  2MASS J20395358+4222505 is an obscured early B supergiant near the massive OB
star association Cyg OB2. Despite its bright infrared magnitude (K$_{s}$=5.82)
it has remained largely ignored because of its dim optical magnitude (B=16.63,
V=13.68). In a previous paper we classified it as a highly reddened,
potentially extremely luminous, early B-type supergiant. We obtained its
spectrum in the U, B and R spectral bands during commissioning observations
with the instrument MEGARA@GTC. It displays a particularly strong H$\alpha$
emission for its spectral type, B1 Ia. The star seems to be in an intermediate
phase between super- and hypergiant, a group that it will probably join in the
near (astronomical) future. We observe a radial velocity difference between
individual observations and determine the stellar parameters, obtaining
T$_{eff}$ = 24000 K, logg$_{c}$= 2.88 $\pm$ 0.15. The rotational velocity found
is large for a B-supergiant, vsini= 110 $\pm$ 25 km s$^{-1}$. The abundance
pattern is consistent with solar, with a mild C underabundance (based on a
single line). Assuming that J20395358+4222505 is at the distance of Cyg OB2 we
derive the radius from infrared photometry, finding R= 41.2 $\pm$ 4.0
R$_{\odot}$, log(L/L$_{\odot}$)= 5.71 $\pm$ 0.04 and a spectroscopic mass of
46.5 $\pm$ 15.0 M$_{\odot}$. The clumped mass-loss rate (clumping factor 10) is
very high for the spectral type, $\dot{M}$ = 2.4x10$^{-6}$ M$_{\odot}$
a$^{-1}$. The high rotational velocity and mass-loss rate place the star at the
hot side of the bi-stability jump. Together with the nearly solar CNO abundance
pattern, they may also point to evolution in a binary system, J20395358+4222505
being the initial secondary.
