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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel 17159
Message-Id: <20250424070517.0C4592880671@server.astronomerstelegram.org>
Date: Thu, 24 Apr 2025 03:05:17 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17159							     ATEL #17159

Title:	X-ray outburst of a radio-loud quasar
Author:	M. Orio (University of Wisconsin and INAF-Padova), E. Behar
		(Technion), N. Nagashima (Chuo U.), K. Fukushima, Y. Kanemaru, S.
		Ogawa (JAXA), M. Audard (U. de Geneve), S. Inoue (Kyoto U.), Y. Ishihara
		(Chuo U.), T. Kohmura (TUS), Y. Maeda (JAXA), M. Mizumoto (UTEF),
		M. Nobukawa (NUE), K. Pottschmidt (UMBC, NASA GSFC, CRESST), M. Shidatsu
		(Ehime U.), H. Sugai (Chuo U.), Y. Terada (Saitama U.), Y. Terashima
		(Ehime U.), Y. Tsuboi (Chuo U.), H. Uchida (Kyoto U.), T. Yoneyama
		(Chuo U.), M. Yoshimoto (Ehime U.)  
Queries:	orio@astro.wisc.edu
Posted:	23 Apr 2025; 14:14 UT
Subjects:Request for Observations, AGN, Quasar, Transient

We report that the XRISM/XTEND Transient Search source XRISM J1826-3651,
observed on 2025-04-12 and reported in ATel #17145 was observed again with
the Swift X-Ray Telescope (XRT) on 2025-04-22 for a total (non continuous)
on-source time of 2642 s. The source is still X-ray luminous, and was detected
with a count rate 0.022&plusmn;0.004 cts/s at this position: alpha=18 26
08.16 and delta=-36 50 46.8, with a position uncertainty of 4.2 arcseconds.
The spectrum is relatively hard and can be fitted with a power law, with
photon index 1.9(+0.8/-0.6), absorbing column density N(H)=2.2(+3.6/-2.1)
cm-2, absorbed flux of 1.0&plusmn;0.5 x 10-12 erg/cm/-2/s,
and unabsorbed flux ~1.3 x 10 -12 erg/cm-2/s. 
The most likely counterpart is the radio-loud quasar and blazar 1WGA J1826.1-3650
at redshift z=0.888 (Veron Cetty et al. 2010, A&A, 518, 10), which also
corresponds to GAIA source 6728071805422016896, at 2.9 arcsec from the
Swift XRT position. This object was serendipitously observed with ROSAT
in X-rays as 1WGA J1826.1-3650 at comparable luminosity in 1992 March,
so this is not the first X-ray active state, but X-ray observations in
the intervening time are missing.

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Password Certification: Marina Orio (orio@astro.wisc.edu)
https://www.astronomerstelegram.org/?read=17159
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