GRB080413A

This page lists all entries on GRB080413A in GRBweb

Summary IPN Swift GCN 7593 GCN 7594 GCN 7595 GCN 7596 GCN 7597 GCN 7602 GCN 7603 GCN 7604 GCN 7605 GCN 7607 GCN 7609 GCN 7614 GCN 7616 GCN 7622 GCN 7624 GCN 7625 GCN 7630

Summary table
Variable Value Source
T0 2:54:19 UTC GCN_circulars,Swift Det
ra 287.2990° Swift
decl -27.6779° Swift
pos_error 6.47e-05° Swift
T90 46.0 s Swift
T90_start 2:54:19 UTC Swift
fluence 3.50e-06 erg/cm² Swift
redshift 2.4330
T100 46.0 s
GBM_located False
mjd 54569.12105324074 GCN_circulars,Swift Det
IPN table
GRB_name GRB080413A
ra 287.2917°
decl -27.6833°
pos_error 5.00e-02°
redshift 2.4330
Swift table
GRB_name GRB080413A
t_trigger 2:54:19 UTC
ra 287.2990°
decl -27.6779°
pos_error 6.47e-05°
T90 46.0 s
fluence 3.50e-06 erg/cm²
redshift 2.4330
GCN 7593 table
GRB_name GRB080413A
GCN_number 7593
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7593 SUBJECT: GRB 080413: ROTSE-III Detection of Optical Counterpart DATE: 08/04/13 03:03:03 GMT FROM: Wiphu Rujopakarn at U AZ/Steward GRB 080413: ROTSE-III Detection of Optical Counterpart E.S. Rykoff (UCSB), W. Rujopakarn (Steward), report on behalf of the ROTSE collaboration: ROTSE-IIIc, located at the H.E.S.S. site at Mt. Gamsberg, Namibia, responded to GRB 080413A (Swift trigger 309096). The first image was at 02:54:39.7 UT, 20.4 s after the burst (6.7 s after the GCN notice time). The unfiltered images are calibrated relative to USNO A2.0. We detect a 12.8 magnitude, fading source with coordinates: 19:09:11.8 -27:40:41.6 (J2000), with positional uncertainty of 1' or better start UT mag mlim(of image) ---------------------------------- 02:54:39.7 12.8 15.3 This source is not visible in DSS (second epoch), 2MASS or the MPChecker database. A jpeg image is available at http://www.rotse.net/images/gsb309096_3c00_img.jpg Note that the object marked 7 is the candidate in question. Continuing observations are in progress.
GCN 7594 table
GRB_name GRB080413A
GCN_number 7594
Detection_method Swift Det
t_trigger 2:54:19 UTC
ra 287.2900°
decl -27.6790°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7594 SUBJECT: GRB 080413: Swift detection of a burst with an optical afterglow DATE: 08/04/13 03:06:53 GMT FROM: David Palmer at LANL A. P. Beardmore (U Leicester), D. N. Burrows (PSU), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC), S. D. Hunsberger (PSU), J. A. Kennea (PSU), C. B. Markwardt (CRESST/GSFC/UMD), K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC), M. Stamatikos (NASA/ORAU) and E. Troja (U Leicester/INAF-IASFPA) report on behalf of the Swift Team: At 02:54:19 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 080413 (trigger=309096). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 287.290, -27.679 which is RA(J2000) = 19h 09m 10s Dec(J2000) = -27d 40' 44" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a triple-peaked structure with a duration of about 55 sec. The peak count rate was ~10000 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 02:55:20.0 UT, 60.7 seconds after the BAT trigger. XRT found a bright, fading uncatalogued X-ray source located at RA, Dec 287.2978, -27.6779 which is equivalent to: RA(J2000) = 19h 09m 11.4s Dec(J2000) = -27d 40' 40.4" with an uncertainty of 4.7 arcseconds (radius, 90% containment). This location is 25 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to assess possible redshift constraints using X-ray spectroscopy and the nH-z relation from Grupe et al. (2007). UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm) filter starting 76 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 19:09:11.76 = 287.2990 DEC(J2000) = -27:40:40.1 = -27.6778 with a 1-sigma error radius of about 0.6 arc sec. This position is 3.9 arc sec. from the center of the XRT error circle. The estimated magnitude is 15.2 with a 1-sigma error of about 0.5 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.16.
GCN 7595 table
GRB_name GRB080413A
GCN_number 7595
Detection_method Optical
ra 287.2994°
decl -27.6786°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7595 SUBJECT: GRB 080413: TAROT Calern observatory optical observations DATE: 08/04/13 03:54:16 GMT FROM: Alain Klotz at CESR-CNRS Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. (LATT-OMP) report: We imaged the field of GRB 080413 detected by SWIFT (trigger 309096) with the TAROT robotic telescope (D=25cm) located at the Calern observatory, France. The observations started 21.8s after the GRB trigger (8.3s after the notice). The elevation of the field increased from from 11 degrees above horizon and weather conditions were poor at the beginning of observations. The first image showing stars started 480s after the trigger. We detected the candidate couterpart mentioned by Rykoff et al. (GCNC 7593) at the following position (+/- 2 arcsec): RA(J2000) = 19h 09m 11.85s DEC(J2000) -27d 40' 43.0" Unfiltered magnitudes are: t0+480s to t0+570s : R > 12.5 t0+1174s to t0+1263s : R = 15.0 +/- 0.2 t0+1470s to t0+1650s : R = 15.3 +/- 0.2 t0+2035s to t0+2215s : R = 15.5 +/- 0.2 Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. N.B. Galactic coordinates are lon= 9.5236 lat=-15.8249 and the galactic extinction in R band is 2.4 magnitudes estimated from D. Schlegel et al. 1998ApJ...500..525S. This message may be cited.
GCN 7596 table
GRB_name GRB080413A
GCN_number 7596
Detection_method Swift-XRT Det
ra 287.2983°
decl -27.6781°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7596 SUBJECT: GRB 080413: Enhanced Swift-XRT position DATE: 08/04/13 06:42:02 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 176 s of overlapping XRT Photon Counting mode and UVOT data for GRB 080413, 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 = 287.29829, -27.67807 which is equivalent to: RA (J2000): 19h 09m 11.59s Dec (J2000): -27d 40' 41.1" with an uncertainty of 2.3 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 http://www.swift.ac.uk/xrt_positions/Goad.pdf), the current algorithm is an extension of this method. This circular was automatically generated, and is an official product of the Swift-XRT team.
GCN 7597 table
GRB_name GRB080413A
GCN_number 7597
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7597 SUBJECT: GRB 080413A: REM detection of the NIR Afterglow DATE: 08/04/13 09:06:15 GMT FROM: Angelo Antonelli at Obs. Astro. di Roma L.A. Antonelli, P. D'Avanzo, D. Malesani, S. Covino, D. Fugazza, L. Calzoletti, S. Campana, G. Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F. D'Alessio, F. Fiore, P. Goldoni, D. Guetta, C. Guidorzi, G.L. Israel, E. Maiorano, N. Masetti, A. Melandri, E.J.A. Meurs, L. Nicastro, E. Palazzi, E. Pian, F. Piranomonte, S. Piranomonte, L. Stella, G. Stratta, G. Tagliaferri, G. Tosti, V. Testa, S.D. Vergani, and F. Vitali, report on behalf of the REM team: The robotic 60-cm REM telescope located at La Silla (Chile) observed automatically the field of the GRB 080413A (Beardmore et al., GCN 7594) starting about 1.3 hours after the burst due to object visibility constraints. Observation started as soon as the object is risen so the Airmass was large. A preliminary investigation of our earliest images (R,z,J,H,K) showed that the candidate optical counterpart (Rykoff et al. GCN 7593, Beardmore et al., GCN 7594, Klotz et al., GCN 7595) is observed in all bands. At the beginning of REM observation, the object had a H mag of about H=15.2 calibrated against 2MASS and not corrected for galactic extinction. This message may be cited.
GCN 7602 table
GRB_name GRB080413A
GCN_number 7602
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7602 SUBJECT: GRB 080413A: VLT/UVES redshift DATE: 08/04/13 12:10:21 GMT FROM: Christina Thoene at Niels Bohr Institute,DARK Cosmo Ctr Christina C. Thoene, Daniele Malesani, Paul M. Vreeswijk, Johan P. U. Fynbo (DARK/NBI), Pall Jakobsson (Univ. of Hertfordshire), Cedric Ledoux and Alain Smette (ESO) report on behalf of a larger collaboration: We observed the afterglow of GRB 080413A (GCN 7593, Rykoff & Rujopakarn; GCN 7594, Stamatikos et al.) on Apr. 13 starting UT 06:36 with UVES at the VLT. Spectra of 2700 s with low S/N were acquired in the DIC 2R and 2B settings covering the wavelength range between 3250 and 9000 AA. We detect several narrow absorption features including SII, Si II, CII, Fe II, AlII, C IV, Si IV as well as broad Lyman alpha absorption at the highest redshift system which has z=2.433 and is very likely the redshift of GRB 080413A. We thank the Paranal staff for executing the observations, in particular Swetlana Hubrig and Jose Cortes.
GCN 7603 table
GRB_name GRB080413A
GCN_number 7603
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7603 SUBJECT: GRB 080413A Bootes observation DATE: 08/04/13 12:50:49 GMT FROM: Petr Kubanek at AIO P. Kubanek, M. Jelinek, J. Gorosabel, A. J. Castro-Tirado (IAA-CSIC Granada), L. Sabau-Graziati (INTA Madrid), A. de Ugarte Postigo (ESO Santiago), R. Hudec (ASU-CAS Ondrejov), P. Perez-Gonzalez and J. Zamorano (UCM Madrid) report on behalf of a larger collaboration: The BOOTES-1 0.3m telescope in South Spain observed GRB 080413A, starting at 02:55:20 UT (46 sec after receiving trigger, 1 minute after GRB). A sequence of preprogrammed 6 sec, 20 and 60 sec exposures was obtained. The optical counterpart reported by Rykoff at al. (GCN 7593) is clearly detected on the initial exposures. Further data were obtained at the 2.5m NOTin La Palma under non-optimal conditions.
GCN 7604 table
GRB_name GRB080413A
GCN_number 7604
Detection_method Swift-BAT Det
ra 287.3010°
decl -27.6770°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7604 SUBJECT: GRB 080413A, Swift-BAT refined analysis DATE: 08/04/13 15:58:16 GMT FROM: Scott Barthelmy at NASA/GSFC J. Tueller (GSFC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), D. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), T. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+454 sec from recent telemetry downlinks, we report further analysis of BAT GRB 080413A (trigger #309096) (Beardmore, et al., GCN Circ. 7594). The BAT ground-calculated position is RA, Dec = 287.301, -27.677 deg, which is RA(J2000) = 19h 09m 12.1s Dec(J2000) = -27d 40' 36.8" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 81%. The mask-weighted light curve shows four peaks. The first starting at T-0.1 sec, peaking at T+2.0 sec. The second peak overlaps with the first and peaks at ~T+7 sec. The third and fourth peaks are well separated with peaks at T+16 and T+47 sec, repsectively. The lightcurve returns to baseline at ~T+80 sec. T90 (15-350 keV) is 46 +- 1 sec (estimated error including systematics). The time-averaged spectrum from T-0.1 to T+50.3 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.57 +- 0.06. The fluence in the 15-150 keV band is 3.5 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+1.64 sec in the 15-150 keV band is 5.6 +- 0.2 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/309096/BA/
GCN 7605 table
GRB_name GRB080413A
GCN_number 7605
Detection_method Swift-XRT Other
redshift 2.4330
Circular_text TITLE: GCN CIRCULAR NUMBER: 7605 SUBJECT: GRB 080413A: Swift-XRT refined analysis DATE: 08/04/13 16:39:02 GMT FROM: Phil Evans at U of Leicester P.A. Evans, K.L. Page, A.P. Beardmore, R.L.C. Starling (U. Leicester) and F.E. Marshall (NASA/GSFC) report on behalf of the Swift-XRT team: We have analysed 5.2 ks of Swift XRT data for GRB 080413A (Beardmore et al. GCN Circ. 7594), from T0+67 s to T0+21000 s. The first 186 s of data were obtained in Windowed Timing (WT mode); the remainder in Photon Counting mode. The best XRT position for this object is the UVOT-enhanced position given in Osborne et al. (GCN Circ. 7596). The X-ray light curve is well fitted by a power-law decay, with an initial decay slope of 2.87 (+/- 0.19) up to T0+175 (+23/-16) s, at which point the decay shallows to a slope of 1.10 (+0.06/-0.07). A spectrum obtained from all of the WT mode data can be modelled with an absorbed power-law with a photon index gamma=3.12 (+0.16/-0.15). A redshifted absorbing column of 1.53 (+0.43/-0.38) x 10^22 cm^-2, at a redshift of z=2.433 (Thoene et al. GCN Circ 7602) is necessary in addition to the Galactic column of 8.71 x 10^20 cm^-2 (Kalberla et al. 2005). The observed (unabsorbed) 0.3-10 keV flux in this spectrum is 4.1 x 10^-10 (1.71 x 10^-9) erg cm^-2 s^-1. If the source continues to decay at the present rate, we predict a count rate of 3.51 x 10^-3 count/sec at T0+24 hours, which correponds to a 0.3-10 keV observed (unabsorbed) flux of 9.54 x 10^-14 (2.72 x 10^-13) erg cms^-2 s^-1. This circular is an official product of the Swift-XRT team.
GCN 7607 table
GRB_name GRB080413A
GCN_number 7607
Detection_method Swift-UVOT Det
ra 287.2990°
decl -27.6779°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7607 SUBJECT: GRB080413A: Swift/UVOT observations DATE: 08/04/13 17:49:17 GMT FROM: Samantha Oates at MSSL S. R. Oates and F. E. Marshall report on behalf of the Swift/UVOT team. The Swift/UVOT observed the field of GRB 080413A starting at 77s after the BAT trigger (Beardmore et al., GCN 7594). We detect the afterglow in white,v,b and u filters at the position: RA(J2000) = 19:09:11.76 DEC(J2000) = -27:40:40.27 with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence). This position is consistent with the enhanced XRT position and the position reported by ROSTE-III (Rykoff et al., GCN 7593). The magnitudes and 3 sigma upper limits are reported below: Filter T_Mid(s) Expo(s) Magnitude/3sigUL ----------------------------------------------------- White 126 98 15.37 +/- 0.01 White 5478 197 19.74 +/- 0.17 v 268 169 15.08 +/- 0.03 v 5888 197 19.16 +/- 0.51 b 5273 197 19.33 +/- 0.21 u 5068 197 19.05 +/- 0.22 w1 4863 197 >19.55 m2 4658 197 >19.48 w2 5684 197 >19.57 ----------------------------------------------------- The above magnitudes are not corrected for the Galactic extinction corresponding to a reddening of E_{B-V} = 0.16 mag (Schlegel et al., 1998, ApJS, 500, 525). The photometry is on the UVOT flight system described in Poole et al. (2008,MNRAS,383,627).
GCN 7609 table
GRB_name GRB080413A
GCN_number 7609
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7609 SUBJECT: GRB 080413a, SMARTS optical/IR afterglow observations DATE: 08/04/13 19:22:38 GMT FROM: Bethany Cobb at Yale U B. E. Cobb (Yale), part of the larger SMARTS consortium, reports: Using the ANDICAM instrument on the 1.3m telescope at CTIO, we obtained optical/IR imaging of the error region of GRB 080413a (GCN 7594, Beardmore et al.), starting at 2008-04-13 05:48 UT, which is ~2.9 hours post-burst. Several dithered images were obtained in each filter, with total summed exposure times of 180s in each of BRIYJK and 120s in each of H and V. The GRB afterglow (GCN 7593 Rykoff & Rujopakarn; GCN 7594, Beardmore et al.) is detected in all our images. At a mid-exposure time of 2008-04-13 06:02 (~3.1 hours post-burst) the afterglow has the following magnitudes (which have not been corrected for Galactic reddening): B= 20.88 +/- 0.10 V= 20.25 +/- 0.11 R= 19.25 +/- 0.05 I= 18.84 +/- 0.06 J= 18.23 +/- 0.23 H= 17.05 +/- 0.15 K= 16.19 +/- 0.12 Optical photometry is calibrated against Landolt standard stars and IR photometry is calibrated against 2MASS stars in the field. Between 3.1 and 5.1 hours post burst, the afterglow decays by ~0.75 magnitudes, indicating an approximate decay rate of alpha = -1.4 (where afterglow flux is proportional to t^alpha).
GCN 7614 table
GRB_name GRB080413A
GCN_number 7614
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7614 SUBJECT: VLA radio observations of GRB 080413A DATE: 08/04/14 14:33:02 GMT FROM: Poonam Chandra at U Virginia/NRAO Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on behalf of the Caltech-NRAO-Carnegie GRB Collaboration: "We used the Very Large Array to observe the field of view toward GRB 080413A (GCN 7594) at a frequency of 8.46 GHz at 2008 April 14.53 UT. We do not detect the GRB afterglow at the ROTSE optical position (GCN 7593). The flux density at the GRB afterglow position is -61 +/- 49 uJy. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc."
GCN 7616 table
GRB_name GRB080413A
GCN_number 7616
Detection_method Other
redshift 2.4300
Circular_text TITLE: GCN CIRCULAR NUMBER: 7616 SUBJECT: GRB 080413A: Gemini-South Spectroscopy DATE: 08/04/14 17:27:38 GMT FROM: Antonino Cucchiara at PSU A. Cucchiara and D. B. Fox (Penn State) with S. B. Cenko (Caltech), report on behalf of a larger collaboration: "Starting on 2008 April 13.27 UT we observed GRB 080413A (GCN 7593 and 7594) with the GMOS spectrograph on the Gemini South telescope. We obtained 2x1200-sec spectra in the wavelength range 3900-8000A. The resolution of our spectrum is 5.2 Ang/pixel (R ~1200 at 6000A). We clearly observe several metal absorption features corresponding to the SiIV (1393,1402 A), CIV (1548, 1550A), SiII (1526A), and AlII (1670A) transitions. A Lyman break is also present at the blue edge of our spectra (~ 4170A). These identifications are consistent with a host galaxy redshift of z = 2.43, confirming the result reported from VLT observations by Thoene et al.(GCN 7602)."
GCN 7622 table
GRB_name GRB080413A
GCN_number 7622
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7622 SUBJECT: GRB 080413A: MOA-II optical afterglow observations DATE: 08/04/15 23:48:14 GMT FROM: Nobuyuki Kawai at Tokyo Tech A. Fukui, Y. Itow, T. Sumi (STE Lab, Nagoya Univ.), and P. Tristram (Canterbury Univ.) on behalf of the MOA Collabration (Bond et al. 2001, Sumi et al. 2003) report: We observed the optical afterglow of GRB080413A (GCN 7593, Rykoff & Rujopakarn; GCN 7594, Beardmore et al.) on Apr. 13 between 12:29:16.4 UTC and 14:13:06.6 UTC, corresponding to about 9.5-11 h after the burst, with the 1.8m MOA-II telescope at Mt. John observatory in New Zealand. Total 5 images were obtained with a wide- band Red filter (center wavelength ~ 750nm and FWHM ~ 250nm) and we could identify the faint afterglow within the error circle (<0.5"). The identified R.A. Dec. are 19:09:11.752 -27:40:39.99 with an uncertainty of 0.14" (radius, 1sigma) and following are the photometric results: I magnitude = 20.24 +/- 0.32 at the mid-exposure time of 2008-04-13 12:29:16.4 UTC, 20.09 +/- 0.19 at 12:51:10.7 UTC, 21.40 +/- 0.61 at 13:03:0.1 UTC, 20.05 +/- 0.17 at 13:42:47.0 UTC, and 20.75 +/- 0.25 at 14:13:06.6 UTC. These photometry were done by using the IRAF and calibrated against the USNO-B1.0 catalog stars, and not corrected for the Galactic extinction. [GCN OPS NOTE(18apr08): By the moderator's choice, the "GCN 7594, Stamatikos et al" wash changed to "GCN 7594, Beardmore et al". Ack to F. Marshall.]
GCN 7624 table
GRB_name GRB080413A
GCN_number 7624
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 7624 SUBJECT: GRB 080413A: Suzaku WAM observation of the prompt emission DATE: 08/04/16 16:11:23 GMT FROM: Kazutaka Yamaoka at Aoyama Gakuin U T. Enoto (Univ. of Tokyo), Y.E. Nakagawa, T. Tamagawa (RIKEN), T. Uehara, T. Takahashi, Y. Fukazawa, C. Kira, Y. Hanabata (Hiroshima U.), K. Yamaoka, S. Sugita (Aoyama Gakuin U.), M. Tashiro, Y. Terada, Y. Urata, A. Endo, K. Onda, N. Kodaka, K. Morigami (Saitama U.), K. Nakazawa, K. Makishima (Univ. of Tokyo), E. Sonoda, M. Yamauchi, H. Tanaka, R. Hara (Univ. of Miyazaki), M. Ohno, M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: The long GRB 080413A (Swift/BAT trigger #309096 ; Beardmore et al., GCN 7594) was detected by the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 02:54:18.648 UT (=T0). The observed light curve shows a clear double-peaked structure at T0+2s and T0+16s, and possible weak peak at T0+45s, with a total duration (T90) of about 19 seconds. The fluence in 150 - 1000 keV was (2.2 +/- 0.5) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0+2s was 0.77 +/- 0.19 photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0+0s to T0+20s is fitted by a single power-law with a photon index of 2.4 +/- 0.4 (chi^2/d.o.f = 15.1/10) in 150 - 1000 keV. All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves with 1-sec time resolution for this burst are now available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html
GCN 7625 table
GRB_name GRB080413A
GCN_number 7625
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7625 SUBJECT: GRB 080413A: Liverpool Telescope and Faulkes Telescope South optical observations DATE: 08/04/16 17:23:09 GMT FROM: Andreja Gomboc at LT,ARI,Liverpool JMU A. Gomboc (Ljubljana), C. Guidorzi (U. Bicocca/INAF-OAB), A. Melandri, I.A. Steele, C.G. Mundell, D.F. Bersier, M.F. Bode, M.J. Burgdorf, S.N. Fraser, S. Kobayashi, C.J. Mottram, R.J. Smith (Liverpool JMU), P. O'Brien, N. Bannister, N. Tanvir (U. Leicester) report on behalf of larger GRB collaboration: The Liverpool Telescope observed the field of GRB 080413A (trigger=309096, Beardmore et al. GCN 7594) under poor weather conditions starting 2-hr after the trigger. Observations continued with the Faulkes Telescope South. In our coadded frames we do not detect any source at the position of the optical afterglow (Beardmore et al. GCN 7594, Rykoff & Rujopakarn GCN 7593) down to the limiting magnitudes reported below. Telescope Filter Tstart(hr) Tstop(hr) Exposure(s) M_lim ---------------------------------------------------------------------- Liverpool R 2.0 2.5 760 15.7 Faulkes South R 12.2 12.2 30 19.2 I 12.2 13.1 2080 21.7 ---------------------------------------------------------------------- Magnitudes were calibrated with respect to USNOB1 R2 and I.
GCN 7630 table
GRB_name GRB080413A
GCN_number 7630
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 7630 SUBJECT: GRB 080413A: Suzaku/WAM and Swift/BAT joint spectral analysis DATE: 08/04/18 21:50:05 GMT FROM: Takanori Sakamoto at NASA/GSFC M. Ohno, M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA) K. Yamaoka, S. Sugita (Aoyama Gakuin U.), T. Enoto (Univ. of Tokyo), Y.E. Nakagawa, T. Tamagawa (RIKEN), T. Uehara, T. Takahashi, Y. Fukazawa, C. Kira, Y. Hanabata (Hiroshima U.), M. Tashiro, Y. Terada, Y. Urata, A. Endo, K. Onda, N. Kodaka, K. Morigami (Saitama U.), K. Nakazawa, K. Makishima (Univ. of Tokyo), E. Sonoda, M. Yamauchi, H. Tanaka, R. Hara (Univ. of Miyazaki), , S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: J. Tueller (GSFC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), D. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), T. Ukwatta (GWU) (i.e. the Swift-BAT team): report: We performed the Suzaku/WAM and Swift/BAT joint fit spectral analysis of GRB 080413A (Swift/BAT trigger #309096; Beardmore et al., GCN 7594). The time interval of the spectral data for each instrument is chosen from T0(WAM)-1 to T0(WAM)+22 sec where T0(WAM) is the trigger time of WAM at 02:54:18.648 UTC. This time interval includes the initial two peaks, but not the relatively soft third peak around T0(WAM)+45 sec which is clearly visible in the BAT data (Tueller et al., GCN 7604). The energy ranges which we used in the joint spectral analysis are 13-150 keV and 150-1000 keV for Swift/BAT and Suzaku/WAM respectively. The spectral data of two instruments are fit with the spectral model multiplied by the constant factor to take into account the systematic uncertainties in the response matrices of each instrument. The spectrum is well fit with a power-law with exponential cutoff model (dN/dE ~ E^{alpha} * exp(-(2+alpha)*E/Epeak)). The constant factors of each instrument agree within 20%. No systematic residual from the best fit model is seen in the spectral data of each instrument. The best fit spectral parameters are: alpha = -1.2 +- 0.1 and Epeak = 170 (-40/+80) keV (chi2/dof = 75/73). The energy fluence in the 15-1000 keV band calculated by a power-law with exponential cutoff model for this 23 sec interval is 4.8 (-1.2/+0.4) x 10^-6 erg/cm2 (assuming the constant factor of the BAT is fixed to 1). Assuming z = 2.433 (Thoene et al., GCN 7602) and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, Omega_\Lambda = 0.73, the isotropic energy release is E_iso ~8x10^52 erg in 1 keV to 10 MeV at the GRB rest frame. All the quoted errors are at the 90% confidence level.