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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 F05BA14569; Mon, 6 Jul 2026 09:07:55 +0200 (CEST) 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 87C4014486 for <stefano@bicar.it>; Mon, 6 Jul 2026 09:07:52 +0200 (CEST) Received: from server.astronomerstelegram.org (localhost [127.0.0.1]) by server.astronomerstelegram.org (Postfix) with ESMTP id 2DF2B28808BF for <stefano@bicar.it>; Mon, 6 Jul 2026 03:07:51 -0400 (EDT) To: stefano@bicar.it From: atel@astronomerstelegram.org Subject: ATel 17872, 17873, 17874 Message-Id: <20260706070751.2DF2B28808BF@server.astronomerstelegram.org> Date: Mon, 6 Jul 2026 03:07:51 -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 #17872 ATEL #17872 Title: GMRT non-detection of pulsed radio emission from EP J223759.5+531421 (EP260628c) Author: Yogesh Maan (NCRA - TIFR), Pulak Mohapatra (NCRA - TIFR), Chandreyee Maitra (IUCAA), Joeri van Leeuwen (ASTRON), Banshi Lal (NCRA - TIFR), Yash Bhusare (NCRA - TIFR) Queries: ymaan@ncra.tifr.res.in Posted: 5 Jul 2026; 08:52 UT Subjects:Radio, Neutron Star, Magnetar A new magnetar candidate, EP260628c, was recently caught in an X-ray outburst by the Einstein Probe's Wide-field X-ray Telescope on June 28, 2026 (Yang et al., Atel #17859). A localization with 10'' precision was obtained using subsequent observations by the Follow-up X-ray Telescope and NuSTAR. Combined timing analysis refined an initial, tentative 3 second period into a coherent, double-peaked X-ray pulsation period of 5.995872(3) second. The slow spin period, a sudden X-ray outburst, and the X-ray spectral properties of EP260628c, now designated as EP J223759.5+531421, suggest the source to be a newly identified magnetar candidate (Rea et al., Atel #17870). We observed EP J223759.5+531421 with the upgraded Giant Metrewave Radio Telescope (GMRT), utilizing 200 MHz of bandwidth centered at 650 MHz. The filterbank data were recorded with a sampling time of 0.16384 ms and 4096 channels across the bandwidth. Two separate scans were conducted on the target, with the start times UTC 2026-07-01T22:57:58 and UTC 2026-07-02T00:03:48, and integration times of 45 and 25 minutes, respectively. Following the excision of radio frequency interference (RFI) using RFIClean (Maan et al. 2021), we searched for any dispersed radio signals at and around the above reported period of 5.995872(3) seconds (ATel #17870) using the pulsar exploration and search toolkit (PRESTO; Ransom et al. 2002) and PSRCHIVE (Hotan et al. 2004), separately in the two scans. We also conducted a general search for any periodic radio signals using PRESTO, up to a maximum dispersion measure (DM) of 700 pc/cc (the YMW16 Galactic electron density model, Yao et al. 2017, suggests a maximum DM of 235 pc/cc along this line of sight). None of the above periodicity searches resulted in a genuine astrophysical signal, with a 10-sigma upper limit of 95 micro-Jy on the flux density, assuming a pulse-width 20% of the period. Our search for isolated, bright radio bursts also did not result in any genuine astrophysical bursts, however, we note that significant RFI contamination in some parts of the data might have affected this search. We place a 10-sigma upper limit of 100 mJy on any bright 10 ms wide pulse in our data. The above non-detection of radio signals suggests the magnetar candidate EP J223759.5+531421 to be either radio quiet or extremely faint. It is also possible that the onset of observable radio emission has not happened yet. Continued sensitive radio observations will help in establishing the radio nature of this source. 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: (1) Maan, Y., van Leeuwen, J., and Vohl, D. 2021, A&A, 650, A80. (2) Ransom, S. M., Eikenberry, S. S., and Middleditch, J. 2002, AJ, 124, 1788. (3) Hotan, A. W., van Straten, W., and Manchester, R. N. 2004, PASA, 21, 302. (4) Yao J. M., Manchester R. N. and Wang N. 2017, ApJ, 835, 29. ------------------------------------------------------------------------------ Password Certification: Yogesh Maan (maan@astron.nl) https://www.astronomerstelegram.org/?read=17872 ============================================================================== ATEL #17873 ATEL #17873 Title: OQ 334 has reached a new maximum optical magnitude of brighter than 13 mag in the R-band Author: S. Krauth, S. Ankara, L. Neisser, M. Grischy, J. Meiler, E. Bommert, S. Duerr, O. Domann, R. Goldbach, M. Heidemann, D. Kuberek, L. Lehmann, N. Mildner, F. Pfeuffer, K. Warmuth, M. Feige, M. Kopp, D. Reinhart, R. Steineke, N. Zottmann, C. Lorey (all Hans-Haffner-Sternwarte, Friedrich-Koenig-Gymnasium, Wuerzburg, Germany) J. Hessdoerfer, M. Kadler, L. Haury, K. Mannheim, F. Roesch (all University of Wurzburg, Germany) D. Elsaesser (TU Dortmund, Germany) Queries: dominik.elsaesser@tu-dortmund.de Posted: 5 Jul 2026; 13:23 UT Subjects:Optical, AGN, Blazar The flat spectrum radio quasar OQ 334, also known as QSO B2 1420+326; ICRS coord. (ep=J2000): RA 14 22 30.38; Dec +32 23 10.44 (Optical); z=0.68144 (Data from SIMBAD (http://simbad.u-strasbg.fr/simbad/) reached an exceptionally high magnitude of 12.754 in the R-band last night. <br /> The object has been in a very active state since early April (ATel #17745) and is showing extreme high states across wavelength ranges (ATel #17782, ATel #17790, ATel #17802, ATel #17821, ATel #17835, ATel #17854). The current phase of activity had already begun to become apparent as early as February 2026 (ATel #17654) or even as early as the end of November 2025 (ATel #17504) and has been growing in intensity ever since. <br /> In mid-March, the optical brightness of the object increased by roughly a magnitude, so that from the end of March onwards it remained between 15.2 and 15.6 mag (R-band) for several weeks. From the beginning of May, the R-band brightness rose sharply by almost 2 magnitudes within 12 days. Since then, the brightness has remained between 13.7 and 13 mag. Over the last two nights, the optical magnitude then significantly exceeded 13 mag, reaching a peak of 12.754 last night at JD 2461226.46905. <br /> <br /> We report the following preliminary R-band magnitudes: <br /> <br /> JD 2461225.3721 12.912 ± 0.024<br /> JD 2461225.4247 12.964 ± 0.016<br /> JD 2461225.4801 12.892 ± 0.010<br /> JD 2461225.5620 12.835 ± 0.015<br /> JD 2461226.3602 12.794 ± 0.025<br /> JD 2461226.4154 12.779 ± 0.006<br /> JD 2461226.4691 12.754 ± 0.033<br /> <br /> <br /> Our measurements are carried out as part of the long-term AGN monitoring program of the Naturwissenschaftliches Labor fuer Schueler am Friedrich-Koenig-Gymnasium (FKG), the Universitaet Wuerzburg, and TU Dortmund University. <br /> Comparison stars and their magnitudes were taken from the APASS DR9 catalogue (Henden et al., 2016). The Sloan magnitudes were transformed to the Johnson-Cousins system with the equations by Lupton (2005). <br /> The optical data were acquired through a Bessel R filter (Chroma) with a 0.5m CDK-astrograph (PlaneWave) and a Moravian C4-16000EC camera at the school and university observatory Hans-Haffner-Sternwarte in 97265 Hettstadt, Germany (https://schuelerlabor-wuerzburg.de/en/observatory/). Hans-Haffner-Sternwarte: https://schuelerlabor-wuerzburg.de/en/observatory/ ------------------------------------------------------------------------------ Password Certification: Dominik Elsaesser (dominik.elsaesser@tu-dortmund.de) https://www.astronomerstelegram.org/?read=17873 ============================================================================== ATEL #17874 ATEL #17874 Title: Follow-up of the ongoing exceptional flare of the FSRQ B2 1420+326 in the R and V optical bands Author: Alessandro Marchini (Astronomical Observatory, DSFTA, University of Siena - Italy); Leonardo Stiaccini, Gaia Verna (Department of Physical Sciences, Earth and Environment (DSFTA), University of Siena - Italy); Simone Leonini, Massimo Conti, Paolo Rosi, Luz Marina Tinjaca Ramirez (Montarrenti Observatory, Sovicille (Siena - Italy)); Ivo Peretto, Giovanni Furlato, Giuseppe Peretto, William Rivato (MarSEC Observatory, Marana di Crespadoro (Vicenza - Italy)); Giacomo Bonnoli (INAF - Brera Astronomical Observatory, Milan - Italy). Queries: gaia.verna@unisi.it Posted: 6 Jul 2026; 00:30 UT Subjects:Optical, AGN, Blazar, Transient We confirm the unprecedent optical flare of the flat-spectrum radio quasar B2 1420+326, also known as OQ 334 and 4FGL J1422.5+3223 (R.A. = 14 22 30.38, Dec. = +32 23 10.44; J2000; Gaia Collaboration 2021, A&A, 649, A1) at redshift at z = 0.682 (Hewett & Wild 2010, MNRAS, 405, 2302). The blazar was recently reported to be flaring in the R-band (ATel#17873). We confirm the exceptionally high magnitude of 12.65 in the R-band last night. In addition, we report the corresponding magnitude of 13.09 in the V-band. The following table reports the brightness recorded in the R-band and in the V-band of the Johnson-Cousins photometric system during the last month. Quoted uncertainty is statistical only. </br></br> Civil Date (UT) Mag (Err) Band - Observatory 2026 June 03.905 13.60 (0.01) V - Montarrenti 2026 June 06.911 13.44 (0.01) V - Montarrenti 2026 June 08.885 13.66 (0.01) V - Montarrenti 2026 June 11.883 14.10 (0.01) V - Siena 2026 June 12.867 14.07 (0.01) V - Siena 2026 June 14.922 13.91 (0.02) V - Montarrenti 2026 June 16.868 13.83 (0.01) V - Montarrenti 2026 June 18.910 13.96 (0.01) V - Montarrenti 2026 July 03.889 13.32 (0.01) V - Siena 2026 July 04.907 13.17 (0.01) V - Siena 2026 July 05.740 13.09 (0.01) V - Montarrenti 2026 June 03.845 13.19 (0.01) R - Siena 2026 June 03.905 13.17 (0.01) R - Montarrenti 2026 June 06.913 13.02 (0.01) R - Montarrenti 2026 June 06.943 12.97 (0.01) R - MarSEC 2026 June 07.705 13.11 (0.01) R - Siena 2026 June 08.850 13.25 (0.01) R - Siena 2026 June 08.885 13.24 (0.01) R - Montarrenti 2026 June 11.873 13.67 (0.01) R - Siena 2026 June 12.868 13.65 (0.01) R - Siena 2026 June 13.873 13.53 (0.01) R - Siena 2026 June 14.922 13.47 (0.01) R - Montarrenti 2026 June 14.935 13.48 (0.01) R - Siena 2026 June 16.869 13.41 (0.01) R - Montarrenti 2026 June 18.910 13.53 (0.01) R - Montarrenti 2026 July 02.928 13.09 (0.01) R - Siena 2026 July 03.889 12.87 (0.01) R - Siena 2026 July 04.907 12.72 (0.01) R - Siena 2026 July 05.868 12.65 (0.01) R - Montarrenti A publicly available plot of the B2 1420+32 data we collected in the last two months is available at <A HREF=https://www.dsfta.unisi.it/en/research/research-facilities/labs/astronomical-observatory/optical-follow-blazar-b2-142032-oq-334>this webpage</A>. Observations were conducted from the 0.30 m telescope of the Astronomical Observatory of the University of Siena (Siena, Italy - IAU MPC observatory code K54), the 0.53 m telescope at Montarrenti Observatory (Sovicille, Italy - C88) and the 0.36 m telescope of the Marana Space Explorer Center - MarSEC (Marana di Crespadoro, Italy - B79). Any inquiry on these observations can be addressed either to Alessandro Marchini (marchini@unisi.it) or to Gaia Verna (gaia.verna@unisi.it). We will continue monitoring the source in the following nights. Multi-wavelength follow-up is strongly encouraged. Brief descriptions of the instrumental setups used for the reported observations are available at the official webpage of the <A HREF="https://www.dsfta.unisi.it/en/research/labs/astronomical-observatory">Astronomical Observatory of the University of Siena</A> , the page of the <A HREF="https://astrofilisenesi.org/?page_id=250">Montarrenti Observatory</A> and the page of the MarSEC Observatory. <center><A HREF="https://www.dsfta.unisi.it/en/research/labs/astronomical-observatory">Astronomical Observatory of the University of Siena - Official Webpage</A></center> ------------------------------------------------------------------------------ Password Certification: Gaia Verna (gaia.verna@unisi.it) https://www.astronomerstelegram.org/?read=17874 ============================================================================== ============================================================================== This is an automatically-generated notice. 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