//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26677 SUBJECT: GRB 200109A: Fermi GBM Final Real-time Localization DATE: 20/01/09 01:56:09 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 01:45:51 UT on 9 Jan 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200109A (trigger 600227156.894404 / 200109074). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 284.7, Dec = 68.9 (J2000 degrees, equivalent to J2000 18h 58m, 68d 54'), with a statistical uncertainty of 10.4 degrees. The angle from the Fermi LAT boresight is 40.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200109074/quicklook/glg_skymap_all_bn200109074.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200109074/quicklook/glg_healpix_all_bn200109074.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200109074/quicklook/glg_lc_medres34_bn200109074.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26678 SUBJECT: GRB 200109A: Swift detection of a burst DATE: 20/01/09 02:00:28 GMT FROM: David Palmer at LANL A. Melandri (INAF-OAB), M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB), J.D. Gropp (PSU), N. J. Klingler (PSU), S Laha (GSFC/UMBC/CRESST), D. M. Palmer (LANL), M. H. Siegel (PSU), K. K. Simpson (PSU) and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory Team: At 01:46:16 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 200109A (trigger=948361). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 307.171, +53.003 which is RA(J2000) = 20h 28m 41s Dec(J2000) = +53d 00' 12" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of 70 sec. The peak count rate was ~1600 counts/sec (15-350 keV), at ~2 sec after the trigger. The XRT began observing the field at 01:47:59.1 UT, 102.9 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 307.1258, 52.9932 which is equivalent to: RA(J2000) = 20h 28m 30.19s Dec(J2000) = +52d 59' 35.5" with an uncertainty of 2.2 arcseconds (radius, 90% containment). This location is 104 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. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 3.98 x 10^21 cm^-2 (Willingale et al. 2013). The initial flux in the 2.5 s image was 1.12e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 109 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. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the sub-image. 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 0.29. Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). 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: 26679 SUBJECT: Swift GRB200109.07: Global MASTER-Net observations report DATE: 20/01/09 02:02:27 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), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE), 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-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB200109.07 (trigger No 948361,20h 28m 41.04s , +53d 00m 10.8s, R=0.05) errorbox 12 sec after notice time and 70 sec after trigger time at 2020-01-09 01:47:26 UT, with upper limit up to 17.9 mag. The observations began at zenith distance = 75 deg. The sun altitude is -31.2 deg. The galactic latitude b = 8 deg., longitude l = 90 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=1254883 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 75 | MASTER-Kislovodsk | P- | 10 | 16.3 | 75 | MASTER-Kislovodsk | P| | 10 | 16.1 | 106 | MASTER-Kislovodsk | P- | 20 | 16.7 | 106 | MASTER-Kislovodsk | P| | 20 | 16.6 | 133 | MASTER-Kislovodsk | P- | 20 | 16.6 | 133 | MASTER-Kislovodsk | P| | 20 | 16.6 | 164 | MASTER-Kislovodsk | P| | 30 | 16.8 | 209 | MASTER-Kislovodsk | P| | 120 | 17.4 | Coadd 205 | MASTER-Kislovodsk | P| | 40 | 16.8 | 257 | MASTER-Kislovodsk | P- | 50 | 17.1 | 322 | MASTER-Kislovodsk | P- | 180 | 17.9 | Coadd 257 | MASTER-Kislovodsk | P| | 50 | 16.9 | 318 | MASTER-Kislovodsk | P- | 60 | 17.2 | 318 | MASTER-Kislovodsk | P| | 60 | 17.0 | 398 | MASTER-Kislovodsk | P| | 220 | 17.7 | Coadd 390 | MASTER-Kislovodsk | P- | 70 | 17.4 | 390 | MASTER-Kislovodsk | P| | 70 | 17.1 | 477 | MASTER-Kislovodsk | P- | 90 | 17.4 | 477 | MASTER-Kislovodsk | P| | 90 | 17.4 | 584 | MASTER-Kislovodsk | P- | 110 | 17.5 | 584 | MASTER-Kislovodsk | P| | 110 | 17.3 | 710 | MASTER-Kislovodsk | P- | 130 | 17.6 | 710 | MASTER-Kislovodsk | P| | 130 | 17.4 | The observation and reduction will continue. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26681 SUBJECT: GRB 200109A: Enhanced Swift-XRT position DATE: 20/01/09 10:09:58 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 406 s of XRT Photon Counting mode data and 1 UVOT images for GRB 200109A, 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 = 307.12462, +52.99363 which is equivalent to: RA (J2000): 20h 28m 29.91s Dec (J2000): +52d 59' 37.1" 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: 26682 SUBJECT: GRB 200109A: Swift-XRT refined Analysis DATE: 20/01/09 10:55:47 GMT FROM: Phil Evans at U of Leicester V. D'Elia (ASDC), D.N. Burrows (PSU), J. D. Gropp (PSU), A. Tohuvavohu (U. Toronto), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), A. D'Ai (INAF-IASFPA) and A. Melandri report on behalf of the Swift-XRT team: We have analysed 6.3 ks of XRT data for GRB 200109A (Melandri et al. GCN Circ. 26678), from 91 s to 24.1 ks after the BAT trigger. The data comprise 48 s in Windowed Timing (WT) mode (the first 7 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN Circ. 26681). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=1.9 (+/-0.3). At T+216 s the decay steepens to an alpha of 8.0 (+0.0, -3.2) before breaking again at T+262 s to a final decay with index alpha=1.50 (+0.28, -0.38). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.70 (+0.32, -0.30). The best-fitting absorption column is 6.9 (+2.7, -2.2) x 10^21 cm^-2, in excess of the Galactic value of 4.0 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.2 x 10^-11 (7.6 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 6.9 (+2.7, -2.2) x 10^21 cm^-2 Galactic foreground: 4.0 x 10^21 cm^-2 Excess significance: 2.2 sigma Photon index: 1.70 (+0.32, -0.30) If the light curve continues to decay with a power-law decay index of 1.50, the count rate at T+24 hours will be 1.3 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.0 x 10^-15 (1.0 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00948361. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26689 SUBJECT: GRB 200109A: Fermi GBM observation DATE: 20/01/09 19:22:09 GMT FROM: Rachel Hamburg at UAH R. Hamburg (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 01:45:51.89 UT on 9 January 2020, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 200109A (trigger 600227156 / 200109074), which also triggered the Swift/BAT approximately 25 s later (Melandri et al. 2019, GCN 26678). The Fermi GBM Final Real-time Localization (GCN 26677) is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 57 degrees. The GBM light curve shows a complex structure with a duration (T90) of about 41 s (50-300 keV). The time-averaged spectrum from T0-0.8 s to T0+41.2 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.98 +/- 0.08 and the cutoff energy, parameterized as Epeak, is 449 +/- 109 keV. The event fluence (10-1000 keV) in this time interval is (6.9 +/- 0.6)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0-0.7 s in the 10-1000 keV band is 2.3 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/" //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26690 SUBJECT: GRB 200109A: Swift/UVOT Upper Limits DATE: 20/01/09 19:26:41 GMT FROM: Kira Simpson at PSU GRB 200109A: Swift/UVOT Upper Limits K. K. Simpson (PSU) and A. Melandri (INAF-OAB) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 200109A 110 s after the BAT trigger (Melandri et al., GCN Circ. 26678). No optical afterglow consistent with the XRT position (Melandri et al. GCN Circ. 26678) 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 110 259 147 >20.5 u_FC 268 518 246 >19.0 white 110 1023 295 >20.9 u 268 518 246 >19.0 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.29 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26692 SUBJECT: GRB 200109A: Swift-BAT refined analysis DATE: 20/01/09 21:24:27 GMT FROM: Amy Lien at GSFC H. A. Krimm (NSF), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), A. Melandri (INAF-OAB), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 200109A (trigger #948361) (Melandri et al., GCN Circ. 26678). The BAT ground-calculated position is RA, Dec = 307.116, 52.988 deg which is RA(J2000) = 20h 28m 27.7s Dec(J2000) = +52d 59' 17.7" with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The mask-weighted light curve shows a weak structure with several overlapping pulses that start at ~T-30 s to ~T+20 s, followed by a weaker tail emission that lasts till ~T+100 s. T90 (15-350 keV) is 112.0 +- 32.0 sec (estimated error including systematics). The time-averaged spectrum from T-31.45 to T+112.55 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.31 +- 0.14. The fluence in the 15-150 keV band is 2.1 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+8.05 sec in the 15-150 keV band is 0.7 +- 0.2 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/948361/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 26710 SUBJECT: GRB 200109A: Insight-HXMT/HE detection DATE: 20/01/12 03:04:57 GMT FROM: Shuo Xiao at IHEP S. Xiao, Y. F. Du, Y. G. Zheng, C. Cai, Q. Luo, Q. B. Yi, Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, 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 2020-01-09T01:45:51.89 (T0), Insight-HXMT/HE detected GRB 200109A (trigger ID: HEB200109073) in a routine search of the data, which also triggered Fermi/GBM (GCN #26689), and Swift (GCN #26678). The Insight-HXMT/HE light curve mainly consists of multiple pulses with a duration (T90) of 36.405 s measured from T0-0.650 s. The 1-ms peak rate, measured from T0+ 9.281 s, is 595 cnts/sec. The total counts from this burst is 6014 counts. URL_LC: http://www.hxmt.org/images/GRB/HEB200109073_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.