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&nbsp;<a href="https://ui.adsabs.harvard.edu/abs/2019ApJ...887..199G/abstract">Gossage et al. 2019</a>&nbsp;(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&nbsp;<a href="https://ui.adsabs.harvard.edu/abs/2018ApJ...863...67G/abstract">Gossage et al. 2018</a>&nbsp;and&nbsp;<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>&nbsp;protosolar abundances \(\rm Z_{\odot}\)&nbsp;= 0.0142).</li> <li>Rotation rates from v/v_crit&nbsp;= 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:&nbsp; <ul> <li>\(\rm \Delta M = 0.05 M_{\odot}\)&nbsp;for \(\rm M &lt; 1 M_{\odot}\)</li> <li>\(\rm \Delta M = 0.04 M_{\odot}\)&nbsp;for \(\rm 1 M_{\odot} \leq M &lt; 2 M_{\odot}\)</li> <li>\(\rm \Delta M = 0.2 M_{\odot}\)&nbsp;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.,&nbsp;\(\texttt{MIST_v1.0_feh_p0.15_rotating_tracks.zip}\), contain theoretical models at a particular metallcity ([Fe/H] = 0.15 in this case), at all rotation rates and masses. The file&nbsp;\(\texttt{MIST_v1.0_feh_m0.15_rotating_tracks.zip}\)&nbsp;contains models at [Fe/H] = -0.15, and so on.&nbsp;\(\texttt{*_tracks.zip}\)&nbsp;contain EEP stellar track files and&nbsp;\(\texttt{*_isochrones.zip}\)&nbsp;files contain theoretical isochrone files, both in the same format as EEP track and theoretical&nbsp;isochrones found on the <a href="https://waps.cfa.harvard.edu/MIST/index.html">MIST website</a>. Zip files labeled, e.g.,\(\texttt{*_isochrones_FILTERSET.zip}\)&nbsp;contain observable isochrones, with synthetic photometry&nbsp;produced&nbsp;for a particular filter set (as on the <a href="https://waps.cfa.harvard.edu/MIST/model_grids.html">MIST packaged grids</a>&nbsp;site, which contains more information on the filter sets), computed without extinction (\(A_V=0\)). At the moment, filter sets for \(\texttt{UBVRIplus}\)&nbsp;(containing Gaia filters),&nbsp;&nbsp;\(\texttt{HST_WFC3}\),&nbsp;\(\texttt{HST_ACSWF}\), \(\texttt{HST_WFPC2}\), and&nbsp;\(\texttt{CFHTugriz}\)&nbsp;are&nbsp;included, but more can be added upon request\(^2\).&nbsp;</p> <p><strong>Notes:</strong></p> <p>\(^1\)&nbsp;These are the same models as featured in&nbsp;<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&nbsp;v/v_crit&nbsp;= 0.6. We include these models from <a href="https://ui.adsabs.harvard.edu/abs/2018ApJ...863...67G/abstract">Gossage et al. 2018</a>&nbsp;here as well. Models at&nbsp;[Fe/H] = -0.60 have been extended to v/v_crit&nbsp;= 0.9, while&nbsp;[Fe/H] = -0.75 only includes up to the original v/v_crit&nbsp;= 0.6.</p> <p>\(^2\)&nbsp;These tracks and isochrones may be converted into observable tracks and isochrones (w/ gravity darkening effects if desired) via Aaron Dotter's&nbsp;<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>