The outbursts of the Halo symbiotic binary and super-soft X-ray source AG Dra are known to come in series (1932-1939, 1949-1955, 1963-1966, 1980-1986, 1994-1996, 2002-2008, 2015-2018, eg. Leedjarv et al. 2016 MNRAS 456, 2558, Galis et al. 2017, OEJV 180, 24, Merc et al. 2018, RNAAS, 2, 142). The less frequent, longer lasting, and larger amplitude eruptions (peaking around V~8.0) are usually of the "cool" type, while the faster-evolving and lower amplitude outbursts (peaking around V~8.8) normally come in trains of 3-4 individual events and are of the "hot" type (Gonzalez-Riestra et al. 1999, A&A 1999, 347, 478). The hot-type outbursts are characterized by a flux ratio HeII/Hbeta rising well above 1 and by the OVI Raman-scattered bands (6825, 7088 Ang) turning stronger compared to quiescence, while during a cool-type event the HeII/Hbeta flux ratio reduces to 0.5 or less and the OVI Raman-scattered bands disappear (Munari et a. 2009, PASP 121, 1070; Shore et al. 2010, A&A 510, A70). Since the 2008 return to quiescence following the major, cool-type outburst of 2006, AG Dra has displayed just one train of four hot-type eruptions peaking in 2015, 2016, 2017, and 2018 (ATel #8975, #10390, #11559). Now, after seven years of further peaceful quiesence, AG Dra is again undergoing a hot-type outburst, possibly the first of a new train. We are constantly collecting spectroscopic and photometric observations of AG Dra with Asiago 1.82m, 1.22m, and 67/92cm telescopes, and an array of other instruments operated by ANS Collaboration, including Stroncone 50cm and Varese 84cm. Our data show that AG Dra left quiescence toward the end of July 2025 (when it was still around B~11.1), and spent the last month and a half at nearly constant brightness around B~10.3. Our last photometric observations read:

Spectroscopically, the peak activity was probably reached around mid-August 2025. On our Asiago 1.82m + Echelle spectrum for Aug 13.832 UT, the HeII/Hbeta flux ratio reached 1.32, and OVI Raman-scattered bands peaked at their highest value in the last eight years. On our latest spectra obtained with the Stroncone 50cm (on Sept. 20.792 UT) and Varese 84cm (on Sept 20.855 UT), the HeII/Hbeta flux ratio lowered to 1.07 in agreement with the post-maximum brightness decline.

The QSO 4C+10.45 was detected in a bright Gamma-ray state on 2025-05-25 by Wagner et al.(ATel #17206). Optical follow-up with the 30 cm telescope of the S. Lucia di Stroncone Observatory (MPC 589) was performed on May 25, 29, and 31 with the BVRI Bessell filters. In the B images the source was detected but poorly measurable, while in the other filters was well measurable and found much brigther than the quiescent level reported in the PanSTARRS-DR1 catalog. Here are our findings: 2025-05-27T23:39 V=17:50, R=17.01, I=16.52; 2025-05-29T22:24 V=17:28, R=16.86, I=16.42; 2025-05-31T01:48 V=16.74, R=16.26, I=15.64. The source appears very active and brightening, further optical follow-up is encouraged.

The transient was found in images obtained with the second NMW camera (135mm f/2.0 telephoto lens + unfiltered STL-11000M CCD) on 2025-05-25.9796 UTC at CV=13.0. The plate-solved FITS images are available at http://scan.sai.msu.ru/~kirx/img/TCPJ02472889+6758170/ The transient coincides with the known variable star Gaia DR3 517539710877791488, which has a magnitude range of 17.93-18.18 G and a period of 0.0182338d according to its AAVSO VSX record: https://www.aavso.org/vsx/index.php?view=detail.top&oid=2841325 The star is listed as a white dwarf by Gentile Fusillo et al. (2019, MNRAS, 482, 4570) and Vincent et al. (2024, A&A, 682, A5). Finally, the transient AT 2010mg (Thevenot et al., 2021, TNS Astronomical Transient Report No. 98120), retrospectively identified in the AllWISE Multiepoch Photometry Table at IRSA, coincides with the newly discovered transient. The available information suggests that the object might be a previously unrecognized outbursting AM CVn type binary.
---- Kirill Sokolovsky, Stanislav Korotkiy (Astroverty, Ka-Dar) for the NMW team

A low-resolution spectrum was obtained on 2025-05-26.833 UT using the 0.5-m telescope equipped with a self-built MARK III spectrograph (resolution: 2.6 Å/pixel), located at S.Lucia di Stroncone (observatory MPC 589), Italy. The spectrum shows a blue continuum with Balmer lines. Notably, Ha (6562.8 Å) is absent, filled up by the disk emission, while the other Balmer lines are broad and appear in absorption.
The FWHM of Hß (4860 Å) is approximately 2000 km/s. These spectral characteristics are consistent with those of a cataclysmic variable (CV). We therefore propose that TCP J02472889+6758170 is a cataclysmic variable.