Erratum
After a thorough comparison with the code of Leitherer & Heckman (1995)
and working on its succesor version (Leitherer, Schaerer, et al., in prep.)
an error was discovered in the code used
in Schaerer & Vacca (1998, ApJ, 497, 618, hereafter SV98).
The bug concerned the normalisation of the fluxes from WR atmosphere
models.
This error affects only some quantities during the WR phases.
There the following quantities are affected:
- integrated photon fluxes (Qi)
- nebular Hbeta, Halpha equivalent widths and line intensities
E.g. the following quantities are NOTaffected or only insignificantly:
- WR populations
- WR line strengths
- colors
- ...
The conclusions of SV98 and the qualitative behaviour of the model
predictions are not changed.
The Figures from SV98 affected by this error have been updated and are
given here:
Fig. 4
Fig. 6
Fig. 7a
Fig. 7b
Fig. 8
Fig. 9
Fig. 12
Fig. 14
Fig. 15
Fig. 16
Fig. 18
Fig. 21
tar-file with all updated Figs.
Some of the changes are:
- in models at solar metallicity and higher (Z>~0.02)
the contribution of WR stars to the ionizing flux is larger than before
- the predicted nebular HeII 4686 emission at low Z is somewhat
increased
- ...
I sincerely apologize for the inconvenience.
Last modified: July 7, 1998 (Daniel Schaerer, schaerer@obs-mip.fr)