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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel  17780, 17781, 17782
Message-Id: <20260509070806.7260A2880995@server.astronomerstelegram.org>
Date: Sat,  9 May 2026 03:08:06 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17780							     ATEL #17780

Title:	Fermi-LAT detection of renewed gamma-ray activity from the
		FSRQ 3C 395
Author:	F. Giacchino (USAL - Universidad de Salamanca, Spain, and
		INFN - Rome Tor Vergata, Sapienza University Rome), P. Monti-Guarnieri
		(University of Trieste and INFN Trieste) and G. La Mura (INAF - O.
		A. Cagliari), on behalf of the Fermi Large Area Telescope Collaboration
Queries:	federica.giacchino@roma2.infn.it
Posted:	8 May 2026; 16:47 UT
Subjects:Gamma Ray, >GeV, AGN, Blazar, Quasar, Fast Radio Burst

The Large Area Telescope (LAT), one of the two instruments on the Fermi
Gamma-ray Space Telescope, has observed renewed gamma-ray activity from
a source positionally consistent with the flat-spectrum radio quasar  3C
395, also known as 4C +31.52, B2 1901+31 and 4FGL J1902.8+3201 (The Fermi-LAT
collaboration 2020, ApJS, 247, 33) with coordinates R.A. = 285.73308 deg,
Decl. = 31.99492 deg (J2000; Xu et al. 2019, ApJS, 242, 5). 3C 395 is a
known radio source showing superluminal motion (Lister et al. 2019, ApJ,
874, 43) and asymmetries between the parsec and kiloparsec scales (Lara
et al. 1997, A&A, 319, 405). The redshift is z=0.634 (Gelderman & Whittle
1994, ApJS, 91, 491).

Preliminary analysis indicates that this source was in an elevated gamma-ray
emission state on May 7, 2026 with a daily averaged gamma-ray flux (E>100MeV)
of (0.7 +/- 0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only).
This corresponds to a flux increase of a factor of more than 30 relative
to the average flux reported in the fourth data release of the fourth Fermi-LAT
catalog (4FGL-DR4, Ballet et al. 2023, arXiv:2307.12546). This is the highest
daily flux ever observed for this source by the LAT. The corresponding
photon index is 2.5 +/-  0.2, consistent with the 4FGL-DR4 value of 2.55
+/- 0.05. The Fermi-LAT Collaboration has previously reported flaring activity
from this source in ATel #14383.

Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray
monitoring of this source will continue. We encourage multifrequency observations
of this source. For this source, the Fermi-LAT contact person is Marcello
Giroletti (marcello.giroletti@inaf.it).

The Fermi-LAT is a pair conversion telescope designed to cover the energy
band from 20 MeV to greater than 300 GeV. It is the product of an international
collaboration between NASA and DOE in the U.S. and many scientific institutions
across France, Italy, Japan and Sweden.

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Password Certification: Federica Giacchino (federica.giacchino@roma2.infn.it)
https://www.astronomerstelegram.org/?read=17780
==============================================================================
ATEL #17781							     ATEL #17781

Title:	SPT-SV J222602.8-540533: South Pole Telescope Reports Detection
		of a Flaring Millimeter-Band Source
Author:	Tarraneh Eftekhari (Northwestern U.) on behalf of the SPT-3G
		Collaboration
Queries:	teftekhari@northwestern.edu
Posted:	8 May 2026; 19:04 UT
Subjects:Millimeter, AGN, Transient

The South Pole Telescope Collaboration reports: The 3rd-generation receiver
on the South Pole Telescope (SPT-3G) detects a flaring millimeter point
source at RA = 336.51170d, DEC = -54.09255  (estimated positional uncertainty
of ~8 arcseconds). Detectable millimeter emission began 2026 April 13 UT
rising to a peak flux density of 25.7 +/- 7.1 mJy (150 GHz) and 15.0 +/-
7.2 mJy (95 GHz) on 2026 April 22 UT. The average quiescent flux density
at this position in 2025 measured via SPT-3G is 3.1 +/- 1.4 mJy (150 GHz)
and 0.8 +/- 1.4 mJy (95 GHz), indicating a factor of >8 increase. At the
time of this alert, the flux density remains above the quiescent level,
reaching a maximum test-statistic of 88.2 on 2026 April 27 UT, corresponding
to a 9.1-sigma significance (Guns et al. 2021, ApJ, 916, 98). We note that
the inverted spectrum indicates the source has likely not yet peaked in
the centimeter band. The 150 GHz light curve also shows some evidence of
flaring in early 2020. All flux calibrations quoted here are preliminary
and are believed to be accurate to 20%. SPT-3G will continue to monitor
this source at hour- to day-long intervals.

The millimeter source is associated with the galaxy LEDA 422944 at a redshift
z = 0.0571. The galaxy is detected in eROSITA at a flux of (3.3+-0.6)e-13
erg/sec (Merloni et al. 2024, A&A, 682, 34), yielding an X-ray luminosity
of 2.6e42 erg/sec, near the border between low-luminosity AGN and standard
Seyfert galaxies, but above the level for all but the most extreme star-forming
galaxies. Inspection of the archival optical spectrum from 2dF (Colless
et al. 2001, MNRAS, 328, 1039) indicates a likely LINER nature.

The South Pole Telescope is a 10-meter telescope designed for observations
of the cosmic microwave background located at Amundsen-Scott South Pole
Station and supported by the National Science Foundation and the US Dept.
of Energy. The SPT online transient program providing data in this telegram
is supported by NSF grants OPP-1852617 and OPP-2332483, and observes 1500
square degrees of the southern sky at 95, 150, and 220 GHz with an average
revisit cadence of 12 hours. For more details on the SPT transient program
and survey strategy, please see Guns et al. 2021, ApJ, 916, 98.

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Password Certification: Tarraneh Eftekhari (teftekhari@northwestern.edu)
https://www.astronomerstelegram.org/?read=17781
==============================================================================
ATEL #17782							     ATEL #17782

Title:	Optical brightening of the blazar TXS 1420+326 (OQ 334)
Author:	Kirill Sokolovsky, Katie Barnhart, Darien Perla, Vallia Antoniou,
		Elias Aydi (Texas Tech University)
Queries:	kirx@kirx.net
Posted:	8 May 2026; 23:43 UT
Subjects:Optical, AGN, Blazar

We report the ongoing optical brightening of the TeV-detected  
(ATel #13412) flat-spectrum radio quasar TXS 1420+326, also known  
as B2 1420+32 and OQ 334. The brightening was observed by  
the NMW-TexasTech transient survey, with the following unfiltered  
magnitudes (APASS V zero-point):

# Date (UTC)       JD(UTC)       CV   mag_err  
2026-05-03.31736 2461163.81736 >15.4    
2026-05-07.42112 2461167.92112  15.03 0.14  
2026-05-07.44878 2461167.94878  14.76 0.08  
2026-05-08.32021 2461168.82021  14.46 0.15  
2026-05-08.36828 2461168.86828  14.35 0.05

The source has reached the optical brightness level seen during its  
2024 flare (ATel #16681, #16700, #16782). Over the last decade,  
TXS 1420+326 has displayed a series of optical flares,  
the brightest of which peaked on 2020-01-19.4874 at r=13.11 +/-0.01  
according to its  
<a href="https://ztf.snad.space/dr23/view/675105100003993">ZTF lightcurve</a>.

The current optical brightening of TXS 1420+326 follows reports of  
its elevated activity in the GeV (ATel #17654)  
and radio (ATel #17745) bands.

The NMW-TexasTech survey operates two unfiltered QHY600M CMOS  
cameras attached to Rokinon 135mm telephoto lenses on ZWO AM5  
mounts located at TTU Preston Gott Skyview Observatory  
(Shallowater, Texas).

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Password Certification: Kirill Sokolovsky (kirx@scan.sai.msu.ru)
https://www.astronomerstelegram.org/?read=17782
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