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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel  17592, 17593
Message-Id: <20260113071139.088912880875@server.astronomerstelegram.org>
Date: Tue, 13 Jan 2026 02:11:39 -0500 (EST)

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Posted: Within the last 24 hours
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ATEL #17592							     ATEL #17592

Title:	Yet, a new NIR Flare of the Blazar PKS0454-234
Author:	L. Carrasco, A. Porras, G. Escobedo, L. Felix, E. Recillas
		(INAOE, Mexico)
Queries:	Carrasco@inaoep.mx
Posted:	12 Jan 2026; 17:16 UT
Subjects:Radio, Infra-Red, Gamma Ray, AGN, Blazar, Quasar, Transient

We report on the recent Giant NIR flare of the high redshift blazar PKS0454-234
(z=1.003), cross identified with the source BZQJ 0454-2324 and the Gamma-ray
source 2FGLJ0457.0-2325. On December 12th, 2025 (JD 2461021.8140), we found
the source with the following fluxes in NIR bands: J = 12.297 +/- 0.04,
H = 11.549 +/- 0.04 and Ks = 10.682 +/- 0.02. These values are to be compared
with our previous observation on JD 2460657.841 , when the source showed
J = 15,233, H = 14.056 and K = 13.942. Hence, the source has had a flux
increment of a factor of 20 in the K band, a factor of 10 in the H band
and a factor of 15 in the J band, during this lapse. This differential
increase may be indicative that the source 
was undergoing a very fast flare while being observed, as the order of
our non simultaneous observations (spread over 20 minutes) was HJK for
the various bands respectively. Worth mentioning is the fact the source
is at maximum light since JD 2454748, 17 years ago when we started monitoring
it in the NIR. The source has shown flare activity in the past (see ATEL
#3722,#4647, #5583, #8045) Our observations are carried out with the 2.1m
telescope of the Guillermo Haro Observatory operated by the National Institute
for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument
CANICA a NIR camera. We strongly encourage further multiwavelength coverage.

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Password Certification: LUIS CARRASCO (carrasco@inaoep.mx)
https://www.astronomerstelegram.org/?read=17592
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ATEL #17593							     ATEL #17593

Title:	Detection of a Low-Brightness Tail in A/2025 Y1
Author:	M. Serra-Ricart (Light Bridges, IAC, ULL), J. Licandro (IAC,
		ULL), M. R. Alarcon (Light Bridges, IAC, ULL)
Queries:	mserra@iac.es
Posted:	12 Jan 2026; 21:39 UT
Subjects:Optical, Asteroid, Comet

Asteroidal object A/2025 Y1 has been extensively monitored since its discovery
on 2025 December 12 using the imaging capabilities of the Two-Meter Twin
Telescope (TTT) at the Observatorio del Teide (IAC, Tenerife, Spain). 
We report the detection of a faint tail associated with A/2025 Y1. Deep
optical images obtained on 2026 January 11 using TTT3 show a low-surface-brightness
tail visible in the stacked data (see attached figure). Standard reduction
procedures (bias subtraction, flat-fielding, and stacking) were applied.

The tail extends up to 4 arcsec from the optocenter (red cross in the attached
image) and has a measured position angle of PA =  291d +/- 1d, consistent
with the projected antisolar direction (PsAng = 292d). The morphology and
orientation of the feature are consistent with a weak dust tail produced
by low-level activity. 
Further observations are encouraged to confirm the persistence and evolution
of this feature. 
TTT3 is a 2 m f/6 Ritchey-Chretien telescope currently in its commissioning
phase. Images from TTT3 were acquired using COLORS, a 2k x 2k camera mounted
at the Nasmyth-2 focus and equipped with a back-illuminated BEX2-DD CCD,
yielding a field of view of 7.85 x 7.85 arcmin and a plate scale of 0.23
arcsec per pixel. 
TTT is operated by Light Bridges in Tenerife, Canary Islands (Spain). The
observation time rights (DTO) used for this research were consumed in the
PEI “PERHELIO26”. This research used storage and computing capacity
in ASTRO POCs EDGE computing center at Tenerife under the form of Indefeasible
Computer Rights (ICR).

Figure 1. Stacked image of A/2025 Y1 obtained on 2026 January 11. The antisolar
direction is indicated by the yellow arrow, and the projected velocity
vector is shown by the red arrow. North is up, east is to the left. The
blue line represents the position angle (PA) of the tail.

TTT3 image with detected faint tail: https://drive.google.com/file/d/1a-Dp_6lkYyjnHd3cY4TGUmMq5hpbwd2-/view?usp=sharing
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Password Certification: Miquel Serra-Ricart (mserra@iac.es)
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