GRB130505A

This page lists all entries on GRB130505A in GRBweb

Summary IPN Swift GCN 14563 GCN 14566 GCN 14567 GCN 14568 GCN 14569 GCN 14570 GCN 14571 GCN 14572 GCN 14573 GCN 14575 GCN 14576 GCN 14577 GCN 14578 GCN 14580 GCN 14585 GCN 14589 GCN 14593 GCN 14595 GCN 14599 GCN 14602

Summary table
Variable Value Source
T0 8:22:27.038 UTC GCN_circulars,Konus-Wind Det
ra 137.0610° Swift
decl 17.4848° Swift
pos_error 6.47e-05° Swift
T90 88.0 s Swift
T90_start 8:22:28 UTC Swift
fluence 2.10e-05 erg/cm² Swift
redshift 2.2700 GCN_circulars,Swift-BAT Det
T100 88.962 s
GBM_located False
mjd 56417.34892405092 GCN_circulars,Konus-Wind Det
IPN table
GRB_name GRB130505A
ra 137.0583°
decl 17.4833°
pos_error 5.00e-02°
redshift 2.2700
Swift table
GRB_name GRB130505A
t_trigger 8:22:28 UTC
ra 137.0610°
decl 17.4848°
pos_error 6.47e-05°
T90 88.0 s
fluence 2.10e-05 erg/cm²
redshift 2.2700
GCN 14563 table
GRB_name GRB130505A
GCN_number 14563
Detection_method Swift Det
t_trigger 8:22:28 UTC
ra 137.0600°
decl 17.4850°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14563 SUBJECT: GRB 130505A: Swift detection of a burst with optical afterglow DATE: 13/05/05 08:36:39 GMT FROM: Scott Barthelmy at NASA/GSFC J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC), C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), P. T. O'Brien (U Leicester), B. Sbarufatti (INAF-OAB/PSU) and M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift Team: At 08:22:28 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 130505A (trigger=555163). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 137.060, +17.485 which is RA(J2000) = 09h 08m 14s Dec(J2000) = +17d 29' 06" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a bright peak followed by a much weaker peak with a total duration of about 20 sec. The peak count rate was ~35,500 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 08:24:04.7 UT, 96.4 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 137.0626, 17.4857 which is equivalent to: RA(J2000) = +09h 08m 15.02s Dec(J2000) = +17d 29' 08.5" with an uncertainty of 4.8 arcseconds (radius, 90% containment). This location is 9.3 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 7.35e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 106 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 09:08:14.64 = 137.06100 DEC(J2000) = +17:29:05.2 = 17.48479 with a 90%-confidence error radius of about 0.74 arc sec. This position is 6.4 arc sec. from the center of the XRT error circle. The estimated magnitude is 14.14 with a 1-sigma error of about 0.14. No correction has been made for the expected extinction corresponding to E(B-V) of 0.04. Burst Advocate for this burst is J. K. Cannizzo (cannizzo 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 14566 table
GRB_name GRB130505A
GCN_number 14566
Detection_method MAXI Det
t_trigger 8:22:29 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14566 SUBJECT: GRB 130505A: MAXI/GSC detection DATE: 13/05/05 10:13:07 GMT FROM: Satoshi Nakahira at JAXA/MAXI GRB 130505A: MAXI/GSC detection S. Nakahira (JAXA), M. Serino (RIKEN), H. Negoro (Nihon U.), S. Ueno, H. Tomida, M. Kimura, M. Ishikawa (JAXA), T. Mihara, M. Sugizaki, M. Morii, T. Yamamoto, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), N. Kawai, R. Usui, K. Ishikawa, T. Yoshii (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Nakano (AGU), H. Tsunemi, M. Sasaki (Osaka U.), M. Nakajima, T. Onodera, K. Fukushima, K. Suzuki (Nihon U.), Y. Ueda, M. Shidatsu, T. Kawamuro, (Kyoto U.), Y. Tsuboi, M. Higa (Chuo U.), M. Yamauchi, K. Yoshidome, Y. Ogawa, H. Yamada (Miyazaki U.), K. Yamaoka (Nagoya U.) report on behalf of the MAXI team At 2013-05-05T08:22:29 UT, the MAXI/GSC detected an uncatalogued X-ray transient source. Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec.) = (136.955 deg, 17.585 deg)= (09 07 49 , +17 35 05)(J2000) with a 90% C.L. statistical error of 0.07 deg and an additional systematic uncertainty of 0.1 deg (90% containment radius). The position and time are consistent with those of GRB 130505A (Cannizzo et al, GCN #14563). The transit by MAXI occurred from 2013-05-05T08:22:18 (=T0-10 s, where T0 is the Swift/BAT trigger time) to T0+40s. The averaged X-ray flux was 3.17 +/- 0.21 Crab (2-20 keV). The spectrum is fitted by a power-law model with a photon index of 1.37 (-0.10/+0.10). There was no significant excess flux at the previous transit at 2013/05/05 06:46 UT and at the next transit at 2013/05/05 09:55 UT with an upper limit of 20 mCrab for each.
GCN 14567 table
GRB_name GRB130505A
GCN_number 14567
Detection_method Swift-BAT Det
redshift 2.2700
Circular_text TITLE: GCN CIRCULAR NUMBER: 14567 SUBJECT: GRB 130505A - Gemini-N/GMOS redshift determination DATE: 13/05/05 10:30:19 GMT FROM: Nial Tanvir at U.Leicester N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), T. Matulonis and A. B. Smith (Gemini) report on behalf of a larger collaboration: We observed the afterglow of GRB 130505A (Cannizzo et al. GCN 14563) with the GMOS-N spectrograph on Gemini-N, beginning approximately 60 min after the BAT trigger. In our provisional reduction we detect numerous absorption lines, including Lyman alpha, SiII/SiII*1260, SiII*1264, OI1302, SiII/OI*1304, SiII*1309, CII/CII* 1334/1335, SiIV1394/1403, SiII 1527, SiII* 1533, CIV 1548/1551, FeII 1608, AlII 1671 and AlIII 1855/1863 at a common redshift of z=2.27. The presence of fine structure lines, in particular, confirms this to be the redshift of this burst.
GCN 14568 table
GRB_name GRB130505A
GCN_number 14568
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 14568 SUBJECT: GRB 130505A: MITSuME Okayama Optical Observation DATE: 13/05/05 12:02:12 GMT FROM: Daisuke Kuroda at OAO/NAOJ D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ), S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto) and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration: We observed the field of GRB 130505A (Cannizzo et al., GCNC 14563) with the optical three color (g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of Okayama Astrophysical Observatory. The observation started on 2013-05-05 10:52:56 UT (~2.5 h after the burst). We detected the previously reported afterglow (Cannizzo et al., GCNC 14563) in all the three bands. Photometric results of the OT are listed below. We used SDSS catalog for flux calibration. #T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err ----------------------------------------------------------------------- 0.11507 11:08:09 1620.0 18.2 0.1 18.2 0.1 17.6 0.1 ------------------------------------------------------------------------ T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec]
GCN 14569 table
GRB_name GRB130505A
GCN_number 14569
Detection_method Swift-XRT Det
ra 137.0607°
decl 17.4847°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14569 SUBJECT: GRB 130505A: Enhanced Swift-XRT position DATE: 13/05/05 13:07:03 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 1875 s of XRT Photon Counting mode data and 5 UVOT images for GRB 130505A, 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 = 137.06069, +17.48471 which is equivalent to: RA (J2000): 09h 08m 14.57s Dec (J2000): +17d 29' 05.0" 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 14570 table
GRB_name GRB130505A
GCN_number 14570
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 14570 SUBJECT: GRB 130505A; Weihai optical observations DATE: 13/05/05 13:43:31 GMT FROM: Dong Xu at DARK/NBI D. Xu (DARK/NBI), C. Cao, S.-M. Hu, J.-M. Ai (SDU) report: We observed the field of GRB 130505A (Cannizzo et al., GCN 14563) with the 1m telescope located in Weihai, Shandong Province, China. We obtained 2x600s frames in the solan r-filter with a mean time of 3.3724 hr after the BAT trigger. The optical afterglow is clearly detected at the UVOT position with r=18.4 +/- 0.1 mag, calibrated against the SDSS field.
GCN 14571 table
GRB_name GRB130505A
GCN_number 14571
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 14571 SUBJECT: GRB 130505A: Xinglong TNT optical observations DATE: 13/05/05 14:32:29 GMT FROM: L.P. Xin at NAOC L. P. Xin, J. Y. Wei, Y. L. Qiu, J. Wang, J. S. Deng, C. Wu, X. H. Han report on behalf of EAFON team: We began to observe the field of GRB 130505A (Cannizzo, et al., GCN 14563) using 80cm TNT telescope located at Xinglong observatory, China at 12:25:39 UT on 2013-05-05. We obtained several R-band images. The reported optical counterpart (Cannizzo, et al., GCN 14563) is detected in all images. A prelinary analysis shows that its brightness is decaying from R~18.05 to R~18.68 mag during 4.05h and 4.85h after the trigger time. These magnitudes are calibrated with USNO B1.0 R2 stars, This message may be cited.
GCN 14572 table
GRB_name GRB130505A
GCN_number 14572
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 14572 SUBJECT: GRB 130505A: iTelescope T12 optical observations DATE: 13/05/05 15:03:03 GMT FROM: Veli-Pekka Hentunen at Taurus Hill Obs,A95 Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill Observatory, Varkaus, Finland) report: We have detected GRB 130505A optical afterglow at iTelescope observatory T12 (Siding Spring, Australia) Takahashi FSQ ED 0.10m/5.0 astrograph and SBIG STL-11000M CCD. Five unfiltered images with 600 sec and 300 sec exposure time were made. The afterglow was detected at following position RA 09:08:14.6 and DEC +17:29:04. The following magnitudes were obtained from the observations using NOMAD1 1075-0205635 (R=14.240) as the comparison: Tmid(sec)+T0 Filter Exp. time Mag Mag err. 2485 unfiltered 600 16.78CR 0.06 3370 unfiltered 3x300 17.15CR 0.02 5061 unfiltered 600 17.45CR 0.08
GCN 14573 table
GRB_name GRB130505A
GCN_number 14573
Detection_method Swift-UVOT Det
ra 137.0610°
decl 17.4848°
redshift 2.2700
Circular_text TITLE: GCN CIRCULAR NUMBER: 14573 SUBJECT: Swift/UVOT observations of GRB130505A DATE: 13/05/05 16:28:36 GMT FROM: Massimiliano de Pasquale at MSSL-UCL M. De Pasquale (MSSL/UCL) and J. K. Cannizzo (NASA/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 130505A 107 s after the BAT trigger (Cannizzo et al., GCN Circ. 14563). A bright but rapidly fading source is detected in the finding chart and initial exposures within the XRT error circle (Evans et al., GCN Circ. 14569). The preliminary UVOT position is: RA(J2000) = 09:08:14.64 = 137.0610 DEC(J2000) = +17:29:05.2 = +17.48478 with a 90%-confidence error radius of about 0.5 arc sec. Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white (FC) 107 256 147 14.14 0.05 white 3952 4151 197 17.96 0.07 v 4362 4561 197 17.50 0.11 b 3503 3946 197 17.71 0.08 u 320 542 218 14.66 0.04 uvw1 4772 4971 197 19.28 0.29 (~3 sigma) uvm2 4567 4766 197 >19.6 uvw2 4158 4357 197 >19.9 The non-detection of the optical source in um2 and uw2 filters is consistent with the redshift z=2.27 found by Tanvir et al (GCN Circ. 14567) The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.04 in the direction of the burst (Schlegel et al. 1998).
GCN 14575 table
GRB_name GRB130505A
GCN_number 14575
Detection_method Konus-Wind Det
t_trigger 8:22:27.038 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14575 SUBJECT: Konus-Wind observation of GRB 130505A DATE: 13/05/05 19:19:22 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 very intense GRB 130505A (Swift-BAT trigger #555136: Cannizzo et al., GCN 14564) triggered Konus-Wind (K-W) at T0=30147.038s UT (08:22:27.038). The K-W light curve shows a bright pulse with a duration of ~5s followed by a weaker decaying emission out to ~T0+30s with a slight increase in the count rate at ~T0+15s. The emission is seen up to ~10 Mev. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB130505_T30147/ As observed by Konus-Wind, the main phase of the burst had a fluence of (3.13 0.06)x10^-4 erg/cm2 and a 64-ms peak flux, measured from T0+2.496 s, of (6.9 0.3)x10^-5 erg/cm2/s (both in the 20 - 1200 keV energy range). The time-averaged spectrum (measured from T0 to T0+21.248 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 = -0.69 0.04, the high energy photon index beta = -2.03 0.03, the peak energy Ep = 631 31 keV, chi2 = 113/92 dof. The spectrum at the maximum count rate (measured from T0+2.304 to T0+2.816 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 = -0.31 0.09, the high energy photon index beta = -2.26 0.07, the peak energy Ep = 604 49 keV, chi2 = 105/90 dof. Assuming z=2.27 (Tanvir et al., GCN 14567) and a standard cosmology model with H_0 = 70 km/s/Mpc, Omega_M = 0.27, and Omega_Lambda = 0.73, the isotropic energy release E_iso is ~3.8x10^54 erg, the peak luminosity (L_iso)_max is ~2.7x10^54 erg/s, and the rest-frame peak energy Ep,i = 2030 keV All the quoted errors are estimated at the 1 sigma confidence level.
GCN 14576 table
GRB_name GRB130505A
GCN_number 14576
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 14576 SUBJECT: GRB 130505A: Largest E_iso ever measured DATE: 13/05/05 20:03:36 GMT FROM: Alexander Kann at TLS Tautenburg D. A. Kann (TLS Tautenburg), and S. Schulze (PUC, MCSS) report: Using the energetics provided by the Konus-Wind detection (Golenetskii et al. 2013, GCN 14575) of the extremely intense Swift GRB 130505A (Cannizzo et al. 2013, GCN 14564), and employing k-correction (Bloom et al. 2003, ApJ, 594, 674), we determine the isotropic energy release in the bolometric band (rest-frame 1 keV - 10 MeV) to be (5.65 +/- 0.13) x 10^54 erg (log E_iso = 54.75 +/- 0.01). The most isotropically energetic GRBs known so far (all in the rest-frame bolometric band) are GRBs 990123, 080916C and 090323, for which log E_iso ~ 54.5 - 54.6 has been found (e.g., Kann et al. 2010, ApJ, 720, 1513). This makes GRB 130505A the most energetic GRB known, and may indicate either an ultra-luminous event or a high degree of collimation. We additionally note that the nearby GRB 130427A (Maselli et al. 2013, GCN 14448; Golenetskii et al. 2013, GCN 14487) is also highly energetic, with log E_iso,bol = 54.21 +/- 0.05, but this is about 3.5 times less than GRB 130505A. This message may be cited.
GCN 14577 table
GRB_name GRB130505A
GCN_number 14577
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14577 SUBJECT: GRB 130505A: Swift-XRT refined Analysis DATE: 13/05/05 20:36:04 GMT FROM: Phil Evans at U of Leicester D.N. Burrows (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), G. Stratta (ASDC), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), J.A. Kennea (PSU), M.C. Stroh (PSU) and J.K. Cannizzo report on behalf of the Swift-XRT team: We have analysed 11 ks of XRT data for GRB 130505A (Cannizzo et al. GCN Circ. 14563), from 102 s to 29.4 ks after the BAT trigger. The data comprise 503 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN. Circ 14569). The late-time light curve (from T0+3.7 ks) can be modelled with a power-law decay with a decay index of alpha=1.06 (+0.03, -0.04). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.86 (+/-0.03). The best-fitting absorption column is 10.0 (+/-0.7) x 10^20 cm^-2, in excess of the Galactic value of 3.6 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 1.92 (+/-0.07) and a best-fitting absorption column of 8.8 (+1.6, -1.5) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.8 x 10^-11 (4.7 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 8.8 (+1.6, -1.5) x 10^20 cm^-2 Galactic foreground: 3.6 x 10^20 cm^-2 Excess significance: 5.6 sigma Photon index: 1.92 (+/-0.07) If the light curve continues to decay with a power-law decay index of 1.06, the count rate at T+24 hours will be 0.27 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x 10^-11 (1.3 x 10^-11) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00555163. This circular is an official product of the Swift-XRT team.
GCN 14578 table
GRB_name GRB130505A
GCN_number 14578
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 14578 SUBJECT: GRB 130505A: correction to GCN 14575 DATE: 13/05/05 21:14:09 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, on behalf of the Konus-Wind team, reports: We have found a typo in our GCN Circ. 14575 "Konus-Wind observation of GRB 130505A": the correct energy range for the K-W energy fluence and peak flux estimations for GRB 130505A is 20-10000 keV, not "20 - 1200 keV", as mentioned. The 20-10000 keV range is a standard for the K-W estimations of GRB energetics in the observer frame. We are sorry for the inconvenience.
GCN 14580 table
GRB_name GRB130505A
GCN_number 14580
Detection_method retraction
Circular_text TITLE: GCN CIRCULAR NUMBER: 14580 SUBJECT: GRB 130505A: E_iso record retraction DATE: 13/05/05 21:56:21 GMT FROM: Alexander Kann at TLS Tautenburg D. A. Kann (TLS Tautenburg), and S. Schulze (PUC, MCSS) report: Following the corrected Konus-Wind energy range (Frederiks, GCN 14578), we recalculated E_iso for GRBs 130505A and 130427A (affected by the same error in GCN 14487, Frederiks, GCN 14579), finding log E_iso,bol = 54.48 +/- 0.01 and 53.89 +/- 0.002, respectively. This makes GRB 130505A comparable to GRB 080916C, and still one of the most energetic GRBs ever discovered, but not the most energetic of all.
GCN 14585 table
GRB_name GRB130505A
GCN_number 14585
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 14585 SUBJECT: GRB 130505A: optical observations DATE: 13/05/06 02:27:34 GMT FROM: Alexei Pozanenko at IKI, Moscow Yu. Krugly (IA KhNU), I. Slyusarev (IA KhNU), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger collaboration: We observed a filed of the Swift GRB 130505A (Cannizzo et al. GCN 14563) with 0.7m telescope of Institute of Astronomy, Kharkiv National University between May 05 (UT) 20:52:35 - 21:19:57. A set of images of 180 s were taken in R-filter. In the combined image we clearly detect optical afterglow (Cannizzo et al., GCN 14563; Tanvir et al., GCN 14567; Kuroda et al., GCN 14568). Preliminary photometry is based on the nearby SDSS stars: T_start (UT) T0+ Filter Exp. OT mid,days s mag 2013-05-05T20:52:35 0.5309 R 8x180 19.4 +/- 0.07
GCN 14589 table
GRB_name GRB130505A
GCN_number 14589
Detection_method Swift-BAT Det
ra 137.0600°
decl 17.4850°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14589 SUBJECT: GRB 130505A, Swift-BAT refined analysis DATE: 13/05/06 17:01:01 GMT FROM: Amy Lien at GSFC A. Y. Lien (NASA/GSFC/ORAU), J. R. Cummings (GSFC/UMBC), T. Sakamoto (AGU), C. B. Markwardt (GSFC), S . D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. K. Cannizzo (NASA/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL), M. Stamatikos (OSU), E. Troja (NASA/GSFC/UMCP), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 130505A (trigger #555163) (Cannizzo, et al., GCN Circ. 14563). The BAT ground-calculated position is RA, Dec = 137.060, 17.485 deg which is RA(J2000) = 09h 08m 14s Dec(J2000) = +17d 29' 06" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 2%. The mask-weighted light curve starts at ~T-3 sec, peaks at ~T+0.3 sec, drops sginificantly at ~T+5 sec, and then has a long tail out to ~T+350 sec. T90 (15-350 keV) is 88 +- 10 sec (estimated error including systematics). The time-averaged spectrum from T-3.0 to T+363.3 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.18 +- 0.07. The fluence in the 15-150 keV band is 2.1 +- 0.1 x 10^-05 erg/cm2. The 1-sec peak photon flux measured from T+1.44 sec in the 15-150 keV band is 30.0 +- 3.1 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The spectral results may be skewed toward harder values because of the effects of the extreme partial coding. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/555163/BA/
GCN 14593 table
GRB_name GRB130505A
GCN_number 14593
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 14593 SUBJECT: GRB 130505A: Tautenburg afterglow observations DATE: 13/05/06 22:41:36 GMT FROM: Alexander Kann at TLS Tautenburg D. A. Kann, B. Stecklum, and F. Ludwig (TLS Tautenburg) report: We observed the optical afterglow (Cannizzo et al., GCN 14563) of the extremely luminous GRB 130505A (Cannizzo et al., GCN 14563; Golenetskii et al., GCN 14575) with the 1.34m Schmidt telescope of the Thueringer Landessternwarte Tautenburg equipped with a 4k CCD camera under good weather conditions. We obtained 3 x 300 sec frames in the Rc band. The afterglow is detected in each frame. For a nearby SDSS star (RA = 137.082047, Dec. = 17.486120), using the transformations of Lupton (2005), we find: B = 18.118, V = 17.080, Rc = 16.501, Ic = 15.967. Using this star for calibration, we derive a preliminary magnitude of Rc = 19.09 +/- 0.06 at 0.49118 days after the GRB. This message may be cited.
GCN 14595 table
GRB_name GRB130505A
GCN_number 14595
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14595 SUBJECT: GRB 130505A: RATIR Optical and NIR Observations DATE: 13/05/07 18:14:30 GMT FROM: Alan M. Watson at Instituto de Astronomia UNAM Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report: We observed the field of GRB 130505A (Cannizzo, et al., GCN Circular 14563) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on Sierra San Pedro Mrtir from 2013/05 7.13 to 2013/05 7.22 UTC (42.84 to 44.87 hours after the BAT trigger), obtaining a total of 0.36 hours exposure in the r' and i' bands and 0.14 hours exposure in the Z, Y, J, and H bands. The optical counterpart (Evans et al., GCN Circular 14569) is clearly identified. We obtain the following detections and 3-sigma upper limits: r' = 21.10 0.27 i' = 20.98 0.23 Z > 21.17 Y > 19.15 J > 18.38 H > 17.15 These magnitudes are in the AB system, are calibrated by comparison with SDSS DR8 and 2MASS, and not corrected for Galactic extinction in the direction of the GRB. The quoted uncertainties on the detections are 1 sigma. We thus confirm the fading reported by other observers at earlier epochs (Kuroda et al., GCN Circular 14568; Xu et al, GCN Circular 14570; Xin et al., GCN Circular 14571; Hentunen et al, GCN Circular 14572; Krugly et al., GCN Circular 14585; and Kann et al., GCN Circular 14593). No further observations of this source are planned. We thank the staff of the Observatorio Astronmico Nacional in San Pedro Mrtir.
GCN 14599 table
GRB_name GRB130505A
GCN_number 14599
Detection_method Suzaku WAM Det
redshift 2.2700
Circular_text TITLE: GCN CIRCULAR NUMBER: 14599 SUBJECT: GRB 130505A: Suzaku WAM observation of the prompt emission DATE: 13/05/08 04:30:49 GMT FROM: Makoto Tashiro at Saitama U/Swift T. Yasuda, M. Tashiro, Y. Terada, Y. Ishida, H. Ueno, S. Sugimoto (Saitama U.), M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.), M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki), K. Yamaoka (Nagoya U.), 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 bright, long GRB 13505A (GCN 14563; Cannizzo et al.) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at UT 08:22:24.527 (=T0). The observed light curve shows a bright peak followed by a weaker emission seen up to T0+30 s with a duration (T90) of about 14 seconds. The fluence in 100 - 1000 keV was 1.06 (+0.05/-0.05) x10^-4 erg/cm^2. The 1-s peak flux measured from T0+4 s was 53.1 (+2.0/-2.5) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-2 s to T0+30 s is well fitted by a GRB Band model as follows. the low-energy photon index alpha: -0.99 (+0.17/-0.11), the high-energy photon index beta: -2.33 (+0.06/-0.07), and the peak energy Epeak: 1094 (+131/-175) keV (chi^2/d.o.f = 23.9/23). Using a redshift of z = 2.27 (Tanvir et al., GCN 14567), we estimate the isotropic energy release in the 1 keV - 10 MeV range to be 2.55 (+0.12/- 0.11) x10^54 erg and the peak energy at the rest frame to be 3615 (+532/-469) keV, where cosmological parameters of the Omega matter, the Omega lambda and the Hubble constant are fixed at 0.27, 0.73 and 70 km/s/Mpc respectively. Due to the brightness of this burst, a 3% systematic error was added for low energy channels. All the quoted errors are at statistical 90% confidence level. 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
GCN 14602 table
GRB_name GRB130505A
GCN_number 14602
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 14602 SUBJECT: GRB 130505A: MITSuME Akeno Optical observation DATE: 13/05/08 11:41:21 GMT FROM: Taketoshi Yoshii at Tokyo Tech T. Yoshii, Y. Yatsu, Y. Yano, R. Usui, Y. Tachibana, K. Ito, S. Kurita, Y. Saito, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We observed GRB 130505A (Maselli et al., GCNC 14563) with an optical tri-color (g, Rc, and Ic) camera attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started at 2013-05-05 11:04:17 UT (9709 sec after the trigger). And we detected the previously reported afterglow . The measured magnitudes were listed below. T0+[MID] MID-UT T-EXP[sec] g' Rc Ic ----------------------------------------------------------------------------------------------------- 15550s 12:41:38 3480 18.8+/-0.1 18.9+/-0.2 18.0+/-0.1 ----------------------------------------------------------------------------------------------------- T-EXP: Total Exposure time [sec] (The photon flux were calibrated against GSC2.3 catalog.)