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[vsnet-obs 5559] comment on V795 Cyg

Comment to CVC 134 (vsnet-alert 843), posted by T. Vanmuster:

The VSNET record of the last outburst in 1995 May plus some info.

> Subject: [vsnet-alert 124] Rare Outburst of V795 Cyg
> 
> Visual magnitude estimates by P. Schmeer, Bischmisheim, Germany:
>  
> V795 CYGNI  (UGSS)
> May   2.09  UT,  13.7:;  3.001,  13.1 ;  3.057,  12.9
> Sequence:   AAVSO WZ Sge
> Instrument: 203-mm SCT
> Uncertain sighting on May 2.09 UT (haze).
> One night later V795 Cyg was considerably brighter.
> The previous outburst was detected by me on 1994 Aug. 26.929 UT at mv= 12.9.
>  
> Regards,
> Patrick

> Subject: [vsnet-alert 125] Re: Rare Outburst of V795 Cyg (& AL Com)
> 
> Dear Colleagues,
> 
>    To make our knowledge of V795 Cyg more complete, I would like to add
> some outburst records of this dwarf nova.
> 
>    The discovery paper in Vatican Ric. Astr. gave following dates of
> maxima.  From this article, I have estimated the outburst duty cycle
> (fraction of observations brighter than mag 14.0) as 0.016.  This value
> is one of the smallest among dwarf novae confirmed or suspected to be
> above the period gap.  The observation of the current outburst might
> provide a clue in understading the physics of dwarf novae of this kind.
> 
>     JD        mpg      comment
>   2433982     13.5     two plates
>     35303     13.5     three plates, fainter than 16.4 on 35309
>     35623     14.6     isolated plate
> 
>    The early VSOLJ record gives two outbursts in 1987 and 1988, the one
> in August 1987 was probably the first visually observed outburst.  Upon
> notification by P. Schmeer, I obtained a 1.5-hour CCD photometry during
> November 1992 outburst.  The current dwarf nova classification (UGSS) is
> based on apparent absence of superhumps in this photometric run.
> 
> Regards,
> Taichi Kato

   Our classification of this star being UGSS was based on this CCD
photometry, which confirmed the earlier claim by S. Fujino (VSOLJ) of the
non-existence of superhumps during the 1987 outburst.  S. Fujino observed
this star serveral hours with his photographic system which had been proven
to be very efficient by detections of superhumps in T Leo, AW Gem, AQ Eri
(cf. VSOLJ Variable Star Bulletin).

Regards,
Taichi Kato