  We analysed a wealth of optical spectroscopic and photometric observations of
the bright (V=11.9) cataclysmic variable BG Tri. TheGaiaDR2 parallax gives a
distance d=334(8)pc to the source, making the object one of the intrinsically
brightest nova-like variables seen under a low orbital inclination angle.
Time-resolved spectroscopic observations revealed the orbital period of
P(orb)=3.h8028(24). Its spectroscopic characteristics resemble RW Sex and
similarnova-like variables. We disentangled the H alpha emission line into two
components, and show that one component forms on the irradiated face of the
secondary star. We suggest that the other one originates at a disc outflow area
adjacent to the L3 point.
