GRB130609B

This page lists all entries on GRB130609B in GRBweb

Summary Fermi GBM IPN Swift GCN 14841 GCN 14847 GCN 14852 GCN 14856 GCN 14857 GCN 14862 GCN 14866 GCN 14867 GCN 14869 GCN 14888 GCN 14915

Summary table
Variable Value Source
GRB_name_Fermi GRB130609902
T0 21:38:35.610 UTC Fermi_GBM
ra 53.7713° Swift
decl -40.1741° Swift
pos_error 6.47e-05° Swift
T90 191.491 s Fermi_GBM
T90_error 2.862 s Fermi_GBM
T90_start 21:38:40.474 UTC Fermi_GBM
fluence 5.44e-05 erg/cm² Fermi_GBM
fluence_error 3.30e-07 erg/cm² Fermi_GBM
T100 214.99 s
GBM_located False
mjd 56452.90180104167 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB130609902
trigger_name bn130609902
ra 53.7700°
decl -40.1761°
pos_error 2.49e+00°
datum 2013-06-09
t_trigger 21:38:35.610 UTC
T90 191.491 s
T90_error 2.862 s
T90_start 21:38:40.474 UTC
fluence 5.44e-05 erg/cm²
fluence_error 3.30e-07 erg/cm²
flux_1024 1.44e+01 erg/cm²/s
flux_1024_error 4.31e-01 erg/cm²/s
flux_1024_time 6.59e+00 erg/cm²/s
flux_64 1.86e+01 erg/cm²/s
flux_64_error 1.82e+00 erg/cm²/s
IPN table
GRB_name GRB130609B
ra 53.7542°
decl -40.1500°
pos_error 5.00e-02°
Swift table
GRB_name GRB130609B
t_trigger 21:38:40 UTC
ra 53.7713°
decl -40.1741°
pos_error 6.47e-05°
T90 210.6 s
fluence 1.60e-05 erg/cm²
GCN 14841 table
GRB_name GRB130609B
GCN_number 14841
Detection_method Swift Det
t_trigger 21:38:40 UTC
ra 53.7540°
decl -40.1530°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14841 SUBJECT: GRB 130609B: Swift detection of a burst with an optical counterpart DATE: 13/06/09 21:46:41 GMT FROM: Scott Barthelmy at NASA/GSFC H. A. Krimm (CRESST/GSFC/USRA), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), J. A. Kennea (PSU), D. Malesani (DARK/NBI), C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC) and A. Maselli (INAF-IASFPA) report on behalf of the Swift Team: At 21:38:40 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 130609B (trigger=557828). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 53.754, -40.153 which is RA(J2000) = 03h 35m 01s Dec(J2000) = -40d 09' 11" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows multiple peaks with a total duration of at least 200 sec. The peak count rate was ~8500 counts/sec (15-350 keV), at ~2 sec after the trigger. The XRT began observing the field at 21:39:56.4 UT, 76.0 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 53.7695, -40.1747 which is equivalent to: RA(J2000) = +03h 35m 4.68s Dec(J2000) = -40d 10' 28.9" with an uncertainty of 4.9 arcseconds (radius, 90% containment). This location is 89 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. UVOT took a finding chart exposure of nominal 150.000 seconds with the White filter starting 84 seconds after the BAT trigger. There is a candidate afterglow in the list of sources generated on-board at RA(J2000) = 03:35:05.11 = 53.77128 DEC(J2000) = -40:10:26.6 = -40.17406 with a 90%-confidence error radius of about 1.10 arc sec. This position is 5.4 arc sec. from the center of the XRT error circle. The estimated magnitude is 15.71. No correction has been made for the expected extinction corresponding to E(B-V) of 0.01. Burst Advocate for this burst is H. A. Krimm (krimm 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 14847 table
GRB_name GRB130609B
GCN_number 14847
Detection_method Swift-XRT Det
ra 53.7710°
decl -40.1741°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14847 SUBJECT: GRB 130609B: Enhanced Swift-XRT position DATE: 13/06/10 06:30:59 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 2407 s of XRT Photon Counting mode data and 5 UVOT images for GRB 130609B, 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 = 53.77097, -40.17407 which is equivalent to: RA (J2000): 03h 35m 5.03s Dec (J2000): -40d 10' 26.7" with an uncertainty of 1.7 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.
GCN 14852 table
GRB_name GRB130609B
GCN_number 14852
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14852 SUBJECT: GRB 130609B: Swift-XRT refined Analysis DATE: 13/06/10 14:46:03 GMT FROM: Phil Evans at U of Leicester C. Pagani (U. Leicester), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), G. Stratta (ASDC), D.N. Burrows (PSU), J.A. Kennea (PSU), M.C. Stroh (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester) and H.A. Krimm report on behalf of the Swift-XRT team: We have analysed 7.0 ks of XRT data for GRB 130609B (Krimm et al. GCN Circ. 14841), from 66 s to 46.7 ks after the BAT trigger. The data comprise 1.4 ks in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN. Circ 14847). The late-time light curve (from T0+5.4 ks) can be modelled with an initial power-law decay with an index of alpha=1.42 (+0.14, -0.56), followed by a break at T+13.6 ks to an alpha of 2.36 (+0.38, -0.22). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.840 (+/-0.029). The best-fitting absorption column is 1.40 (+0.08, -0.07) x 10^21 cm^-2, in excess of the Galactic value of 1.4 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.01 (+/-0.10) and a best-fitting absorption column of 1.28 (+0.26, -0.24) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (5.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.28 (+0.26, -0.24) x 10^21 cm^-2 Galactic foreground: 1.4 x 10^20 cm^-2 Excess significance: 7.6 sigma Photon index: 2.01 (+/-0.10) If the light curve continues to decay with a power-law decay index of 2.36, the count rate at T+24 hours will be 8.4 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x 10^-13 (4.1 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00557828. This circular is an official product of the Swift-XRT team.
GCN 14856 table
GRB_name GRB130609B
GCN_number 14856
Detection_method Konus-Wind Det
t_trigger 21:38:36.818 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14856 SUBJECT: Konus-Wind observation of GRB 130609B DATE: 13/06/10 16:22:33 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline, on behalf of the Konus-Wind team, report: The long-duration intense GRB 130609B (Swift-BAT trigger 557828: Krimm, et al., GCN 14841) triggered Konus-Wind at T0=77916.818 s UT (21:38:36.818) The light curve consists of two major emission episodes: the first one with a bright multi-peaked structure from ~T0-30 s to ~T0+55 s, and the second, much weaker and softer episode, from ~T0+170 s to ~T0+210 s. The emission is seen up to 7 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB130609_T77916/ As observed by Konus-Wind, the burst had a fluence of (9.4 0.7)x10-5 erg/cm2, and a 64-ms peak flux, measured from T0+3.712 s, of (9.5 0.6)x10-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the first emission episode (measured from T0 to T0+54.528 s) is best fit in the 20 keV - 18 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.84 0.05, the high energy photon index beta = -2.39 0.15, the peak energy Ep = 397 26 keV, chi2 = 97/97 dof. The time-averaged spectrum of the second emission episode (measured from T0+169.216 to T0+210.176 s) is best fit in the 20 keV - 18 MeV range by the cutoff power law with the following model parameters: the photon index alpha = -1.64 0.21, the peak energy Ep = 198 105 keV, chi2 = 93.7/98 dof. The spectrum at the maximum count rate (measured from T0 to T0+6.656 s) is best fit in the 20 keV - 18 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.70 0.07, the high energy photon index beta = -3.0 0.3, the peak energy Ep = 740 90 keV, chi2 = 105/97 dof. All the quoted results are preliminary.
GCN 14857 table
GRB_name GRB130609B
GCN_number 14857
Detection_method Swift-UVOT Det
ra 53.7713°
decl -40.1741°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14857 SUBJECT: GRB 130609B: Swift/UVOT Observations DATE: 13/06/10 16:46:41 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and H. A. Krimm (CRESST/GSFC/USRA) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 130609B 85 s after the BAT trigger (Krimm et al., GCN Circ. 14841). A fading source consistent with the XRT position (Goad et al. GCN Circ. 14847) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 03:35:05.11 = 53.77128 (deg.) Dec (J2000) = -40:10:26.7 = -40.17409 (deg.) with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence). Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first and second orbit exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white (fc) 84 234 147 15.47+-0.02 white 577 1891 283 17.36+-0.03 white 6046 7681 393 18.39+-0.05 v 799 1941 136 16.89+-0.09 v 6457 6657 196 18.00+-0.15 b 552 1866 136 17.32+-0.06 b 5841 7476 393 18.46+-0.09 u (fc) 297 546 245 16.31+-0.04 u 700 1841 116 17.15+-0.08 u 5636 7271 393 18.15+-0.09 uvw1 676 1816 136 17.61+-0.12 uvw1 5432 7067 393 18.75+-0.15 uvm2 823 1791 116 19.12+-0.35 uvm2 6662 6861 196 >19.66 uvw2 603 1916 116 >19.51 uvw2 6252 7855 362 >20.39 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.01 in the direction of the burst (Schlegel et al. 1998).
GCN 14862 table
GRB_name GRB130609B
GCN_number 14862
Detection_method Swift-BAT Det
ra 53.7760°
decl -40.1680°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14862 SUBJECT: GRB 130609B, Swift-BAT refined analysis DATE: 13/06/10 21:39:05 GMT FROM: Hans Krimm at NASA-GSFC A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team): Using the data set from T-60 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 130609B (trigger #557828) (Krimm, et al., GCN Circ. 13841). The BAT ground-calculated position is RA, Dec = 53.776, -40.168 deg which is RA(J2000) = 03h 35m 06.2s Dec(J2000) = -40d 10' 04.0" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 43%. The mask-weighted light curve shows an initial complex of two main overlapping peaks with numerous subsidiary peaks, with strong emission between T-10 and T+50 sec and low-level emission between T-30 and T+120 sec. The highest points are at T+4 and T+18 sec. Then there is a second, weaker and softer pair of overlapping peaks between T+160 sec and T+220 sec. This second set of peaks is consistent with a flare seen in the Swift-XRT. T90 (15-350 keV) is 191.98 +- 2.44 sec (estimated error including systematics) We note that receipt of the full event data for GRB 130609B may reveal further late-time peaks and require a revision of the T90 estimate. We will report on the full data set in a later Circular. The time-averaged spectrum from T-7.84 to T+213.25 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.23 +- 0.04. The fluence in the 15-150 keV band is 1.6 +- 0.0 x 10^-05 erg/cm2. The 1-sec peak photon flux measured from T+16.78 sec in the 15-150 keV band is 8.5 +- 0.4 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/557828/BA/
GCN 14866 table
GRB_name GRB130609B
GCN_number 14866
Detection_method GROND
Circular_text TITLE: GCN CIRCULAR NUMBER: 14866 SUBJECT: GRB 130609B: GROND observations DATE: 13/06/11 13:16:42 GMT FROM: Andrea Rossi at TLS Tautenburg S. Schmidl, A. Rossi (both TLS Tautenburg), and J. Greiner (MPE Garching) report on behalf of the GROND team: We observed the field of GRB 130609B (Swift trigger 557828; Krimm et al., GCN #14841) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla Observatory (Chile). Observations started at 09:30 UT on 11th June 2013, 35.9 hours after the GRB trigger. They were performed at an average seeing of 1.6" and at an average airmass of 2.2. We detect a source at the position of the UVOT afterglow (Siegel et al.; GCN #14857), and based on images taken at a mid-time of 09:45 UT, with total exposures of 25 minutes in g'r'i'z' and 20 minutes in JHK, we estimate preliminary magnitudes (all in AB) of g' = 22.2 +/- 0.1 mag, r' = 21.7 +/- 0.1 mag, i' = 21.1 +/- 0.2 mag, z' = 20.9 +/- 0.2 mag, J = 20.6 +/- 0.3 mag, H = 19.8 +/- 0.4 mag, and K = 19.4 +/- 0.4 mag. The source is brighter than what one could expect extrapolating the early UVOT data (Siegel et al.; GCN #14857) and could be either a plateau/flare, or due to the contribution of the host galaxy. Given magnitudes are calibrated against GROND zeropoints as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.01 mag in the direction of the burst (Schlegel et al. 1998).
GCN 14867 table
GRB_name GRB130609B
GCN_number 14867
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14867 SUBJECT: GRB 130609B, Further Swift-BAT refined analysis DATE: 13/06/11 13:22:03 GMT FROM: Hans Krimm at NASA-GSFC H. A. Krimm (GSFC/USRA) and J. R. Cummings (GSFC/UMBC) for the Swift-BAT team: Using the full data set from T-239 to T+963 sec from the recent telemetry downlink, we report final analysis of BAT GRB 130609B (trigger #557828) (Krimm, et al., GCN Circ. 14841; Lien at al., GCN Circ. 14862). In addition to the peaks described in Lien at al., GCN Circ. 14862, we report that there is a small peak in the BAT at around T+270 sec, coincident with a second flare in the XRT. T90 (15-350 keV) is 210.6 +- 15.1 sec (estimated error including systematics). The time-averaged spectrum from T-7.8 to T+307.6 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.32 +- 0.04. The fluence and peak photon flux are as reported in GCN Circ. 14862. The quoted error is at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/557828/BA/
GCN 14869 table
GRB_name GRB130609B
GCN_number 14869
Detection_method Fermi GBM Det
t_trigger 21:38:35.610 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14869 SUBJECT: GRB 130609B: Fermi GBM observation DATE: 13/06/11 14:52:13 GMT FROM: Veronique Pelassa at UAH V. Pelassa (UAH) reports on behalf of the Fermi GBM Team: "At 21:38:35.61 UT on 09 June 2013, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 130609B (trigger 392506718 / 130609902), which was also detected by the Swift/BAT (H.A. Krimm et al. 2013, GCN 14841). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 117 degrees. The GBM light curve consists of two bright peaks within 30s of trigger and a fainter bump at 170s after trigger with a duration (T90) of about 191 s (50-300 keV). The time-averaged spectrum from T0+0.003s to T0+28.672s is well fit by a power law function with an exponential high-energy cutoff. The power law index is -0.70 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 536 +/- 18 keV (Castor statistics 474 for 365 d.o.f.). The event fluence (10-1000 keV) in this time interval is (6.02 +/- 0.07)E-05 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+6.592 s in the 10-1000 keV band is 13.6 +/-0.4 ph/s/cm^2. A Band function fits the spectrum equally well (Castor statistics 468 for 364 d.o.f.) with Epeak= 491 +/- 20 keV, alpha = -0.66 +/- 0.02 and beta = -2.6 +/- 0.2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 14888 table
GRB_name GRB130609B
GCN_number 14888
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14888 SUBJECT: GRB 130609B: Theoretical redshift estimation DATE: 13/06/12 18:57:55 GMT FROM: Remo Rufinni at ICRA R. Ruffini, C.L. Bianco, M. Enderli, M. Muccino, A.V. Penacchioni, G.B. Pisani, J.A. Rueda, N. Sahakyan, Y. Wang, L. Izzo report: The late X-ray observations of GRB 130609B evidences a pattern typical of a family of GRBs associated to Supernovae following the Induced Gravitational Collapse (IGC) paradigm. We estimate a cosmological redshift for the GRB of approximately z=1.3. We encourage observations.
GCN 14915 table
GRB_name GRB130609B
GCN_number 14915
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14915 SUBJECT: GRB 130609B: Suzaku WAM observation of the prompt emission DATE: 13/06/18 02:17:01 GMT FROM: Masanori Ohno at Hiroshima U K. Takaki, M. Ohno, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.), M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida, H. Ueno, S. Sugimoto (Saitama U.), K. Yamaoka (Nagoya U.), M. Yamauchi, M. Akiyama, N. Ohmori (Univ. of Miyazaki), S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri(RIKEN), Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report: The long GRB 130609B (Krimm et al., GCN14841) triggered by the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 21:38:35 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0, ending at T0+30 s with a duration (T90) of about 19.6 seconds. The fluence in 100 - 1000 keV was 3.77 (+0.24/-0.70) x10^-5 erg/cm^2. The 1-s peak flux measured was 7.03 (+0.39/-2.80) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0 to T0+30 s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 1.48 (+0.40/-0.41), and Epeak 845 (+179/-147) keV (chi^2/d.o.f. = 15.2/24). Due to the brightness of this burst, a 5% systematic error was added for low energy channels. All the quoted errors are at statistical 90% confidence level. The light curves for this burst will be available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html