[Aavso-photometry] Optical transient OT_J021110.2+171624 : UGSU dwarf nova nature confirmed

Fri Feb 1 12:08:57 EST 2008

Dear colleagues,

A very quick message (I leave on holiday in a few hours) to inform you that
subsequent observations of  OT_J021110.2+171624 by CBA observer Tom Krajci
(obtained on JD +497.5) clearly confirm the SU UMa-type nature of this dwarf
nova. I will publish a detailed analysis in about a week from now, but Tom's
observations show full-grown superhumps with an amplitude of 0.35 mag and a
period close to 0.082 +/- 0.002 d.

Best regards,
Tonny Vanmunster

Tonny Vanmunster
CBA Belgium Observatory
http://www.cbabelgium.com <http://www.cbabelgium.com/> 

PERANSO : The Light Curve and Period Analysis Software
http://www.peranso.com <http://www.peranso.com/> 

  _____  

From: cvnet-outburst at yahoogroups.com [mailto:cvnet-outburst at yahoogroups.com]
On Behalf Of Tonny Vanmunster
Sent: Thursday, January 31, 2008 12:29 AM
To: aavso-photometry at mira.aavso.org; cvnet-discussion at yahoogroups.com;
'CVnet outburst'
Cc: Cba-Chat; cba-news
Subject: [cvnet-outburst] Optical transient OT_J021110.2+171624 is most
likely a new UGSU-type dwarf nova

Dear colleagues,

Earlier today, Patrick Wils announced (on cvnet-discussion) the detection by
the Catalina Sky Survey of an optical transient (mag 14.3) on Jan 29th, that
was suspected to be an outburst of USNO-B1.0 1072-0031053 (position RA =
02:11:10.19, Decl = +17:16:24.4, J2000.0), a star which is normally R=19.2.
Patrick furthermore reported that object appeared bright on 2 out of 9
POSSII images.

Following Patrick's announcement, I started unfiltered CCD time-series
observations of the new OT at CBA Belgium Observatory on Jan 30.833 UT,
2008, using a 0.35-m f/6.3 telescope and ST-7XME CCD camera. Sky conditions
were good, and the session lasted for 2 hours. The resulting light curve is
presented at my website (www.cbabelgium.com) and shows a superhump-like
structure with an amplitude of 0.15 mag. Given the short duration of the
session, it's difficult to accurately establish the hump period. Using
Peranso's implementation of the ANOVA method, I find a value of 0.063 +/-
0.009 d. The ANOVA period window and phase diagram for P = 0.063d are
presented as well.

Follow-up CCD and spectroscopic observations are highly needed to further
study the lightcurve characteristics of this dwarf nova and to firmly secure
its UGSU nature. 

Tonny Vanmunster
CBA Belgium Observatory
http://www.cbabelgi <http://www.cbabelgium.com> um.com 

PERANSO : The Light Curve and Period Analysis Software
http://www.peranso. <http://www.peranso.com> com

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