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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 C90631453F; Sat, 17 Jan 2026 08:18:02 +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=-0.0 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 96A6A14491 for <stefano@bicar.it>; Sat, 17 Jan 2026 08:17:32 +0100 (CET) Received: from server.astronomerstelegram.org (localhost [127.0.0.1]) by server.astronomerstelegram.org (Postfix) with ESMTP id B01C32880A42 for <stefano@bicar.it>; Sat, 17 Jan 2026 02:17:31 -0500 (EST) To: stefano@bicar.it From: atel@astronomerstelegram.org Subject: ATel 17605, 17606, 17607 Message-Id: <20260117071731.B01C32880A42@server.astronomerstelegram.org> Date: Sat, 17 Jan 2026 02:17:31 -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 #17605 ATEL #17605 Title: Renewed activity of Cygnus X-3 observed with the Nasu telescope array at 1.4 GHz Author: K. Tsubono (Univ. Tokyo), K. Asuma (Kawaguchi-Kita High School), K. Niinuma (Yamaguchi Univ.), K. Takefuji (JAXA) and T. Daishido (Waseda Univ.) Queries: tsubono@phys.s.u-tokyo.ac.jp Posted: 16 Jan 2026; 12:38 UT Subjects:Radio, Binary, Black Hole, Transient Following the initial report by RATAN-600 (ATel #17600), we independently detected renewed radio emission from Cygnus X-3 with the Nasu telescope array. Cygnus X-3 is known to exhibit recurrent radio outbursts on timescales of several years. A recent example is the detection of strong radio flaring activity by the RATAN radio monitoring program in July 2024 (ATel #16738). From mid-November 2025, Cygnus X-3 appears to have entered a quenched hard X-ray state, as indicated by recent Swift/BAT observations in the 15-50 keV band (see https://swift.gsfc.nasa.gov/results/transients/CygX-3/), which show a pronounced suppression of the hard X-ray flux. An increase in the soft X-ray flux from Cygnus X-3 has been reported in ATel #17585 and suggested as a possible precursor to a forthcoming major radio flare. Such X-ray behavior has historically been observed shortly before strong radio outbursts in this source. Using the Nasu telescope array, we detected renewed brightening of the radio emission from Cygnus X-3 on 2026 January 16, following approximately 50 days of quiescence. The flux density was measured to be approximately 2.3 Jy at 1.4 GHz (UT 03:30). This renewed radio activity occurs during a prolonged quenched hard X-ray state, a condition historically associated with major radio flaring in Cygnus X-3. The observed behavior may therefore represent the early phase of a larger radio outburst. We will continue radio monitoring of Cygnus X-3. The Nasu telescope array is a spatial fast Fourier transform (FFT) interferometer consisting of eight linearly aligned antennas with 20 m spherical dishes. This type of interferometer was developed to survey transient radio sources, providing an angular resolution comparable to that of a 160 m dish and a field of view equivalent to that of a 20 m dish. Nasu telescope array HP: https://nasu-radio-telescope.space ------------------------------------------------------------------------------ Password Certification: Kimio Tsubono (tsubono@phys.s.u-tokyo.ac.jp) https://www.astronomerstelegram.org/?read=17605 ============================================================================== ATEL #17606 ATEL #17606 Title: Updated CHIME/FRB Baseband Localization of FRB 20251229A Author: Mason Ng (McGill University, Trottier Space Institute) on behalf of the CHIME/FRB Collaboration Queries: mason.ng@mcgill.ca Posted: 16 Jan 2026; 17:23 UT Subjects:Radio, Fast Radio Burst In ATel #17574, we reported the discovery of the potentially hyperactive repeating fast radio burst source, FRB 20251229A. In that ATel, we published best-fit localization coordinates from an initial analysis of the raw voltage (baseband) data using an older version of the localization pipeline (Michilli et al. 2021). Here, we update the best-fit baseband localization for FRB 20251229A using a newer version of the pipeline, with the latest calibration methods. The new localization, which is approximately 35" away from the previously reported localization (ATel #17574), is the following with errors quoted at 1σ uncertainty: RA (J2000): 20h 41m 23.9s +/- 1.8s Dec. (J2000): 16° 01' 31" +/- 36" RA (J2000): 310.3494 +/- 0.0077 deg. Dec. (J2000): 16.0252 +/- 0.0099 deg. ------------------------------------------------------------------------------ Password Certification: Mason Ng (masonng@mit.edu) https://www.astronomerstelegram.org/?read=17606 ============================================================================== ATEL #17607 ATEL #17607 Title: MAXI monitoring of Hercules X-1 entering the extended low state in 2025 Author: T. Mihara, K. Asai (RIKEN), M. Nakajima, H. Negoro, K. Takagi, H. Takahashi, H. Nishio (Nihon U.), 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, S. Kobayashi (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.), S. Yamada (Tohoku U), reports on behalf of the MAXI team: Queries: tmihara@riken.jp Posted: 17 Jan 2026; 01:26 UT Subjects:X-ray, Binary, Neutron Star, Pulsar Her X-1 is a well-studied binary X-ray pulsar. It has the 35 day super orbital cycle besides 1.24 s spin period and 1.70 day orbital period (e.g. Du et al. 2026). MAXI/GSC has been monitoring the 35-day cycle since 2009. It had repeated regular 35-day cycle until the cycle number 212 in 2025 May. The cycle number is defined by Leahy and Wang (2020) based on the Swift/BAT data. The flux of the main-on is decreasing since then, as shown in https://maxi.riken.jp/plot/cyc211_218.png The normalization (relative flux with respect to the average) changed as 1.1, 0.63, 0.39 and 0.11 in cycle number 212, 214, 216 and 218, respectively. In the last cycle, the flux dropped to ∼1/10 of the regular flux and was barely detected with MAXI/GSC. Still some source flux remains as the periodical flux drop due to eclipses are seen at around 61012.0, 61013.5, 61015.0 MJD. https://maxi.riken.jp/plot/herx1_2025.jpg Note the observation pattern of MAXI repeats according to the 70 day precession cycle of the ISS orbit. Her X-1 is located in a region covered by the broken cameras. Therefore the observation of the main-on is once in two cycles. At present, the observations are done in the even-numbered cycle. Her X-1 seems to be entering the extended low-state (LS). The extended LS was first reported by EXOSAT observations in Parmar et al. (1985). There were two extended LS in the RXTE/ASM era. The last one occurred around 53000 MJD (2003 December) (Leahy et al. 2010). The current one is the first one since then after 22 years. The decreasing trend of the flux is similar to the previous two extended LS with RXTE/ASM. https://maxi.riken.jp/plot/herx1_lowstate_asm_gsc.png ------------------------------------------------------------------------------ Password Certification: Tatehiro Mihara (mihara@crab.riken.jp) https://www.astronomerstelegram.org/?read=17607 ============================================================================== ============================================================================== 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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