//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20462 SUBJECT: GRB 170115A: Swift detection of a burst DATE: 17/01/15 21:15:39 GMT FROM: David Palmer at LANL K. L. Page (U Leicester), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), A. Cholden-Brown (PSU), C. Gronwall (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/NSF/USRA), F. E. Marshall (NASA/GSFC) and D. M. Palmer (LANL) report on behalf of the Swift Team: At 20:50:08 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 170115A (trigger=733103). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 332.154, +13.781 which is RA(J2000) = 22h 08m 37s Dec(J2000) = +13d 46' 51" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve is only immediately available until T+8 seconds due to a telemetry gap, showing a rise to a maximum rate of ~800 counts/s at the end of that period. The XRT began observing the field at 20:51:39.5 UT, 91.5 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 332.1390, 13.7283 which is equivalent to: RA(J2000) = +22h 08m 33.36s Dec(J2000) = +13d 43' 41.9" with an uncertainty of 6.3 arcseconds (radius, 90% containment). This location is 196 arcseconds from the BAT onboard position, outside the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. The initial flux in the 2.5 s image was 5.14e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 99 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 0.07. Burst Advocate for this burst is K. L. Page (klp5 AT leicester.ac.uk). 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: 20463 SUBJECT: GRB 170115B: Fermi GBM detection DATE: 17/01/16 00:02:09 GMT FROM: Rachel Hamburg at UAH R. Hamburg (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 17:49:14.03 UT on 15 January 2017, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 170115B (trigger 506195359 / 170115743). The on-ground calculated location, using the GBM trigger data, is RA = 189.03, DEC = -51.55, with an uncertainty of 1.43 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 trigger resulted in an Autonomous Repoint Request (ARR) by the GBM Flight Software owing to the high peak flux of the GRB. This ARR was accepted and the spacecraft slewed to the GBM in-flight location. The initial angle from the Fermi LAT boresight to the GBM ground location is 32 degrees. The GBM light curve consists of multiple peaks with a duration (T90) of about 44 s (50-300 keV). The time-averaged spectrum from T0-0.6 s to T0+42.4 s is well fit by a power law function with an exponential high-energy cutoff. The power law index is -0.89 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 1656 +/- 81 keV. A Band function fits the spectrum equally well with Epeak= 1563 +/- 106 keV, alpha = -0.88 +/- 0.01 and beta = -2.47 +/- 0.36. The event fluence (10-1000 keV) in this time interval is (5.98 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.77 s in the 10-1000 keV band is 15.1 +/- 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: 20464 SUBJECT: GRB 170115B: Fermi-LAT detection DATE: 17/01/16 00:33:21 GMT FROM: Julie McEnery at NASA/GSFC J.E. McEnery, J. Racusin (NASA/GSFC) and E. Bissaldi (Politecnico & INFN Bari) report on behalf of the Fermi-LAT team: At 17:49:14.03 on January 15, 2017 Fermi-LAT detected high-energy emission from GRB 170115B, which was also detected by Fermi-GBM (GCNC 20463). The best LAT on-ground location is found to be RA, Dec = 189.12, -46.85 (J2000) with an error radius of 0.26 deg (90 % containment, statistical error only). This was ~40 deg from the LAT boresight at the time of the trigger and triggered an autonomous repoint of the spacecraft. The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the trigger with high significance. A Swift ToO has been requested for this burst. The Fermi-LAT point of contact for this burst is Elisabetta Bissaldi (elisabetta.bissaldi@ba.infn.it). 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20465 SUBJECT: GRB 170115A: Enhanced Swift-XRT position DATE: 17/01/16 03:35:10 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 615 s of XRT Photon Counting mode data and 1 UVOT images for GRB 170115A, 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 = 332.13844, +13.72836 which is equivalent to: RA (J2000): 22h 08m 33.23s Dec (J2000): +13d 43' 42.1" with an uncertainty of 3.7 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: 20466 SUBJECT: GRB 170115B: AstroSat CZTI (Veto) detection DATE: 17/01/16 07:35:52 GMT FROM: Vidushi Sharma at IUCAA V. Sharma, V. Bhalerao and D. Bhattacharya (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 GRB170115B (Fermi detection: R. Hamburg et al., GCN Circ. 20463) in the 40-200 keV energy range. The light curve shows multiple peaks structure with main peak at 17:49:14.03 UT, coincident with Fermi trigger. The measured peak count rate is 618.7 counts/sec above the background in combined data of four quadrants, with a total of 4196.9 counts. The local mean background count rate was 372.3 counts/sec. Using cumulative rates, we measure a T90 of 15.3 secs. It was clearly detected in the CsI anticoincidence detector (Veto) also as bright detection in the 100-500 keV energy range. 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: 20467 SUBJECT: GRB 170115B: Tiled Swift observations DATE: 17/01/16 09:04:15 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a series of observations, tiled on the sky, of the Fermi/LAT GRB 170115B. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00062 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20470 SUBJECT: GRB 170115A: Swift-XRT refined Analysis DATE: 17/01/16 15:12:26 GMT FROM: Kim Page at U.of Leicester K.L. Page and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: We have analysed 3.9 ks of XRT data for GRB 170115A, from 82 s to 40.4 ks after the BAT trigger. The data comprise 224 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 light curve can be modelled with a power-law decay with a decay index of alpha=1.54 (+0.06, -0.05). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.22 (+0.17, -0.16). The best-fitting absorption column is 1.3 (+0.5, -0.4) x 10^21 cm^-2, in excess of the Galactic value of 6.1 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 2.9 x 10^-11 (4.0 x 10^-11) erg cm^-2 count^-1. A summary of the WT-mode spectrum is thus: Total column: 1.3 (+0.5, -0.4) x 10^21 cm^-2 Galactic foreground: 6.1 x 10^20 cm^-2 Excess significance: 2.6 sigma Photon index: 2.22 (+0.17, -0.16) If the light curve continues to decay with a power-law decay index of 1.54, the count rate at T+24 hours will be 4.1 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.2 x 10^-14 (1.7 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/00733103. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20471 SUBJECT: GRB 170115A: Swift-BAT refined analysis DATE: 17/01/16 19:22:36 GMT FROM: Hans Krimm at NSF/NASA-GSFC D. M. Palmer (LANL), 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), K. L. Page (U Leicester), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+450 sec from the recent telemetry downlink, we report further analysis of BAT GRB 170115A (trigger #733103) (Page, et al., GCN Circ. 20462). The BAT ground-calculated position is RA, Dec = 332.145, 13.750 deg which is RA(J2000) = 22h 08m 34.9s Dec(J2000) = +13d 45' 01.6" with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The mask-weighted light curve shows a single FRED-shaped peak, starting at T+0, peaking at around T+10 sec and decaying to background by around T+50 sec. The spacecraft entered the SAA at around T+400 seconds, so there is no data after this time. T90 (15-350 keV) is 48.0 +- 22.6 sec (estimated error including systematics). The time-averaged spectrum from T-7.6 to T+40.4 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.45 +- 0.25. The fluence in the 15-150 keV band is 4.7 +- 0.8 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+15.94 sec in the 15-150 keV band is 0.2 +- 0.1 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/733103/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20474 SUBJECT: GRB 170115B: AGILE detection DATE: 17/01/16 22:48:39 GMT FROM: Francesco Verrecchia at ASDC F. Verrecchia (ASDC and INAF/OAR), A. Ursi (INAF/IAPS), F. Lucarelli (ASDC and INAF/OAR), F. Longo (Univ. Trieste and INFN Trieste), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata) report: AGILE detected the long GRB 170115B, reported by Fermi-GBM (Hamburg et al. GCN #20463) and Fermi-LAT (McEnery et al. GCN #20464), at favourable off-axis angles between 0 and 30 deg. The AGILE-GRID detected the burst at about 4-sigma above 30 MeV with an extended gamma-ray emission lasting about 60 sec. The AGILE MiniCaLorimeter (MCAL), sensitive in the energy range from 400 keV to 100 MeV, detected this burst that triggered the on-board sub-millisecond timescale logic. The MCAL light curve shows multiple peaks, from T0 until the end of the acquisition at T0 + 10.5 s. Three main peaks are evident during the first 2.5 sec following T0. During this time interval, the total number of counts is ~5500 for a background rate of 580 counts/s. This measurement was obtained with AGILE observing a large portion of the sky in spinning mode. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20475 SUBJECT: IPN Triangulation of GRB 170115B DATE: 17/01/17 08:43:56 GMT FROM: Anna Kozlova at Ioffe Institute K. Hurley, on behalf of the IPN, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team, A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, on behalf of the Fermi GBM team, A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on behalf of the GRS-Odyssey GRB team, report: The long-duration GRB 170115B (Fermi GBM detection: Hamburg et al., GCN 20463) has been detected by Fermi(GBM), Konus-Wind, INTEGRAL (SPI-ACS), and Mars-Odyssey(HEND), so far, at about 64154 s UT (17:49:14). We have triangulated it to a Konus-HEND annulus centered at RA(2000)=171.562 deg (11h 26m 15s) Dec(2000)=+4.317 deg (+4d 19' 01"), whose radius is 53.310 +/- 0.093 deg (3 sigma). This annulus intersects the Fermi-LAT 90% CL error circle (McEnery et al., GCN Circ. 20464) to form an error box whose area is about 2 times smaller than that of the LAT error circle, and whose corners are: ----------------------------------------------- RA(2000), deg Dec(2000), deg ----------------------------------------------- Corners: 189.426 -46.696 189.079 -46.592 188.888 -46.644 188.743 -46.884 ----------------------------------------------- The box area is about 260 sq. arcmin. This box may be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB170115_T64155/IPN/ The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20476 SUBJECT: Konus-Wind observation of GRB 170115B DATE: 17/01/17 09:01:14 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline, on behalf of the Konus-Wind team, report: The long GRB 170115B (Fermi-GBM detection: Hamburg & Meegan, GCN 20463; Fermi-LAT detection: McEnery et al., GCN 20464; AstroSat CZTI observation: Sharma et al., GCN 20466; POLAR observation: Xiao et al., GCN 20469; AGILE detection: Verrecchia et al., GCN 20474; IPN triangulation: Hurley et al., GCN 20475) triggered Konus-Wind at T0=64155.241 s UT (17:49:15.241). The light curve shows a bright, hard, multi-peaked pulse followed by a weaker emission; the total duration of the burst is ~50 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of (1.26 ± 0.12)x10^-4 erg/cm2 and a 64-ms peak energy flux, measured from T0+0.512, of (3.1 ± 0.2)x10^-5 erg/cm2 (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+38.144 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.86 (-0.06,+0.06), the high energy photon index beta = -2.49 (-0.90,+0.31), the peak energy Ep = 1114 (-156,+180) keV, chi2 = 94/97 dof. The spectrum near the peak count rate (measured from T0 to T0+6.912 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.61 (-0.08,+0.08), the high energy photon index beta = -2.59 (-1.30,+0.32), the peak energy Ep = 1278 (-175,+223) keV, chi2 = 94/97 dof. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB170115_T64155/ All the quoted errors are estimated at the 90% confidence level. All the presented results are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20477 SUBJECT: GRB 170115B: Swift-XRT observations DATE: 17/01/17 09:15:10 GMT FROM: Sarah Gibson at U.of Leicester P. D'Avanzo (INAF-OAB), S. J. LaPorte (PSU), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), K.L. Page (U. Leicester), B. Mingo (U. Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 170115B in a series of observations tiled on the sky. The total exposure time is 4.7 ks, distributed over 5 tiles; the maximum exposure at a single sky location was 3.3 ks. The data were collected between T0+54.5 ks and T0+66.3 ks, and are entirely in Photon Counting (PC) mode. One uncatalogued X-ray source has been detected, it is below the RASS limit and shows no definitive signs of fading. Therefore, at the present time we cannot confirm this as the afterglow. Details of this source are given below: Source 1: RA (J2000.0): 189.0597 = 12:36:14.34 Dec (J2000.0): -46.8311 = -46:49:52.1 Error: 6.5 arcsec (radius, 90% conf.) Count-rate: 0.0117 +/- 0.0029 ct s^-1 Distance: 163 arcsec from Fermi/LAT position. The results of the XRT-team automatic analysis of the tiled XRT observations, including a position-specific upper limit calculator, are available at http://www.swift.ac.uk/xrt_products/TILED_GRB00062. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20478 SUBJECT: GRB 170115A: Swift/UVOT Upper Limits DATE: 17/01/17 16:39:49 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and K. L. Page (U. Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 170115A 100 s after the BAT trigger (Page et al., GCN Circ. 20462). No optical afterglow consistent with the enhanced XRT position (Osborne et al. GCN Circ. 20465) 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) 100 250 147 >20.40 white 4804 6335 291 >20.66 v 5214 35195 816 >19.67 b 4599 40415 838 >20.68 u (fc) 260 328 67 >18.98 u 5829 6029 196 >19.65 uvw1 5624 5824 196 >19.32 uvm2 5419 5619 196 >19.37 uvw2 5009 11435 992 >20.69 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.07 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20479 SUBJECT: GRB 170115A : AbAO optical upper limit DATE: 17/01/17 17:16:40 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Pozanenko (IKI), R. Inasaridze (AbAO), A. Volnova (IKI), V. Ayvazian (AbAO), O.Kvaratskhelia (AbAO), G. Inasaridze (AbAO), I. Molotov (KIAM), report on behalf of larger GRB follow-up collaboration: We observed the field of the GRB 170115A (Page et al., GCN Circ. 20462) with AS-32 (0.7m) telescope of Abastumani Observatory on Jan., 16 (UT) 14:57:24. We obtained several unfiltered images of the field. No source is found within enhanced XRT position (Osborne et al. GCN Circ. 20465). Preliminary photometry of the field is following Date UT start t-T0 Filter Exp. OT Err UpLim (3 sigma) (mid, days) (s) 2017-01-16 14:57:24 0.78450 CR 49*60 n/d n/d 22.5 Photometry is based on nearby SDSS_DR9 stars SDSS_DR9_id R(Lupton) J220832.66+134330.8 18.50 J220831.22+134259.5 18.59 J220831.94+134225.7 18.57 J220847.68+134539.9 16.60 J220833.30+133952.6 16.32 J220835.19+134539.0 17.66 J220837.56+134537.8 15.86 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20483 SUBJECT: GRB 170115B: CALET Gamma-Ray Burst Monitor detection DATE: 17/01/19 04:50:32 GMT FROM: Takanori Sakamoto at AGU Y. Shimizu (Kanagawa U), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, Y. Yamada (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena) and the CALET collaboration: The long-duration GRB 170115B (Hamburg et al., GCN Circ. 20463; McEnery et al., GCN Circ. 20464; Sharma et al., GCN Circ. 20466; Xiao et al., GCN Circ. 20469; Verrecchia et al., GCN Circ. 20474; Frederiks et al., GCN Circ. 20476) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 17:49:12.63 on 15 January 2017. The burst signal was only seen by the SGM instrument. The light curve of the SGM shows several overlapping pulses starting at T0, peaking at T+3 sec and ending at T+15 sec. The T90 duration measured by the SGM data is 12.0 +- 0.9 sec (40-1000 keV). The light curve is available at http://cgbm.calet.jp/cgbm_trigger/flight/1168537525/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20525 SUBJECT: GRB 170115B: AGILE/SuperAGILE localisation DATE: 17/01/25 15:51:18 GMT FROM: Ettore Del Monte at IASF/INAF Y. Evangelista, L. Pacciani, E. Del Monte and I. Donnarumma (INAF/IAPS), A. Trois (INAF/OAC) on behalf of the AGILE Team, report: SuperAGILE localised the long-duration GRB 170115B (Hamburg et al., GCN 20463; McEnery et al., GCN 20464; Sharma et al., GCN 20466; Xiao et al., GCN 20469; Verrecchia et al., GCN 20474; Frederiks et al., GCN 20476, Shimizu et al., GCN 20483) on 15 January 2017, at 17:49:14 UT. The event had a duration of about 50.0 s in the 18-60 keV energy range, with a multi-peaked structure. The burst position was reconstructed as: RA(J2000): 189.011 deg (12h 36m 02.64s) DEC(J2000): -46.796 deg (-46d 47' 45.58") with an uncertainty of 5' (radius). The uncertainty accounts for both the statistical and systematic errors. The SuperAGILE error box is completely contained in the FERMI-LAT error box (McEnery et al., GCN 20464) and partially intersects the IPN annulus (Hurley et al., GCN 20475). The Swift-XRT afterglow candidate (D'Avanzo et al., GNC 20477) is also contained in the SuperAGILE error box. Due to telemetry downlink restrictions, the SuperAGILE experiment has been kept on but with no telemetry download since late 2012. The full telemetry link for the AGILE mission has now been restored and the data of SuperAGILE are again routinely downloaded. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20529 SUBJECT: GRB 170115A: 15 GHz upper limits from AMI DATE: 17/01/26 11:30:40 GMT FROM: Kunal Mooley at Oxford U K. P. Mooley, 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 robotically triggered on the Swift alert for GRB 170115A (Page et al., GCN 20462) as part of the 4pisky program, and subsequent follow up observations were obtained up to 10 days post-burst. Our observations at 15 GHz on 2016 Jan 16.42, Jan 17.59, Jan 18.67 and Jan 23.51 (UT) do not reveal any radio source at the XRT location (Osborne et al., GCN 20465), with 3sigma upper limits of 300 uJy, 78 uJy, 72 uJy and 81 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/.