  We report CCD photometry of the dwarf nova BF Ara throughout fifteen
consecutive nights in quiescence. Light curve in this interval is dominated by
a large amplitude around 0.8 mag modulation consisting two periods. Higher
amplitude signal is characterized by period of 0.082159(4) days, which was
increasing at the rate of dotP/Psh = 3.8(3)* 10^{-5}. Weaker and stable signal
has period of 0.084176(21) days. Knowing the superhump period of BF Ara
determined by Kato et al. (2003) and equal to 0.08797(1) days, the first
modulation is interpreted as quiescent negative superhump arising from
retrograde precesion of titled accretion disk and the latter one as an orbital
period of the binary. The respective period excess and defect are epsilon_+ =
4.51% +/- 0.03% and epsilon_- = -2.44% +/- 0.02%. Thus BF Ara is yet another
in-the-gap nova with mass ratio q of around 0.21.
