Dear colleagues,
I have just finished analysing my unfiltered CCD observations of
ASASSN-22ho, obtained on 2022, June 02/03 at CBA Belgium Observatory, using
a 0.40-m f/10.0 telescope and QHY-286M CMOS camera under clear skies.
Regular superhumps with an amplitude of 0.35 mag are very clearly visible in
the resulting light curve, establishing ASASSN-22ho as a new SU UMa-type
dwarf nova. A period analysis using the ANOVA, Lomb-Scargle,
Generalized-Lomb-Scargle and PDM methods (Peranso 3.0), yields a combined
(long) superhump period of 0.0902 +/- 0.0025d. The object was at mag CV =
16.5 on Jun 03rd.
I will send my observations to AAVSO, CBA and VSNET for further analysis.
Best regards
Tonny
---
Tonny Vanmunster
CBA Belgium Observatory
CBA Extremadura Observatory
http://www.cbabelgium.com
PERANSO : The Light Curve and Period Analysis Software
http://www.peranso.com
Dear colleagues,
I have just finished analysing my unfiltered CCD observations of TCP
J22561804+4109534, obtained on 2022, July 04/05 at CBA Belgium Observatory,
using a 0.40-m f/10.0 telescope and QHY-286M CMOS camera under clear skies.
I have been observing this object during multiple nights between June 27th
and now. On all previous nights, no obvious modulations were visible in the
light curve, except for last night when superhumps with an amplitude of 0.14
mag became very clearly visible. A period analysis using the ANOVA,
Lomb-Scargle, Generalized-Lomb-Scargle and PDM methods (Peranso 3.0), yields
a combined superhump period of 0.0650 +/- 0.0011d. The object was at mag CV
= 15.3 on Jul 05th.
The superhump profile shows no signs of a double-waved pattern, and I could
not detect early superhumps in my data. Yet, the large outburst amplitude of
~7.4 mag, and the long time for superhumps to develop (approx. 9 days) make
this a very likely WZ Sge-type dwarf nova. Follow-up observations are
recommended to further track the evolution of the superhumps.
I will send my observations to AAVSO, CBA and VSNET for further analysis.
Best regards
Tonny
---
Tonny Vanmunster
CBA Belgium Observatory
CBA Extremadura Observatory
http://www.cbabelgium.com
PERANSO : The Light Curve and Period Analysis Software
http://www.peranso.com
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> This long outburst began between 2022 July 16 and 21. It was
> observed at mag. 13 for five days, followed by a rapid fading
> on July 27. The outburst was considerably longer than short
> outbursts of this dwarf nova, but shorter than standard UGSU
> superoutbursts (~14 days).
Might be an EI Psc star, although the peak M_V is not
too faint.
Variable Reticuli 2005 (UGSU:)
https://www.aavso.org/vsx/index.php?view=detail.top&oid=161100
Recent ASAS-SN Sky Patrol (Shappee et al. 2014ApJ...788...48S
and Kochanek et al. 2017PASP..129j4502K) light curve and data:
https://asas-sn.osu.edu/sky-patrol/coordinate/38d59ff4-1572-40ef-a0c5-e280e…
This long outburst began between 2022 July 16 and 21. It was
observed at mag. 13 for five days, followed by a rapid fading
on July 27. The outburst was considerably longer than short
outbursts of this dwarf nova, but shorter than standard UGSU
superoutbursts (~14 days).
Regards,
Patrick
TCP J22561804+4109534 rebrightenings
Tamas Tordai has reported further observations.
Five rebrightenings have been recorded up to July 24.
The amplitudes, however, are decreasing and frequent
small-amplitude rebrightenings resemble those of WZ Sge.
This phenomenon is atypical for this orbital period.
TCP J22561804+4109534 second rebrightening
Tamas Tordai reported the second rebrightening
on July 19-20.
See [vsnet-alert 26866]
It would be worth noting that the period 0.065 d is
long for a WZ Sge star. If this is indeed a WZ Sge star,
it must be a period bouncer.