  The UV excess shown by elliptical galaxies in their spectra is believed to be
caused by evolved low-mass stars, in particular sdB stars. The stellar system
most similar to the ellipticals for age and metallicity, in which it is
possible to resolve these stars, is the bulge of our Galaxy. sdB star
candidates were observed in the color magnitude diagram of a bulge region by
Zoccali et al. (2003). The follow-up spectroscopic analysis of these stars
confirmed that most of these stars are bulge sdBs, while some candidates turned
out to be disk sdBs or cool stars. Both spectroscopic and photometric data and
a spectral library are used to construct the integrated spectrum of the
observed bulge region from the UV to the optical: the stars in the color
magnitude diagram are associated to the library spectra, on the basis of their
evolutionary status and temperature. The total integrated spectrum is obtained
as the sum of the spectra associated to the color magnitude diagram.
  The comparison of the obtained integrated spectrum with old single stellar
population synthetic spectra calculated by Bruzual & Charlot (2003) agrees with
age and metallicity of the bulge found by previous work. The bulge integrated
spectrum shows only a very weak UV excess, but a too strict selection of the
sample of the sdB star candidates in the color magnitude diagram and the
exclusion of post-Asymptotic Giant Branch stars could have influenced the
result.
