  The quantitative analysis of low resolution spectra of A and B supergiants is
used to determine a distance modulus of 24.99 +/- 0.10 mag (995 +/- 46 Kpc) to
the Local Group galaxy WLM. The analysis yields stellar effective temperatures
and gravities, which provide a distance through the Flux weighted
Gravity--Luminosity Relationship (FGLR). Our distance is 0.07 mag larger than
the most recent results based on Cepheids and the tip of the RGB. This
difference is within the 1-sigma overlap of the typical uncertainties quoted in
these photometric investigations. In addition, non-LTE spectral synthesis of
the rich metal line spectra (mostly iron, chromium and titanium) of the A
supergiants is carried out, which allows the determination of stellar
metallicities. An average metallicity of -0.87 +/- 0.06 dex with respect to
solar metallicity is found.
