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 22. May 2026, replacing the older version which, for reference, is still accessible by choosing "WC-2018" in the drop-down menu. In the 2026 version the high resolution spectra now cover the whole range from 920 Å up to 30 μm without gaps.
For the following models a larger iron data file (doubled the number of superlevels by bisecting each energy band) was used:
16-18 16-22 16-23 17-23 18-19 18-26 19-25
If you are interested in WO models, feel free to contact us.
| Ion | No. of levels | |
|---|---|---|
| H I | 30 | 0 |
| H II | 1 | 0 |
| He I | 45 | 35 |
| He II | 30 | 26 |
| He III | 1 | |
| N I | 10 | 0 |
| N II | 38 | 0 |
| N III | 87 | 0 |
| N IV | 6 | 0 |
| C I | 15 | 0 |
| C II | 32 | 3 |
| C III | 40 | |
| C IV | 25 | |
| C V | 1 | |
| O I | 13 | 0 |
| O II | 37 | 36 |
| O III | 33 | |
| O IV | 2 | 29 |
| O V | 0 | 36 |
| Ion | No. of levels | |
|---|---|---|
| O VI | 0 | 16 |
| O VII | 0 | 1 |
| S II | 32 | 0 |
| S III | 23 | 0 |
| S IV | 25 | 0 |
| S V | 1 | 0 |
| Mg II | 32 | 0 |
| Mg III | 43 | 0 |
| Si II | 20 | 0 |
| Si III | 24 | 0 |
| Si IV | 55 | 0 |
| Si V | 1 | 0 |
| P III | 47 | 0 |
| P IV | 12 | 0 |
| P V | 3 | 0 |
| Al II | 10 | 0 |
| Al III | 10 | 0 |
| Al IV | 10 | 0 |
| Ne I | 8 | 0 |
| Ion | No. of levels | |
|---|---|---|
| Ne II | 18 | 0 |
| Ne III | 18 | 0 |
| G I | 1 | 0 |
| G II | 3 | 0 |
| G III | 13 | 1 |
| G IV | 18 | 36 |
| G V | 1 | 42 |
| G VI | 0 | 58 |
| G VII | 0 | 37 |
| G VIII | 0 | 28 |
| G IX | 0 | 30 |
| G X | 0 | 50 |
| G XI | 0 | 48 |
| G XII | 0 | 21 |
| G XIII | 0 | 26 |
| G XIV | 0 | 26 |
| G XV | 0 | 18 |
| G XVI | 0 | 11 |
| 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.
For a couple of lines, contour plots of the equivalent width have been prepared. The contours are labeled with Wλ in Angstroem:
| logQ | HII | ps | png | txt | |
| logQ | HeI | ps | png | txt | |
| logQ | HeII | ps | png | txt | |
| He I | 5876 | ps | png | ||
| He II | 5412 | ps | png | ||
| C III | 5696 | ps | png | ||
| C IV | 5470 | ps | png | ||
| C IV | 5801-5812 | ps | png | ||
| O V | 5590 | ps | png |
The following contour plot relates the stellar temperature T, which refers to the hydrostatic radius, to the "effective" temperature T2/3 referring to the radius of the optical depth 2/3. The contours are labeled with log T2/3 in Kelvin.
| ps | png | txt |
Parameters of the grid models: parameters.txt
The corresponding contour plots for the outdated 2018 version of the WC grid can still be found here for reference.