripts to read and plot the data are also included in the extended dataset.</p> <p>A explanatory README is contained within the tar file.</p>
Ages and metallicities of stellar clusters using S-PLUS narrow-band integrated photometry: the Small Magellanic Cloud
<p>These are the final photometric quantities measured in the work "Ages and metallicities of stellar clusters using S-PLUS narrow-band integrated photometry: the Small Magellanic Cloud". The raw S-PLUS images are available upon request to the corresponding author. Nevertheless, the complete S-PLUS data will become publicly available alongside the next data release, scheduled for 2023.</p>
Calibration Data for Kinematic Stellar Age Models
<p>https://github.com/ssagear/KinematicAgePredictor</p>
Efficacy and Safety of LX102 Gene Therapy in Patients With Neovascular Age-related Macular Degeneration (nAMD) (STELLAR)
ClinicalTrials.gov study NCT07317934. IPD Sharing: Not stated. Countries: 1. Publications: 0.
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