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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel  17432, 17433
Message-Id: <20251005071714.8B396288078D@server.astronomerstelegram.org>
Date: Sun,  5 Oct 2025 03:17:14 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17432							     ATEL #17432

Title:	Liverpool Telescope SPRAT spectrum of PNV J01350197+3043202:
		a potential recurrence of M33N 2021-08a
Author:	M. J.Darnley (LJMU), Jingyuan Zhao, Ziyang Mai, Jianlin Xu,
		Hualin Li, Mi Zhang, Wenjie Zhou, Guoyou Sun, Jiangao Ruan, Xing Gao
		(Xingming Observatory)
Queries:	M.J.Darnley@ljmu.ac.uk
Posted:	4 Oct 2025; 10:14 UT
Subjects:Optical, Nova, Transient

A potential nova was discovered in M33 on 2025 Oct 02.65: http://www.cbat.eps.harvard.edu/unconf/followups/J01350197+3043202.html

Due to its spatial proximity, this has been identified as a potential recurrence
of M33N 2021-08a (AT 2021wfc).

We obtained a single 600s spectrum of PNV J01350197+3043202 with the SPRAT
instrument on the Liverpool Telescope on 2025 Oct 03.9758 (mid-point).

Although the signal-to-noise of the source was low in the spectrum, there
is a clear detection of broad and double peaked H&alpha; emission.

The H&alpha; emission has a half-width of around 4800 km/s. The separation
of the two peaks is around 5000 km/s.

There is also evidence of a N II, or possibly He I, emission line at around
5010 Angstroms.

Although there is negligible evidence for H&beta;, there is double peaked
emission around H&gamma; also showing a ~5000 km/s separation between the
peaks.

As such, we conclude that the most likely source of this new transient
is a nova eruption in M33.

<u>If</u> the spatial coincidence with M33N 2021-08a is confirmed, then
this suggests a nova with a recurrence period of four years, or shorter:
another rapid-recurrent nova.

This would, we believe, be the first recurrent nova confirmed in M33.

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Password Certification: Matt Darnley (matt_darnley@icloud.com)
https://www.astronomerstelegram.org/?read=17432
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ATEL #17433							     ATEL #17433

Title:	FRB 251004A: DDOTI Upper Limit on the Optical Counterpart
Author:	Rosa L. Becerra (U Roma), Alan M. Watson (UNAM), Camila Angulo
		Valdez (UNAM), Sahil Atri (U Roma), Nat Butler (ASU), Simone Dichiara
		(Penn State University), Tsvetelina Dimitrova (ASU), Alexander Kutyrev
		(GSFC/UMD), William H. Lee (UNAM), Océlotl López (UNAM), Margarita
		Pereyra (UNAM) and Eleonora Troja (U Roma)
Queries:	rosa.becerra@roma2.infn.it
Posted:	4 Oct 2025; 13:34 UT
Subjects:Optical, Fast Radio Burst

We observed the field of FRB 251004A (ID=1134535058) detected by CHIME/FRB
and distributed by the VOEvents service (https://www.chime-frb.ca/voevents)
with the DDOTI/OAN wide-field imager at the Observatorio Astronomico Nacional
on the Sierra of San Pedro Martir (http://ddoti.astroscu.unam.mx) on the
night of 2025-10-04 UTC.

DDOTI imaged the CHIME error region from 08:30 to 09:02 UTC (T+6.1 to T+6.6
hours after the trigger) obtaining a total exposure of 24 minutes.

Comparing our observations to the USNO-B1 and Pan-STARRS PS1 DR2 catalogues,
we detect no uncatalogued fading sources within the observed field down
to a 10-sigma limiting AB magnitude of:

w > 19.04

In our visual inspection, we identify a bright source at RA, Dec (J2000)=19:08:08,
+53:22:03, consistent with the High Proper Motion Star 2139664063041544576
in the Gaia DR3 Catalog (Gaia Collaboration, 2023).

Further observations and analysis are planned.

We thank the staff of the Observatorio Astronomico Nacional on the Sierra
of San Pedro Martir.

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Password Certification: Rosa Leticia Becerra Godinez (rosa.becerra@roma2.infn.it)
https://www.astronomerstelegram.org/?read=17433
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