The ACS Survey of Galactic Globular Clusters. II. Stellar Evolution Tracks, Isochrones, Luminosity Functions, and Synthetic Horizontal-Branch Models

By Aaron Dotter, B. Chaboyer, Darko Jevremovic, Eddie Baron, J. Ferguson, A. Sarajedini, Jay Anderson. 2007

242 citations recorded by the source corpus.

The ACS Survey of Galactic Globular Clusters, an HST Treasury Project, will deliver high-quality, homogeneous photometry of 65 globular clusters. This paper introduces a new collection of stellar evolution tracks and isochrones suitable for analyzing the ACS survey data. Stellar evolution models were computed at [Fe/H] = -2.5, -2.0, -1.5, -1.0, -0.5, and 0; [α/Fe] = -0.2, 0, 0.2, 0.4, 0.6, and 0.8; and three initial He abundances for masses from 0.1 to 1.8 M⊙ and ages from 2 to 15 Gyr. Each isochrone spans a wide range in luminosity, from MV ∼ 14 up to the tip of the red giant branch. These are complemented by a set of He-burning tracks that extend from the zero-age horizontal branch to the onset of thermal pulsations on the asymptotic giant branch. In addition, a set of computer programs are provided that make it possible to interpolate the isochrones in [Fe/H], generate luminosity functions from the isochrones, and create synthetic horizontal-branch models. The tracks and isochrones have been converted to the observational plane with two different color-Teff transformations, one synthetic and one semiempirical, in ground-based B, V, and I, and F606W and F814W for both ACS WFC and WFPC2 systems. All models and programs presented in this paper are available at the Dartmouth Stellar Evolution Database and the Multimission Archive at the Space Telescope Science Institute.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9d448af197b1cc433a8fe8a83247d4e48157269e

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In Astronomy and Astrophysics

1. Aaron Dotter
2. Jay Anderson
3. S. Majewski
4. C. Conroy
5. A. Milone
6. G. Piotto
7. A. Sarajedini
8. L. Bedin

Citations in the corpus

• AGE DETERMINATION OF SIX INTERMEDIATE-AGE SMALL MAGELLANIC CLOUD STAR CLUSTERS WITH HST/ACS (2008, unknown): “The Dartmouth isochrone model provided by Dotter et al. (2007) yields the best fit to the CMD (Fig.”
• A Comprehensive Maximum Likelihood Analysis of the Structural Properties of Faint Milky Way Satellites (2008, methodology): “Using the distance listed in Table 1, the luminosity of stars below the magnitude limit is accounted for by using luminosity function (LF) corrections derived from the LFs of Dotter et al. (2007) with the metallicity and age closest to each model population.”
• The ACS survey of Galactic globular clusters. XII. Photometric binaries along the main sequence (2011, methodology): “To do this we converted the mean F814W magnitudes of the single stars contained in each of these regions into masses through the Dotter et al. (2007) massluminosity relations.”
• Accreted versus in situ Milky Way globular clusters (2010, methodology): “The mean absolute age of the metal-poor GCs is 12.80 Gyr (using the Dartmouth models of Dotter et al. 2007), which we adopt as the normalisation to derive absolute ages.”
• THE ACS SURVEY OF GALACTIC GLOBULAR CLUSTERS. VII. RELATIVE AGES (2008, methodology): “We have primarily used the most recent state−of−art models of Dotter et al. (2007) (hereafter D07), transformed to the observational plane with an empirical Color−Teff transformation.”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, methodology): “This was done six times: once, as the control case, using only DSEP routines and no MESA modules; next, using each of four MESA modules individually; and, finally, using the four MESA modules at the same time in DSEP.”
• WIYN OPEN CLUSTER STUDY. LXII. COMPARISON OF ISOCHRONE SYSTEMS USING DEEP MULTI-BAND PHOTOMETRY OF M35 (2014, methodology): “High-Mass Stars Each system employs vastly different physical assumptions for higher mass stars (M> 0.7 M ): for example, Dartmouth’s equation of state model is a simple ideal gas, with a correction for coulomb interaction, while FreeEOS (used by PARSEC) handles ionization, degeneracy pressure and r”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane I. From the ZAMS to the TP-A (2008, background): “Unlike these authors, very recently Dotter et al. (2007) presented new stellar tracks and isochrones for three initial helium abundances in the rangeof mass between 0.1 and 1.8M⊙ for scaled solar andα-enhanced chemical compositions.”
• The Dartmouth Stellar Evolution Database (2008, methodology): “The collection of Fortran 77 programs introduced by Dotter et al. (2007) have been updated to deal with the expanded compositions and photometric systems presented in this paper but are otherwise largely unchanged.”
• The Pisa pre-main sequence tracks and isochrones - A database covering a wide range of Z, Y, mass, and age values (2011, methodology): “…several generations of theoreticalpreMS models have been developed following improvements to the physical inputs to provide progressively more accurate theoretical predictions (e.g. Baraffe et al. 1998; D’Antona & Mazzitelli 1997; Siess et al. 2000; Dotter et al. 2007; Di Criscienzo et al. 2009).”
• The ACS Survey of Galactic Globular Clusters. III. The Double Subgiant Branch of NGC 1851 (2007, background): “Comparison with the theoretical models of Dotter et al. (2007) shows that this separation corresponds to an age difference of 1 Gyr, with the fSGB older than the bSGB.”