//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11588 SUBJECT: GRB 110120A: MASTER optical observations DATE: 11/01/20 18:04:51 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov Sternberg Astronomical Institute, Moscow State University V.Krushinski, I.Zalozhnich, A. Popov Ural State University, Kourovka K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres, S.Yazev, N.M.Budnev, Irkutsk State University A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina Blagoveschensk Educational State University, Blagoveschensk MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Kislovodsk was pointed to the GRB110120.67 24 sec s after notice time and 63 sec after GRB time at 2011-01-20 16:00:42.913 UT. On our first (10s exposure) set we haven`t found optical transient within FERMI LAT error-box (ra=04 22 36 dec=-18 21 00 r=0.016667). The 5-sigma upper limit has been about 13 mag. The message generated automaticaly. *Add: The observations was done at high zenith distance. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11591 SUBJECT: GRB 110120A: Fermi GBM detection DATE: 11/01/21 16:23:22 GMT FROM: Lin Lin at UAH/NAOC Lin Lin (UAH) reports on behalf of the Fermi GBM Team: "At 15:59:39.23 UT on 20 January 2011, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 110120A (trigger 317231981 / 110120666). The on-ground calculated location, using the GBM trigger data, is RA = 64.54, DEC = -17.06 (J2000 degrees, equivalent to 04 h 18 m 09.6 s, -17 d 03 ' 36.0 "), with an uncertainty of 1.08 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 15 degrees. This burst triggered the Fermi spacecraft slew because of high peak flux. The GBM light curve shows a ~5 s peak followed by a ~40 s tail with a duration (T90) of about 27 s (50-300 keV). The time-averaged spectrum from T0+0.003 s to T0+43.393 s is acceptably fit by a power law function with an exponential high-energy cutoff. The power law index is -0.87 +/- 0.04 and the cutoff energy, parameterized as Epeak, is 1156 +/- 172 keV (C-Stat 666.26 for 487 d.o.f.). The event fluence (10-1000 keV) in this time interval is (2.55 +/- 0.05)E-5 erg/cm^2. The 64 ms peak photon flux measured starting from T0+0.384 s in the 10-1000 keV band is 15.03 +/- 1.35 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: 11595 SUBJECT: IPN triangulation of GRB 110120A DATE: 11/01/23 00:07:18 GMT FROM: Valentin Pal'shin at Ioffe Inst K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team, S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and T. Cline, on behalf of the Konus-Wind team, V. Connaughton, M. Briggs, and C. Meegan, on behalf of the Fermi GBM team, J. Cummings, D. Palmer, S. Barthelmy, N. Gehrels, and H. Krimm, on behalf of the Swift-BAT team, and K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima, on behalf of the Suzaku WAM team, report: Fermi (GBM), Konus-Wind, Swift (BAT), MESSENGER (GRNS), and Suzaku (WAM) observed the long, hard GRB 110120A at about 15:59:39 UT (Fermi/GBM trigger 317231981: Lin, GCN 11591). The burst was outside the coded field of view of the BAT. We have triangulated it to a 3 sigma error box whose coordinates are: ----------------------------------------------- RA(2000), deg Dec(2000), deg ----------------------------------------------- Center: 60.481 (04h 01m 55s) -10.548 (-10d 32' 51") Corners: 56.433 (03h 45m 44s) -5.247 (-05d 14' 48") 62.714 (04h 10m 51s) -13.354 (-13d 21' 16") 64.578 (04h 18m 19s) -14.953 (-14d 57' 11") 58.278 (03h 53m 07s) -7.456 (-07d 27' 21") ----------------------------------------------- The error box area is 2.548 sq. deg. This error box may be improved. Because the Earth, the Wind, and the MESSENGER satellites are nearly aligned at the moment (the angular distance between Wind and MESSENGER is only 5.7 deg), the annuli intersect at grazing incidence and the resulting 3-sigma box is long. A map is posted at http://www.ioffe.ru/LEA/GRBs/GRB110120_T57582/IPN/ showing the GBM best-fit position (blue star and circle), the IPN annuli (solid lines with centers dot-dashed), and the box (solid black closed polyline). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11597 SUBJECT: GRB 110120A: Fermi LAT detection DATE: 11/01/24 07:50:35 GMT FROM: Nicola Omodei at Standford Nicola Omodei (Stanford University), James Chiang (SLAC/KIPAC), Valerie Connaughton (UAH) and Yasuyuki Tanaka (ISAS/JAXA) report on behalf of the Fermi Large Area Telescope (LAT) collaboration. Based on an on-ground analysis, the Large Area Telescope (LAT), on-board the Fermi Gamma-ray Space Telescope, detected high energy emission up to ~2 GeV associated with the GBM-detected burst GRB 110120A (Lin, GCN 11591). The emission in the LAT lasts over 100 seconds, with the highest-energy photon arriving 72 sec after the GBM trigger time. The best localization is RA, DEC (J2000 deg) = 61.6, -12.0 (04h 06m 24s, -12d 00' 00"), with an error of 0.4 deg (68% CL), compatible with the IPN triangulation from Hurley et al. (GCN 11595). Further analysis is ongoing. The Fermi LAT point of contact for this burst is Yasuyuki Tanaka (tanaka@astro.isas.jaxa.jp). 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. [GCN OPS NOTE(24jan11): Per author's request, his affilation and address were updated.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11598 SUBJECT: GRB 110120A: MASTER optical observations DATE: 11/01/24 14:56:32 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov Sternberg Astronomical Institute, Moscow State University V.Krushinski, I.Zalozhnich, A. Popov Ural State University, Kourovka K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres, S.Yazev, N.M.Budnev, Irkutsk State University A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina Blagoveschensk Educational State University, Blagoveschensk MASTER very wide field cameras (MASTER-Net: http://observ.pereplet.ru, 6 cameras 11 Mpix, 85, 1/1.2. 1 sec exposition, comonn FOW is 2400 square degrees) located in Kislovodsk was pointed to the GRB110120A 24 sec s after notice time and 64 sec after GRB time at 2011-01-20 16:00:42.913 UT. The sky near horizont is not clear. On our 60 coaded images we haven`t found optical transient within common area of the FERMI LAT error-box (Nicola Omodei et al., GCN Circ 11597) and (Hurley et al., GCN 11595). The 5-sigma upper limit has been about 10 mag (mean time = 94 sec after trigger). The image is available at http://observ.pereplet.ru/images/GRB110120A/grb.html The MASTER II telescopes FOW was out of the final error box and our previous results (Gorbovskoy et al., GCN Circ 11588) not valid. The observations was done at high zenith distance. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11601 SUBJECT: Konus-Wind observation of GRB 110120A DATE: 11/01/25 14:44:44 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The long hard GRB 110120A, (Fermi/GBM trigger 317231981/ 110120666: Lin Lin, GCN 11591; localized by IPN: Hurley et.al, GCN 11595; detected by Fermi/LAT: Omodei et al., 11597) triggered Konus-Wind at T0=57582.268s UT (15:59:42.268) The burst light curve starts with a hard bright pulse, followed by a softer decaying tail. The total duration of the burst is ~42 s. The emission is seen up to ~5 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB110120_T57582/ As observed by Konus-Wind the burst had a fluence of (3.1 ± 0.3)x10-5 erg/cm2, and a 64-ms peak flux, measured from T0+0.128s, of (1.6 ± 0.5)x10-5 erg/cm2/s (both in the 20 keV - 5 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+41.216 s) is best fit in the 20 keV - 5 MeV range by a power law with exponential cutoff model, for which alpha = -0.6 (-0.2, +0.2), and Ep = 680(-120, +160) keV, chi2 = 64.5/74 dof. The spectrum at the initial part of the burst (measured from T0 to T0+0.256 s) is best fit in the 20 keV - 5 MeV range by a power law with exponential cutoff model, for which alpha = 0.0 (-0.3, +0.4), and Ep = 1193(-244, +349) keV, chi2 = 18.0/23 dof. All the quoted results are preliminary. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11609 SUBJECT: GRB 110120A: Suzaku WAM observation of the prompt emission DATE: 11/01/28 14:57:51 GMT FROM: Yuji Urata at Nat. Central U. P. Tsai, Y. Urata (NCU), T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.), N. Vasquez (Tokyo Tech.), K. Yamaoka (Aoyama Gakuin U.), S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, S. Hong, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.), M. Ohno, M. Serino, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki), K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The log GRB 110120A (Fermi/GBM trigger 317231981 / 110120666 ; Lin et al., GCN 11591; Omodei et al., GCN 11597) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 2011/01/20 15:59:39.22 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-0.7s, ending at T0+8s, with a duration (T90) of about 6.4 seconds. The fluence in 100 - 1000 keV was 2.32 (+/-0.16) x 10^-5 ergs/cm^2. The 1-s peak flux measured from T0+0.38s was 30.40 (+/-0.93) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-0.7s to T0+8s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 1.34 (-0.51, +0.40), and Epeak 418.60 (-84.64, +110.46) keV (chi^2/d.o.f. = 39.92/40). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves for this burst are available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html