The Victoria-Regina Stellar Models: Evolutionary Tracks and Isochrones for a Wide Range in Mass and Metallicity that Allow for Empirically Constrained Amounts of Convective Core Overshooting VandenBerg, D.A., Bergbusch, P.A., & Dowler, P.D., 2006 ApJS, 162, 375 First Release September 29, 2005 This ftp archive contains the grids of evolutionary tracks and the accompanying software (written in FORTRAN 77) for interpolating isochrones, isochrone population functions, luminosity functions, and color functions as described in VandenBerg, Bergbusch & Dowler 2005, Astrophysical Journal Supplement Series, in press. The BVRI color-Teff relations employed in the code are those described by VandenBerg & Clem 2003, The Astronomical Journal, vol. 126, pp. 778-802; the ubvy color transformations are those published by Clem et al 2004, The Astronomical Journal, vol. 127, p. 1227. WARNING: The new grids of evolutionary tracks CANNOT be processed with the software from the 2001 release, Bergbusch & VandenBerg 2001, Astrophysical Journal, vol. 556, pp. 322-339. (BV2001). You MUST DOWNLOAD THE NEW SOFTWARE in the /src directory to process the new model grids prefixed with "vr". REFERENCING: In papers employing these models, authors should refer to "isochrones by VandenBerg, Bergbusch & Dowler (2006) with BVRI color-Teff relations as described by VandenBerg \& Clem (2003)" ... OR "with uvby color transformations as described by Clem et al (2004)". ABSTRACT: Seventy-two grids of stellar evolutionary tracks, along with the capability to generate isochrones and luminosity/color functions from them, are presented in this investigation. Sixty of them extend (and encompass) the sets of models reported by VandenBerg et al.~(2000, ApJ, 532, 430) for 17 [Fe/H] values from -2.31 to -0.30 and alpha-element abundances corresponding to [alpha/Fe] = 0.0, 0.3, and 0.6 (at each iron abundance) to the solar metallicity and to sufficiently high masses (up to ~ 2.2 Msol) that isochrones may be computed for ages as low as 1 Gyr. The remaining grids contain tracks for masses from 0.4 to 4.0 Msol and 12 [Fe/H] values between -0.60 and +0.49 (assuming solar metal-to-hydrogen number abundance ratios): in this case, isochrones may be calculated down to ~ 0.2 Gyr. The extent of convective core overshooting has been modelled using a parameterized version of the Roxburgh (1989, A&A, 211, 361) criterion, in which the value of the free parameter at a given mass and its dependence on mass have been determined from analyses of binary star data and the observed color-magnitude diagrams for several open clusters. Because the calculations reported herein satisfy many empirical constraints, they should provide useful probes into the properties of both simple and complex stellar populations. MODEL GRIDS: The model grids are archived as (unix) compressed tar files. Each one contains the .eep files that tabulate the evolutionary tracks, the zahb*.data files that tabulate the raw zero-age horizontal branch models, the color-Teff transformation files bvrihi.data, bvrilo.data, uvbyhi.data, uvbylo.data, and a template VRISO.OPT file required by the program vriso.f. You will probably want to unpack each compressed and tarred file (alpha*.tar.Z) into its own directory --- if you do each directory will have all the files necessary for the accompanying software to work. Before unpacking a grid, you should create a directory for it. move the respective tar file into the new directory and untar it. vr0a.tar.Z [alpha/Fe] = 0.0 19 grids -2.31 <= [Fe/H] <= 0.0 vr2a.tar.Z [alpha/Fe] = 0.3 19 grids -2.31 <= [Fe/H] <= 0.0 vr4a.tar.Z [alpha/Fe] = 0.6 19 grids -2.31 <= [Fe/H] <= 0.0 vrss.tar.Z Scaled-Solar 12 grids -0.60 <= [Fe/H] <= +0.49 SOURCE CODE: The code is derived from the earlier suite of FORTRAN programs (mkiso.f, mkipf.f, pabiso.f) described in BV2001. The programs should be completely unix friendly --- they compile without complaint on my machine and I fixed any problems arising from the peculiarities of other, less forgiving compilers that were brought to my attention with the 2001 release. All you should have to do is compile and link the programs to the "vr" subroutine libraries. For example, all I do is type > f77 -o $HBIN/vriso vriso.f vrutil.f vrakm.f vrcolor.f to produce an executable called vriso in my personal binary directory. Here's what you get in the /src directory vriso.f main program to interpolate isochrones on the (log L)--(log Teff) plane vrcmd.f main program to transform the isochrones from the (log L)--(log Teff) plane onto the observer's plane. The V/y magnitude together with the standard BVRI and uvby indices are tabulated at 250 roughly equally spaced points. vripf.f main program to generate the distribution functions (IPFs, LFs and CFs) for a given passband (currently BVRI) and color index vrzahb.f main program to transform the zahbs from the (log L)--(log Teff) plane onto the observer's plane. The tabulations are the same as those produced by vrcmd.f vrutil.f library of utility subroutines required by vriso.f, vrcmd.f, and vripf.f vrakm.f library of Akima spline routines required by vriso.f, vrcmd.f, and vripf.f vrcolor.f library of color-Teff transformation routines required by vrcmd.f and vripf.f Currently, the program vriso assumes that an options file (like the template file VRISO.OPT) is to be found in the same directory as the tracks (.eep files) that you are processing. Similarly, the programs vrcmd, vripf, and vrzahb assume that the files bvrilo.data, bvrihi.data, uvbylo.data, and uvbyhi.data are to be found in the same directory as the tracks. DISCLAIMER: It should be obvious that I'm not a software designer, but I hope that the code is reasonably transparent. I will try to construct a users' manual in the near future, but in the meantime, if the software baffles you, send me an email. Have fun! <><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><> Peter A. Bergbusch > Phone [306]-585-4205 Department of Physics < FAX [306]-585-5659 University of Regina > Regina, SK < email: bergbush@phys.uregina.ca Canada S4S 0A2 > http://hyperion.cc.uregina.ca/~bergbusp/ <><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><><>