Dear colleagues,
TCP J06364062+3318310 was discovered by K. Sokolovsky et al. (NMW Survey) on
2025 Nov 17.99 at mag 13.6CV. The quiescent counterpart is a 21.3 r mag
star, implying an outburst amplitude of ~8 mag.
I have just completed the analysis of my unfiltered CCD time-series
observations of TCP J06364062+3318310, obtained on 2025 Nov 25/26 at CBA
Extremadura Observatory. The data were acquired under clear skies with a
0.40-m f/5.1 telescope and a Moravian G2-4000 CCD camera.
I also obtained observations on several nights prior to Nov 25/26, but those
did not reveal any obvious modulation. In contrast, the Nov 25/26 light
curve clearly shows regular superhump modulations with an amplitude of 0.30
mag. A period analysis using ANOVA, Lomb-Scargle, Generalized-Lomb-Scargle
and PDM methods (Peranso 3.1) yields a combined superhump period of 0.0661
+/- 0.0008d. The object was measured at mag CV = 15.3 on Nov 26th.
Image calibration and photometry were carried out using the latest release
of Phoranso, which enabled simultaneous photometry of several additional
variable stars in the same field of view.
These results establish TCP J06364062+3318310 as a new SU UMa-type dwarf
nova. Further follow-up observations are strongly encouraged to refine the
superhump period and study its evolution.
I will submit my observations to AAVSO, CBA and VSNET for further analysis.
With kind regards,
Tonny
---
Tonny Vanmunster
CBA Belgium Observatory
CBA Extremadura Observatory
http://www.cbabelgium.co <http://www.cbabelgium.com/> m
PERANSO : The Light Curve and Period Analysis Software
http://www.peranso.co <http://www.peranso.com/> m
PHORANSO: Photometric Reduction and Analysis Software
http://www.phoranso.com <http://www.phoranso.com/>
TCP J05384230+7051377: new WZ Sge-type dwarf nova
We posted our spectroscopic follow-up result of TCP J05384230+7051377 to
ATel.
ATel #17485: Spectroscopic confirmation of TCP J05384230+7051377 as a WZ
Sge-type dwarf nova <https://www.astronomerstelegram.org/?read=17485>
We concluded that this object is a new WZ Sge-type dwarf nova because Hα
has a narrow emission core and its spectrum shows a blue continuum with
the Balmer and HeI absorption lines.
Also, we estimated this object as p ~ 0.06d from Itoh-san's data.
However p ~ 0.06d is a weak signal, so further observation will provide
a more accurate estimate of the period.
best regard,
Hiromasa Hoke
TCP J09370380+1657350: possible new superoutburst
Gavin Ramsay reported that GOTO detected TCP J09370380+1657350
in outburst on 2025 Nov 18 03:41:50 UT (20251118.1534).
Reported magnitude: L = 16.18 (400–700 nm).
This object was previously identified as a WZ Sge-type system.
For reference, see also the past report:
[vsnet-alert 25216] TCP J09370380+1657350: new WZ Sge-type dwarf nova
[vsnet-alert 25218] Spectrum of TCP J09370380+1657350
http://www.astronomerstelegram.org/?read=14309https://vsx.aavso.org/index.php?view=detail.top&oid=2215274
Dear colleagues,
TCP J21314718+3825463 was discovered by XOSS (Xingming Observatory Sky
Survey) on 2025 Nov 07.6 at mag 14.70C. The quiescent counterpart is a 22.5
g mag star, implying an outburst amplitude of ~8 mag.
I have just completed the analysis of my unfiltered CCD observations of TCP
J21314718+3825463, obtained on 2025 Nov 11/12 and Nov 14/15 at CBA
Extremadura Observatory. The data were acquired under clear skies with a
0.40-m f/5.1 telescope and a Moravian G2-4000 CCD camera.
The Nov 11/12 light curve did not reveal any obvious modulation. However,
the Nov 14/15 light curve clearly shows regular superhump modulations with
an amplitude of 0.23 mag. A period analysis performed with ANOVA,
Lomb-Scargle, Generalized-Lomb-Scargle and PDM methods (Peranso 3.1) yields
a combined superhump period of 0.0567 +/- 0.0016d. The object was measured
at mag CV = 16.0 on Nov 15th.
Image calibration and photometry were carried out using the latest release
of Phoranso, which enabled simultaneous photometry of several additional
variable stars in the same field of view.
These results establish TCP J21314718+3825463 as a new SU UMa-type dwarf
nova. Further follow-up observations are strongly encouraged to refine the
superhump period and study its evolution.
I will submit my observations to AAVSO, CBA and VSNET for further analysis.
With kind regards,
Tonny
---
Tonny Vanmunster
CBA Belgium Observatory
CBA Extremadura Observatory
http://www.cbabelgium.co <http://www.cbabelgium.com/> m
PERANSO : The Light Curve and Period Analysis Software
http://www.peranso.co <http://www.peranso.com/> m
PHORANSO: Photometric Reduction and Analysis Software
http://www.phoranso.com <http://www.phoranso.com/>