GRB080319C

This page lists all entries on GRB080319C in GRBweb

Summary IPN Swift GCN 7441 GCN 7442 GCN 7443 GCN 7454 GCN 7457 GCN 7460 GCN 7468 GCN 7475 GCN 7477 GCN 7483 GCN 7487 GCN 7497 GCN 7508 GCN 7517

Summary table
Variable Value Source
T0 12:25:56 UTC GCN_circulars,Swift Det
ra 258.9812° Swift
decl 55.3918° Swift
pos_error 6.86e-05° Swift
T90 34.0 s Swift
T90_start 12:25:56 UTC Swift
fluence 3.60e-06 erg/cm² Swift
redshift 1.9500 GCN_circulars,Other
T100 34.0 s
GBM_located False
mjd 54544.518009259256 GCN_circulars,Swift Det
IPN table
GRB_name GRB080319C
ra 258.9750°
decl 55.4167°
pos_error 5.00e-02°
redshift 1.9500
Swift table
GRB_name GRB080319C
t_trigger 12:25:56 UTC
ra 258.9812°
decl 55.3918°
pos_error 6.86e-05°
T90 34.0 s
fluence 3.60e-06 erg/cm²
redshift 1.9500
GCN 7441 table
GRB_name GRB080319C
GCN_number 7441
Detection_method Other
ra 258.9814°
decl 55.3919°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7441 SUBJECT: GRB 080319C: KAIT OA candidate DATE: 08/03/19 12:33:15 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS W. Li, R. Chornock, and A. V. Filippenko, University of California at Berkeley, on behalf of the KAIT GRB team, report: KAIT responded to GRB 080319C (Swift trigger 306778) and was taking images. There is an afterglow candidate at position RA = 17:15:55.54 DEC = +55:23:30.8 (equinox J2000) The measured magnitude is R = 17.4 at 12:27:55 UT. Further observations are ongoing.
GCN 7442 table
GRB_name GRB080319C
GCN_number 7442
Detection_method Swift Det
t_trigger 12:25:56 UTC
ra 258.9730°
decl 55.4100°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7442 SUBJECT: GRB 080319C: Swift detection of a burst with an optical afterglow DATE: 08/03/19 12:45:58 GMT FROM: Scott Barthelmy at NASA/GSFC C. Pagani (PSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), D. N. Burrows (PSU), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), O. Godet (U Leicester), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), V. Mangano (INAF-IASFPA), J. P. Osborne (U Leicester), K. L. Page (U Leicester), A. M. Parsons (GSFC), J. L. Racusin (PSU), B. Sbarufatti (INAF-IASFPA), M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester), G. Stratta (ASDC) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 12:25:56 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 080319C (trigger=306778). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 258.973, +55.410 which is RA(J2000) = 17h 15m 54s Dec(J2000) = +55d 24' 35" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows several overlapping FRED-like peaks starting at T+0 and ending around T+20 sec. The peak count rate was ~8000 counts/sec (15-350 keV), at ~T+0 sec after the trigger. The XRT began observing the field at 12:29:40 UT, 224 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 258.9828, 55.3920 which is equivalent to: RA(J2000) = 17h 15m 55.86s Dec(J2000) = +55d 23' 31.2" with an uncertainty of 4.5 arcseconds (radius, 90% containment). This location is 3 arcseconds from the optical afterglow candidate position. UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm) filter starting 227 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 17:15:55.51 = 258.9813 DEC(J2000) = +55:23:30.8 = +55.3919 with a 1-sigma error radius of about 0.5 arc sec. This position is 67.4 arc sec. from the center of the BAT error circle. This is consistent with the KAIT position (Li et al., 2008, GCNC 7441). The estimated magnitude is white = 18.8 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 0.03. Burst Advocate for this burst is C. Pagani (pagani AT astro.psu.edu). 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 7443 table
GRB_name GRB080319C
GCN_number 7443
Detection_method Other
ra 258.9654°
decl 55.3940°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7443 SUBJECT: GRB 080319C: Early Super-LOTIS Observations DATE: 08/03/19 13:30:10 GMT FROM: Grant Williams at Steward Observatory G. G. Williams (MMTO) and P. A. Milne (Steward Observatory), on behalf of the Super-LOTIS Collaboration, report: The robotic 0.6-m Super-LOTIS telescope began observing the error box of GRB 080319C (Swift Trigger 306778, Pagani et al. GCN 7442) at 12:26:38.5 UT, 42.5 seconds after the trigger. Our initial observations include 5 x 10s exposures, 5 x 20s exposures, and 30 x 60s exposures, all in the R-band. We detect the afterglow reported by Li et al. (GCN 7441) in our earliest 10 second exposure. Using the USNO-B1.0 star (453-025776) at RA=17:15:51.7, Dec=55:23:38.4 with R2MAG=14.61, we estimate the following R-band magnitude for the OT: t_start (UT) exp t (s) t_start-t_0 (s) R Mag ---------------------------------------------------------------- 12:26:38.5 10 42.5 R = 16.83 +/- 0.13 Additional observations and analysis are ongoing.
GCN 7454 table
GRB_name GRB080319C
GCN_number 7454
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7454 SUBJECT: GRB 080319C: MASTER-VWF-Kislovodsk optical observation DATE: 08/03/19 17:46:32 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs MASTER-Net Team: V. Lipunov, V.Kornilov, D.Kuvshinov, E.Gorbovskoy, N.Tyurina, A.Belinski, A.Krylov, N.Shatskiy, A.Sankovich, V.Vladimirov, P.Gritsyk, V.Vibornov, A.Kuznetsov, P.Balanutsa Sternberg Astronomical Institute, Moscow Union 'Optic' A. Tlatov, I.Golubov Kislovodsk Solar Station of the Pulkovo observatory K.Ivanov Irkutsk State University I.Zalognikh Ural State University, Kourovka MASTER Very Wide Field Camera located at Kislovodsk Solar Station (http://observ.pereplet.ru, D=70 mm, 420 square degrees, 11 Mpixel's CCD) has moved to the Swift-BAT trigger 306793 and it has taken a series of 5s exposures starting 92 s after notice arrivel time 708 s after GRB time at 17 16 57 UT under good weather condition and moon. There is no OT was found inside Swift error box brighter than 11.5m. MASTER-Net team congratulate "Pi of the Sky" - Team with wonderfull and long-awaited result (Cwiok et al. GCN 7445)! This message can be cited. Mailto: lipunov@sai.msu.ru
GCN 7457 table
GRB_name GRB080319C
GCN_number 7457
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7457 SUBJECT: GRB 080319C: AGILE-MCAL observation of the prompt emission DATE: 08/03/19 19:09:02 GMT FROM: Sandro Mereghetti at IASF/CNR M. Marisaldi (INAF/IASF Bologna), F. Fornari (INAF/IASF Milano), C. Labanti, F. Fuschino, M. Galli, A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco (INAF/IASF Bologna), E. Costa, E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci, I. Lapshov, F. Lazzarotto, L. Pacciani, M. Rapisarda, P. Soffitta (INAF/IASF Roma), A. Giuliani, S. Vercellone, A. Chen, S. Mereghetti, A. Pellizzoni, F. Perotti, M. Fiorini, P. Caraveo (INAF/IASF Milano), M. Tavani, G. Pucella, F. D'Ammando, V. Vittorini, A. Argan, A. Trois (INAF/IASF Rome), G. Barbiellini, F. Longo, E. Vallazza (INFN Trieste), P. Picozza, A. Morselli (INFN Roma-2), M. Prest (Universita' dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), and P. Giommi, C. Pittori, (ASDC) and L. Salotti (ASI), on behalf of the AGILE Team, report: "The Swift localized GRB 080319C (Pagani et al., GCN 7442) triggered the Mini-Calorimeter (MCAL) instrument onboard the AGILE satellite at 12:25:56 UT (=T0). The MCAL instrument covers the energy range 350 keV - 10 MeV, without imaging capabilities. The MCAL light curve shows two main overlapping broad peaks, the first peaking at T0 and the second peaking at T0+9s in the 350-700 keV energy band. Above 700 keV only the first peak is still detected, with 5 sigma detection also in the 1.4-2.8 MeV energy band. Using the preliminary in-flight calibration, we can estimate the 1-s peak flux in the 350-700 keV energy band at T0 to be 2.0(-0.8,+0.9) photons/cm2/s. The Swift localization is out of the field of view of the AGILE Gamma-Ray Imaging Detector (GRID), sensitive in the 50 MeV - 50 GeV energy range. Analysis of the GRID count rate does not show any detection. The event was well outside of the SuperAGILE field of view as well, but the event passed through the collimator shield and was weakly detected in the count rate." We incidentally note that the brighter GRB 080319B (Racusin et al. GCN 7427) was not observed by the AGILE instruments due to Earth occultation. This message may be cited.
GCN 7460 table
GRB_name GRB080319C
GCN_number 7460
Detection_method Swift-XRT Other
ra 258.9798°
decl 55.3920°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7460 SUBJECT: GRB 080319C: Swift-XRT Team Refined Analysis DATE: 08/03/19 20:13:43 GMT FROM: Claudio Pagani at PSU/Swift-XRT C. Pagani, J. L. Racusin, J.A. Kennea, D. N. Burrows (PSU) and P. A. Evans (U Leicester) report on behalf of the Swift-XRT team: The Swift-XRT started observing GRB 080319C (trigger=306778, Pagani et al. GCN 7442) at 12:29:40 UT, 224 seconds after the BAT trigger. The Swift slew to the burst was delayed because of an Earth constraint. The current dataset consist of 2.2ks of Photon Counting mode data from the first orbit of observation. Using 595 s of overlapping XRT Photon Counting mode and UVOT data, 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 = 258.97980, 55.39197 which is equivalent to: RA (J2000): 17 15 55.15 Dec (J2000): +55 23 31.1 with an uncertainty of 1.7 arcsec (radius, 90% confidence). The 0.3-10 keV X-ray light curve starts at a count rate of ~7 counts/s and peaks at ~18 counts/s at T+360 seconds, after which it shows a decline with a decay slope of 0.9 +/- 0.1 with hints of superimposed flaring activity. The spectrum of the PC data can be well fit by an absorbed powerlaw with photon index 1.73 +/- 0.06 and column density of (1.5 +/- 0.1)e21 cm^-2, in excess of the Galactic column density of 2.21e20 cm^-2 in this direction. The average observed 0.3-10 keV flux is 1.0e-10 erg cm^-2 s^-1, which corresponds to an unabsorbed flux of 1.3e-10 erg cm^-2 s^-1. The counts to observed flux conversion factor at the time of this spectrum is 4.3e-11 erg cm^-2 count^-1. If the underlying powerlaw decay continues as is, we predict an XRT count rate of 0.11 counts/s at T+24hr, which corresponds to an observed 0.3-10keV flux of 4.7e-12 erg cm^-2 s^-1. This circular is an official product of the Swift-XRT team.
GCN 7468 table
GRB_name GRB080319C
GCN_number 7468
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7468 SUBJECT: GRB 080319C - SDSS Pre-Burst Observations DATE: 08/03/19 23:20:53 GMT FROM: Richard J. Cool at U.of AZ/Steward Obs Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona), David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel (LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report: The Sloan Digital Sky Survey (SDSS) imaged the field of burst GRB080319C prior to the burst. As these data should be useful as a pre-burst comparison and for calibrating photometry, we are supplying the images and photometry measurements for this GRB field to the community. Data from the SDSS, including 5 FITS images, 3 JPGS, and 3 files of photometry and astrometry, are being placed at http://mizar.as.arizona.edu/~grb/public/GRB080319C We supply FITS images in each of the 5 SDSS bands of a 8'x8' region centered on the GRB position (ra=258.983 (17:15:55.9), dec=55.3920 (55:23:31.2); GCN 7442), as well as 3 gri color-composite JPGs (with different stretches). The units in the FITS images are nanomaggies per pixel. A pixel is 0.396 arcsec on a side. A nanomaggie is a flux-density unit equal to 10^-9 of a magnitude 0 source or, to the extent that SDSS is an AB system, 3.631e-6 Jy. The FITS images have WCS astrometric information. In the file GRB080319C_sdss.calstar.dat, we report photometry and astrometry of 467 bright stars (r<20.5) within 15' of the burst location. The magnitudes presented in this file are asinh magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118, 1406). Beware that some of these stars are not well-detected in the u-band; use the errors and object flags to monitor data quality. In the files GRB080319C_sdss.objects_flux.dat and GRB080319C_sdss.objects_magnitudes.dat, we report photometry of 508 objects detected within 6' of the GRB position. We have removed saturated objects and objects with model magnitudes fainter than 23.0 in the r-band. The fluxes listed in GRB080319C_sdss.objects_flux.dat are in nanomaggies while the magnitudes listed in GRB080319C_sdss.objects_magnitudes.dat are asinh magnitudes. All quantities reported are standard SDSS photometry, meaning that they are very close to AB zeropoints and magnitudes are quoted in asinh magnitudes. Photometric zeropoints are known to about 2% rms. None of the photometry is corrected for dust extinction. The Schlegel, Finkbeiner, and Davis (1998) predictions for this region are A_U=0.134 mag, A_g=0.098 mag, A_r = 0.071 mag, A_i=0.054 mag, and A_z=0.038 mag. The file GRB080319C_sdss.spectro.dat contains a list of the 4 objects with SDSS spectroscopy within 6 arcminutes of the GRB position. In addition to the redshift and 1-sigma error for each object, this file also lists the object spectroscopic classification. SDSS astrometry is generally better than 0.1 arcsecond per coordinate. Users requiring high precision astrometry should take note that the SDSS astrometric system can differ from other systems such as those used in other notices; we have not checked the offsets in this region. More detailed information pertaining to our SDSS GRB releases can be found in our initial data release paper (Cool et al. 2006, PASP 118, 733). See the SDSS DR4 documentation for more details: http://www.sdss.org/dr5. These data have been reduced using a slightly different pipeline than that used for SDSS public data releases. We cannot guarantee that the values here will exactly match those in the data release in which these data are included. In particular, we expect the photometric calibrations to differ by of order 0.01 mag. This note may be cited, but please also cite the SDSS data release paper, Adelman-McCarthy et al. (2007, ApJS, 172, 634), when using the data or referring to the technical documentation.
GCN 7475 table
GRB_name GRB080319C
GCN_number 7475
Detection_method KAIT
Circular_text TITLE: GCN CIRCULAR NUMBER: 7475 SUBJECT: GRB 080319C: KAIT OA observations DATE: 08/03/20 05:43:41 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS W. Li and A. V. Filippenko, University of California, Berkeley, report on behalf of the KAIT GRB team: We have analyzed the KAIT observations of the optical afterglow (OA) of GRB 080319C (GCN 7442, GCN 7460) as reported in GCN 7441. Our first 5 s unfiltered observation started at 12:27:11 UT, 75 s after the BAT trigger. Four subsequent 5 s exposures from t = 81 s to 100 s indicate a smoothly decaying behavior (but perhaps not power law). After reaching a minimum at t = 180 s (or perhaps a bit earlier), the OA brightened steeply to a second prominent peak centered at t ~ 320 s, after which the OA decayed as an approximate power law, with evidence for a gradually steepening decay index. Selected photometry, all unfiltered but calibrated to the R band via USNO B1: t_start (s) exp (s) mag mag_err 75 5.0 17.353 0.057 100 5.0 17.71 0.062 180 20.0 17.95 0.051 271 20.0 17.322 0.022 362 20.0 17.32 0.023 453 20.0 17.487 0.027 845 20.0 18.06 0.048 1429 20.0 18.866 0.096
GCN 7477 table
GRB_name GRB080319C
GCN_number 7477
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7477 SUBJECT: GRB 080319C: Early RAPTOR Observations DATE: 08/03/20 06:07:34 GMT FROM: James Wren at LANL J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis of Los Alamos National Laboratory report: Our RAPTOR telescopes responded to Swift trigger 306778 (Pagani et al., GCN 7442) at 12:26:30.66 UTC, 33.70 seconds after the trigger. We detect the optical counterpart initially reported by Li (GCN 7441). Our measurements are consistent with those reported by KAIT (GCN 7441 and 7475) and Super-LOTIS (7443). Our images became dominated by the morning twilight at about 12:35 UTC. The unfiltered measurements reported in the following table are calibrated to the USNO-B1 R band. t-mid(s) exp(s) mag mag-err ----------------------------------------- 47.60 5.0 16.97 0.32 85.27 80.3 17.65 0.18 177.36 61.5 18.22 0.36 228.87 61.1 17.32 0.16 293.28 61.7 17.41 0.20 358.12 62.1 17.13 0.16
GCN 7483 table
GRB_name GRB080319C
GCN_number 7483
Detection_method Swift-BAT Det
ra 259.0060°
decl 55.3930°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7483 SUBJECT: GRB 080319C, Swift-BAT refined analysis DATE: 08/03/20 13:57:13 GMT FROM: Scott Barthelmy at NASA/GSFC M. Stamatikos (GSFC/ORAU), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), C. Pagani (PSU), D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), J. Tueller (GSFC), T. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-120 to T+88 sec from recent telemetry downlinks, we report further analysis of BAT GRB 080319C (trigger #306778) (Pagani, et al., GCN Circ. 7442). The BAT ground-calculated position is RA, Dec = 259.006, 55.393 deg which is RA(J2000) = 17h 16m 01.4s Dec(J2000) = +55d 23' 33.0" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 30%. For the limited event-by-event data we have received on this burst, the mask-weighted light curve shows 2 (possibly 3) overlapping FRED-like peaks starting at T-0.5 sec, peaking at T+0.2 sec, and ending at ~T+50 sec. The event-by-event data for this m-w lightcurve ends at T+88 sec. The on-board raw countrate lightcurve shows no activity after the T+88 sec limit of the event data, but the sensitivity is significantly less for this data product. T90 (15-350 keV) is 34 +- 9 sec (estimated error including systematics). The time-averaged spectrum from T-0.3 to T+51.2 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.37 +- 0.07. The fluence in the 15-150 keV band is 3.6 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+0.13 sec in the 15-150 keV band is 5.2 +- 0.3 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/306778/BA/ If we receive any more data on this burst and it shows any on-going activity beyond the current data limit of T+88 sec, then we will issue a revised circular.
GCN 7487 table
GRB_name GRB080319C
GCN_number 7487
Detection_method Konus-Wind Det
t_trigger 12:25:57.938 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 7487 SUBJECT: Konus-Wind observation of GRB 080319C DATE: 08/03/20 14:34:46 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and T. Cline on behalf of the Konus-Wind team report: The long GRB 080319C (Swift-BAT trigger #306778: Pagani et al., GCN 7442, Stamatikos et al., GCN 7483) triggered Konus-Wind at T0=44757.938 s UT (12:25:57.938). The burst light curve shows a multipeaked structure with a total duration of ~15 s. As observed by Konus-Wind the burst had a fluence of 1.50(-0.21, +0.34)x10^-5 erg/cm2, and a 256-ms peak flux measured from T0+0.256 s of 3.35(-0.70, +0.79)x10^-6 erg/cm2/s (both in the 20 keV - 4 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+16.640 s) is well fitted (in the 20 keV-4 MeV range) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.20 +/- 0.10, and Ep = 594(-131, +224) keV (chi2 = 79.3/73 dof). Fitting by GRBM (Band) model yields: the low-energy photon index is alpha = -1.01 +/- 0.13, the high energy photon index beta = -1.87(-0.63, +0.15), the peak energy Ep = 307(-92, +141) keV (chi2 = 76.1/72 dof). All the quoted errors are at the 90% confidence level. The Konus-Wind light curve of this GRB is available at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080319_T44757/
GCN 7497 table
GRB_name GRB080319C
GCN_number 7497
Detection_method Swift-BAT Det
ra 258.9812°
decl 55.3918°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7497 SUBJECT: GRB 080319C: UVOT Observations DATE: 08/03/21 11:37:34 GMT FROM: Stephen Holland at USRA/NASA/GSFC/SSC S. T. Holland (CRESST/USRA/GSFC) & C. Pagani (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT observed the field of GRB 080319C starting 210 s after the BAT trigger (Pagani et al., GCN Circ. 7442). We detect the optical afterglow in the v, b, u, and white filters at location of the KAIT optical afterglow (Li, et al., 2008, GCNC 7441). The UVOT source position is RA(J2000) = 17:15:55.49 Dec(J2000) = +55:23:30.6 with an estimated uncertainty of +/-0.53 arcsec (radius, 90% confidence). Magnitudes and upper limits are reported below. Filter T_start (s) T_stop Exposure Mag Err Comment v 334 353 19 18.09 0.30 b 433 443 10 19.02 0.53 u 408 581 39 19.08 0.36 uvw1 383 2410 214 >20.0 3-sigma UL uvm2 358 2385 175 >19.6 3-sigma UL uvw2 463 2336 175 >19.9 3-sigma UL white 227 327 98 18.81 0.08 The above magnitudes are not corrected for the Galactic extinction corresponding to a reddening of E_{B-V} = 0 .03 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). The non-detections in the three ultraviolet filters may indicate that the redshift is z >~ 3.
GCN 7508 table
GRB_name GRB080319C
GCN_number 7508
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 7508 SUBJECT: GRB 080319C: Suzaku WAM observation of the prompt emission DATE: 08/03/23 23:47:34 GMT FROM: Makoto Tashiro at Saitama U/Swift K.Onda, M. Tashiro, Y. Terada, Y. Urata, A. Endo, M. Suzuki, N. Kodaka, K. Morigami (Saitama U.), M. Ohno, T. Uehara, T. Takahashi, Y. Fukazawa, C. Kira, Y. Hanabata (Hiroshima U.), T. Tamagawa (RIKEN), K. Yamaoka, Y. E. Nakagawa, S. Sugita (Aoyama Gakuin U.), T. Enoto, R. Miyawaki, K. Nakazawa, K. Makishima (Univ. of Tokyo), E. Sonoda, M. Yamauchi, H. Tanaka, R. Hara (Univ. of Miyazaki), M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: The long GRB 080319C (Swift/BAT trigger #306778 ; Pagani et al., GCN 7442) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 12:25:56 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0s, ending at T0+14s with a duration (T90) of about 13 seconds. The fluence in 100 - 1000 keV was 6.4(+0.4, -0.9)*10^-6 erg/cm^2. The 1-s peak flux measured from T0+2s was 4.2(+0.2, -0.3) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0s to T0+13s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 0.67(+0.30, -0.36), and Epeak 761(+255, -136) keV (chi^2/d.o.f. = 32.2/23). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. 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 7517 table
GRB_name GRB080319C
GCN_number 7517
Detection_method Other
redshift 1.9500
Circular_text TITLE: GCN CIRCULAR NUMBER: 7517 SUBJECT: GRB 080319C: Gemini-North spectroscopic redshift DATE: 08/03/25 18:37:49 GMT FROM: Klaas Wiersema at U of Leicester K. Wiersema, N. Tanvir (University of Leicester), P. Vreeswijk, J. Fynbo (DARK Cosmology Centre), R. Starling, E. Rol (Leicester) and P. Jakobsson (Hertfordshire) report on behalf of a large collaboration: We observed the afterglow of GRB 080319C (GCN 7442) with Gemini North, using the GMOS-N instrument. We took spectra using the B600 grism (exposure time 4 x 900s) in bad weather conditions: exposures were taken through holes in the cloud deck. Observations started at 14:51 UT on March 19th. The spectrum shows several absorption lines of C IV, Al II, Si II, Al III, Mg I and the CrII / ZnII blend. From these we find the redshift z = 1.95. We are very grateful to the Gemini staff, in particular Paul Hirst, for executing these observations.