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h="ATskLdcvdyDQgaK69xXyAJ/4Bq3KRWke0qvDG39lAXXlhqMUCQ==" X-Original-Sender: Tonny.Vanmunster@gmail.com X-Original-Authentication-Results: gmr-mx.google.com; dkim=pass header.i=@gmail.com header.s=20251104 header.b=PvGXYEbe; spf=pass (google.com: domain of tonny.vanmunster@gmail.com designates 2a00:1450:4864:20::32f as permitted sender) smtp.mailfrom=tonny.vanmunster@gmail.com; dmarc=pass (p=NONE sp=QUARANTINE dis=NONE) header.from=gmail.com; dara=pass header.i=@googlegroups.com X-Spam-Checked-In-Group: cbastro-chat@googlegroups.com X-Google-Group-Id: 24034821666 This is a multipart message in MIME format. ------=_NextPart_000_04F7_01DD2C5C.DE627230 Content-Type: text/plain; charset="UTF-8" Content-Transfer-Encoding: quoted-printable Dear colleagues, =20 The outburst of TCP J14515140+6613240 was discovered by the = NMW-TexasTech survey team on 2026 Jul 29.3 UT at mag g =3D 13.2. The = quiescent counterpart is a 21.2 g mag Pan-STARRS1 star, implying an = outburst amplitude of ~8 mag. =20 I have completed the analysis of my unfiltered CCD time-series = observations of TCP J14515140+6613240, obtained on 10 out of 11 nights = between 2026 Aug 03/04 and 13/14 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.=20 =20 The combined light curve clearly shows regular superhump modulations = with an amplitude of 0.34 mag. A period analysis using ANOVA, = Lomb-Scargle, Generalized-Lomb-Scargle and PDM methods (Peranso 3.1) = yields a combined superhump period of 0.0566 +/- 0.0002d. The object was = measured at mag CV =3D 15.7 on Aug 14th. =20 Superhumps were absent till 2026 Aug 08/09, when they first started to = appear. No early superhumps were detected with sufficient evidence. =20 Image calibration and photometry were carried out using the latest = release of Phoranso, which enabled simultaneous photometry of additional = variable stars in the same field of view. =20 The detection of superhumps with a period of 0.0566 d securely = establishes TCP J14515140+6613240 as an SU UMa-type dwarf nova. The = large outburst amplitude (~8 mag) might be consistent with a WZ Sge-type = classification, but the absence of early superhumps does not (yet) = support such classification.=20 =20 Continued monitoring is strongly encouraged. =20 I will submit my observations to AAVSO, CBA and VSNET for further = analysis. =20 With kind regards, Tonny =20 --- =20 Tonny Vanmunster CBA Belgium Observatory CBA Extremadura Observatory http://www.cbabelgium.co m =20 --=20 You received this message because you are subscribed to the Google = Groups "CBA Chat" group. To unsubscribe from this group and stop receiving emails from it, send = an email to cbastro-chat+unsubscribe@googlegroups.com = . To view this discussion visit = https://groups.google.com/d/msgid/cbastro-chat/04dd01dd2c3a%24d480a970%24= 7d81fc50%24%40gmail.com = . ------=_NextPart_000_04F7_01DD2C5C.DE627230 Content-Type: text/html; boundary="----=_NextPart_000_04DE_01DD2C4B.980A3CC0"; charset="UTF-8" Content-Transfer-Encoding: quoted-printable

Dear colleagues,

 

The outburst = of TCP J14515140+6613240 was discovered by the NMW-TexasTech survey team = on 2026 Jul 29.3 UT at mag g =3D 13.2.  The quiescent counterpart = is a 21.2 g mag Pan-STARRS1 star, implying an outburst amplitude of ~8 = mag.

 

I have = completed the analysis of my unfiltered CCD time-series observations of = TCP J14515140+6613240, obtained on 10 out of 11 nights between 2026 Aug = 03/04 and 13/14 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 combined light curve clearly shows regular = superhump modulations with an amplitude of 0.34 mag. A period analysis = using ANOVA, Lomb-Scargle, Generalized-Lomb-Scargle and PDM methods = (Peranso 3.1) yields a combined superhump period of 0.0566 +/- 0.0002d. = The object was measured at mag CV =3D 15.7 on Aug = 14th.

 

Superhumps = were absent till 2026 Aug 08/09, when they first started to appear. No = early superhumps were detected with sufficient = evidence.

 

Image = calibration and photometry were carried out using the latest release of = Phoranso, which enabled simultaneous photometry of additional variable = stars in the same field of view.

 

The detection of superhumps with a period of 0.0566 d securely establishes TCP J14515140+6613240 as = an SU UMa-type dwarf nova. The large outburst amplitude (~8 mag) might be consistent with a = WZ Sge-type classification, but the absence of early = superhumps does not (yet) support such classification. =

 

Continued = monitoring is strongly = encouraged.

 

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.com

 

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