We report on time-resolved CCD photometry during the 2005 June outburst of a dwarf nova , ASAS160048-4846.2 .
The observed light curves unambiguously showed embryonic humps with a period of 0.063381 ( 41 ) days , after which genuine superhumps emerged with a period of 0.064927 ( 3 ) days .
Based on evidence for double-peaked humps in the earlier stage of the outburst , this object might be qualified as the seventh member of WZ Sge-type dwarf novae after Var Her 04 .
If the former period is the same as , or very close to the orbital period of the system , as in other WZ Sge systems , the fractional superhump excess is about 2.4 { \% } .
This value is unexpectedly larger than that of other WZ Sge-type dwarf novae .
The early phase of our observing run provided evidence for the transition from chaotic humps to genuine superhumps , together with increasing the amplitude .