//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20349 SUBJECT: GRB 170101A: Swift detection of a burst DATE: 17/01/01 02:47:02 GMT FROM: Kim Page at U.of Leicester A. Y. Lien (GSFC/UMBC), D. Malesani (DARK/NBI and DTU Space), B. Mingo (U Leicester), K. L. Page (U Leicester) and T. N. Ukwatta (LANL) report on behalf of the Swift Team: At 02:26:01 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 170101A (trigger=729293). The BAT on-board calculated location is RA, Dec 267.103, +11.654 which is RA(J2000) = 17h 48m 25s Dec(J2000) = +11d 39' 15" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 5 sec. The peak count rate was ~28000 counts/sec (15-350 keV), at ~0 sec after the trigger. Due to a Sun observing constraint, Swift cannot slew to the BAT position until 23:58 UT on 2017 January 19. There will thus be no XRT or UVOT data for this trigger before this time. The Swift team wishes the astronomical community a happy 2017. Burst Advocate for this burst is A. Y. Lien (amy.y.lien AT nasa.gov). 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/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20350 SUBJECT: GRB 170101B: Fermi GBM detection DATE: 17/01/01 10:24:47 GMT FROM: Andreas von Kienlin at MPE P Veres (UAH) and C Meegan (UAH) report on behalf of the Fermi GBM Team: "At 02:47:17.87 UT on 01 January 2017, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 170101B (trigger 504931642 / 170101116). The on-ground calculated location, using the GBM trigger data, is RA = 70.6, DEC = -1.6 (J2000 degrees, equivalent to 04 h 43 m, -1 d 35 '), with an uncertainty of 1.2 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a core-plus-tail model, with 90% of GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ). The angle from the Fermi LAT boresight at the GBM trigger time is 65 degrees. The GBM light curve shows/consists of two overlapping pulses with a duration (T90) of about 12.8 s (50-300 keV). The time-averaged spectrum from T0 to T0 + 15.7 s is best fit by a Band function with Epeak = 213 +/- 13 keV, alpha = -0.57 +/- 0.05, and beta = -2.29 +/- 0.12. The event fluence (10-1000 keV) in this time interval is (1.26 +/- 0.03)E-5 erg/cm^2. The 1-sec peak photon flux measured starting from T0 + 6.1 s in the 10-1000 keV band is 7.0 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20351 SUBJECT: GRB 170101B: Astrosat CZTI detection DATE: 17/01/01 17:05:46 GMT FROM: Vedant Kumar at Astrosat/CZTI/IUCAA V. Kumar, D. Bhattacharya and V. Bhalerao (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data showed clear detection of GRB170101B (Fermi-GBM detection: Andreas von Kienlin et al., GCN 20350) in the 40-200 keV energy range. The light curve shows dual peak structure with stronger peak at 02:47:25.870 UT, 8 secs after the Fermi- GBM trigger(consistent with GCN 20350). The measured peak count rate is 209.80 counts/sec above the background in combined data of four quadrants, with a total of 1751 counts. The local mean background count rate was 377 counts/sec. Using cumulative rates, we measure a T90 of 14.3 sec. 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: 20353 SUBJECT: GRB 170101A: Swift-BAT refined analysis DATE: 17/01/02 02:07:41 GMT FROM: Amy Lien at GSFC S. D. Barthelmy (GSFC), J. R. Cummings (CPI), N. Gehrels (GSFC), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), J. P. Norris (BSU), 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-119 to T+303 sec from the recent telemetry downlink, we report further analysis of BAT GRB 170101A (trigger #729293) (Lien et al., GCN Circ. 20349). The BAT ground-calculated position is RA, Dec = 267.089, 11.642 deg which is RA(J2000) = 17h 48m 21.3s Dec(J2000) = +11d 38' 29.9" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 14%. T90 (15-350 keV) is 2.43 +- 0.49 sec (estimated error including systematics). The mask-weighted light curve shows a single FRED-like pulse that starts at ~T-0.2 s, peaks at ~T0, and ends at ~T+3 s. In addition, there seems to be some weak emission prior to the FRED-like pulse that starts at ~T-1.6 s, and a weak tail afterwards that lasts till ~T+8 s. T90 (15-350 keV) is 3.2 +- 0.9 sec (estimated error including systematics). The time-averaged spectrum from T-1.6 to T+8.5 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.87 +- 0.06. The fluence in the 15-150 keV band is 6.0 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-0.22 sec in the 15-150 keV band is 54.4 +- 2.0 ph/cm2/sec. All the quoted errors are at the 90% confidence level. Using a 16-ms binned light curve, the lag analysis finds a lag of 39 +/- 8 ms for the 100-350 keV to 25-50 keV, and 37 +/- 7 ms for the 50-100 keV to 15-25 keV band, which is consistent with those of a long GRB. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/729293/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20355 SUBJECT: GRB 170101A: POLAR observation DATE: 17/01/02 13:57:14 GMT FROM: Hancheng Li at IHEP/POLAR Hancheng Li (IHEP), Yuanhao Wang (IHEP), Zhengheng Li (IHEP) report on the behalf of the POLAR collaboration: At 2017-01-01T02:26:00.66 UT (T0), during a routine on-ground search of data, POLAR detected the GRB 170101A, which was also detected by the Swift/BAT (trigger #729293). The POLAR light curve consists of a single peak, with a duration (T90) of 2.82 s measured from T0+0.00 s. The 0.2-s peak rate measured from T0+0.20 s is 8836 cnts/s, the total counts is about 5379 cnts. The above measurements are in the energy range of approximately 80-500 keV. LC_URL: http://polar.ihep.ac.cn/grb/2017/01/GRB170101A/lc/GRB170101A.png Using the best location from the Swfit/BAT, which is (J2000): RA: 267.103 [deg] Dec: +11.654 [deg] Err: 3.00 [arcmin] the incident angle in POLAR coordinate at T0 is: theta: 6.04 [deg] phi: 72.86 [deg] The Minimum Detectable Polarization(MDP) for this burst is estimated to be ~6.0% [1-sigma, statistical only]. Follow-up observations are strongly encouraged. All analysis results presented above are preliminary. POLAR is a dedicated Gamma-Ray Burst polarimeter (50-500 keV) on-board the Chinese space laboratory Tiangong-2 launched on Sep 15, 2016. More information about POLAR can be found at: http://polar.ihep.ac.cn/en/ , http://isdc.unige.ch/polar/ and http://polar.psi.ch/html/ . //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20359 SUBJECT: GRB 170101A: Lomonosov BDRG gamma ray discovery DATE: 17/01/03 12:07:50 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.V.Bogomolov, N.L.Dzhioeva, S.I.Svertilov, A.M.Amelushkin, V.O.Barinova, M.I.Panasyuk, A.V.Bogomolov, A.F.Iyudin, V.V.Kalegaev, D.Nguen, V.L. Petrov, I.V.Yashin, P.S.Kazarian Physics Department, Skobel`tsyn Institute of Nuclear Physics, Lomonosov Moscow State University V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov Lomonosov Moscow State University, Sternberg Astronomical Institute I. Park, J. Lee, S. Jeong Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, Korea A. J. Castro-Tirado Instituto de Astrofisica de Andalucia (IAA-CSIC) and Universidad de Malaga, Spain At 02:26:12 UT on 01 Jan 2017, the Lomonosov BDRG Gamma-ray Burst Monitor (http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg), triggered GRB 170101A (A. Y. Lien (GSFC/UMBC), GCN 20349), total duration ~3s, the energy range 30-800 keV. LC is available at: https://downloader.sinp.msu.ru/static/grb_catalog/lc/grb_20170101_022612.png More information is available at: https://downloader.sinp.msu.ru/grb_catalog/ This Notice was ground-generated. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20360 SUBJECT: GRB 170101B: Lomonosov BDRG gamma ray discovery DATE: 17/01/03 12:10:03 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs N.L.Dzhioeva,V.V.Bogomolov, S.I.Svertilov, A.M.Amelushkin, V.O.Barinova, M.I.Panasyuk, A.V.Bogomolov, A.F.Iyudin, V.V.Kalegaev, D.Nguen, V.L. Petrov, I.V.Yashin, P.S.Kazarian Physics Department, Skobel`tsyn Institute of Nuclear Physics, Lomonosov Moscow State University V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov Lomonosov Moscow State University, Sternberg Astronomical Institute I. Park, J. Lee, S. Jeong Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, Korea A. J. Castro-Tirado Instituto de Astrofisica de Andalucia (IAA-CSIC) and Universidad de Malaga, Spain At 02:47:22 UT on 01 Jan 2017, the Lomonosov BDRG Gamma-ray Burst Monitor (http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg), triggered GRB 170101B (P Veres (UAH), GCN 20350), total duration ~13s, the energy range 30-300 keV. LC is available at: https://downloader.sinp.msu.ru/static/grb_catalog/lc/grb_20170101_024722.png More information is available at: https://downloader.sinp.msu.ru/grb_catalog/ This Notice was ground-generated. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20361 SUBJECT: GRB 170101B: POLAR observation DATE: 17/01/03 15:05:07 GMT FROM: Yuanhao Wang at IHEP/CAS Hancheng Li (IHEP), Yuanhao Wang (IHEP), Zhengheng Li (IHEP) report on the behalf of the POLAR collaboration: At 2017-01-01T02:47:18.27 UT (T0), during a routine on-ground search of data, POLAR detected the GRB 170101B, which was also detected by the Fermi/GBM (trigger 504953918/170101374). The POLAR light curve consists of multiple peaks, with a duration (T90) of 11.2 s measured from T0+0.3 s. The 0.2-s peak rate measured from T0+8.1 s is 968 cnts/s, the total counts is about 5217 cnts. The above measurements are in the energy range of approximately 80-500 keV. LC_URL: http://polar.ihep.ac.cn/grb/2017/01/GRB170101B/lc/GRB170101B.JPG Using the best location from the Fermi/GBM, which is (J2000): RA: 70.640[deg] Dec: -1.580[deg] Err: 1.2[deg] the incident angle in POLAR coordinate at T0 is: theta: 63.43[deg] phi: -110.01[deg] The Minimum Detectable Polarization(MDP) for this burst is estimated to be ~23.5% [1-sigma, statistical only]. All analysis results presented above are preliminary. POLAR is a dedicated Gamma-Ray Burst polarimeter (50-500 keV) on-board the Chinese space laboratory Tiangong-2 launched on Sep 15, 2016. More information about POLAR can be found at:http://polar.ihep.ac.cn/en/, http://isdc.unige.ch/polar/and http://polar.psi.ch/html/. [GCN OPS NOTE(03jan17): Per operator, the SUBJECT-line was corrected from "170101A" to "170101B".] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20362 SUBJECT: Konus-Wind observation of GRB 170101A DATE: 17/01/03 19:54:15 GMT FROM: Anastasia Tsvetkova at Ioffe Institute A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline on behalf of the Konus-Wind team, report: The long-duration, intense GRB 170101A (Swift-BAT trigger #729293: Lien et al., GCN 20349; Barthelmy et al., GCN 20353; POLAR observation: Li et al., GCN 20355; Lomonosov BDRG observation: Bogomolov et al., GCN 20359) triggered Konus-Wind at T0=8757.802 s UT (02:25:57.802). The burst light curve shows a single FRED-like pulse with a total duration of ~4 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of 1.35(-0.18,+0.20)x10^-5 erg/cm2, and a 64-ms peak energy flux, measured from T0+0.264 s, of 1.86(-0.23,+0.24)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+9.472 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -1.44(-0.13,+0.17), the high energy photon index beta = -2.49(-0.65,+0.23), the peak energy Ep = 123(-21,+23) keV, chi2 = 101/97 dof. The spectrum near the peak count rate (measured from T0 to T0+1.280 s) is best fit in the 20 keV - 10 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -1.07(-0.15,+0.17), the high energy photon index beta = -2.48(-0.22,+0.14), the peak energy Ep = 124(-15,+18) keV, chi2 = 57/56 dof. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB170101_T08757/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20449 SUBJECT: GRB 170101A: 15 GHz upper limits from AMI DATE: 17/01/13 12:19:27 GMT FROM: Kunal Mooley at Oxford U K. P. Mooley (Hintze Fellow, Oxford), T. D. Staley, R. P. Fender (Oxford), G. E. Anderson (Curtin), T. Cantwell (Manchester), D. Titterington, S. H. Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K. Grainge, A. Scaife (Manchester) The AMI Large Array triggered on the Swift alert for GRB 170101A (Lien et al., GCN 20349) as part of the 4pisky program, and follow up observations were obtained up to 10 days post-burst. Our observations at 15 GHz on 2016 Jan 03.33, Jan 04.45, Jan 05.46 and Jan 07.45 (UT) do not reveal any radio source in the BAT error circle (Barthelmy et al., GCN 20353), with 3sigma upper limits of 105 uJy, 132 uJy, 78 uJy and 120 uJy respectively. We thank the AMI staff for scheduling these observations. The AMI-GRB database is a log of all GRB follow up observations with the AMI, and is available at http://4pisky.org/ami-grb/.