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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel 17484, 17485, 17486
Message-Id: <20251109071639.06F7D288079B@server.astronomerstelegram.org>
Date: Sun, 9 Nov 2025 02:16:39 -0500 (EST)

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Posted: Within the last 24 hours
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ATEL #17484							     ATEL #17484

Title:	MAXI/GSC detection of renewed activity from GX 339-4
Author:	H. Negoro, M. Nakajima, K. Takagi, H. Takahashi, H. Nishio
		(Nihon U.),  T. Mihara, T. Tamagawa, N. Kawai, M. Matsuoka (RIKEN),
		 T. Sakamoto, M. Serino, S. Sugita, Y. Kawakubo, H. Hiramatsu, Y.
		Kondo, A. Yoshida (AGU),  Y. Tsuboi, H. Sugai, N. Nagashima, Y. Ishihara
		(Chuo U.),  M. Shidatsu, C. Kang, T. Nakamoto, M. Uenishi, T. Usuki,
		S. Yatsuzuka (Ehime U.), I. Takahashi, Y. Yatsu (Science Tokyo), S.
		Nakahira, S. Ueno, H. Tomida, M. Ishikawa,  S. Ogawa, M. Kurihara
		(JAXA), Y. Ueda, K. Fujiwara (Kyoto U.),  M. Yamauchi, M. Nishio,
		C. Hiraizumi (Miyazaki U.), K. Yamaoka (Nagoya U.), M. Sugizaki (Kanazawa
		U.), W. Iwakiri (Chiba U.), T. Kawamuro (Osaka U.),  and S. Yamada
		(Tohoku U).
Queries:	negoro.hitoshi@nihon-u.ac.jp
Posted:	8 Nov 2025; 08:47 UT
Subjects:X-ray, Black Hole

The black-hole X-ray binary GX 339-4 exhibited a new outburst from August
9 2025 (Saikia et al. ATel #17327). MAXI GSC light curves obtained with
the image-fit method show that the 2-20 keV X-ray flux increased relatively
rapidly after the EP FXT detection on August 12 (Zhao et al. ATel #17330),
and peaked at approximately 28 mCrab on August 21 (MJD 60908). The X-ray
flux decreased gradually, and the GSC had not detected the source in one
day since September 2 (MJD 60920).

The 2-10 keV X-ray flux gradually increased again from around October 17
(MJD 60965), reaching approximately 20 mCrab on November 4-5. This renewed
activity might be a continuation of the low-level activity observed from
August.

MAXI GSC data for GX 339-4: https://maxi.riken.jp/v7l3h/J1702-487/
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Password Certification: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)
https://www.astronomerstelegram.org/?read=17484
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ATEL #17485							     ATEL #17485

Title:	Spectroscopic confirmation of TCP J05384230+7051377 as a WZ
		Sge-type dwarf nova 
Author:	Hiromasa Hoke, Keisuke Isogai (Kyoto University), Yusuke Tampo
		(South African Astronomical Observatory, University of Cape Town)
		
Queries:	hoke@kusastro.kyoto-u.ac.jp
Posted:	8 Nov 2025; 11:24 UT
Subjects:Optical, Binary, Cataclysmic Variable, Transient, Variables

We report on spectral features in the transient TCP J05384230+7051377 on
2025-11-07.6332 UT obtained with a fiber-fed integral field spectrograph
(KOOLS-IFU; Matsubayashi et al. <a href="https://ui.adsabs.harvard.edu/abs/2019PASJ...71..102M/abstract"
target="_blank">2019</a>, <a href="https://ui.adsabs.harvard.edu/abs/2025PASJ...77.1065M/abstract"
target="_blank">2025</a>) attached to one of the Nasmyth focuses of the
3.8-m telescope Seimei at Okayama Observatory of Kyoto University. In short,
we conclude that this object is a WZ Sge-type dwarf nova.

According to <a href="http://www.cbat.eps.harvard.edu/unconf/followups/J05384230+7051377.html"
target="_blank">CBAT</a>, the outburst of TCP J05384230+7051377 was discovered
at CV=12.9 mag on 2025-11-07.0576 UT by the NMW survey. There is a likely
counterpart in Pan-STARRS and GALEX, whose brightnesses are g=20.4, r=20.3,
i=20.5, z=20.5, FUV=20.7, and NUV=21.1. The absolute magnitude is estimated
to be Mg = 12.0+0.5-0.6 by the distance
of Gaia EDR3 (<a href="https://ui.adsabs.harvard.edu/abs/2021yCat.1352....0B/abstract"
target="_blank">Bailer-Jones et al. 2021</a>). <a href="https://ui.adsabs.harvard.edu/abs/2021yCat..75083877G/abstract">Gentile
Fusillo et al. (2021)</a> reported that this object is a white dwarf candidate
based on Gaia's HR diagram. Judging from the outburst amplitude of &sim;7.5mag,
Mg, and its quiescent color, this object was expected to be
a WZ Sge-type dwarf nova.

We obtained <a href="https://www.kusastro.kyoto-u.ac.jp/~hoke/ATel/TCPJ0538.pdf"
target="_blank">an optical spectrum</a> on 2025-11-07.6332 UT. Our quick
look spectrum shows a blue continuum with the Balmer and HeI absorption
lines. Also, H&alpha; has a narrow emission core. From these spectral features,
we conclude that this object is a new bright WZ Sge-type dwarf nova.

Our spectrum: https://www.kusastro.kyoto-u.ac.jp/~hoke/ATel/TCPJ0538.pdf
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Password Certification: Keisuke Isogai (isogai@kusastro.kyoto-u.ac.jp)
https://www.astronomerstelegram.org/?read=17485
==============================================================================
ATEL #17486							     ATEL #17486

Title:	A glitch in the highly magnetised radio pulsar PSR B1737-30
Author:	Benjamin Shaw (University of Manchester), Danai Antonopoulou
		(UoM), Michael J. Keith (UoM), Andrew G. Lyne (UoM), Mitchell B. Mickaliger
		(UoM), Benjamin W. Stappers (UoM), Patrick Weltevrede (UoM).
Queries:	benjamin.shaw@manchester.ac.uk
Posted:	8 Nov 2025; 15:44 UT
Subjects:Radio, Neutron Star, Pulsar, Magnetar

We report the detection of a glitch in the radio pulsar PSR B1737-30 (PSR
J1740-3015), which we monitor as part of the Jodrell Bank Pulsar Timing
Programme. PSR B1737-30 is observed approximately weekly with the Lovell
Telescope at the Jodrell Bank Observatory, using a 384 MHz bandwidth centred
at 1532 MHz.

This is the 38th glitch observed in this pulsar, occurring roughly three
years after the previously reported event in 2022. Preliminary analysis
indicates a fractional rotational frequency increase of dF0/F0 = 2.810(3)e-06
(1 sigma uncertainty). This makes it the largest glitch recorded in this
source, marginally exceeding the previous record event (dF0/F0 = 2.663e-6).
The glitch epoch is currently estimated as MJD 60980(5).

At present, we find no evidence for transient post-glitch recovery or any
significant change in the spin-down rate of the star. We continue to monitor
the pulsar daily with enhanced cadence in order to refine the glitch measurement.

PSR B1737-30 is among the most strongly magnetised rotation-powered pulsars
known, with a surface dipole magnetic flux density of approximately 1.7e13
G. Observations at other facilities, particularly high-energy instruments,
are encouraged to confirm the glitch and to search for any radiative changes
associated with this event.

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Password Certification: Benjamin Shaw (benjamin.shaw@manchester.ac.uk)
https://www.astronomerstelegram.org/?read=17486
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