GRB080330A

This page lists all entries on GRB080330A in GRBweb

Summary IPN Swift GCN 7536 GCN 7537 GCN 7538 GCN 7539 GCN 7540 GCN 7541 GCN 7542 GCN 7543 GCN 7544 GCN 7545 GCN 7546 GCN 7547 GCN 7549 GCN 7550 GCN 7552 GCN 7553 GCN 7554 GCN 7555 GCN 7556 GCN 7559 GCN 7560 GCN 7561 GCN 7568 GCN 7580 GCN 7583 GCN 7585

Summary table
Variable Value Source
T0 3:41:16 UTC GCN_circulars,Swift Det
ra 169.2688° Swift
decl 30.6228° Swift
pos_error 1.29e-04° Swift
T90 61.0 s Swift
T90_start 3:41:16 UTC Swift
fluence 3.40e-07 erg/cm² Swift
redshift 1.5100 GCN_circulars,Optical
T100 61.0 s
GBM_located False
mjd 54555.153657407405 GCN_circulars,Swift Det
IPN table
GRB_name GRB080330A
ra 169.3000°
decl 30.5667°
pos_error 5.00e-02°
redshift 1.5100
Swift table
GRB_name GRB080330A
t_trigger 3:41:16 UTC
ra 169.2688°
decl 30.6228°
pos_error 1.29e-04°
T90 61.0 s
fluence 3.40e-07 erg/cm²
redshift 1.5100
GCN 7536 table
GRB_name GRB080330A
GCN_number 7536
Detection_method Optical
ra 169.2667°
decl 30.6239°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7536 SUBJECT: GRB 080330: TAROT Calern observatory optical detection DATE: 08/03/30 04:02:13 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 080330 detected by SWIFT (trigger 308041) with the TAROT robotic telescope (D=25cm) located at the Calern observatory, France. The observations started 20.4s after the GRB trigger (4.5s after the notice). The elevation of the field decreased from from 26 degrees above horizon and weather conditions were good. We detect a new raising source in the error box given by SWIFT We detected the candidate couterpart in the XRT location at the following position (+/- 1 arcsec): RA(J2000) = 11h 17m 04s47 DEC(J2000) +30d 37' 26"90 OT was R~16.8 at 300s after GRB. Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. N.B. Galactic coordinates are lon=197.8461 lat=+69.1207 and the galactic extinction in R band is 0.0 magnitudes estimated from D. Schlegel et al. 1998ApJ...500..525S. This me
GCN 7537 table
GRB_name GRB080330A
GCN_number 7537
Detection_method Swift Det
t_trigger 3:41:16 UTC
ra 169.3020°
decl 30.5700°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7537 SUBJECT: GRB 080330: Swift detection of a burst with an optical counterpart DATE: 08/03/30 04:02:22 GMT FROM: David Palmer at LANL J. Mao (INAF-OAB), W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), K. M. McLean (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC), M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester), T. N. Ukwatta (GSFC/GWU) and D. E. Vanden Berk (PSU) report on behalf of the Swift Team: At 03:41:16 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 080330 (trigger=308041). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 169.302, +30.570 which is RA(J2000) = 11h 17m 12s Dec(J2000) = +30d 34' 13" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multiple-peak structure with a duration of about 60 sec. The peak count rate was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 03:42:27.4 UT, 70.5 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source located at RA, Dec 169.26095, 30.62298 which is equivalent to: RA(J2000) = 11h 17m 2.63s Dec(J2000) = +30d 37' 22.7" with an uncertainty of 3.077 arcseconds (radius, 90% containment). This location is 229 arcseconds from the BAT onboard position, outside the BAT error circle. A power-law fit to a spectrum formed from promptly downlinked event data does not constrain the column density, so we cannot provide limits on the redshift using spectroscopy and the relation from Grupe et al. (2007). A summary of the promptly downlinked data is given at http://www.swift.ac.uk/sper/308041/. The initial flux in the 2.5 s image was 2.03e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of nominal 100 seconds with the White (160-650 nm) filter starting 82 seconds after the BAT trigger. There is a candidate afterglow in the list of sources generated on-board at RA(J2000) = 11:17:04.51 = 169.2688 DEC(J2000) = +30:37:22.1 = 30.6228 with a 1-sigma error radius of about 1.0 arc sec. This position is 6.1 arc sec. from the center of the XRT error circle. The estimated magnitude is 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 0.02. Burst Advocate for this burst is J. Mao (jirong.mao AT brera.inaf.it). 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 7538 table
GRB_name GRB080330A
GCN_number 7538
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7538 SUBJECT: GRB 080330A: ROTSE-III Detection of Optical Counterpart DATE: 08/03/30 04:04:25 GMT FROM: Brad Schaefer at LSU B. E. Schaefer (Louisiana State) and T. Guver (U Istanbul) report on behalf of the ROTSE collaboration: ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 080330A (Swift trigger 308041). The first image was at 03:41:39.2 UT, 22.4 s after the burst (7.2 s after the GCN notice time). The unfiltered images are calibrated relative to USNO A2.0. We detect a new object, not visible in the DSS (second epoch), with coordinates: 11:17:04.5 +30:37:24.0 (J2000), with positional uncertainty of 1" or better. This is inside the XRT error box. The object is roughly 17.5 magnitude, and it declined immediately only to rise again to a peak at 16.9 mag roughly ~300 seconds after the burst. A jpeg image is available at http://www.rotse.net/images/gsb308041_3b00_img.jpg Continuing observations are in progress.
GCN 7539 table
GRB_name GRB080330A
GCN_number 7539
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7539 SUBJECT: GRB 080330: Liverpool Telescope Optical observations DATE: 08/03/30 04:21:17 GMT FROM: Andreja Gomboc at LT,ARI,Liverpool JMU A. Gomboc (University of Ljubljana), C. Guidorzi (U. Bicocca & INAF-OAB), A. Melandri, C. G. Mundell, A. Monfardini, R.J. Smith, I.A. Steele,D. Bersier, S. Kobayashi, M. Burgdorf, D. Carter (Liverpool JMU) report: The 2-m Liverpool Telescope reacted robotically to GRB 080330 (Swift trigger 308041) starting 3 min after the GRB trigger time. We detect initially rising and subsequently fading optical candidate in r', i' and g' filters at the posotion consistent with XRT source, UVOT (Mao et al., GCN 7537) and TAROT optical candidate (Klotz, Boer & Atteia, GCN 7536). The magnitude of the source in first frames is r'=17.3 +-0.1.
GCN 7540 table
GRB_name GRB080330A
GCN_number 7540
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 7540 SUBJECT: GRB080330 - SDSS Pre-Burst Observations DATE: 08/03/30 04:24:11 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 GRB080330 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/GRB080330 We supply FITS images in each of the 5 SDSS bands of a 8'x8' region centered on the GRB position (ra=169.302 (11:17:12.5), dec=30.5700 (30:34:12.0); Swift-BAT 308041), 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 GRB080330_sdss.calstar.dat, we report photometry and astrometry of 219 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 GRB080330_sdss.objects_flux.dat and GRB080330_sdss.objects_magnitudes.dat, we report photometry of 1512 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 GRB080330_sdss.objects_flux.dat are in nanomaggies while the magnitudes listed in GRB080330_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=0.082 mag, A_g=0.060 mag, A_r = 0.044 mag, A_i=0.033 mag, and A_z=0.023 mag. The file GRB080330_sdss.spectro.dat contains a list of the 2 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 7541 table
GRB_name GRB080330A
GCN_number 7541
Detection_method Optical
ra 169.2707°
decl 30.6223°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7541 SUBJECT: GRB 080330: error in reported XRT position DATE: 08/03/30 04:36:19 GMT FROM: David Burrows at PSU/Swift D. N. Burrows (PSU) reports on behalf of the Swift XRT team: The XRT position for GRB 080330 that was distributed in GCN Circ. 7537 was incorrect. The initial on-board XRT position determined immediately after the spacecraft slew was GRB_RA: 169.2707d {+11h 17m 04.9s} (J2000), GRB_DEC: +30.6223d {+30d 37' 20.2"} (J2000), with a nominal error circle radius of 5.0 arcseconds. This position was 6.1 arcseconds from the UVOT position. It appears that shortly after arriving on-target, the spacecraft began slowly drifting because the star tracker did not lock properly on the star field. The updated XRT position based on promptly downloaded data was determined using inaccurate aspect information from the satellite and was therefore incorrect. We apologize for any confusion that this may have caused. We reiterate that the XRT position appears to be consistent with the optical position.
GCN 7542 table
GRB_name GRB080330A
GCN_number 7542
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7542 SUBJECT: GRB 080330A: PAIRITEL Infrared Detections DATE: 08/03/30 05:22:44 GMT FROM: Josh Bloom at UC Berkeley J. S. Bloom (UC Berkeley) and D. L. Starr (UCB; LCOGT) report: "We began observing the field of GRB 080330A (Mao et al. GCN 7537) at 2008-03-30 03:53:24.8 UT with PAIRITEL. In a stack of the first 33 frames (each 7.8 sec) exposures, consistent with the BAT/XRT/UVOT (7537, also Burrows et al. GCN 7541) and groundbased position (7536, 7539, 7538), we find a point source in JHKs bands. The preliminary photometry yields: # t (MJD) terr (day) filt mag merr 54555.164606 0.001499 h 15.33 0.04 54555.164606 0.001499 k 14.59 0.04 54555.164606 0.001499 j 16.00 0.04 We find a position relative to 2MASS of (700 mas rms uncertainty): ra = 11:17:04.496 dec = +30:37:23.53 J2000 Observations are ongoing."
GCN 7543 table
GRB_name GRB080330A
GCN_number 7543
Detection_method Optical
ra 169.2667°
decl 30.6231°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7543 SUBJECT: GRB 080330: TAROT Calern observatory optical observations DATE: 08/03/30 06:31:40 GMT FROM: Alain Klotz at CESR-CNRS Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. (LATT-OMP) report: We complete the TAROT analysis of GRB 080330 detected by SWIFT (trigger 308041) at the location of the rising afterglow detected by Klotz et al. (GCNC 7536). We refined the coordinates (better than 1 arcsec) : RA(J2000) = 11h 17m 04s49 DEC(J2000) +30d 37' 23"5 We consider the date of trigger : t0 = 2008-03-30T03:41:17 The first image is trailed with a duration of 60.0s (see the description in Klotz et al., 2006, A&A 451, L39). We do not detect the OT with a limiting magnitude of: t0+20.4s to t0+80.4s : R > 17.0 This limiting magnitude is compatible with the detection R~17.5 by ROTSE-IIIb (Schaefer et Guver GCNC 7538) at ~t0+25s. The later images, in tracking mode, show the afterglow. We measured the alpha index considering flat flux is proportional to t^-alpha: t0+ 88s to t0+ 332s : alpha=-0.8 (rise) t0+332s to t0+ 428s : maximum of brightness R~16.8 t0+428s to t0+1068s : alpha=+0.4 (decay) t0+1068s : R~17.2 Two images were taken between t0+1177s and t0+1363s during the dawn. They seem to show a plateau or even a rebrightening. Observations are now stoped at Calern. This message may be cited.
GCN 7544 table
GRB_name GRB080330A
GCN_number 7544
Detection_method Optical
ra 169.2398°
decl 30.6310°
redshift 1.5100
Circular_text TITLE: GCN CIRCULAR NUMBER: 7544 SUBJECT: GRB 080330: NOT redshift DATE: 08/03/30 07:19:56 GMT FROM: Daniele Malesani at Niels Bohr Inst,Dark Cosmology Center Daniele Malesani, Johan P.U. Fynbo (DARK), Pall Jakobsson (Univ. Hertfordshire), Paul M. Vreeswijk (DARK), Sami-Matias Niemi (NOT), report on behalf of a larger observation: We observed the afterglow of GRB 080330 (Mao et al., GCN 7537) with the NOT equipped with ALFOSC. We clealy detect the optical counterpart (Klotz et al., GCN 7536; Mao et al., GCN 7537, Schaefer & Guver, GCN 7538; Gomboc et al., GCN 7539; Bloom & Starr, GCN 7542). We measure R = 17.55 on March 30.17596 UT (32.1 min after the GRB), assuming R = 17.61 for the USNO star 1206-0188558 at RA = 11:16:57.541, Dec = +30:37:51.51. A 1800 s spectrum with ALFOSC was acquired starting 46 min after the GRB, covering the range 3700-8000 AA. A preliminary reduction of the data reveals absorption features in the spectrum from C IV, Zn II, Fe II, and Mg II at redshift z=1.51. We acknowledge excellent support from the NOT staff
GCN 7545 table
GRB_name GRB080330A
GCN_number 7545
Detection_method GROND
ra 169.2687°
decl 30.6234°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7545 SUBJECT: GRB 080330: GROND Observations DATE: 08/03/30 10:06:42 GMT FROM: Christian Clemens at MPE C. Clemens, A. Kupcu Yoldas, J. Greiner, A. Yoldas, T. Kruehler (all MPE Garching) and G. Szokoly (Eoetvoes Univ., Budapest and MPE Garching) report on behalf of the GROND team: We observed the field of GRB 080330 (Swift trigger 308041; Mao et al., GCN #7537) simultaneously in g', r', i', z', J, H and K with GROND (Greiner et al. 2008, PASP) mounted at the 2.2m ESO/MPI telescope at La Silla Observatory (Chile). Observations started at 03:44:23 UT on March, 30th, 2008, about 3.1 mins after the GRB trigger. We found a bright point source at RA (J2000) = 11h 17m 04.48s DEC (J2000) = 30d 37' 24.4'', coincident with the optical afterglow first reported by Klotz et al. (GCN #7536 and #7543). Based on the first 240 s of effective exposures in J and H, we estimate magnitudes of J=15.92 +/- 0.02 and H=15.45 +/- 0.01, calibrated against 2MASS stars.
GCN 7546 table
GRB_name GRB080330A
GCN_number 7546
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7546 SUBJECT: GRB080330: LOAO R-band Detection DATE: 08/03/30 12:06:18 GMT FROM: Myungshin Im at Seoul Nat U M. Im, I. Lee (Seoul National Univ.), Y. Urata (Saitama U/ASIAA), J.W. Lee, J. Yoon, S.-L. Kim, C.-U. Lee (KASI), on behalf of EAFON team. We took R-band images of GRB080330 (Hao et al. GCN 7537) using the 1.0m telescope at Mt. Lemmon (Arizona, US) operated by the Korea Astronomy Space Science Institute. The R-band imaging started at March 30, 06:57:55.1 UT (3:15:56 after the burst). We clearly detect the afterglow at the location reported by Schaefer et al. (GCN 7538). Start time Mid-point Rmag ------------------------------------------------------------- 06:57:55.1 07:11:50.4 19.63 +- 0.05 (3hr15m after burst) (3hr30m after burst) The magnitude is calibrated with a GSC2.2 star at (11:16:56.54, +30:37:51.4). The afterglow faded by more than 2 magnitudes since the detections shoftly after the burst (GCN 7536, 7538, 7543). This message may be cited.
GCN 7547 table
GRB_name GRB080330A
GCN_number 7547
Detection_method Optical
redshift 1.5100
Circular_text TITLE: GCN CIRCULAR NUMBER: 7547 SUBJECT: GRB 080330: Redshift Confirmation from Hobby-Eberly Telescope Spectroscopy DATE: 08/03/30 15:21:39 GMT FROM: Antonino Cucchiara at PSU A. Cucchiara & D. B. Fox (PSU) report on behalf of a larger collaboration: "Starting on 2008 March 30.35 UT we used the Marcario LRS spectrograph on the Hobby-Eberly Telescope (R ~ 230 ) to obtain 2 x 1000s spectra of the optical afterglow (Mao et al., GCN 7537) of GRB 080330. The spectrum covers the wavelength range 4100 to 10,500 Angstrom. We observe multiple metal absorption features including the MgII doublet (2796, 2803 A) and MgI (2852 A), FeII (2586, 2600 A), ZnII (2026 A) and NiII (1741,1751 A) at redshift z = 1.51. Our observations are consistent with the redshift and features reported by Malesani et al. (GCN 7544)."
GCN 7549 table
GRB_name GRB080330A
GCN_number 7549
Detection_method Swift-BAT Det
ra 169.2780°
decl 30.6070°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7549 SUBJECT: GRB 080330, Swift-BAT refined analysis DATE: 08/03/30 16:39:37 GMT FROM: Scott Barthelmy at NASA/GSFC C. Markwardt (GSFC/UMD), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), J. Mao (INAF-OAB), K. McLean (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+963 sec from recent telemetry downlinks, we report further analysis of BAT GRB 080330 (trigger #308041) (Mao, et al., GCN Circ. 7537). The BAT ground-calculated position is RA, Dec = 169.278, 30.607 deg, which is RA(J2000) = 11h 17m 06.7s Dec(J2000) = +30d 36' 24.1" with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment). The partial coding was 53%. The mask-weighted light curve shows an initial set of 3 overlapping peaks (the brightest first) starting at ~T_zero, and the 3rd ending at ~T+15 sec, then it returns to baseline. A 4th peak starts at roughly T+50 sec and ends at roughly T+70 sec. T90 (15-350 keV) is 61 +- 9 sec (estimated error including systematics). The time-averaged spectrum from T-0.5 to T+71.9 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.53 +- 0.45. The fluence in the 15-150 keV band is 3.4 +- 0.8 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+0.44 sec in the 15-150 keV band is 0.9 +- 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/308041/BA/ We note that the fluence ratio in a simple power-law fit between the 25-50 keV band and the 50-100 keV band is 1.44. This fluence ratio is larger than 1.32 which can be achieved in the Band function of alpha=-1.0, beta=-2.5, and Epeak=30 keV. Thus, preliminary analysis shows that Epeak of the burst is very likely around or below 30 keV. Therefore the burst can be classified as an X-ray flash (e.g. Sakamoto et al. ApJ in press, arXiv:0801.4319).
GCN 7550 table
GRB_name GRB080330A
GCN_number 7550
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7550 SUBJECT: GRB080330: TNT optical observations DATE: 08/03/30 16:49:47 GMT FROM: L.P. Xin at NAOC X.F.Wang, J.Z.Li, Q.C.Feng, L.P.Xin, M.Zhai, Y.L.Qiu, J.Y.Wei, J.Y.Hu, J.S.Deng, J.Wang, Y.Urata and W.K.Zheng on behalf of EAFON report: We have observated the field of GRB080330 (Mao et al. GCN 7537) in R band with TNT at Xinglong observatory, the magnitude of afterglow derieved from USNO-b1.0 is R=20.4+/-0.2 with the mean time of 9.4hr after the burst. This message may be cited For more information about Xinglong GRBs Follow-up observations, please visit the website: http://www.xinglong-naoc.org/grb/
GCN 7552 table
GRB_name GRB080330A
GCN_number 7552
Detection_method Swift-UVOT Other
redshift 1.5100
Circular_text TITLE: GCN CIRCULAR NUMBER: 7552 SUBJECT: GRB 080330 Swift-UVOT refined analysis DATE: 08/03/30 23:28:41 GMT FROM: Paul Kuin at MSSL N.P.M. Kuin (MSSL/UCL) and J.Mao (INAF) report on behalf of the Swift-UVOT team: The Swift/UVOT started observations of GRB 080330 (Mao et al, GCN Circ. 7537) with a settling exposure in the UVOT v-filter starting 2008-03-30 at 03:42:19 U, 63 seconds after the BAT trigger, and a finding chart exposure in the white filter starting 83 seconds after the trigger. During the subsequent exposure in the V filter, starting at 189 seconds after the trigger, the spacecraft lost lock and drifted. In the V image, a clear trail is visible that all the stars in the field follow. In other filters, there is no clear evidence of lost counts, except in one image in b. Those exposures are short, or have much background (white), which suggest that only a fraction of the counts is lost. The extraction of the magnitudes below relies on a 5 aperture around the source. No counts are visible due to the source outside the aperture in the images. However, these magnitudes should be regarded as upper limits until a more detailed reduction can be done. Based on some tests, the magnitude may be underestimated as much as 0.7 magnitudes. The v-filter data were extracted using an aperture closely matching the shape of the trail and were measured from the event data. There is an uncertainty in this approach as well, since it is not clear what part of the PSF is sampled. Therefore the V magnitudes can be over-or underestimated by 0.25 magnitudes. The observations start before a peak is reached. In the white filter, a peak is apparent at T+128 +/- 5 seconds. In the v filter data, two peaks may be present at T+ 438 and 1038 +/- 25s. It is unlikely that the satellite drift caused these variations because the aperture included the whole trail. The uvw1 magnitude has upper limits until quite late in the burst, and must rise between T+791 and T+1416s. This is an indication of achromatic evolution in this burst. Only an upper limit is found in the uvw2 and uvm2 filters, which is consistent with the reported redshift of 1.51 (Malesani, et al. GCN 7544, and Cucchiara et al. GCN 7547). Filter Tstart(s) Tstop(s) Exp(s) Mag Mag-error [systematic error] wh 83 183 98 18.2 0.06 [+0.7] v 189 588 399.8 18.5-17.2 0.3 [+/-0.25] (*) uvm2 594 1390 58.4 >18.55 (3 sigma UL) uvw1 619 638 19.5 >18.02 (3 sigma UL) u 644 664 19.4 17.14 0.16 [+0.7] b 669 678 9.6 18.9 0.6 [+0.7] wh 683 693 9.8 17.76 0.14 [+0.7] uvw2 698 870 38.9 >18.77 (3 sigma UL) uvw1 772 791 19.8 >18.04 (3 sigma UL) u 796 815 19.4 16.66 0.17 [+0.7] b 822 832 9.6 17.66 0.22 [+0.7] white 836 979 107.8 17.55 0.03 [+0.7] v 985 1384 400 18.0-17.2 0.3 [+/-0.25] (*) uvw1 1416 1436 19.4 17.7 0.3 [+0.7] b 1464 1483 19.8 18.14 0.22 [+0.7] white 1490 1499 9.6 17.91 0.15 [+0.7] (*) For the V magnitudes the range is given as seen in the event data. The values quoted above are not corrected for the expected Galactic extinction corresponding to a reddening of E_{B-V} = 0.02 mag in the direction of the burst (Schlegel et al. 1998).
GCN 7553 table
GRB_name GRB080330A
GCN_number 7553
Detection_method Optical
ra 169.2639°
decl 30.6420°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7553 SUBJECT: GRB 080330, SMARTS optical/IR afterglow observations DATE: 08/03/31 01:58:36 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 080330 (GCN 7537, Mao et al.), with a mid-exposure time of 2008-03-30 04:17:29 UT, which is ~36 minutes 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 7537, Mao et al.) is detected in all our images with the following magnitudes (which have not been corrected for Galactic reddening): B= 18.27 +/- 0.04 V= 17.90 +/- 0.04 R= 17.59 +/- 0.03 I= 17.09 +/- 0.03 J= 16.36 +/- 0.07 H= 15.76 +/- 0.07 K= 15.14 +/- 0.06 Optical photometry is calibrated against Landolt standard stars and IR photometry is calibrated against the 2MASS star at coordinates RA/DEC=11:17:03.34 +30:38:31.1. The afterglow clearly decays between individual images. In R-band images taken between 20 and 52 minutes post-burst, the afterglow decays by 0.7 magnitudes, indicating an approximate decay rate of alpha = -0.7 (where afterglow flux is proportional to t^alpha).
GCN 7554 table
GRB_name GRB080330A
GCN_number 7554
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7554 SUBJECT: GRB 080330: REM optical observations DATE: 08/03/31 08:35:23 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, S. Covino, D. Fugazza, L.A. Antonelli, 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. Meurs, L. Nicastro, E. Palazzi, E. Pian, S. Piranomonte, L. Stella, G. Stratta, G. Tagliaferri, G. Tosti, V.Testa, S.D. Vergani, 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 080330 (Mao et al., GCN 7537) on March 30 03:42:11 UT (about 55 seconds after the burst). We clearly detect the afterglow reported in GCNs 7536 (Klotz et al.), 7537 (Mao et al.) 7538 (Schaefer & Guver), 7539 (Gomboc et al.), 7542 (Bloom & Starr), 7544 (Malesani et al.), 7545 (Clemens et al.), 7546 (Lee et al.), 7550 (Wang et al.). The R-band light curve between 70s < t-t0 < 1800s clearly shows an initial rising with a maximum around 330s < t-t0 < 450s and a subsequent plateau with a possible rebrightening at 900s < t-t0 < 1100s, as noted in GCNs 7538 (Schaefer & Guver), 7543 (Klotz et al.) and 7552 (Kuin & Mao). Further analysis is in progress.
GCN 7555 table
GRB_name GRB080330A
GCN_number 7555
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7555 SUBJECT: GRB080330: Swift XRT refined analysis DATE: 08/03/31 12:26:12 GMT FROM: Jirong Mao at INAF-OAB GRB080330: Swift XRT refined analysis J. Mao, A. Moretti, and C. Guidorzi (INAF-OAB) report on behalf of the Swift-XRT team: We have analysed the Swift-XRT data obtained for BAT GRB 080330 (trigger #308041, Mao et al., GCN Circ. 7537). The data consist of 57 s in Windowed Timing (WT) mode, starting 77s after the BAT trigger and 1.36 ks in Photon Counting (PC) mode. The best X-ray position is given in Burrows GCN 7541. The XRT light-curve can be fit by a power-law with a slope of alpha1=5.22+/-0.30 up to a break at t=167.9+/-7.3 s, which is followed by a shallow decay with a slope of alpha2=0.20+/-0.07. The spectrum formed from all the WT data can be modeled with a power-law of photon index Gamma=2.03+/-0.09, with the fixed absorbing Galactic column of NH=1.23e20 cm^-2. The spectrum formed from the PC data can be modeled with a power-law of photon index Gamma=1.91 0.09, with an absorbing column of NH=(2.78+/-1.22)e21 cm^-2 (in excess with respect to the Galactic value of 1.23e20 cm^-2). If the light-curve continues to decay with a slope of 0.20, after 48 hours, the light curve will have count rate of 0.18 count s^-1, corresponding to an observed (unabsorbed) flux of 5.4e-12(1.3e-11) ergcm^-2 s^-1. This circular is an official product of the Swift-XRT team.
GCN 7556 table
GRB_name GRB080330A
GCN_number 7556
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7556 SUBJECT: GRB080330: optical observations DATE: 08/04/01 00:18:24 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Sergeev, M. Andreev (Terskol Branch of Institute of Astronomy), V. Petkov, A. Kurenya (BNO INR RAS), A. Pozanenko (IKI) on behalf of larger GRB follow up collaboration report: We observed the afterglow of GRB 080330 (Mao et al., GCN 7537) with the Zeiss-2m telescope of Mt.Terskol observatory on March 30. The optical counterpart (Klotz et al., GCN 7536; Mao et al., GCN 7537, Schaefer & Guver, GCN 7538; Gomboc et al., GCN 7539; Bloom & Starr, GCN 7542) is clearly detected. The photometry of the afterglow against of the SDSS calibration stars (Cool et al., GCN 7540) of the two epochs of combined images in R is following T0+ exposure R_mag Mid time 0.575 d 4x900 s 21.05 +/-0.1 0.654 d 4x900 s 21.28 +/-0.1 Taking into account previous observation (R=20.4+/-0.2 at 9.4 hours after burst, Wang et al., GCN 7550) and our observations one can suggest the steepening of a power law decay index up to ~ 1.5 between 9.4 and 15.7 hours after burst.
GCN 7559 table
GRB_name GRB080330A
GCN_number 7559
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7559 SUBJECT: GRB080330: optical observations DATE: 08/04/01 11:28:09 GMT FROM: Vladimir Sokolov at SAO RAS A. S. Moskvitin, T. A. Fatkhullin, V. N. Komarova, A. N. Burenkov (SAO-RAS, Nizhnij Arkhyz) on behalf of larger GRB follow up collaboration report: We observed the GRB 080330 afterglow (Mao et al., GCN 7537) in the R-band (exposure 3x600 sec) with the 1-m telescope of SAO RAS on March 30.928, 18.58 hours after the trigger. The weather conditions were tolerable. The optical transient (Klotz et al., GCN 7536; Mao et al., GCN 7537, Schaefer & Guver, GCN 7538; Gomboc et al., GCN 7539; Bloom & Starr, GCN 7542; A. Sergeev et al., GCN 7556) is clearly detected. The photometry of the afterglow is calibrated against 8 stars from USNO-A2.0. The R-magnitude of the object is 21.49+/-0.28. This message may be cited.
GCN 7560 table
GRB_name GRB080330A
GCN_number 7560
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 7560 SUBJECT: GRB 080330: Prompt PROMPT Observations DATE: 08/04/02 14:47:56 GMT FROM: Mark Schubel at UNC/PROMPT M. Schubel, D. Reichart, M. Nysewander, A. LaCluyze, K. Ivarsen, J. A. Crain, A. Foster, T. Brennan, J. Haislip, J. Styblova, and A. Trotter report: Skynet observed the localization of GRB 080330 (Mao et al., GCN 7537) with two of the 16" PROMPT telescopes at CTIO beginning 31 seconds after the trigger (15 seconds after notification) in VRI. We detect the afterglow (Klotz et al., GCN 7536) in all filters. At 200 seconds after the burst we measure R ~ 17.3 mag (calibrated to 11 USNO B1 stars), at 246 seconds we measure I ~ 16.8 mag (calibrated to 11 USNO B1 stars), and at 292 seconds we measure V ~ 16.6 mag (calibrated to 8 NOMAD stars).
GCN 7561 table
GRB_name GRB080330A
GCN_number 7561
Detection_method Swift Other
ra 169.2584°
decl 30.6229°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7561 SUBJECT: GRB080330: Improved Swift XRT Position DATE: 08/04/03 09:58:40 GMT FROM: Jirong Mao at INAF-OAB GRB080330: Improved Swift XRT Position J. Mao (INAF-OAB) report on behalf of the Swift-XRT team: Since the spacecraft began slowly drifting because the star tracker did not lock properly on the star field, the XRT position for GRB 080330 that was distributed in GCN Circ. 7537 (Mao et al.) was incorrect. The initial on-borad XRT position determined immediately after the spacecraft slew was given by D. N. Burrows (GCN Circ. 7541). The final accurate XRT position from download data of Malindi is: RA=169.2584d {11h 17m 02.02s} (J2000) Dec=30.6229d{+30d 37' 22.58"} (J2000) with the error radius 3.62 arcsec.
GCN 7568 table
GRB_name GRB080330A
GCN_number 7568
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7568 SUBJECT: GRB 080330: RAPTOR detection of prompt optical flash DATE: 08/04/07 20:55:40 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 308041 (Mao et al., GCN 7537) at 03:41:39.93 UTC, 23.1 seconds after the trigger. Our observations show an optical flash (about 10 s duration) at T ~ 60 s that is simultaneous with the fourth gamma-ray peak detected by that BAT (Markwardt et al., GCN 7549). Subsequently, we detect the rise of an optical afterglow starting at T ~ 150 s that levels off to a flat plateau at around T ~ 300 s and then starts to rapidly decay after about T ~ 2000 s. The unfiltered measurements reported in the following table are calibrated to the USNO-B1 R band. t-mid(s) exp(s) mag mag-err ----------------------------------------- 38.78 31.4 (18.3) 5 sigma limit 58.88 5.0 17.46 0.22 83.15 31.3 (18.4) 5 sigma limit 141.96 22.7 17.62 0.10 294.80 22.7 17.03 0.07 504.74 15.0 17.15 0.06
GCN 7580 table
GRB_name GRB080330A
GCN_number 7580
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 7580 SUBJECT: GRB 080330 optical observations DATE: 08/04/09 18:36:58 GMT FROM: AAVSO GRB Network at AAVSO A. Block (Seeing In The Dark Internet Telescope, and Steward Observatory, Tucson, AZ) and M. Templeton (AAVSO) report on behalf of the AAVSO International High Energy Network the following observations and analysis of the optical afterglow of GRB 080330 (Mao et al., GCN Circular #7537; Klotz, Boer, and Atteia, GCN #7536): Adam Block reports unfiltered photometry of the GRB 080330 afterglow spanning 2008 March 30.1675 UT to 2008 March 30.3273, taken with the Seeing In The Dark Internet Telescope 14-inch Celestron SCT, using an SBIG ST1001 camera, located near Mayhill, New Mexico. Forty-seven, 300-second unfiltered exposures were obtained beginning 20 minutes post-burst, and continuing through t0 + 0.1736 days. Data acquisition began after the reported peak (D'Avanzo, et al., GCN #7554), but during the early decay epoch. A break in the light curve is apparent at approximately 25 minutes after the trigger; only one data point was obtained prior to this point, and so a slope cannot be reliably derived. After t0 + 25 minutes, the data are reasonably well fit with a power law index of -1.104 +/- 0.001, with a zero point unfiltered magnitude of 22.65 (m = m(t+1day)). However, the light curve appeared to briefly rebrighten by more than 0.2 magnitudes (1-sigma error = 0.09 mag) approximately 70 minutes post-burst, suggesting a late-time manifestation of the rebrightening seen during early light (Schaefer and Guver, GCN #7538). These observations are consistent with other optical observations taken during this time frame; observations through t0 + 250 minutes do not show evidence for the steeper slope described by Sergeev et al (GCN #7556) for data taken at t > t0 + 0.5 days, suggesting this break occurred between the end of these observations and the start of observations by Sergeev et al. A report detailing these observations is available at the following URL: ftp://ftp.aavso.org/grb/AdamBlock_GRB080330_2454558.33910_.txt The initial image of the GRB field is available at the following URL: ftp://ftp.aavso.org/grb/AdamBlock_GRB080330_2454558.33910_.fits A light curve of the unfiltered photometry is available at the following URL: http://www.caelumobservatory.com/outgoing/grb080330LOG.jpg Photometry and a full description of the observations will appear in the Journal of the AAVSO, and are available from A. Block upon request to ngc1535@caelumobservatory.com. The AAVSO thanks the Curry Foundation for their continued support of the AAVSO International High Energy Network.
GCN 7583 table
GRB_name GRB080330A
GCN_number 7583
Detection_method retraction
ra 169.2695°
decl 30.6236°
Circular_text TITLE: GCN CIRCULAR NUMBER: 7583 SUBJECT: GRB 080330: Swift-XRT refined position retraction DATE: 08/04/11 14:32:16 GMT FROM: Jirong Mao at INAF-OAB J. Mao and C. Guidorzi (INAF-OAB) on behalf of the Swift-XRT team report: A re-examination of the XRT data on GRB080330 (Mao et al. GCN Circ. 7537) taken during the first orbit revealed that the XRT improved position distributed by Mao (GCN Circ. 7561) is incorrect due to star tracker loss-of-lock problems already mentioned by Burrows (GCN Circ. 7541). We re-processed the first orbit PC data and extracted the following refined position from 136 to 311 s after the burst, when the star tracker drifting seems to have little impact: RA, Dec = 169.26950, +30.62355 which is equivalent to: RA (J2000): 11h 17m 04.68s Dec (J2000): +30d 37' 24.78" with an uncertainty of 4.0 arcsec (radius, 90% confidence). This is consistent with the optical ground-based position (2.7 arcsec away from the PAIRITEL position reported by Bloom and Starr, GCN Circ. 7542). This is an official product of the Swift XRT team.
GCN 7585 table
GRB_name GRB080330A
GCN_number 7585
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 7585 SUBJECT: GRB080330: MAGIC telescope GeV observation DATE: 08/04/11 23:41:23 GMT FROM: Markus Garczarczyk at MPI/MAGIC Gaug M., Garczarczyk M., Antonelli A., Bastieri D., Covino S., Galante N., La Barbera A., Longo F. and Scapin V. for the MAGIC collaboration The MAGIC Imaging Atmospheric Cherenkov Telescope performed a follow-up observation of the BAT burst GRB080330 (GCN circular 7537, Mao et al.). We received the GCN alert at 03:41:33 UT (T0+16s), data taking with MAGIC started at 03:42:47 UT (T0+91s), short after the prompt emission phase measured to be T90=61+/-9s. The observation was carried out at a zenith angle of 48 degrees. The observation continued for 1039s. No evidence for VHE gamma-ray emission above the analysis threshold of 313 GeV was found. The observation was carried out in (less sensitive) moon-observation mode. A preliminary analysis, for the hypothesis of steady emission and assumption of a differential photon spectral index of -2.5, yields the following 95% CL differential flux upper limits, including a 30% systematic uncertainty on the telescope efficiency: E (175- 300 GeV): 0.36 * 10^-10 erg/cm^-2/s E (300-1000 GeV): 0.49 * 10^-10 erg/cm^-2/s for a time window from 03:42:47 UT to 03:59:01 UT We can also exclude emission of a constant flux in any 100s time bin smaller than: E (175- 300 GeV): 8.42 * 10^-10 erg/cm^-2/s E (300-1000 GeV): 2.05 * 10^-10 erg/cm^-2/s for a time window from 03:42:47 UT to 03:59:01 UT This message can be cited.