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Return-Path: <atel@astronomerstelegram.org> Delivered-To: stefano@bicar.it Received: by mail.planetcloud-host.com (Postfix, from userid 1016) id C931B14602; Thu, 16 Jul 2026 09:15:40 +0200 (CEST) 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, 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 274D3145D9 for <stefano@bicar.it>; Thu, 16 Jul 2026 09:15:37 +0200 (CEST) Received: from server.astronomerstelegram.org (localhost [127.0.0.1]) by server.astronomerstelegram.org (Postfix) with ESMTP id 7B8682880A8B for <stefano@bicar.it>; Thu, 16 Jul 2026 03:15:36 -0400 (EDT) To: stefano@bicar.it From: atel@astronomerstelegram.org Subject: ATel 17892, 17893, 17894, 17895, 17896, 17897 Message-Id: <20260716071536.7B8682880A8B@server.astronomerstelegram.org> Date: Thu, 16 Jul 2026 03:15:36 -0400 (EDT) ------------------------------------------------------------------------------ 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 #17892 ATEL #17892 Title: Low frequency upper limits on continuum radio emission from EP J223759.5+531421 (EP260628c) Author: Pulak Mohapatra (NCRA - TIFR, India), Yogesh Maan (NCRA - TIFR), Yash Bhusare (NCRA - TIFR), Chandreyee Maitra (IUCAA, MPE), Joeri van Leeuwen (ASTRON), Banshi Lal (NCRA - TIFR) Queries: pulakmohapatra02@gmail.com Posted: 15 Jul 2026; 09:37 UT Subjects:Radio, Magnetar EP J223759.5+531421 (EP260628c) was recently discovered with the Wide-field X-ray Telescope which was further localized to 10 arcseconds precision by the Follow-up X-ray Telescope, both on board the Einstein Probe, where a tentative 3 second periodicity was seen (Yang et al., Atel #17859). Further follow up observations revealed a 5.995872(2)s periodic pulsed X-ray emission, which, along with the X-ray outburst, pulse-profile and spectral properties, confirmed it to be a magnetar candidate (Rea et al., Atel #17870). We conducted observations of EP260628c using Band-4 (550 - 750 MHz) and Band-5 (1060- 1460 MHz) of the upgraded Giant Metrewave Radio Telescope (uGMRT). We previously reported non-detection and subsequent upper limits on the pulsed emission at 650 MHz (Maan et al., Atel #17872). Here we present the upper limits on the continuum emission from both the bands and on the pulsed emission from Band-5 observation. We had a total of 1 hr 10 minutes and 1 hr 23 minutes of on-source observing time in Band-4 and Band-5 respectively. We carried out the radio imaging by using a combination of automated imaging using CAPTURE (R. Kale & C. H. Ishwara-Chandra 2020) with manual intervention, wherever necessary. Since the source is near the galactic plane, and there are multiple bright extended sources in the field, the image has some low-level systematic artifacts. However, the upper limits presented here are unlikely to be affected by these low-level systematic artifacts. We also cross matched the positions of the bright sources with the available data from NASA/IPAC Extragalactic Database (NED), and find that the positions are consistent within the synthesized beam size (i.e., the resolution of the radio image). We used Briggs weighting with a robust parameter of 0.5 so that the image has optimum sensitivity along with minimal artifacts. We obtain RMS noise of 24.0 micro-Jy/beam and 16.9 micro-Jy/beam in Band-4 and Band-5, respectively. Given the low-level systematics in the image, we place conservative, 5-sigma upper limits of 120 micro-Jy/beam and 84.5 micro-Jy/beam, at Band-4 and Band-5, respectively. The final images are accessible at the link provided below. The image in the left subplot is the Band-5 image and the one on the right is the Band-4 image. The yellow dashed circle represents the 10" localization uncertainty region. The closest detected source is ~55" away from the target's best position. The synthesized beam size is denoted by the gray ellipse at the bottom left of both the images. The colorbar represents the flux density in units of Jy/beam. We also conducted the search for any pulsed radio signals at or around the period of the magnetar candidate as well as for any bright, isolated bursts, using the time-series data. The procedure followed for these searches was similar to that used for the Band-4 data (Atel #17872). No genuine pulsed signal was found, and we place 10-sigma upper limits of 65 micro-Jy on periodic emission (assuming 10% pulse duty cycle) and 100 mJy on any 10 ms wide bright pulses. Given these upper limits, the pulsed radio emission from the magnetar candidate is expected to be either very faint, or the onset of radio activity has not started yet. Our upper limits on the continuum emission also constrain the presence of any persistent emission counterpart, e.g., an associated magnetar wind nebula or radio emission from large plasma outflows. We would like to thank the scheduling team and the observatory for the prompt scheduling of our observations. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. References: Camilo, F., et al. 2006, Nature, 442, 892. Kale, R., & Ishwara-Chandra, C. H. 2020, ExA, 51, 95. NASA/IPAC Extragalactic Database (NED) 2019, NASA/IPAC Extragalactic Database (NED), IPAC, doi:10.26132/NED1 ------------------------------------------------------------------------------ Password Certification: Yogesh Maan (maan@astron.nl) https://www.astronomerstelegram.org/?read=17892 ============================================================================== ATEL #17893 ATEL #17893 Title: Addendum: Low frequency upper limits on continuum radio emission from EP J223759.5+531421 (EP260628c) Author: Pulak Mohapatra (NCRA - TIFR, India), Yogesh Maan (NCRA - TIFR), Yash Bhusare (NCRA - TIFR), Chandreyee Maitra (IUCAA, MPE), Joeri van Leeuwen (ASTRON), Banshi Lal (NCRA - TIFR) Queries: pulakmohapatra02@gmail.com Posted: 15 Jul 2026; 09:44 UT Subjects:Radio, Magnetar We note that the link intended to be included at the end of ATel #17892 is missing. Here is the link to the radio images discussed in ATel #17892: https://drive.google.com/file/d/1Gw45GV7I3Gpm0PfalacP2hZW9oOqYuKw/view https://drive.google.com/file/d/1Gw45GV7I3Gpm0PfalacP2hZW9oOqYuKw/view: https://drive.google.com/file/d/1Gw45GV7I3Gpm0PfalacP2hZW9oOqYuKw/view ------------------------------------------------------------------------------ Password Certification: Yogesh Maan (maan@astron.nl) https://www.astronomerstelegram.org/?read=17893 ============================================================================== ATEL #17894 ATEL #17894 Title: Spectroscopic Classification of AT2026rwn with the Lick Shane Telescope Author: FirstnJ. Karcheski, K. C. Patra, K. W. Davis, R. J. Foley (UCSC) Queries: jkarches@ucsc.edu Posted: 15 Jul 2026; 20:16 UT Subjects:Optical, Supernovae, Transient We report the classification of the astrophysical transient 2026rwn from spectroscopic observations with the Kast spectrograph on the Shane telescope obtained on 2026 July 07 UT. The target was supplied by ZTF and identified using the target management platform YSE-PZ (Coulter et al., 2023, PASP, 135, 4501). The classification was aided by SNID-SAGE (Toppa & Smartt, 2026, MNRAS, 549, 4). Name | IAU Name | RA (J2000) | Dec (J2000) | z | Type | Phase | Notes ZTF26abfftwf | AT2026rwn | 22:11:52.17 | +00:06:31.21 | 0.0334 | SN | rising | (1) Notes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) The spectrum displays a blue continuum consistent with a young CCSN at the host redshift. Superimposed on the continuum is a narrow (FWHM ~ 700 km/s) He II 4686 emission line. We do not detect any other emission features from the SN. We encourage follow-up observations. ------------------------------------------------------------------------------ Password Certification: Ryan Foley (foley@ucsc.edu) https://www.astronomerstelegram.org/?read=17894 ============================================================================== ATEL #17895 ATEL #17895 Title: Fermi-LAT detection of renewed gamma-ray activity from the TeV BL Lac VER J0521+211 Author: E. Bronzini (INAF-OAS), P. Monti-Guarnieri (University of Trieste & INFN Trieste), C. Bartolini (INFN Bari), G. La Mura (INAF-O. A. Cagliari), on behalf of the Fermi Large Area Telescope Collaboration Queries: ettore.bronzini@inaf.it Posted: 15 Jul 2026; 21:09 UT Subjects:Gamma Ray, >GeV, AGN, Blazar 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 TeV BL Lac VER J0521+211, associated with the radio source TXS 0518+211 (a.k.a. RGB J0521+212) and the GeV gamma-ray source 4FGL J0521.7+2112 (Abdollahi et al. 2022, ApJS, 260, 53), with coordinates R.A. = 80.44152 deg, Dec. = +21.21429 deg (J2000; Beasley et al. 2002 ApJS, 141, 13), and at uncertain redshift (Archambault et al. 2013, ApJ, 776, 2, 69; Paiano et al. 2017, ApJ, 837, 2, 144). Preliminary analysis indicates that this source was in an elevated gamma-ray emission state on 14 July 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 about 10 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). The corresponding photon index is 1.9+/-0.2 and is consistent with the 4FGL-DR4 value of 1.95+/-0.01 within the uncertainties. The enhanced state led to the detection of seven high-energy photons associated with the source at a confidence level p > 0.85 between July 01, 2026 and July 14, 2026. The highest energy event was a 80 GeV photon observed on July 14, 2026 at 06:35:23 UT. The Fermi LAT Collaboration has previously reported gamma-ray flaring activity from VER J0521+211 in ATels #5472, #13528. Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source belongs to the "LAT Monitored Sources" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT is available at <a href="https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/VER_0521p211">VER J0521+211</a>. The gamma-ray light curve of the source is also available through the Fermi-LAT Light Curve Repository (LCR) at <a href="https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.html?source_name=4FGL_J0521.7+2112">TXS 0518+211</a>. For this source, the Fermi-LAT contact person is Sara Buson (sara.buson@gmail.com). 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. ------------------------------------------------------------------------------ Password Certification: Ettore Bronzini (ettore.bronzini@inaf.it) https://www.astronomerstelegram.org/?read=17895 ============================================================================== ATEL #17896 ATEL #17896 Title: SN 2026sqf: upper limits from an IceCube neutrino search Author: Yuhua Yao (University of Wisconsin-Madison), Anna Franckowiak (Ruhr-University Bochum) for the IceCube Collaboration Queries: anna.franckowiak@desy.de Posted: 15 Jul 2026; 21:26 UT Subjects:Neutrinos, Supernovae The IceCube Collaboration (http://icecube.wisc.edu/) reports: IceCube has performed a search for track-like muon neutrino events arriving from the direction of SN 2026sqf following the report from BHTOM (AstroNote: https://www.wis-tns.org/astronotes/astronote/2026-214), in a time range of six days (2026-07-03 06:01:09.000 UTC to 2026-07-09 06:01:09.000 UTC), during which IceCube was collecting good quality data. The search window extends from five days before to one day after the reported discovery time, 2026-07-08 06:01:09 UTC. The five-day pre-discovery interval accounts for the uncertainty in the explosion and shock-breakout time, while the additional day after discovery includes the earliest follow-up observations. We report a p-value of 1.00, consistent with no significant excess track events with respect to the atmospheric background only hypothesis. We accordingly derive a time-integrated muon-neutrino flux upper limit for this source of E^2 dN/dE = 7.4e-2 GeV cm^-2 at 90% CL, for an E^-2 power law. 90% of events IceCube would detect from a source at this declination with an E^-2 spectrum are between approximately 600 GeV and 250 TeV. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu. ------------------------------------------------------------------------------ Password Certification: Anna Franckowiak (anna.franckowiak@desy.de) https://www.astronomerstelegram.org/?read=17896 ============================================================================== ATEL #17897 ATEL #17897 Title: BVRI photometry of B2 1420+326 Author: E. Zaharieva, B. Aleksandrov, V. Efremov, M. Petrova, A. Todorov, E. Ovcharov (Sofia University, Bulgaria) Queries: evgeni@phys.uni-sofia.bg Posted: 15 Jul 2026; 22:44 UT Subjects:Optical, Blazar Following the recent reports of an exceptionally high optical state of the changing-look blazar B2 1420+326 (OQ 334, z=0.68) - ATel #17884, #17873, #17874 and references therein - we performed BVRI photometric monitoring of this object with the 35 cm Schmidt Cassegrain telescope + CCD SBIG STX-16803 in BVRI bands at the student Space and Earth Sciences Summer School "Prof. Marin Bachevarov", Dren, Bulgaria, during the nights of July 13/14 and 14/15, 2026. The preliminary nightly magnitudes are listed below: JD            Filter     mag ± err 2461236.3364   B   13.472 ± 0.063 2461236.3387   B   13.523 ± 0.030 2461236.3409   B   13.574 ± 0.033 2461236.3432   B   13.612 ± 0.0243 2461236.3454   B   13.616 ± 0.072 2461235.4186   I   12.375 ± 0.06 2461235.4208   I   12.390 ± 0.17 2461235.4231   I   12.437 ± 0.261 2461235.4253   I   12.535 ± 0.155 2461236.3703   I   12.382 ± 0.018 2461236.3726   I   12.39 ± 0.023 2461236.3748   I   12.376 ± 0.023 2461236.3771   I   12.378 ± 0.026 2461236.3793   I   12.384 ± 0.030 2461235.3868   R   12.795 ± 0.021 2461235.3891   R   12.789 ± 0.019 2461235.3913   R   12.784 ± 0.013 2461235.4050   R   12.785 ± 0.012 2461235.4073   R   12.797 ± 0.021 2461235.4095   R   12.775 ± 0.018 2461235.4118   R   12.789 ± 0.014 2461235.4141   R   12.783 ± 0.015 2461236.3590   R   12.824 ± 0.013 2461236.3613   R   12.825 ± 0.013 2461236.3635   R   12.829 ± 0.016 2461236.3658   R   12.827 ± 0.013 2461236.3680   R   12.832 ± 0.015 2461236.4105   R   12.840 ± 0.016 2461236.4127   R   12.859 ± 0.019 2461236.4150   R   12.886 ± 0.055 2461235.3938   V   12.995 ± 0.02 2461235.3960   V   13.008 ± 0.017 2461235.3983   V   12.979 ± 0.027 2461235.4005   V   13.011 ± 0.03 2461236.3477   V   13.058 ± 0.020 2461236.3500   V   13.044 ± 0.025 2461236.3522   V   13.035 ± 0.018 2461236.3545   V   13.043 ± 0.020 2461236.3567   V   13.043 ± 0.021 Compared to the R-band magnitudes reported in ATel #17884 (R = 12.42 on July 9th), our measurements indicate that the source has faded by about 0.4 mag and continues a gradual decline from its historical optical maximum, while still remaining in an exceptionally bright state. Comparison stars and their magnitudes were taken from the APASS DR9 catalogue (Henden et al., 2016). The study was supported by the National Program 'Education with Science' D01-172/18.09.2024 and the National RI Roadmap Project D01-109/30.06.2025 with the Ministry of Education and Science of the Republic of Bulgaria. ------------------------------------------------------------------------------ Password Certification: Evgeni Ovcharov (evgeni@phys.uni-sofia.bg) https://www.astronomerstelegram.org/?read=17897 ============================================================================== ============================================================================== 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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