This web site hosts a suite of tools that are useful for the study of stars and stellar populations. The main three products are: a set of stellar interior models computed with JMSTAR, a set of single synthetic stellar populations based on JMSTAR stellar tracks and a set of IDL codes that compute the spectral evolution of complex stellar populations: both the stellar and the dust (far-IR and CO) emission.
This project was borne out of the necessity to have a set of integrated stellar population models that were accurate enough as to model spectra from the new generation of 10m class telescopes. We were also interested in having a trully independent stellar evolution code in order to be able to estimate systematic errors in building stellar populations.
The stellar interior models will be of interest to researchers that would like to predict properties of individual stars and also to those who would like to use them as interior models to build their own synthetic stellar population models.
The set of single stellar populations will be of interest to researchers that would like to predict the spectral energy distribution of single bursts as a function of age and metallicity.
This work is a collaborative effort by Raul Jimenez (UPenn), James MacDonald (U. of Delaware), James Dunlop (Edinburgh), Paolo Padoan (UCSD), John Peacock(Edinburgh).
Synthetic stellar populations: single stellar populations, stellar interior models and primordial proto-galaxies, MNRAS, 349, 240 (Jimenez et al. 2004)
See also the paper with the previous release (1998) of the models and the paper (Jimenez et al. 2000, ApJ, 532, 152) where we describe the dust and CO emission model.
The SSPs are provided as ASCII files. Each of of them contains 40 ages (0.001 to 14 Gyr) for a given chemical composition (the chemical compositions range 0.01 to 2.5 solar, for example speed0040_25_kroupa.spec contains all ages for Z=0.0040 and Y=0.25 for a kroupa IMF). We also provide binary(linux) files to be used with the IDL routines (see below).
In order to facilitate easy comparison between our models and those of Bruzual & Charlot, we make available the most commonly used BC2003 model (the low-resolution Salpeter IMF with Padova 1994 tracks) in our format. We also provide our models in the BC2003 ASCII format, replacing their SED data with the SPEED results, but leaving all header information unaltered. Since we sample at different ages and metallicities, interpolation is required: we assume that log(SED) changes linearly with time and metallicity. For t > 14 Gyr (our maximum age), we adopt the simple prescription of exponential decay with 15 Gyr time-constant.
Download the files at this link for SSPs (i.e. populations formed in a single burst) for metallicities between 1/100 and 2.5 solar and ages 0.001 to 14 Gyr and a Kroupa IMF. Download the binary file here and the BC-format ascii data here.
Download the files at this link for SSPs (i.e. populations formed in a single burst) for metallicities between 1/100 and 2.5 solar and ages 0.001 to 14 Gyr and a Salpeter (x=-1.35, minimun mass 0.1 Msun) IMF. Download the binary file here and the BC-format ascii data here.
Download the files at this link for SSPs (i.e. populations formed in a single burst) for metallicities between 1/100 and 2.5 solar and ages 0.001 to 14 Gyr and a power law (x=-0.9, minimun mass 0.1 Msun) IMF. Download the binary file here and the BC-format ascii data here.
Download the files at this link for SSPs (i.e. populations formed in a single burst) for metallicities between 1/100 and 2.5 solar and ages 0.001 to 14 Gyr and a power law (x=-1.6, minimun mass 0.1 Msun) IMF. Download the binary file here and the BC-format ascii data here.
Download the files at this link for the BC2003 low-resolution Salpeter model with Padova 1994 tracks in the identical format to the SPEED models. Download the binary file here
The codes below are provided in source form as .pro files. Please, do not use them as black boxes ( specially the complex dust emission code). Read the header of each .pro which contains instructions on how to run the codes and the format of the input and output. For the codes to work, you need to download the idlsave version of the SSPs (above) for the desired IMF.
SPEEDmetage: This code allows you to build a single stellar population of arbitrary metallicity and age.
SPEEDchemo: This code builds the spectral energy distribution of a stellar population as a function of time for any star formation and chemical evolution history that you provide. Here is an example for the kind of input file that is required. You do not have to be careful in defining bins in the star formation history small enough to obtain good accuracy. The code will automatically create an adaptive mesh to make sure all ages are computed accurately. The code returns the spectral energy distribution as a function of time in the restframe of the galaxy.
SPEEDdust: This code builds the spectral energy distribution of a stellar population as a function of time for any star formation history and provides dust emission (and attenuated stellar ) spectra and corresponding CO lines as a function of time in the restframe of the galaxy. You need an auxiliary file for the CO lines.
The files below contain stellar interior models (for solar scaled chemical compositions) computed with JMSTAR. For each chemical composition there is one tar.gz file. In every tar.gz file there are individual ASCII files which contain a single mass model for the corresponding chemical composition and where each column corresponds to:
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raul.jimenez [[at] gmail.com
last update: 28-February-2011