We report on our photometric observations of the 2016 superoutburst of ASASSN-16eg .
This object showed a WZ Sge-type superoutburst with prominent early superhumps with a period of 0.075478 ( 8 ) d and a post-superoutburst rebrightening .
During the superoutburst plateau , it showed ordinary superhumps with a period of 0.077880 ( 3 ) d and a period derivative of 10.6 ( 1.1 ) \times 10 ^ { -5 } in stage B .
The orbital period ( P _ { orb } ) , which is almost identical with the period of early superhumps , is exceptionally long for a WZ Sge-type dwarf nova .
The mass ratio ( q = M _ { 2 } / M _ { 1 } ) estimated from the period of developing ( stage A ) superhumps is 0.166 ( 2 ) , which is also very large for a WZ Sge-type dwarf nova .
This suggests that the 2:1 resonance can be reached in such high- q systems , contrary to our expectation .
Such conditions are considered to be achieved if the mass-transfer rate is much lower than those in typical SU UMa-type dwarf novae that have comparable orbital periods to ASASSN-16eg and a resultant accumulation of a large amount of matter on the disk is realized at the onset of an outburst .
We examined other candidates of long-period WZ Sge-type dwarf novae for their supercycles , which are considered to reflect the mass-transfer rate , and found that V1251 Cyg and RZ Leo have longer supercycles than those of other WZ Sge-type dwarf novae .
This result indicates that these long-period objects including ASASSN-16eg have a low mass-transfer rate in comparison to other WZ Sge-type dwarf novae .