The HST/ACS Survey of Galactic Globular Clusters: New Stellar Evolution Tracks, Isochrones and Luminosity Functions

Details The HST/ACS Survey of Galactic Globular Clusters: New Stellar Evolution Tracks, Isochrones and Luminosity Functions The HST/ACS Survey of Galactic Globular Clusters: New Stellar Evolution Tracks, Isochrones and Luminosity Functions

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20910010c&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #100.10; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

Scientific paper

To aid in the analysis of the HST/ACS survey of Galactice globular clusters, we have calculated a new set of stellar evolution tracks, isochrones and luminosity functions. The stellar evolution tracks use an updated set of basic physics, including the FreeEOS equation of state, new opacities and surface boundary conditions from the PHOENIX model atmosphere code, and include the diffusion of metals and helium. The stellar evolution tracks start on the pre-main sequence and terminate at the onset of thermal pulsations on the asymptotic giant branch. Models with masses from 0.1 to 1.5 solar masses are computed from [Fe/H] = -2.5 to [Fe/H] = 0., in steps of 0.5 dex. For each [Fe/H] value, tracks and isochrones with [α/Fe] = -0.2, 0.0, +0.2, +0.4, +0.6 and +0.8 are available.
Isochrones were calculated using two independant color calibrations, and are available in F606W and F814W ACS-WFC filters, F606W and F814W WFPC2 filters, and ground based BVI. These isochrones range in age from 2 to 15 Gyr. Portable Fortran codes are provided that can:
(1) interpolate the isochrones to any [Fe/H] within the bounds of the original calculations,
(2) create luminosity functions with a power law IMF from the isochrones, and
(3) create synthetic horizontal branches for older stellar populations.
The stellar evolution tracks, isochrones, and Fortran codes are available at: http://stellar.dartmouth.edu/ models/hst_gc.html
Support for this work (GO-10775) was provided by NASA through a grant from the Space Telescope Science Institute which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.

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