We report on time-resolved photometry of the superoutburst of an SU UMa-type dwarf nova , SDSS J013701.06-091234.9 in 2003 December-2004 January .
The obtained light curves definitely show superhumps with a period of 0.056686 ( 12 ) d , which is one of the shortest superhump periods among those of SU UMa-type dwarf novae ever observed .
Considering quiescent photometric studies , we estimated the fractional superhump excess to be 0.024 .
Spectroscopic observations by \citet szk03CVSDSS provided evidence for TiO bands despite the short orbital period , implying that the system has a luminous secondary star .
We draw a color-color diagram of SU UMa-type dwarf novae in quiescence using 2MASS archives , revealing that the location of this star in the color-color diagram is deviated from the general trend .
The distance to the system was roughly estimated to be 300 { \pm } 80 pc , using the empirical period-absolute magnitude relation and based on the proper motion .