Daisaku Nogami
(vsnet-alert 362,Berto Monard)
The dwarf nova VZ Pyxidis was seen in outburst with the apogee 40x120.
0857-24 VZ Pyxidis
UT Magn
March 16.747 12.3 vs GSC sequences.
also (in follow up) 0854-41CU Velorum March 16.736 11.0
Best regards,
Berto Monard,
Pretoria
Follow up observations on the active dwarf novae VZ Pyxidis and CU Velorum with the apogee 40x120
UT Magn CU VEL in March 96 16.907 11.0 17.022 11.0 17.768 10.8 17.857 10.9 and still going strong! VZ PYX in March 96 16.906 12.3 17.817 12.2 17.862 12.1 I will keep you posted from Pretoria if the nice weather holds out. Regards, Berto Monard
(vsnet-alert 365, T. Kato)
Upon notification of an outburst of VZ Pyx by Berto Monard (vsnet-alert 362), we obtained V-band CCD observations on Mar. 18 at Ouda Station, Kyoto University. The resultant data clearly show superhumps with an amplitude of 0.25 mag, and a period of 0.076 day. The humps show sharp rising branches and slower declines, which are characteristic of superhumps during the early stage of a superoutburst. The present observations thus clearly established the SU UMa-type nature of this object. VZ Pyx is probably the first object below the period gap, which shows both characterstics of an SU UMa-type dwarf nova and an intermediate polar (from a period of 0.812 hr during the decline from outbursts; see Remiilard et al. below)
Regards,
Taichi Kato and Ouda team
VZ Pyx was originally discovered as an X-ray source, H0857-242, which was subsequenly identified to be a cataclysmic variable. References:
De Martino et al. 1992, IAUC No. 5481
Barwig et al. 1993, IAUC No. 5689
Remillard et al. 1994, ApJ 428, 785
(vsnet-alert 369)
Dear colleagues,
We (Ouda Team) succeeded in observing VZ Pyx on March 17 and 20 at the Ouda Station. The improved superhump period is 0.07576 (+- 0.00003) day. The observation on March 20 shows the secondary peaks in superhumps seems to have been growing.
Best regards,
Daisaku Nogami
Return to HomePage