GRB170510A

This page lists all entries on GRB170510A in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 21080 GCN 21081 GCN 21082 GCN 21085 GCN 21086 GCN 21087 GCN 21090 GCN 21091 GCN 21093 GCN 21103 GCN 21105 GCN 21110

Summary table
Variable Value Source
GRB_name_Fermi GRB170510217
T0 5:12:25.730 UTC GCN_circulars,Fermi GBM Det
ra 159.9125° IPN
decl -39.3333° IPN
pos_error 3.33e-01° IPN
T90 127.746 s Fermi_GBM
T90_error 0.923 s Fermi_GBM
T90_start 5:12:28.551 UTC Fermi_GBM
fluence 4.39e-05 erg/cm² Fermi_GBM
fluence_error 7.64e-08 erg/cm² Fermi_GBM
T100 130.567 s
GBM_located False
mjd 57883.216964467596 GCN_circulars,Fermi GBM Det
Fermi GBM table
GRB_name_Fermi GRB170510217
trigger_name bn170510217
ra 159.9108°
decl -39.3281°
pos_error 2.52e+00°
datum 2017-05-10
t_trigger 5:12:25.735 UTC
T90 127.746 s
T90_error 0.923 s
T90_start 5:12:28.551 UTC
fluence 4.39e-05 erg/cm²
fluence_error 7.64e-08 erg/cm²
flux_1024 1.70e+01 erg/cm²/s
flux_1024_error 4.42e-01 erg/cm²/s
flux_1024_time 2.18e+01 erg/cm²/s
flux_64 2.22e+01 erg/cm²/s
flux_64_error 1.81e+00 erg/cm²/s
IPN table
GRB_name GRB170510A
ra 159.9125°
decl -39.3333°
pos_error 3.33e-01°
Fermi LAT table
GRB_name_Fermi GRB170510217
GRB_name GRB170510A
MET 516085950.73
datum 2017-05-10
t_trigger 5:12:26.730 UTC
ra 159.9110°
decl -39.3280°
pos_error 3.40e-01°
GCN 21080 table
GRB_name GRB170510A
GCN_number 21080
Detection_method Fermi LAT Det
t_trigger 5:12:25.730 UTC
ra 159.9100°
decl -39.3200°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21080 SUBJECT: GRB 170510A: Fermi-LAT detection DATE: 17/05/10 10:55:57 GMT FROM: Elisabetta Bissaldi at U.Innsbruk/IAPP E. Bissaldi (Politecnico & INFN Bari), M. Axelsson (Stockholm Univ. & KTH), and F. Longo (University & INFN, Trieste) report on behalf of the Fermi-LAT team: At 05:12:25.73 UT on May 10, 2017 Fermi-LAT detected high-energy emission from GRB 170510A, which was also detected by Fermi-GBM (trigger 516085950/170510217). The best LAT on-ground location is found to be RA, Dec = 159.91, -39.32 (J2000) with an error radius of 0.34 deg (90 % containment, statistical error only). This was ~67 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. The highest-energy photon is a 1.8 GeV event which is observed 410 seconds after the GBM trigger. A total of 15 photons were detected in the first 500 seconds after the trigger, after which time the spacecraft entered the SAA. A Swift ToO has been approved 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.
GCN 21081 table
GRB_name GRB170510A
GCN_number 21081
Detection_method Fermi LAT Det
t_trigger 5:12:25.730 UTC
ra 159.9100°
decl -39.3200°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21081 SUBJECT: GRB 170510A: Fermi-LAT detection DATE: 17/05/10 11:01:32 GMT FROM: Elisabetta Bissaldi at U.Innsbruk/IAPP E. Bissaldi (Politecnico & INFN Bari), M. Axelsson (Stockholm Univ. & KTH), and F. Longo (University & INFN, Trieste) report on behalf of the Fermi-LAT team: At 05:12:25.73 UT on May 10, 2017 Fermi-LAT detected high-energy emission from GRB 170510A, which was also detected by Fermi-GBM (trigger 516085950/170510217). The best LAT on-ground location is found to be RA, Dec = 159.91, -39.32 (J2000) with an error radius of 0.34 deg (90 % containment, statistical error only). This was ~67 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. The highest-energy photon is a 1.8 GeV event which is observed 410 seconds after the GBM trigger. A total of 15 photons were detected in the first 500 seconds after the trigger, after which time the spacecraft entered the SAA. A Swift ToO has been approved 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.
GCN 21082 table
GRB_name GRB170510A
GCN_number 21082
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21082 SUBJECT: GRB 170510A: Tiled Swift observations DATE: 17/05/10 11:58:15 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 170510A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00067 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.
GCN 21085 table
GRB_name GRB170510A
GCN_number 21085
Detection_method Fermi GBM Det
t_trigger 5:12:25.730 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 21085 SUBJECT: GRB 170510A: Fermi GBM observation DATE: 17/05/10 17:47:13 GMT FROM: Oliver J Roberts at USRA/NASA O.J. Roberts (USRA/NASA), E. Bissaldi (Politecnico & INFN Bari) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 05:12:25.73 UT on 10 May 2017, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 170510A (trigger 516085950 / 170510217), which was also detected by the Fermi/LAT (Bissaldi et al. 2017, GCN 21081). The GBM on-ground location is consistent with the LAT position. 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 angle from the Fermi LAT boresight is 67 degrees. The GBM light curve consists of multiple peaks with a duration (T90) of about 128 s (50-300 keV). The time-averaged spectrum from T0+2.0 s to T0+130.0 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.82 +/- 0.03 and the cutoff energy, parameterized as Epeak, is 302 +/- 13 keV. A Band function fits the spectrum equally well with Epeak= 264 +/- 17 keV, alpha = -0.77 +/- 0.04 and beta = -2.33 +/- 0.16. The event fluence (10-1000 keV) in this time interval is (4.78 +/- 0.11)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+21.8 s in the 10-1000 keV band is 17.0 +/- 0.4 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 21086 table
GRB_name GRB170510A
GCN_number 21086
Detection_method Swift-XRT Other
ra 160.1539°
decl -39.2124°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21086 SUBJECT: GRB 170510A: Swift-XRT observations DATE: 17/05/10 22:22:51 GMT FROM: Antonino D'Ai at IASF-PA A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), A. Cholden-Brown (PSU), S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC) 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 170510A (Bissaldi et al. GCN Circ. 21080) in a series of observations tiled on the sky. The total exposure time is 4.7 ks, distributed over 7 tiles; the maximum exposure at a single sky location was 1.4 ks. The data were collected between T0+24.3 ks and T0+36.2 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): 160.15394 = 10:40:36.95 Dec (J2000): -39.21244 = -39:12:44.8 Error: 2.3 arcsec (radius, 90% conf. [Enhanced position]) Count-rate: 0.0630 [+0.0091, -0.0090] ct s^-1 Distance: 794 arcsec from Fermi/LAT position. Flux: (1.76 [+0.26, -0.25])e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV) Two catalogued sources were also detected. 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_GRB00067. This circular is an official product of the Swift-XRT team.
GCN 21087 table
GRB_name GRB170510A
GCN_number 21087
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21087 SUBJECT: GRB 170510A: LCO possible counterpart DATE: 17/05/11 04:14:49 GMT FROM: Bruce Gendre at UVI A. Cucchiara, D. Morris (U. of Virgin Islands), C. Guidorzi (U. Ferrara), B. Gendre (U. of Virgin Islands), reports on behalf of a larger collaboration: "On May 10 at 16:46 UT (T_0 +11.4h) we began observing the center of the field of LAT GRB 170510A (Bissaldi et al. GCN #21080) using the Las Cumbres Observatory 1m Sutherland facility. We covered 50% of the LAT error region and we obtained a series of 5x120s observations in R band, for a total of 10 minutes on sky. We identified a possible optical counterpart of GRB170510A located at the same position of candidate #1 from the Swift-XRT tiled observations (Evans et al. GCN #21082, Melandri et al. GCN #21086). Our preliminary photometry for this source is: R = 19.6 +/- 0.2 mag At the moment we cannot establish the temporal variability of this source. This magnitude is calibrated against nearby USNO-B1 sources, and is not corrected for Galactic Extinction."
GCN 21090 table
GRB_name GRB170510A
GCN_number 21090
Detection_method Konus-Wind Det
t_trigger 5:12:30.788 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 21090 SUBJECT: Konus-Wind observation of GRB 170510A DATE: 17/05/12 14:07:37 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, A. Tsvetkova, A. Lysenko, A.Kozlova, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 170510A (Fermi-LAT detection: Bissaldi, et al., GCN Circ. 21080; Fermi-GBM detection: Roberts, et al., GCN Circ. 21085) triggered Konus-Wind at T0=18750.788 s UT (05:12:30.788). The burst light curve shows a multipeaked structure which starts at ~T0-2 s and has a total duration of ~141 s. The emission is seen up to ~18 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB170510_T18750/ As observed by Konus-Wind, the burst had a fluence of 5.70(-0.70,+1.51)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+20.688 s, of 5.60(-1.12,+1.63)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+137.216 s) is best fit in the 20 keV - 18 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -0.84(-0.14,+0.17), the high energy photon index beta = -3.12(-6.88,+0.73), the peak energy Ep = 261(-36,+42) keV (chi2 = 76/96 dof). The spectrum near the maximum count rate (measured from T0+16.640 to T0+22.528 s) is best fit in the 20 keV - 18 MeV range by a power law with exponential cutoff model (CPL): dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.72(-0.09,+0.10) and Ep = 331(-25,+29) keV (chi2 = 89/92 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.56 (chi2 = 88/91 dof). In this (and only this) time interval, a prominent count excess over the Band (and CPL) function is seen in the ~2-18 MeV range, suggesting a presence of a hard spectral component. Fitting this spectrum by a CPL + power law (PL) model yields alpha = -0.48(-0.31,+0.44), Ep = 301(-31,+50) keV, and PL photon index of about -1.6 (chi2 = 85/90 dof), with the component energy flux ratio (PL to CPL) of ~ 0.6 (20 keV - 10 MeV). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 21091 table
GRB_name GRB170510A
GCN_number 21091
Detection_method Optical
ra 10.0000°
decl 40.0000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21091 SUBJECT: GRB 170510A: Global MASTER Net possible OT observations DATE: 17/05/12 14:36:50 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, D.Kuvshinov, A.V.Krylov, I.Gorbunov, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D. Vlasenko Lomonosov Moscow State University, Sternberg Astronomical Institut D.Buckley, S. Potter, A.Kniazev, M.Kotze South African Astronomical Observatory 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 K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk, O. Ershova Irkutsk State University V.Yurkov, Yu.Sergienko Blagoveschensk Educational State University, Blagoveschensk A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias MASTER-SAAO robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in SAAO was starting survey on the LAT GRB170510.22 error-box (Bissaldi et al., GCN #21080) 22480 sec after notice time and 41530 sec after trigger time at 2017-05-10 16:44:36 UT. The 5-sigma upper limit on our first (180s exposure) set is about 18.9 mag We marginaly see optical candidate (Cucchiara et al. GCN 21087) at XRT (Evans et al. GCN #21082, Melandri et al. GCN #21086) position with unfiltered mag ~ 19 m . Ra, Dec = 10 40 36.76 -39 12 43.8 (+/-1 arcsec) We did not see object 2.5 hours late with limit 19.5 . So X-ray Source 1 (Melandri et al. GCN #21086) is possible OT. The message may be cited.
GCN 21093 table
GRB_name GRB170510A
GCN_number 21093
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21093 SUBJECT: GRB 170510A: AstroSat CZTI(Veto) detection DATE: 17/05/14 18:59:22 GMT FROM: Vidushi Sharma at IUCAA V. Sharma (IUCAA), V. Bhalerao (IIT-B), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the Astrosat CZTI collaboration: The bright long GRB170510A (Bissaldi E. et al., GCN Circ. 21080) was detected using the CsI veto detectors on Astrosat CZTI (Bhalerao et al., arXiv:1608.03408). The source was clearly detected in the 125-250 keV energy range. The light curve shows a multiple peak structure. The peak count rate in the CsI detectors was 940.2 counts/sec above the background (four quadrants summed together), with a total of 699536 counts. The local mean background count rate was 1365.7 counts/sec. Using cumulative rates, we measure a T90 of 67.8 secs. 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.
GCN 21103 table
GRB_name GRB170510A
GCN_number 21103
Detection_method Swift-XRT Other
ra 160.1539°
decl -39.2124°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21103 SUBJECT: GRB 170510A: Swift-XRT afterglow detection DATE: 17/05/18 15:59:27 GMT FROM: Antonino D'Ai at IASF-PA A. Cholden-Brown (PSU), S. J. LaPorte (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), B. Mingo (U. Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), J.A. Kennea (PSU) 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 170510A (Bissaldi et al. GCN Circ. 21080). The observations now extend from T0+24.7 ks to T0+713.5 ks, and are entirely in Photon Counting (PC) mode. The source previously reported by Melandri et al. (GCN Circ. 21086), "Source 1", is fading with 3-sigma significance, and is therefore likely the GRB afterglow. Using 1264 s of PC mode data and 4 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 160.15394, -39.21244 which is equivalent to: RA (J2000): 10h 40m 36.95s Dec(J2000): -39d 12' 44.8" with an uncertainty of 2.3 arcsec (radius, 90% confidence). This position is 13.2 arcmin from the Fermi/LAT position. The source is fading with alpha >0.9. A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.8 (+0.8, -0.4). The best-fitting absorption column is consistent with 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 3.2 x 10^-11 (3.5 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 6 (+/-24) x 10^20 cm^-2 Galactic foreground: 6.1 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 1.8 (+0.8, -0.4) The results of the XRT-team automatic analysis of the likely afterglow are at http://www.swift.ac.uk/xrt_products/TILED_GRB00067/Source1.php. The results of the full analysis of the tiled XRT observations are available at http://www.swift.ac.uk/xrt_products/TILED_GRB00067. Swift/UVOT observed "Source 1" at T0+696 ks. We did not find an optical counterpart. We measured a 3 sigma upper limit >21 mag in the UVW1 filter, using an exposure of 1671 s. This circular is an official product of the Swift-XRT and UVOT teams.
GCN 21105 table
GRB_name GRB170510A
GCN_number 21105
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 21105 SUBJECT: GRB 170510A CALET Gamma-Ray Burst Monitor detection DATE: 17/05/19 02:55:29 GMT FROM: Takanori Sakamoto at AGU A. Tezuka, A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, Y. Yamada, S. Matsukawa (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence), A. V. Penacchioni, P. S. Marrocchesi (U of Siena) and the CALET collaboration: The long-duration GRB 170510A (Roberts et al., GCN Circ. 21085; Bissaldi et al., GCN Circ. 21080; Svinkin et al. GCN Circ. 21090; Sharma et al. GCN Circ. 21093; INTEGRAL SPI-ACS trigger #7841) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 05:12:23.19 on 10 May 2017. The burst signal was seen by all CGBM instruments. The light curve of the SGM shows multiple peaks. The emission starts from T+5 sec, peaks at T+25 sec and ends at T+35 sec. The T90 duration measured by the SGM data is 24.9 +- 1.0 sec (40-1000 keV). The light curve is available at http://cgbm.calet.jp/cgbm_trigger/flight/1178427921/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.
GCN 21110 table
GRB_name GRB170510A
GCN_number 21110
Detection_method Swift-XRT Other
ra 160.1537°
decl -39.2126°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21110 SUBJECT: GRB 170510A: LCO Siding Springs early observations DATE: 17/05/19 13:47:40 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), A. Gomboc (U. Nova Gorica), C.G. Mundell (U. Bath), A. Cucchiara, D. Morris, B. Gendre (U. of Virgin Islands) on behalf of a large collaboration report: We began observing Fermi GRB 170510A (Bissaldi et al. GCN 21081) on May 10, 12:14 UT (7.0 hours since the GRB) with a 1-m LCO unit with the SDSS i filter. Within the Swift-XRT error circle (Cholden-Brown et al. GCN 21103) we clearly detect the optical afterglow candidate (Cucchiara et al. GCN 21087; Lipunov et al. GCN 21091) at the following position: RA(J2000) = 10:40:36.89 DEC(J2000)= -39:12:45.2 with an error radius of 1.0", with the following value: Mid Time Exposure Filter Magnitude (AB) (hours) (s) ------------------------------------------------------- 7.1 5x120 SDSS-I 18.60 +- 0.07 ------------------------------------------------------- as calibrated against nearby UCAC4 stars.