  A quantitative spectral analysis of BA-type supergiants and bright giants in
an inner spiral arm region of the nearby spiral galaxy NGC 300 is presented,
based on observations with the Multi Unit Spectroscopic Explorer (MUSE) on the
European Southern Obsevatory, Very Large Telescope (ESO, VLT). The
flux-weighted gravity-luminosity relationship (FGLR), a stellar spectroscopic
distance determination method for galaxies, is extended towards stars at lower
luminosities. Point spread function fitting 3D spectroscopy was performed with
PampelMUSE on the datacube. The 16 stars with the highest signal-to-noise
ratios ($S/N s$) are classified with regard to their spectral type and
luminosity class using Galactic templates. They were analysed using hybrid
non-local thermodynamic equilibrium (non-LTE) model spectra to fit the
strongest observed hydrogen, helium, and metal lines in the
intermediate-resolution spectra. Supplemented by photometric data, this
facilitates fundamental stellar parameters and interstellar reddening which
have yet to be determined. Effective temperatures, surface gravities, reddening
$E(B-V)$, bolometric magnitudes and luminosities, as well as radii and masses
are presented for the sample stars. The majority of the objects follow the FGLR
as established from more luminous BA-type supergiants in NGC 300. An increase
in the scatter in the flux-weighted gravity-luminosity plane is observed at
these lower luminosities, which is in line with predictions from population
synthesis models.
