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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel 17425, 17426
Message-Id: <20250930071034.C46D52880784@server.astronomerstelegram.org>
Date: Tue, 30 Sep 2025 03:10:34 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17425							     ATEL #17425

Title:	Swift-XRT detection of supersoft emission in V572 Vel
Author:	K. L. Page (U. Leicester),  G. J. M. Luna (UNAHUR/CONICET)
		and N. P.M. Kuin (UCL/MSSL)
Queries:	kpa@star.le.ac.uk
Posted:	29 Sep 2025; 16:08 UT
Subjects:X-ray, Nova

The eruption of V572 Vel (Nova Vel 2025; PNV J10251200-5331109) was 
discovered on June 25.44 (CBET #5574). Swift monitoring started less 
than a day later (ATel #17262), although no X-rays were detected at 
this time. Regular observations continued, with the first detection of

X-ray emission occurring on August 31 (67 days after eruption; ATel 
#17367). At this time, the X-ray spectrum was heavily absorbed, and a 
count rate of 0.030 +0.005/-0.004 count s-1 was measured.

Observations on September 6 and 10 also revealed heavily-absorbed 
X-ray spectra which could be characterised by a single temperature 
optically-thin component. The next observation, taken on September 28 
(day 95), however, showed a factor of greater than three increase in 
count rate (0.158 +0.019/-0.017 count s-1 compared with 
0.042 +/- 0.005 count s-1 on September 10), with a new, 
much softer component. The soft emission can be roughly parameterised 
with a blackbody of kT = 15 +4/-3 eV. The underlying optically-thin 
component remains, and NH has decreased to a value 
consistent with the ISM absorption in this direction (2.8 x 
1021 cm-2). The 0.3-10 keV observed flux is now 
1.2 x 10-11 erg cm-2 s-1.

Continued Swift monitoring has been requested.  We thank the Swift PI 
and deputies for approving these observations, and the Swift 
operations team for implementing them.

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Password Certification: Kim Page (kpa@star.le.ac.uk)
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ATEL #17426							     ATEL #17426

Title:	PRIME discovery and SOAR confirmation of a very bright symbiotic
		nova PRIME25aaghjd near the Galactic center
Author:	R. Hamada (UOsaka), K. De (Columbia), D. Suzuki (UOsaka),
		T. Sumi (UOsaka), A. Idei (UOsaka), S. Makida (UOsaka), T. Nagano
		(UOsaka), S. Nakayama (UOsaka), R. Ogawa (UOsaka), Y. Okumoto (UOsaka),
		Y. K. Satoh (Kanto Gakuin U), T. Tamaoki (UOsaka)
Queries:	kd3038@columbia.edu
Posted:	30 Sep 2025; 04:06 UT
Subjects:Infra-Red, Optical, Cataclysmic Variable, Nova, Transient,
		Variables

We report the discovery and spectroscopic classification of a very bright
NIR transient during the Galactic bulge survey carried out by the PRime-focus
Infrared Microlensing Experiment (PRIME). PRIME is a 1.8m telescope with
1.56 square degree FOV (0.5 arcsec/pixel) located in Sutherland, South
Africa at the South African Astronomical Observatory (Sumi et al. 2025).
PRIME25aaghjd was first detected as a candidate transient generated in
our custom image reduction and subtraction pipeline based on the ZOGY algorithm
(Zackay et al. 2016, De et al. 2020) at a H-band mag of 8.7 +/- 0.1 mag
(in the Vega system) on UT 2025-02-16, and at J2000 coordinates

RA 17:48:14.63

Dec -29:51:18.95

The transient is located ~1.1 degrees away from the Galactic center, with
a corresponding integrated line of sight extinction of ~8 mags in V-band
(Schalfly et al. 2011). We caution that the first detection of the transient
was brighter than the nominal saturation level of the detector, and immediately
after the resumption of Galactic bulge 2025 observations; therefore the
transient erupted likely before and was brighter than the quoted measurement.
The source is coincident with a faint IR source in the archival VVV catalog
within ~ 1” with a magnitude of H = 14.1 +/- 0.1 mag. The implied amplitude
of the outburst is > 5 mags. Subsequent detections of the source indicate
a monotonically fading light curve, decaying to H ~ 14.0 mag by 2025-07-31.

On UT 2025-09-28, we obtained a near-infrared spectrum of the source with
the Triplespec spectrograph on the SOAR telescope as part of our Target
of Opportunity Program (SOAR 2025B-002; PI: De). The reduced spectrum shows
a red continuum peaking in H-band, with broad emission lines of He I, Pa
gamma and Pa beta with FWHM ~ 1100 km/s. On top of the continuum, we detect
strong CO absorption in the first overtone near 2.29 micron, indicative
of a cool red giant spectrum. The combination of broad emission lines,
cool giant spectrum and quiescent IR counterpart suggest the source to
be a new symbiotic nova (e.g. Mikolajewska 2010, Munari 2024) towards the
Galactic center.

We encourage multi-wavelength follow-up of the source. We thank the AEON
observers at the SOAR telescope for carrying out these observations.

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Password Certification: Kishalay De (kde1@mit.edu)
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