[vsnet-outburst 23796] Re: (cba:chat) ASASSN-19pe: new SU UMa-type dwarf nova

[Tonny Vanmunster tonny.vanmunster@gmail.com via vsnet-outburst]

Dear colleagues,


Short update based on tonight’s (2019, Jun 12/13) V-filtered CCD photometry session of ASASSN-19pe, obtained again at CBA Extremadura Observatory, and covering an almost identical time span as yesterday’s session.

ASASSN-19pe is still bright at mag 12.25 (V) and the light curve still shows a complex structure with 0.06-0.08 mag modulations, which do not allow to firmly distinguish between an SU UMa-type or WZ Sge-type dwarf nova classification. Combining the two sessions, we still obtain a superhump period of 0.054 +/- 0.003d.

 

We will continue observing this target during the next evenings, hoping for the emergence of larger amplitude signals.

 

Best regards

Tonny

 

 

From: cba-chat [mailto:cba-chat-bounces at cbastro.org] On Behalf Of Tonny Vanmunster
Sent: woensdag 12 juni 2019 3:10
To: cba-chat at cbastro.org; 'Tonny Vanmunster'; 'Taichi Kato'; 'VSNET''; vsnet-campaign-dn at ooruri.kusastro.kyoto-u.ac.jp; vsnet-newvar at yahoogroups.com; 'vsnet-outburst'; vsnet-outburst at yahoogroups.com
Subject: (cba:chat) ASASSN-19pe: new SU UMa-type dwarf nova

 

Dear colleagues,

I have just concluded the analysis of my 2019, Jun 11/12 V-filtered CCD photometry session of ASASSN-19pe. Observations were made at CBA Extremadura Observatory, using a 0.40-m f/5.1 telescope and Trius SX-46 CCD camera, under clear skies. Due to the low position of this target in the evening sky, the duration of my session was limited to 2.6 hours, and affected by high airmass towards the end of the observations.

 

The resulting light curve apparently shows the presence of superhumps with an amplitude of 0.08 mag. Although the amplitude is rather small, the profile suggests an SU UMa-type dwarf nova classification. We do not exclude a WZ Sge-type classification either, due to the presence of very low amplitude modulations in the superhump structure. More observations during the following nights will provide more clarity. A period analysis using the ANOVA, Lomb-Scargle and PDM methods (Peranso), yields a combined superhump period of 0.054 +/- 0.003d. The object was at mag 12.07 (V) on Jun 11th. 

 

I will send my observations to AAVSO, CBA and VSNET for further analysis. 

 

Follow-up observations are recommended.

 

Best regards
Tonny


 

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

 <http://www.peranso.com> www.peranso.com

 

 

 

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