Dear colleagues,
ASASSN-25dt was discovered by the ASAS-SN Survey (Ohio State University) on
2025 Sep 05.3 at mag 14.5 V/g. The quiescent counterpart is a 20.1 g mag
Pan-STARRS1 object, implying an outburst amplitude of ~5-6 mag.
I have just completed the analysis of my unfiltered CCD observations of
ASASSN-25dt, obtained on 2025 Sep 10/11 and Sep 11/12 at CBA Extremadura
Observatory. The data were acquired under (mostly) clear skies with a 0.40-m
f/5.1 telescope and a Moravian G2-4000 CCD.
The Sep 10/11 light curve showed only irregular, small-amplitude
variability. However, the Sep 11/12 light curve clearly exhibits superhump
modulations with an amplitude of 0.27 mag. Period analysis with ANOVA,
Lomb-Scargle, Generalized-Lomb-Scargle and PDM methods (Peranso 3.1) yields
a combined superhump period of 0.0605 +/- 0.0008d. The object was measured
at mag CV = 15.9 on Sep 12th.
Image calibration and photometry were carried out with the latest release of
Phoranso.
These results establish ASASSN-25dt as a new SU UMa-type dwarf nova.
Follow-up observations are encouraged.
I will submit my observations to AAVSO, CBA and VSNET for further analysis.
With kind regards,
Tonny
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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 J21091443-0917104 (=ASASSN-25dq): new SU UMa-type dwarf nova
NMW Survey discovered TCP J21091443-0917104 at 12.4 mag on 2025 08 22.8877
UCT. They suspected it could be a new UV Cet star based on its coincidence
with the bright Gaia object (Gaia DR3 6896395696896704000; G=14.44,
Plx=3.12 +/-0.04 mas).
https://vsx.aavso.org/index.php?view=detail.top&oid=10867963http://www.cbat.eps.harvard.edu/unconf/followups/J21091443-0917104.html
S. Brincat and J. Hambsch have reported the time-resolved observations.
Combining the observations by W. Goltz on AAVSO, I obtained a single-peak
variation with a period of 0.05887(3) d, from the outburst maximum.
ZTF light curve also shows a slow decline over the last two weeks, which is
unlike a UV Cet star but agrees with a dwarf nova outburst.
https://alerce.online/object/ZTF21abtlwbr
Thus TCP J21091443-0917104 is most likely a new SU UMa-type dwarf nova.
Considering its relatively short superhump period and expected large
amplitude of outburst, the Gaia object can be a foreground star. The object
is currently g=14.2 mag.
Best regards,
Yusuke
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South African Astronomical Observatory, Postdoc fellow
Yusuke TAMPO / 反保 雄介
EMAIL: tampo(a)kusastro.kyoto-u.ac.jp
ALT. EMAIL: yusuke(a)saao.ac.za
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