  In this paper we report on spatial intensity interferometry measurements
within the H$\alpha$ line on two stars: the Luminous Blue Variable supergiant
\PCygni\,and the late-type B supergiant Rigel. The experimental setup was
upgraded to allow simultaneous measurement of two polarization channels,
instead of one in our previous setup, and the zero baseline correlation
function on-sky to validate independent estimates obtained from the stellar
spectrum and the instrumental spectral throughput. Combined with simultaneous
spectra measurements and based on radiative transfer models calculated with the
code CMFGEN, we were able to fit our measured visibility curves to extract the
stellar distances. Our distance determinations for both \PCygni\ (1.61 $\pm$
0.18 kpc) and Rigel (0.26 $\pm$ 0.02 kpc) agree very well with the values
provided by astrometry with the Gaia and Hipparcos missions, respectively. This
result for Rigel was obtained by adopting a stellar luminosity of $L_{\star}$ =
123000 $L_{\odot}$, which is reported in the literature as being consistent
with the Hipparcos distance to Rigel. However, due to the lack of consensus on
Rigel's luminosity, we also explore how the adoption of the stellar luminosity
in our models affects our distance determination for Rigel. In conclusion, we
support, in an independent way, the distance to Rigel as the one provided by
the Hipparcos mission, when taking the luminosity of 123000 $L_{\odot}$ at face
value. This study is the first successful step towards extending the
application of the Wind Momentum Luminosity Relation method for distance
calibration from an LBV supergiant to a more normal late-type B supergiant.
