V_HWHM(5007) vs. V_HWHM(Hβ) for four 0.625 M_⊙ and two 0.605 M_⊙ sequences with different metallicities as indicated in the legend. Evolution proceeds always from low towards higher velocities. Plotted are only the evolutionary phases with T_eff ≤ T_max. The models are compared with recent HWHM velocity measurements of Milky Way bulge objects, either with apparently unsplit line profiles (filled symbols) or with split profiles (open symbols), provided to us by Richer (see also Richer et al. 2008, 2009, 2010a), and assuming that the halfwidth velocities of Hβ and Hα are the same. Only objects with 5007 Å line strengths greater than Hβ are considered. Accordingly, thin line sections at low velocities indicate models for which L(5007) ≤ L(Hβ). The model profiles are broadened by a Gaussian with FWHM of 11 km s^-1 in order to comply with the spectral resolution of the observations. Crossed symbols mark objects which are known to posses [WC]-type central stars (see Górny et al. 2004).