//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29004 SUBJECT: Swift GRB201209.24: Global MASTER-Net observations report DATE: 20/12/09 05:52:09 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D.Kuvshinov, D. Cheryasov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich, Yu. Sergienko (Blagoveschensk Educational State University) MASTER-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB201209.24 (trigger No 1011980,01h 32m 25.44s , -01d 45m 46.8s, R=0.05) errorbox 29 sec after notice time and 51 sec after trigger time at 2020-12-09 05:45:44 UT, with upper limit up to 16.8 mag. The observations began at zenith distance = 75 deg. The sun altitude is -33.0 deg. The galactic latitude b = -62 deg., longitude l = 147 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=1499038 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 57 | MASTER-OAFA | C | 10 | 16.8 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29005 SUBJECT: GRB 201209A: Swift detection of a burst DATE: 20/12/09 05:56:54 GMT FROM: David Palmer at LANL J.D. Gropp (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC), M. J. Moss (GWU), D. M. Palmer (LANL), T. Sakamoto (AGU), B. Sbarufatti (PSU), M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory Team: At 05:44:52 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 201209A (trigger=1011980). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 23.106, -1.763 which is RA(J2000) = 01h 32m 25s Dec(J2000) = -01d 45' 47" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a double-peaked structure with a duration of about 30 sec. The peak count rate was ~8000 counts/sec (15-350 keV), at ~7 sec after the trigger. The XRT began observing the field at 05:46:44.1 UT, 111.7 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 23.09079, -1.75347 which is equivalent to: RA(J2000) = 01h 32m 21.79s Dec(J2000) = -01d 45' 12.5" with an uncertainty of 3.5 arcseconds (radius, 90% containment). This location is 64 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. We cannot determine whether the source is fading at the present time. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 3.60 x 10^20 cm^-2 (Willingale et al. 2013). The initial flux in the 2.5 s image was 6.48e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 121 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.04. Burst Advocate for this burst is J.D. Gropp (jdg44 AT psu.edu). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29006 SUBJECT: GRB 201209A: FRAM-Auger optical limit DATE: 20/12/09 06:50:15 GMT FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ), Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek, Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza (Institute of Physics, Prague, CZ) report: The 30cm robotic telescope FRAM-Auger in Malargue (Argentina) reacted robotically to the Swift/BAT alert of GRB201209A (Gropp et al., GCNC 29005), starting with a series of 20 s R-band images at 05:45:40 UT, i.e. 48 s post trigger. We do not detect any new or strongly variable source at or around the reported X-ray error box in single frames nor in a combined 20 x 20 s image spanning the period from 0.8 min to 11.9 min after the initial trigger. The combined exposure has a 3-sigma limiting magnitude R(Vega) ~ 17.4. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29007 SUBJECT: GRB 201209A: KAIT Optical Upper Limit DATE: 20/12/09 07:05:46 GMT FROM: Weikang Zheng at UC Berkeley The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, responded to Swift GRB 201209A (Gropp et al., GCN 29005) starting at 05:48:09 UT, 197 s after the burst under cloudy condition. Observations were performed with an automatic sequence in the clear (roughly R), V, and I filters, and the exposure time was 20 s per image. We do not detect any optical afterglow candidate within the XRT position error circle (Gropp et al., GCN 29005), neither in single image, nor in the co-add images. The typical limiting magnitude of our single clear image is about 15.0 mag calibrated to the USNOB1.0 catalog. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29009 SUBJECT: GRB 201209A: Enhanced Swift-XRT position DATE: 20/12/09 09:32:44 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 1536 s of XRT Photon Counting mode data and 2 UVOT images for GRB 201209A, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 23.09069, -1.75468 which is equivalent to: RA (J2000): 01h 32m 21.77s Dec (J2000): -01d 45' 16.8" with an uncertainty of 1.7 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29011 SUBJECT: GRB 201209A: AstroSat CZTI detection DATE: 20/12/09 12:05:42 GMT FROM: Gaurav Waratkar at IIT Bombay D. Nadella (NITK), G. Waratkar (IITB), A. Vibhute (IUCAA), S. Gupta (IUCAA), P. Sawant (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al, 2020, arxiv:2011.07067) showed detection of a long GRB 201209A, which was also detected by Swift-BAT (GCN #29005). The source was clearly detected in the 20-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-12-09 05:44:56.500 UT. The measured peak count rate associated with the burst is 456 (+51, -54) cts/s above the background in the combined data of four quadrants, with a total of 3215 (+719, -885) cts. The local mean background count rate was 557 (+4, -3) cts/s. Using cumulative rates, we measure a T90 of 23 (+14, -12) s. It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-12-09 05:44:56.336 UT. The measured peak count rate is 697 (+81, -89) cts/s above the background in the combined Veto data of four quadrants, with a total of 4866 (+1506, -1667) cts. The local mean background count rate was 1856 (+6, -7) cts/s. We measure a T90 of 25 (+26, -15) s from the cumulative Veto light curve. CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29013 SUBJECT: GRB 201209A: Xinglong-2.16m likely optical afterglow detection DATE: 20/12/09 15:24:53 GMT FROM: Dong Xu at NAOC/CAS Z.P. Zhu (NAOC, HUST), S.Y. Fu, X. Liu, D. Xu (NAOC) report on behalf of a larger collaboration: We observed the field of GRB 201209A (Gropp et al., GCN 29005) using the 2.16-m optical telescope located at Xinglong, Hebei, China, equipped with the BFOSC camera. Observations started at 13:05:43 UT on 2020-12-09, and 2x360 s, 3x600 s R-band frames were obtained. An uncatalogued source is detected in our stacked image at coordinates R.A. (J2000) = 1:32:21.76 Dec. (J2000) = -1:45:17.13 with an uncertainty of ~0.5 arcsec, being fully consistent with the Enhanced XRT position (Goad et al., GCN 29009). Calibrated with nearby PS1 stars, the source has m(R) = 22.05 +/- 0.16 mag at a median time of 0.321 days post-burst, whereas PS1 is deeper but no object is present at the position. We thus conclude that the source is likely the optical afterglow of the burst. We acknowledge excellent support from the Xinglong-2.16m observing staff, in particular Aiying Zhou and Jie Zheng. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29014 SUBJECT: GRB 201209A: Swift-XRT refined Analysis DATE: 20/12/09 15:38:51 GMT FROM: Phil Evans at U of Leicester J. D. Gropp (PSU), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB), T. Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB) and J.D. Gropp report on behalf of the Swift-XRT team: We have analysed 6.2 ks of XRT data for GRB 201209A (Gropp et al. GCN Circ. 29005), from 117 s to 29.1 ks after the BAT trigger. The data comprise 43 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN Circ. 29009).A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.98 (+/-0.08). The best-fitting absorption column is 1.54 (+0.26, -0.25) x 10^21 cm^-2, in excess of the Galactic value of 3.6 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.5 x 10^-11 (4.3 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.54 (+0.26, -0.25) x 10^21 cm^-2 Galactic foreground: 3.6 x 10^20 cm^-2 Excess significance: 7.9 sigma Photon index: 1.98 (+/-0.08) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01011980. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29021 SUBJECT: GRB 201209A: Swift-BAT refined analysis DATE: 20/12/09 23:01:54 GMT FROM: Hans Krimm at NSF/NASA-GSFC M. Stamatikos (OSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 201209A (trigger #1011980) (Gropp, et al., GCN Circ. 29005). The BAT ground-calculated position is RA, Dec = 23.096, -1.762 deg which is RA(J2000) = 01h 32m 23.0s Dec(J2000) = -01d 45' 43.8" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 11%. The mask-weighted light curve shows some early emission starting at ~T-20 sec, and two bright, symmetrical peaks centered at T+0 and T+7 sec. The burst has faded to background by T+30 sec. T90 (15-350 keV) is 48.0 +- 16.0 sec (estimated error including systematics). The time-averaged spectrum from T-31.66 to T+32.34 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.56 +- 0.06. The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from T+7.84 sec in the 15-150 keV band is 12.2 +- 1.1 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/1011980/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29026 SUBJECT: GRB 201209A: Swift/UVOT Upper Limits DATE: 20/12/11 13:01:06 GMT FROM: Kira Simpson at PSU GRB 201209A: Swift/UVOT Upper Limits K. K. Simpson (PSU) and J. D. Gropp (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 201209A 121 s after the BAT trigger (Gropp et al., GCN Circ. 29005). No optical afterglow consistent with the XRT position (Goad et al. GCN Circ. 29009) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 121 271 147 >20.1 u_FC 334 584 246 >20.3 white 121 1706 412 >20.9 v 663 1583 117 >19.2 b 590 1682 117 >19.5 u 334 1657 343 >20.7 w1 712 1632 97 >19.8 m2 688 1260 39 >19.2 w2 1018 1211 39 >19.4 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.04 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29050 SUBJECT: GRB 201209A: Insight-HXMT/HE detection DATE: 20/12/15 14:40:28 GMT FROM: Y Q Zhang at IHEP Y. Q. Zhang, C. Cai, J. C. Liu, Q. Luo, S. Xiao, W. C. Xue, Q. B. Yi, C. Zheng，Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, X. Y. Song, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: At 2020-12-09T05:44:52.53 (T0), Insight-HXMT/HE detected GRB 201209A (trigger ID: HEB201209239) in a routine search of the data, which also triggered Swift/BAT (Gropp J. et al., GCN #29005) and AstroSat/CZTI ( Nadella D. et al., GCN #29011).. The Insight-HXMT/HE light curve mainly consists of multiple pulses with a duration (T90) of 9.99 s measured from T0-1.09 s. The 1-ms peak rate, measured from T0+7.16 s, is 778 cnts/sec. The total counts from this burst is 2926 counts. URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB201209239_lc.jpg All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (deposited energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the telescope. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information about it could be found at: http://www.hxmt.org. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29094 SUBJECT: GRB 201209A: Mondy optical observations, afterglow confirmation DATE: 20/12/20 10:46:03 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE), A. Pozanenko (IKI), A. Volnova (IKI), S. Belkin (IKI), E. Klunko (ISTP) report on behalf of IKI GRB FuN: We observed the field of GRB 201209A (Gropp et al., GCN 29005) with AZT-33IK telescope of Sayan observatory (Mondy) starting on Dec. 09 (UT) 11:41:13 (i.e. 0.28 days) and next epochs later. We detected a weak source within enhanced XRT position (Goad et al., GCN 29005) at ~1.4 days after GRB 201209A trigger and not detected in other epochs. Thus we confirm the optical afterglow detection on 0.321 days at R = 22.05 +/- 0.16 (Zhu et al. GCN 29013). Preliminary photometry of the field and afterglow is following Date UT start t-T0 Filter Exp. OT Err. UL(3sigma) (mid, days) (s) 2020-12-09 11:41:13 42*120 R 0.27873 n/d n/d 21.7 2020-12-10 14:26:13 45*120 R 1.39332 23.4 0.3 23.5 2020-12-12 11:14:21 39*120 R 3.25868 n/d n/d 22.2 2020-12-13 12:03:41 38*120 R 4.26307 n/d n/d 22.9 The photometry is based on nearby USNO-B1.0 stars.