The quantitative analysis of low resolution spectra of A and B supergiants is used to determine a distance modulus of 24.99 \pm 0.10 mag ( 995 \pm 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 \displaystyle \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 \pm 0.06 dex with respect to solar metallicity is found .