Each Tarball contains subdirectories for every grid model.
In each subdirectory, the file "flux_calib.dat" contains an xy-table with wavelengths and absolute flux (models have log L/L☉ = 5.3), whereas the file "flux.pdf" contains a log-log diagram of the SED for quick inspection. Please refer to the PoWR homepage for detailed information about these grids.
Please, don't forget to cite the corresponding papers:
WC grid, Galactic WN grids, LMC WN grids
SMC grids: Hainich et al. (2015)
WN grids in general: Todt et al. (2015)
Line-blanketed model atmospheres for WR stars
A temperature correction method for expanding atmospheres
Grids of model spectra for WN stars, ready for use
Range is 200 - 80000 Å, resolution is 0.3 vDopp = 30 km/s.
About the WC gridNote that we offer currently only a grid of WC models for Galactic (=solar) metallicity, i.e. the abundances of the iron group elements are solar.
The PDF below contains SEDs and continuum-normalized spectra of three WC models for Galactic, LMC, and SMC iron group abundances (other parameters kept constant) to demonstrate the impact of the different metallicities on the UV flux and the optical/IR spectral lines. The Models correspond to the WC grid index 11-16 (Teff=79kK, log Rt/R☉=0.5), typical for the spectral subtype WC6.
WC metallicity comparison (PDF 310 KB)
Moreover the ionizing fluxes (log Q) of these three models are as follows:
About the ionizing fluxes (log Q)We prepared a tarball containing the number of ionizing photons for H I, He I, and He II:
Also note, if you encounter values like this:
EDGE INTEGRATED UP TO LOG OF NUMBER OF PHOTONS PER SECOND Ly Alpha for Helium models 911.33 911.30 48.66 He I edge for Helium models 504.30 504.26 0.00 He II edge for Helium models 227.85 227.84 32.53
it means that there is only a hydrogen ionizing flux. The He I-ionizing flux is marked as zero and the He II-ionizing flux is 15 orders of magnitude below the hydrogen ionizing flux. This means that this flux is actually zero but has only due to numerical round-off errors a finite value.
Low-resolution COLI fluxes