Details of the WC models

In its original form, this grid of WC models was established in Sander, Hamann & Todt (2012). This current version of the grid has been published here on 10. April 2018, replacing the older version which, for reference, is still accessible by choosing "WC-2014" in the drop-down menu. The major improvement of the current version concerns the iron-group elements. The superlevels are now grouped by states of the same parity. This avoids the spurious emission from Fe III that had been present in the UV spectra of the coolest models in the previous version. Moreover, the model atom for C II has been extended for the coolest, densest models, while higher ions of iron are accounted for in the hot part of the grid.

The grid has been extended to cooler, denser models and should now also cover the spectral type WC9. If you are interested in WO models, feel free to contact us.

Summary of the model atoms:

IonNo. of levels
He I 35
He II 26
He III 1
C II 32 3
C III 40
C IV 25
C V 1
O II 36
O III 33
O IV 29
IonNo. of levels
O V 36
O VI 16
G IV 18
G V 22
G VI 29
G VII 19
IonNo. of levels
G IX 15
G X 28
G XI 26
G XII 13
G XIV 14
G XV 1 10
G XVI 0 9
G XVII 0 1

Notes: Element "G" stands for the generic iron-group element, which combines the elements from Sc to Ni in solar relative mixture. In case of the "G" element, the number of levels given in the above table actually refers to superlevels.

Contour plots

For a couple of lines, contour plots of the equivalent width have been prepared. The contours are labeled with Wλ in Angstroem:

He I5876 ps pdf png
He II5412 ps pdf png
C III5696 ps pdf png
C IV5470 ps pdf png
C IV5801-5812 ps pdf png
O V5590 ps pdf png
Original web interface developed by Daniel M. Hamann and Wolf-Rainer Hamann in 2004. PHP-based rework by Andreas Sander (2016).
In case of problems with the PoWR website please contact Wolf-Rainer Hamann (
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