(Wide-field outburst image by Berto Monard)
(Superhumps observed by Roland Santallo and Greg Bolt)
V877 Ara (=NSV08383) outburst
Rod Stubbings reports that this dwarf nova is undergoing a bright outburst! This object is a candidate SU UMa-type dwarf nova (the last likely superoutburst occurred in 2001 August). Observers are strongly urged to make time-series CCD observations to detect superhumps!
YYYYMMDD(UT) mag observer 20020529.369 <142 (Rod Stubbings) 20020529.740 <143 (Berto Monard) 20020601.406 <146 (Rod Stubbings) 20020602.392 <144 (Rod Stubbings) 20020603.419 <144 (Rod Stubbings) 20020604.521 <144 (Rod Stubbings) 20020607.424 138 (Rod Stubbings) 20020607.450 139 (Rod Stubbings)
Dear Colleagues,
Roland Santallo (Southern Stars Observatory, Tahiti French Polynesia) just reported time-series photometry of V877 Ara (NSV08383) taken on June 9. The data show fully developed superhumps (amplitude 0.25-0.30 mag), establishing that V877 Ara is a new member of SU UMa-type dwarf novae. Although exact period determination is still difficult on single-night data, the system has a relatively long (around 0.08 d) superhump period. Observers are strongly urged to continue observation as long as possible (prefreably more than two superhump cycles per night) in order to precisely determine the superhump period.
Congratulations to Roland Santallo on this breath-taking success!
We hope we will later prepare a special VSNET page on this discovery.
Regards, Taichi Kato VSNET Collaboration team
Dear Colleagues,
We have received a report of V877 Ara on June 10 from Stan Walker. The report and the light curve indicates the superhump period of 0.0842 d. This period confirms the initial period determined from the single-night observation by Roland Santallo. Since the period is close to the border of the period gap, further intensive observations are very strongly encouraged.
Regards, Taichi Kato VSNET Collaboration team
V877 Ara image and position
Roland Santallo (Southern Stars Observatory, Tahiti French Polynesia) has kindly sent images. The JPEG file is placed at:
USNO0225.27372547 171653.966 -653251.46 (2000.0) 20.3 21.6
which is different from previous identidications. More detailed identification awaits Yamaoka-san's astrometry. The quiescent counterpart seems to be much fainter than was previously thought. This is consistent with the superhump detection.
Anyway, observers should refer to the above image before observing, since the position has a large offset from the GCVS/NSV/Downes catalogs. Further obseravtions are very strongly requested!
Regards, Taichi Kato VSNET Collaboration team
Return to Daisaku Nogami's page
Return to HomePage