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 ( \sim 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 \dot { P } / P _ { sh } = 3.8 ( 3 ) \cdot 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 \% \pm 0.03 \% and \epsilon _ { - } = -2.44 \% \pm 0.02 \% .
Thus BF Ara is yet another in-the-gap nova with mass ratio of around q \approx 0.21 .

Key words : Stars : individual : BF Ara – binaries : close – novae , cataclysmic variables