GRB170626A

This page lists all entries on GRB170626A in GRBweb

Summary Fermi GBM IPN Swift GCN 21264 GCN 21266 GCN 21267 GCN 21268 GCN 21269 GCN 21270 GCN 21271 GCN 21272 GCN 21273 GCN 21274 GCN 21276 GCN 21277 GCN 21278 GCN 21460

Summary table
Variable Value Source
GRB_name_Fermi GRB170626401
T0 9:37:20.048 UTC GCN_circulars,Konus-Wind Det
ra 165.3936° Swift
decl 56.4768° Swift
pos_error 4.53e-04° Swift
T90 12.288 s Fermi_GBM
T90_error 0.362 s Fermi_GBM
T90_start 9:37:22.466 UTC Fermi_GBM
fluence 1.51e-05 erg/cm² Fermi_GBM
fluence_error 6.00e-08 erg/cm² Fermi_GBM
T100 15.892 s
GBM_located False
mjd 57930.40092648148 GCN_circulars,Konus-Wind Det
Fermi GBM table
GRB_name_Fermi GRB170626401
trigger_name bn170626401
ra 165.4142°
decl 56.4689°
pos_error 2.65e+00°
datum 2017-06-26
t_trigger 9:37:21.954 UTC
T90 12.288 s
T90_error 0.362 s
T90_start 9:37:22.466 UTC
fluence 1.51e-05 erg/cm²
fluence_error 6.00e-08 erg/cm²
flux_1024 3.72e+01 erg/cm²/s
flux_1024_error 4.60e-01 erg/cm²/s
flux_1024_time 1.09e+00 erg/cm²/s
flux_64 4.40e+01 erg/cm²/s
flux_64_error 1.91e+00 erg/cm²/s
IPN table
GRB_name GRB170626A
ra 165.4125°
decl 56.4667°
pos_error 5.00e-02°
Swift table
GRB_name GRB170626A
t_trigger 9:37:23 UTC
ra 165.3936°
decl 56.4768°
pos_error 4.53e-04°
T90 12.94 s
fluence 8.20e-06 erg/cm²
GCN 21264 table
GRB_name GRB170626A
GCN_number 21264
Detection_method Swift Det
t_trigger 9:37:23 UTC
ra 165.4140°
decl 56.4690°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21264 SUBJECT: GRB 170626A: Swift detection of a burst DATE: 17/06/26 09:53:22 GMT FROM: David Palmer at LANL F. E. Marshall (NASA/GSFC), A. P. Beardmore (U Leicester), A. A. Breeveld (UCL-MSSL), D. N. Burrows (PSU), S. W. K Emery (UCL-MSSL), P. A. Evans (U Leicester), N. P. M. Kuin (UCL-MSSL), K. L. Page (U Leicester), D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team: At 09:37:23 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 170626A (trigger=758766). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 165.414, +56.469 which is RA(J2000) = 11h 01m 39s Dec(J2000) = +56d 28' 09" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 15 sec. The peak count rate was ~35000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 09:38:21.6 UT, 58.5 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 165.3927, 56.4759 which is equivalent to: RA(J2000) = +11h 01m 34.25s Dec(J2000) = +56d 28' 33.2" with an uncertainty of 5.3 arcseconds (radius, 90% containment). This location is 49 arcseconds from the BAT onboard position, within 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 1.52e-09 erg cm^-2 s^-1 (0.2-10 keV). The XRT position is 5.4 arcmin away from a magnitude 2 star (Merak), therefore there are no UVOT data for this burst. Burst Advocate for this burst is F. E. Marshall (marshall AT milkyway.gsfc.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.)
GCN 21266 table
GRB_name GRB170626A
GCN_number 21266
Detection_method Fermi GBM Det
t_trigger 9:37:21.950 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 21266 SUBJECT: GRB 170626A: Fermi GBM observation DATE: 17/06/26 19:12:51 GMT FROM: Rachel Hamburg at UAH R. Hamburg (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 09:37:21.95 UT on 26 June 2017, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 170626A (trigger 520162646 / 170626401) which was also detected by the Swift/BAT (Marshall et al. 2017, GCN 21264). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 75 degrees. The GBM light curve shows one main peak with a duration (T90) of about 12 s (50-300 keV). The time-averaged spectrum from T0+0.00 to T0+13.6 s is best fit by a Band function with Epeak = 94 +/- 2 keV, alpha = -0.74 +/- 0.03, and beta = -2.7 +/- 0.1. The event fluence (10-1000 keV) in this time interval is (1.57 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+1.09 s in the 10-1000 keV band is 37.2 +/- 0.5 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 21267 table
GRB_name GRB170626A
GCN_number 21267
Detection_method Swift-XRT Other
ra 165.3936°
decl 56.4768°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21267 SUBJECT: GRB 170626A: Swift-XRT refined Analysis DATE: 17/06/26 20:01:54 GMT FROM: Phil Evans at U of Leicester A. Cholden-Brown (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), S. J. LaPorte (PSU), J.A. Kennea (PSU) and F.E. Marshall report on behalf of the Swift-XRT team: We have analysed 9.4 ks of XRT data for GRB 170626A (Marshall et al. GCN Circ. 21264), from 51 s to 28.8 ks after the BAT trigger. The data comprise 1.2 ks in Windowed Timing (WT) mode (the first 6 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The refined XRT position is RA, Dec = 165.3936, +56.4768 which is equivalent to: RA (J2000): 11 01 34.46 Dec(J2000): +56 28 36.5 with an uncertainty of 3.5 arcsec (radius, 90% confidence). The late-time light curve (from T0+5.4 ks) can be modelled with a power-law decay with a decay index of alpha=1.22 (+/-0.09). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.019 (+/-0.025). The best-fitting absorption column is 3.2 (+/-0.5) x 10^20 cm^-2, in excess of the Galactic value of 6.7 x 10^19 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.73 (+/-0.08) and a best-fitting absorption column of 3.2 (+1.8, -1.7) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (3.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.2 (+1.8, -1.7) x 10^20 cm^-2 Galactic foreground: 6.7 x 10^19 cm^-2 Excess significance: 2.4 sigma Photon index: 1.73 (+/-0.08) If the light curve continues to decay with a power-law decay index of 1.22, the count rate at T+24 hours will be 0.039 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.4 x 10^-12 (1.5 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00758766. This circular is an official product of the Swift-XRT team.
GCN 21268 table
GRB_name GRB170626A
GCN_number 21268
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21268 SUBJECT: GRB 170626A: SAO RAS possible OT detection DATE: 17/06/26 21:46:26 GMT FROM: Moskvitin Alexander at SAO RAS A. S. Moskvitin report on behalf of larger GRB follow-up team: We observed the field of the GRB 170626A (Marshall et al., GCNC 21264) with the 1-m telescope of SAO RAS, Zeiss-1000 on June, 26. The observations started at 19:57:42 UT. We obtained several images in Rc band and detected possible OT within the refined XRT error box (Cholden-Brown et al., GCNC 21267). The coordinates of object are: R. A. (2000) = 11:01:34.0 Decl. (2000) = +56:28:35.3 the error is about 0.5". Preliminary photometry of the object: R = 19.7 +/- 0.2, T - T0 = 10.575 hours (calibration was done by the nearby SDSS stars, and Lupton 2005 transformation equations). Due to absence of the observed object at SDSS we can suggest that it can be GRB OT.
GCN 21269 table
GRB_name GRB170626A
GCN_number 21269
Detection_method Other
ra 165.3920°
decl 56.4765°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21269 SUBJECT: GRB 170626A: Afterglow detection from 1.5m OSN DATE: 17/06/26 22:27:03 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), and F. Aceituno, D.A. Kann, L. Izzo, C. Thoene (IAA-CSIC) report on behalf of a larger collaboration: We observed the field of GRB 170626A (Marshal et al. GCN 21264) with the 1.5m OSN telescope in Sierra Nevada Observatory (Granada, Spain). Observation consisted of a series of 240 s R-band exposures, starting at 20:56:49 UT (11.32 hr after the burst). The afterglow is well detected at a position consistent with the one reported by Moskvitin et al. (GCN 21268), (J2000, +/-0.5”): R.A.: 11:01:34.09 Dec.: +56:28:35.4 In the combination of the first 12x240s exposures we measure a magnitude of R(AB) = 20.6+/- 0.2 as compared to SDSS stars.
GCN 21270 table
GRB_name GRB170626A
GCN_number 21270
Detection_method Optical
ra 165.3918°
decl 56.4764°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21270 SUBJECT: GRB 170626A: TNG optical observations DATE: 17/06/26 22:28:12 GMT FROM: Andrea Melandri at INAF-OAB A. Melandri, P. D'Avanzo (INAF-OAB), V. D'Elia (INAF/OAR & ASI/ASDC), D. Carosati, G. Andreuzzi (INAF-TNG) report on behalf of the CIBO collaboration: We observed the field of GRB 170626A (Marshall et al., GCN Circ. 21264; Hamburg & Meegan, GCN Circ. 21266) with the 3.6m Telescopio Nazionale Galileo (TNG) equipped with DOLoRes. Observations were carried out in the r-sdss filter. Observations started on Jun 26 at 21:07:35 UT (~11.53 hours after the burst) and consist in a single image lasting 180 seconds. At the edge of the refined XRT position (Cholden-Brown et al., GCN Circ. 21267) we detect a candidate optical afterglow at the following coordinates: RA(J2000) = 11:01:34.04, Dec(J2000) = +56:28:35.0, with an uncertainty of 0.5". This position is in agreement with the one reported by Moskvitin (GCN Circ. 21268). The optical afterglow is detected with a magnitude r(AB) = 20.2 +/- 0.2 (calibrated against nearby stars reported in the PAN-STARSS catalogue).
GCN 21271 table
GRB_name GRB170626A
GCN_number 21271
Detection_method Swift-BAT Det
ra 165.4090°
decl 56.4790°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21271 SUBJECT: GRB 170626A: Swift-BAT refined analysis DATE: 17/06/27 01:57:25 GMT FROM: Amy Lien at GSFC S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), F. E. Marshall (NASA/GSFC), 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 170626A (trigger #758766) (Marshall et al., GCN Circ. 21264). The BAT ground-calculated position is RA, Dec = 165.409, 56.479 deg which is RA(J2000) = 11h 01m 38.1s Dec(J2000) = +56d 28' 45.4" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 96%. The mask-weighted light curve shows a multi-peaked structure. The main emission starts at ~ T-1 s, peaks at ~T0, and ends at ~T+12 s. In addition, there are some weak emissions that start prior to the main pulse at ~T-20 s, and another weak pulse at ~T+80 s. T90 (15-350 keV) is 12.94 +- 0.34 sec (estimated error including systematics). The time-averaged spectrum from T-21.34 to T+17.92 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.26 +- 0.14, and Epeak of 120.9 +- 31.0 keV (chi squared 51.05 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 8.2 +- 0.2 x 10^-6 erg/cm2 and the 1-sec peak flux measured from T-0.06 sec in the 15-150 keV band is 23.6 +- 0.6 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.60 +- 0.03 (chi squared 69.77 for 57 d.o.f.). 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/758766/BA/
GCN 21272 table
GRB_name GRB170626A
GCN_number 21272
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21272 SUBJECT: GRB 170626A: MASTER-Tunka OT detection. DATE: 17/06/27 13:49:43 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs O.Gres, N.M.Budnev, O.Ershova Irkutsk State University V. Lipunov, E.Gorbovskoy, N.Tyurina, V.Kornilov, A.Kuznetsov, V.Vladimirov, I.Gorbunov, D.Kuvshinov, A.V.Krylov, P.Balanutsa, V.V.Chazov, D. Vlasenko Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory A.Gabovich, V.Yurkov, Yu.Sergienko Blagoveschensk Educational State University, Blagoveschensk D.Buckley, S. Potter, A.Kniazev, M.Kotze South African Astronomical Observatory R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias R.Podesta, C.Lopez, F. Podesta Observatorio Astronomico Felix Aguilar (OAFA), National University of San Juan, Argentina H. Levato, C. Saffe Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE), San Juan, Argentina MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Tunka was starting inspection on the Swift GRB 170626A error-box (ra=11 01 34 dec=+56 28 36 r=0.05) 22799 sec after notice time and 24464 sec after trigger time at 2017-06-26 16:45:56 UT. The 5-sigma upper limit on our added image (3x180s exposure) set is about 19.8 mag . We see OT with unfiltered magnitude 19.8 +0.2/-0.3 mag at Moskvitin et al. (GCN #21268) position (see also A. de Ugarte Postigo et al.,GCN #21269; Melandri et al., GCN #21270; ). The message may be cited.
GCN 21273 table
GRB_name GRB170626A
GCN_number 21273
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 21273 SUBJECT: GRB 170626A: OASDG optical observations DATE: 17/06/27 14:15:22 GMT FROM: Luca Izzo at IAA-CSIC L. Izzo (IAA-CSIC), L. D'Avino, A. Noschese, M. Mollica, L. Morrone, N. Ruocco, A. Vecchione (AC-OASDG) report: We observed the field of GRB 170626A (Marshall et al. GCN 21264) with the 0.5m telescope of the Osservatorio Astronomico S. Di Giacomo located in Agerola, Italy ( http://acgo.it/oa ). We obtained a series of 18x180 s images in the Rc filter, starting at 20:48:16 UT, ~ 11.2 hrs after the GRB trigger. We detect the GRB afterglow (Moskvitin GCN 21268, de Ugarte Postigo et al. GCN 21269, Melandri et al. GCN 21270, Lipunov et al. GCN 21272) and measure a magnitude of R(AB) = 20.1 +- 0.5. An image of the field can be seen at http://acgo.it/grb26a
GCN 21274 table
GRB_name GRB170626A
GCN_number 21274
Detection_method Insight-HXMT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 21274 SUBJECT: GRB 170626A: Insight-HXMT observation DATE: 17/06/27 15:29:39 GMT FROM: Shaolin Xiong at IHEP Y. P. Xu, M. Y. Ge, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, J. Y. Liao, X. B. Li, C. K. Li, Y. Huang, Z. Chang, X. F. Lu, J. L. Zhao, A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), Y. P. Chen, M. Gao (IHEP), T. P. Li (IHEP/THU), G. Li, M. S. Li, H. W. Liu, F. J. Lu, L. M. Song, W. H. Tao, H. Y. Wang, Y. H. Wang, X. Y. Wen, M. Wu, H. Xu, C. M. Zhang, F. Zhang, J. Zhang, T. Zhang, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: During the commissioning phase, at 2017-06-26T09:37:22.32 (T0), Insight-HXMT detected GRB 170626A (trigger ID: HEB170626400) in a routine search of the data, which was also observed by the Swift/BAT (Marshall et al. 2017, GCN 21264) and the Fermi/GBM (Hamburg et al. 2017, GCN 21266). The Insight-HXMT light curve mainly consists of several pulses with a duration (T90) of 12.1 s measured from T0-0.43 s. The 1-second peak rate, measured from T0+0.5 s, is 3275.0 cnts/sec. The total counts from this burst is 9887 counts. All measurements above are made with the CsI detectors in the energy range of about 80-840 keV. Please note that this is the deposited energy, rather than the incident photon energy. URL_LC: http://www.hxmt.org/images/GRB/HEB170626400_lc.jpg The time-averaged spectrum from T0-2.5s to T0+12.5 s is adequately fit by a Power Law model with spectral index = -1.85 +/- 0.03. The event fluence (200 -50000 keV) in this time interval is (1.86 +/- 0.09)E-05 erg/cm^2. The analysis results presented above are preliminary; final results will be published elsewhere. 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 this telescope could be found at: http://www.hxmt.org/index.php/enhome .
GCN 21276 table
GRB_name GRB170626A
GCN_number 21276
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 21276 SUBJECT: GRB 170626A: TShAO optical observations DATE: 17/06/27 16:50:15 GMT FROM: Alexei Pozanenko at IKI A. Volnova (IKI), A. Pozanenko (IKI), I. Reva (Fesenkov Astrophysical Institute), E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), report on behalf of larger GRB follow-up collaboration: We observed the field of the Swift GRB 170626A (Marshall et al., GCN Circ. 21264; Hamburg & Meegan, GCN Circ. 21266) with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting on May 20 (UT) 18:42:38. We took several images in R-filter with total exposure of 1130 s. The optical afterglow (Moskvitin et al., GCN 21268; de Ugarte Postigo, et al., GCN 21269) is clearly visible in a stacked image. Preliminary photometry of the afterglow is following: Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) (3 sigma) 2016-06-26 16:47:33 0.30832 R 1130 19.87 0.13 21.0 The magnitude is also compatible with a magnitude of the afterglow reported by Lipunov (GCN 21272) after observation at the same epoch. Taken into account that between our observation at ~7.4 hours (mid time) and TNG observation at 11.53 hours (Melandri et al., GCN 21270) the magnitude of the aftegrlow did not change one may suggest either flare like activity or plateau phase of the afterglow and the burst can interesting for follow up observations. The finding chart can be found at http://grb.rssi.ru/GRB170626A/GRB170626a-fc_TShAO.png The photometry is based on nearby SDSS stars, part of them already used in Moskvitin et al. (GCN 21169). SDSS_id R_Lupton Err J110107.23 +564104.2 15.987 0.013 J110157.37 +563628.5 15.225 0.013 J110211.15 +563624.1 15.177 0.012 J110206.51 +563744.1 14.808 0.012 J110111.46 +563755.3 15.480 0.012 (GCN 21169) J110106.88 +563153.7 16.389 0.013 J110125.73 +563134.0 18.332 0.023 J110124.28 +563251.1 17.839 0.017
GCN 21277 table
GRB_name GRB170626A
GCN_number 21277
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21277 SUBJECT: GRB 170626A: SAO RAS confirmation of OT fading DATE: 17/06/27 22:58:52 GMT FROM: Moskvitin Alexander at SAO RAS A. Moskvitin (SAO RAS), A. Volnova (IKI RAS), A. Pozanenko (IKI RAS), I. Reva (Fesenkov Astrophysical Institute), report on behalf of larger GRB follow-up team: We observed the field of the GRB 170626A (Marshall et al., GCNC 21264) with the 1-m telescope of SAO RAS, Zeiss-1000 on June, 27. The OT observed by numerous telescopes (de Ugarte Postigo et al., GCNC 21269; Melandri et al., GCNC 21270; Gres et al. GCNC 21272; Izzo et al., GCNC 21273; Volnova et al., GCNC 21276) is approx. 0.9 magnitude fainer than in previous SAO epoch. F ~ (t-T0)^ alpha. The decay slope alpha is about -0.7. ftp://ftp.sao.ru/pub/grb/GRB170626A/GRB170626A_2epochs.png The result of the first SAO epoch (GCNC 21268) were checked with the full 1.5 hour stack obtained during the first night. The stacked frames of both epochs were re-calibrated against all standards mentioned by Volnova et al. (GCNC 21276). The results are presented in the following table. The errors are statistical only. Date UT start T_mid - T0, d Filter Exp., s mag_OT Err. 2016.06.26 19:57:42 0.4695 Rc 18 x 300 19.83 +/- 0.04 (GCNC 21268) 2016.06.27 18:50:27 1.4079 Rc 12 x 300 20.68 +/- 0.07
GCN 21278 table
GRB_name GRB170626A
GCN_number 21278
Detection_method Konus-Wind Det
t_trigger 9:37:20.048 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 21278 SUBJECT: Konus-Wind observation of GRB 170626A DATE: 17/06/28 12:47:29 GMT FROM: Anna Kozlova at Ioffe Institute A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 170626A (Swift-BAT trigger #758766: Marshall et al., GCN 21264; Barthelmy et al., GCN 21271; Fermi GBM observation: Hamburg et al., GCN 21266; Insight-HXMT observation: Xu et al., GCN 21274) triggered Konus-Wind at T0=34640.048 s UT (09:37:20.048). The burst light curve shows a multipeaked structure started at ~T0-0.4 s with a total duration of ~12.8 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of 1.22(-0.05,+0.05)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+0.576 s, of 6.70(-0.97,+0.98)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+15.360 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.23(-0.10,+0.11) and Ep = 110(-7,+8) keV (chi2 = 92/99 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, the high energy photon index beta = -3.3 (-0.9,+0.4) (chi2 = 90/98 dof) The spectrum near the maximum count rate (measured from T0+0.256 to T0+7.168 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model with alpha = -1.17(-0.10,+0.11) and Ep = 123(-8,+9) keV (chi2 = 78/95 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, the high energy photon index beta = -3.5 (-3.1,+0.4) (chi2 = 77/94 dof) The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB170626_T34640/ All the quoted errors are at the 90% confidence level, except for beta errors, which are at the 68% confidence level. All the quoted values are preliminary.
GCN 21460 table
GRB_name GRB170626A
GCN_number 21460
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21460 SUBJECT: GRB 170626A: 15 GHz upper limits from AMI DATE: 17/08/11 17:48:40 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 robotically triggered on the Swift alert for GRB 170626A (Marshall et al., GCN 21264) 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 Jun 26.51, Jun 28.76, Jun 29.67 and Jul 04.66 (UT) do not reveal any radio source at the XRT location (Cholden-Brown et al., GCN 21267), with 3sigma upper limits of 120 uJy, 138 uJy, 84 uJy and 132 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/.