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Return-Path: <atel@astronomerstelegram.org> Delivered-To: stefano@bicar.it Received: by mail.planetcloud-host.com (Postfix, from userid 99) id 0498E14603; Tue, 24 Feb 2026 08:18:52 +0100 (CET) X-Spam-Checker-Version: SpamAssassin 3.4.0 (2014-02-07) on mail.planetcloud-host.com X-Spam-Level: * X-Spam-Status: No, score=1.0 required=5.0 tests=RCVD_IN_DNSWL_BLOCKED, RCVD_IN_VALIDITY_RPBL_BLOCKED,RCVD_IN_VALIDITY_SAFE_BLOCKED,SPF_HELO_NONE, SPF_PASS,URIBL_BLOCKED autolearn=disabled version=3.4.0 Received-SPF: Pass (sender SPF authorized) identity=mailfrom; client-ip=174.142.199.243; helo=server.astronomerstelegram.org; envelope-from=atel@astronomerstelegram.org; receiver=stefano@bicar.it Received: from server.astronomerstelegram.org (astronomerstelegram.org [174.142.199.243]) by mail.planetcloud-host.com (Postfix) with ESMTP id 918A51447F for <stefano@bicar.it>; Tue, 24 Feb 2026 08:18:11 +0100 (CET) Received: from server.astronomerstelegram.org (localhost [127.0.0.1]) by server.astronomerstelegram.org (Postfix) with ESMTP id 39E6628808D6 for <stefano@bicar.it>; Tue, 24 Feb 2026 02:18:10 -0500 (EST) To: stefano@bicar.it From: atel@astronomerstelegram.org Subject: ATel 17695, 17696, 17697 Message-Id: <20260224071810.39E6628808D6@server.astronomerstelegram.org> Date: Tue, 24 Feb 2026 02:18:10 -0500 (EST) ------------------------------------------------------------------------------ The Astronomer's Telegram is free to read, free to publish, free to use. Thanks to the support of our patrons, we can continue to keep it free. https://www.patreon.com/astronomerstel ------------------------------------------------------------------------------ The Astronomer's Telegram http://www.astronomerstelegram.org ------------------------------------------------------------------------------ Posted: Within the last 24 hours ============================================================================== ATEL #17695 ATEL #17695 Title: XRISM/Xtend Transient Search (XTS) detected an X-ray flare possibly from 1BMW 045320.6+025843 Author: Y. Motogami (Saitama U.), H. Noda (Tohoku U.), K. Fukushima, Y. Kanemaru, S. Ogawa, Y. Uchida, T. Yoneyama (JAXA), M. Audard (U. de Geneve), E. Behar (Technion), T. Hakamata (UOsaka), S. Inoue (Kyoto U.), Y. Ishihara (Chuo U.), C. Kang (Ehime U.), T. Kiyomoto (Saitama U.), T. Kohmura (TUS), H. Kuramoto (UOsaka), J. Kurashima (U. of Miyazaki), Y. Maeda (JAXA), H. Matsumoto (UOsaka), T. Matsushima (U. of Miyazaki), A. Miyamoto (UOsaka), M. Mizumoto (UTEF), K. Mori (U. of Miyazaki), N. Nagashima (Chuo U.), T. Narita (Kyoto U.), M. Nobukawa (NUE), Y. Sakamoto (Tohoku U.), M. Shidatsu (Ehime U.), H. Sugai (Chuo U.), H. Takahashi (Hiroshima U.), T. Takagi (Ehime U.), S. Takatsuka (UOsaka), R. Takemoto (U. of Miyazaki), Y. Terada (Saitama U., JAXA), Y. Terashima (Ehime U.), Y. Tsuboi (Chuo U.), H. Uchida (Kyoto U.), A. Yoshimoto (NWU), M. Yoshimoto (Ehime U.), A. Sarkar (U. of Arkansas) Queries: hirofumi.noda@astr.tohoku.ac.jp Posted: 23 Feb 2026; 15:12 UT Subjects:X-ray, Binary, Star, Transient, Young Stellar Object XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J0453+0259 on 2026-02-22 TT. The source position is determined to be (R.A., Dec.) = (73.339, +2.979), with a systematic error of ∼ 40 arcsec. One of the plausible counterparts is 1BMW 045320.6+025843, located ∼ 11 arcsec apart from the position of XRISM J0453+0259. The flare started at 2026-02-22 at ∼ 01:47 TT. The flare reached its peak on 2026-02-22 at ∼ 02:38. The flare exponentially decayed in 10<sup>4</sup> sec. The peak flux is calculated as 3 × 10<sup>-12</sup> erg s<sup>-1</sup> cm<sup>-2</sup> (0.4 - 10.0 keV). A systematic error of roughly 20% should be added to the statistical error. We derived the above systematic error for the flux by comparing our derived values for the sources detected with XTS in several observations with those for the corresponding X-ray counterparts. We estimated the systematic error for the source position from the separations between the detected sources with the corresponding counterparts in the same field of view. ------------------------------------------------------------------------------ Password Certification: Hirofumi Noda (hirofumi.noda@astr.tohoku.ac.jp) https://www.astronomerstelegram.org/?read=17695 ============================================================================== ATEL #17696 ATEL #17696 Title: Fermi-LAT detection of enhanced gamma-ray activity from the FSRQ 4C +51.37 Author: S. Rani (Michigan Technological University), T. Lewis (Michigan Technological University), P. Monti-Guarnieri (University of Trieste and INFN Trieste), on behalf of the Fermi Large Area Telescope Collaboration Queries: imc@umd.edu Posted: 24 Feb 2026; 01:25 UT Subjects:Gamma Ray, >GeV, Blazar The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed an enhanced gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar 4C +51.37, associated with 4FGL J1740.5+5211 (Abdollahi et al. 2022, ApJS, 260, 53), with coordinates R.A. = 265.15407 deg, Dec. = 52.19539 deg (J2000), and a redshift of z = 1.381 (Xiao et al. 2022, ApJ, 936, 146). Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on February 22, 2026, with a daily averaged gamma-ray flux (E > 100 MeV) of (0.6 +/- 0.1) e-06 ph cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase by a factor of more than 10 relative to the average flux reported in the fourth Fermi-LAT catalog, Data Release 4 (4FGL-DR4; Ballet et al. 2023, arXiv:2307.12546). The corresponding photon index is 2.41 +/- 0.18, consistent within uncertainties with the 4FGL-DR4 value of 2.47 +/- 0.02. This is the highest daily flux observed by LAT from this source so far. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency follow-up observations to investigate the nature and evolution of this flare. A preliminary light curve for 4FGL J1740.5+5211 can be accessed via the Fermi-LAT Light-Curve Repository at <a>https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.html?source_name=4FGL_J1740.5+5211<a>. For this source, the LAT contact persons are S. Rani (rani@mtu.edu) and P. Monti-Guarnieri (pietro.monti-guarnieri@phd.units.it). The Fermi-LAT is a pair-conversion telescope designed to cover the energy range from 20 MeV to beyond 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. ------------------------------------------------------------------------------ Password Certification: Israel Martinez (imc@umd.edu) https://www.astronomerstelegram.org/?read=17696 ============================================================================== ATEL #17697 ATEL #17697 Title: 2nd XRISM follow-up observation of the black hole X-ray binary GS 1354-64 Author: D. Miura (U. of Tokyo), K. Fukushima, Y. Kanemaru, S. Ogawa, Y. Uchida, T. Yoneyama (JAXA/ISAS), C. Baluta (NASA/GSFC), Y. Terada (Saitama U.), E. Costantini (SRON), M. Guainazzi (ESA/ESTEC), R. Kelley (NASA/GSFC), K. Matsushita (TUS), R. Petre, B. Williams (NASA/GSFC), H. Yamaguchi, S. Watanabe (JAXA/ISAS), M. Tashiro (Saitama U.) Queries: kxfukushima@gmail.com Posted: 24 Feb 2026; 05:24 UT Subjects:X-ray, Black Hole, Transient XRISM has observed the black hole X-ray binary GS 1354-64 from 2026-02-19T17:24:00 to 2026-02-20T21:14:00 (UTC), using 49 ks exposure time in the Director's Discretionary Time (DDT) allocation for XRISM Cycle 2. MAXI/GSC found a new outburst for this target on 2025-12-25 (ATel #17563). Since then, multi-wavelength follow-up observations were carried out (ATels #17582, #17583, #17586, #17611, #17612, #17618). XRISM observed GS 1354-64 as a DDT target from 2026-01-20T03:37:00 to 2026-01-23T04:00:00 (ATel #17625). After the XRISM follow-up observation, the transition to the soft state has been confirmed for this source (ATels #17638, #17650, #17673). Then, the second DDT observation of GS 1354-64 was requested and carried out as above. We fit the 1.8–12 keV Resolve spectrum, extracted from quick-look events, with TBabs × (diskbb + powerlaw) and determine the disc temperature to be kT<sub>in</sub> = 1.032 +/- 0.011 keV, and the power-law index to be Γ = 2.683 +/- 0.017, with an unabsorbed X-ray flux of F<sub>2–13 keV</sub> = (5.634 +/- 0.005) × 10<sup>-9</sup> erg s<sup>-1</sup>cm<sup>-2</sup>. The absorption column density is fixed as NH = 1.40 × 10<sup>22</sup> cm<sup>-2</sup> (ATel #17583). The current total flux is substantially contributed by the disc component at about 30%, whereas previous XRISM observation indicated a mere fraction of about 3%. Follow-up observations are encouraged. ------------------------------------------------------------------------------ Password Certification: Kotaro Fukushima (kxfukushima@gmail.com) https://www.astronomerstelegram.org/?read=17697 ============================================================================== ============================================================================== This is an automatically-generated notice. You can remove yourself permanently from receiving both the Daily Email Digest and Instant Email Notices from The Astronomer's Telegram by following this link: https://www.astronomerstelegram.org?unsubscribe&confirmation=a803d34e7ea924f9a4142bac00763549&address=stefano@bicar.it
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