  We search for LBV stars in galaxies outside the Local Group. Here we present
a study of two bright $H\alpha$ sources in the NGC 247 galaxy. Object
j004703.27-204708.4 ($M_V=-9.08 \pm 0.15^m$) shows the spectral lines typical
for well-studied LBV stars: broad and bright emission lines of hydrogen and
helium He I with P Cyg profiles, emission lines of iron Fe II, silicon Si II,
nitrogen N II and carbon C II, forbidden iron [Fe II] and nitrogen [N II]
lines. The variability of the object is $\Delta B = 0.74\pm0.09^m$ and $\Delta
V = 0.88\pm0.09^m$, which makes it reliable LBV candidate. The star
j004702.18-204739.93 ($M_V=-9.66 \pm 0.23^m$) shows many emission lines of iron
Fe II, forbidden iron lines [Fe II], bright hydrogen lines with broad wings,
and also forbidden lines of oxygen [O I] and calcium [Ca II] formed in the
circumstellar matter. The study of the light curve of this star also did not
reveal significant variations in brightness ($\Delta V = 0.29\pm0.09^m$). We
obtained estimates of interstellar absorption, the photosphere temperature, as
well as bolometric magnitudes $M_\text{bol}=-10.5^{+0.5}_{-0.4}$ and
$M_\text{bol}=-10.8^{+0.5}_{-0.6}$, which corresponds to bolometric
luminosities $\log(L_\text{bol}/L_{\odot})=6.11^{+0.20}_{-0.16}$ and
$6.24^{+0.20}_{-0.25}$ for j004703.27-204708.4 and j004702.18-204739.93
respectively. Thus, the object j004703.27-204708.4 remains a reliable LBV
candidate, while the object j004702.18-204739.93 can be classified as
B[e]-supergiant.
