This file contains both GRBs: 080229A and 080229B //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7335 SUBJECT: GRB 080229: Swift detection of a bright burst DATE: 08/02/29 17:31:15 GMT FROM: Scott Barthelmy at NASA/GSFC J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester), O. Godet (U Leicester), C. Gronwall (PSU), S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU), S. Immler (CRESST/GSFC/UMD), J. A. Kennea (PSU), V. Mangano (INAF-IASFPA), C. B. Markwardt (CRESST/GSFC/UMD), K. M. McLean (GSFC/UMD), A. Moretti (INAF-OAB), P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester), C. Pagani (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (NASA/UMBC), G. Sato (GSFC/ISAS), B. Sbarufatti (INAF-IASFPA), M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester), G. Stratta (ASDC) and E. Troja (U Leicester/INAF-IASFPa) report on behalf of the Swift Team: At 17:04:59 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 080229 (trigger=304379). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 228.217, -14.712 which is RA(J2000) = 15h 12m 52s Dec(J2000) = -14d 42' 43" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed three or four bright peaks with the brightest at ~T+40 sec with a duration of about 60 sec. The peak count rate was ~7000 counts/sec (15-350 keV), at ~40 sec after the trigger. The XRT began observing the field at 17:06:29.9 UT, 90.3 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source with an enhanced position: RA, Dec 228.21888, -14.70536 which is equivalent to: RA(J2000) = 15h 12m 52.53s Dec(J2000) = -14d 42' 19.3" with an uncertainty of 2.7 arcseconds (radius, 90% containment). This location is 24 arcseconds from the BAT onboard position, within the BAT error circle. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 8.97e+20 cm^-2 (Kalberla et al. 2005), so we cannot constrain the redshift at this time using the relation from Grupe et al. (2007). A summary of the promptly downlinked data is given at http://www.swift.ac.uk/sper/304379/. The initial flux in the 2.5 s image was 5.98e-09 erg cm^-2 s^-2 (0.2-10 keV). UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm) filter starting 100 seconds after the BAT trigger. A 400 second image in V band was also taken 207 seconds after the trigger. No afterglow candidate has been found in the either image. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 18.5 mag in white and 18.0 in V. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.15. There is a F0 star with R1~13.3 in the USNO catalog nearby the XRT position which appears in DSS images. 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.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7336 SUBJECT: GRB 080229A: ROTSE-III Optical Limits DATE: 08/02/29 17:42:42 GMT FROM: Brad Schaefer at LSU B. E. Schaefer (Louisiana State) and E.S. Rykoff (UCSB), report on behalf of the ROTSE collaboration: ROTSE-IIIa, located at Siding Spring Observatory, Australia, responded to GRB 080229A (Swift trigger 304379; Cannizzo et al. 2008, GCN 7335), producing images beginning 9.8 s after the GCN notice time. An automated response took the first image at 17:05:31.8 UT, 32.3 s after the burst, and during the gamma-ray emission, under excellent conditions. We took 10 5-sec, 10 20-sec and 20 60-sec exposures, with continuing exposures now ongoing. These unfiltered images are calibrated relative to USNO A2.0 (R). Comparison to the DSS (second epoch) reveals no new sources within the 3-sigma Swift/BAT error circle; the field is not crowded. Unfortunately, the XRT position is close to a star of moderate brightness, so the optical transient could possibly be hidden by the light from this star. We do not see any indication that the image of the star is not that of the PSF, and preliminary image subtractions do not reveal any extra sources. Individual images have limiting magnitudes ranging from 14.7-16.1; we set the following specific limits. start UT end UT t_exp(s) mlim t_start-tGRB(s) Coadd? -------------------------------------------------------------------- 17:05:31.8 17:05:36.8 5 14.7 32.3 N //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7337 SUBJECT: GRB 080229: Faulkes Telescope South optical limit DATE: 08/02/29 20:43:58 GMT FROM: James Smith at ARI,Liverpool John Moors U R.J. Smith, D.F. Bersier, S. Kobayashi, A. Monfardini, C.G. Mundell, I. A. Steele (Liverpool JMU), A. Gomboc (U. Ljubljana), C. Guidorzi (U. Bicocca & INAF-OAB) P. O'Brien, E. Rol, N. Bannister (Leicester) report: The 2-m Faulkes Telescope South (Siding Spring) robotically followed up GRB080229 (SWIFT trigger 304379) starting 4.6 min after the GRB trigger time. The automatic "detection mode" procedure did not find any afterglow. In manual inspection of later observations we do not find any optical candidate corresponding to the XRT X-ray afterglow (Cannizzo et al., GCN 7335) to the following limiting magnitudes. Magnitude zero points are relative to the USNO measure of R=13.3 for the adjacent bright star. ----------------------------------------------- Mid Time Filter Tot.Exposure Lim. Mag. since GRB 10.95 min R 60s 18.7 28.10 min R 180s 21.9 ----------------------------------------------- [GCN OPS NOTE(29feb08): Per editor's choice, the Subject-line was changed from "071021" to "080229".] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7338 SUBJECT: GRB 080229, Swift-BAT refined analysis DATE: 08/03/01 00:15:19 GMT FROM: Scott Barthelmy at NASA/GSFC C. Markwardt (GSFC/UMD), S. D. Barthelmy (GSFC), J. K. Cannizzo (NASA/UMBC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), 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-239 to T+303 sec from recent telemetry downlinks, we report further analysis of BAT GRB 080229 (trigger #304379) (Cannizzo, et al., GCN Circ. 7335). The BAT ground-calculated position is RA, Dec = 228.220, -14.697 deg, which is RA(J2000) = 15h 12m 52.7s Dec(J2000) = -14d 41' 50" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 18%. The mask-weighted light curve shows an initial small peak starting at ~T-3 sec, peaking at T_zero, and ending at ~T+12 sec. Then there are two smaller peaks centered on T+18 and T+28 sec. Then comes two overlapping large peaks on T+35 and T+39 sec with the latter tailing out to ~T+85 sec. T90 (15-350 keV) is 64 +- 16 sec (estimated error including systematics). The time-averaged spectrum from T-15.1 to T+64.9 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.91 +- 0.06. The fluence in the 15-150 keV band is 9.0 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+40.36 sec in the 15-150 keV band is 5.7 +- 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/304379/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7339 SUBJECT: UVOT analysis for GRB080229 DATE: 08/03/01 00:34:09 GMT FROM: Paul Kuin at MSSL N.P.M. Kuin (MSSL/UCL) and J. K. Cannizzo (NASA/UMBC) report on behalf of the Swift-UVOT team: The Swift/UVOT observed the field of GRB 080229 (trigger #304379), Canizzo et al. GCN CIRC. 7335) starting 2008:02:29 at 17:06:22 UT with a 9.4 s setling image followed at 17:06:41 UT with a finding chart. No afterglow is detected at the position of the enhanced XRT position in the finding chart, nor in the three subsequent exposures. The source is near a bright star and may be affected by it. Therefore a small aperture was used and the background was determined for a region at equal distance to the nearby star. The following 3-sigma upper limits (in the UVOT photometric system, Breeveld et al., GCN Circ. 6614) were determined at the XRT position (RA=15:12:52.53, DEC= -14:42:19.3, J2000): Filter Tstart(s) Tstop(s) Exp(s) Mag (3-sigma Upper Limits) wh 101 200 99.8 > 20.9 v 208 608 400.0 > 19.9 wh 856 956 99.8 > 20.9 v 962 1362 400.0 > 19.9 The values quoted above are not corrected for the expected Galactic extinction corresponding to a reddening of E_{B-V} = 0.15 mag in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7340 SUBJECT: GRB 080229B: Gamma Ray Burst Localization by SuperAGILE DATE: 08/03/01 02:48:00 GMT FROM: Marco Feroci at IASF/INAF Y. Evangelista, E. Del Monte, M. Feroci, E. Costa, I. Donnarumma, I. Lapshov, F. Lazzarotto, L. Pacciani, M. Rapisarda, P. Soffitta (INAF/IASF Rome), A. Giuliani, S. Vercellone, A. Chen, S. Mereghetti, A. Pellizzoni, F. Perotti, F. Fornari, M. Fiorini, P. Caraveo, A. Zambra (INAF/IASF Milan), A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti, F. Fuschino, M. Marisaldi, M. Galli, (INAF/IASF Bologna), M. Tavani, G. Pucella, F. D'Ammando, V. Vittorini, A. Argan, A. Trois (INAF/IASF Rome), G. Barbiellini, F. Longo (INFN Trieste), P. Picozza, A. Morselli (INFN Roma-2), M. Prest, E. Vallazza (Universita` dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), and P. Giommi, C. Pittori, L. A. Antonelli (ASDC) and L. Salotti (ASI), on bhealf of the AGILE Team, report: "SuperAGILE detected and localized a gamma ray burst on February 29th, at 23:33:01 UT. The event was approximately 13 degrees off-axis. The observed duration in the 20-60 keV energy range is above 100 seconds, with time structure. The burst was triggered and localized during on ground data processing. The burst position was reconstructed as (RA, Dec) (199.221 deg, -64.878 deg), which is: RA(J2000) = 13h 16m 53.13s Dec(J2000) = -64d 52' 40.8" with an uncertainty of 3' radius. The given uncertainty accounts for both the statistical and systematic errors. An analysis of the AGILE Gamma Ray Imager (GRID) data is in progress." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7341 SUBJECT: GRB080229: Possible optical afterglow DATE: 08/03/01 03:16:54 GMT FROM: Michitoshi Yoshida at Okayama Astrophysical Obs M. Yoshida, K. Yanagisawa, Y. Shimizu, S. Nagayama, H. Toda (OAO, NAOJ) and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We performed optical imaging observations (g', Rc, and Ic) of the field of GRB 080229 (Cannizzo et al. GCN 7335) with 50cm MITSuME telescope at Okayama Astrophysical Observatory from UT 17:06:55 (117sec after the trigger) to UT 17:24:40 on Feb 29 2008. We found a faint fading source in the XRT error circle (Cannizzo et al: GCN 7335) only in the Ic band. There was no source in the g' and the Rc bands. Together with the UVOT results (Kuin and Cannizzo GCN7339), this may suggest that this GRB is a high- redshift one. Follow-up observations in infrared bands are encouraged. The magnitude of the fading source and 3-sigma upper limits are summarized below. Observation date 2008-02-29 UT mid-UT exp-T g' Rc Ic --------------------------------------------- 17:09:40 5 min >17.5 >17.8 17.1+-0.3 17:18:58 11 min >17.6 >18.2 >18.0 --------------------------------------------- The values quoted above are not corrected for the Galactic extinction. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7342 SUBJECT: GRB 080229: REM NIR observations DATE: 08/03/01 07:00:23 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, L.A. Antonelli, 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. 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 080229 (Cannizzo et al., GCN 7335) on March 01.154 UT (about 10.6 hours after the burst). We do not detect any afterglow candidate inside the XRT error box down to the following limiting magnitudes (3sigma c.l., calibrated against the 2MASS catalog): J > 16.3 H > 15.6 K > 14.4 Further analysis is in progress. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7343 SUBJECT: GRB 080229: Enhanced Swift-XRT position DATE: 08/03/01 07:18:20 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 1276 s of overlapping XRT Photon Counting mode and UVOT V-band data for GRB 080229, 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 = 228.21828, -14.70467 which is equivalent to: RA (J2000): 15h 12m 52.39s Dec (J2000): -14d 42' 16.8" with an uncertainty of 1.4 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). This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7344 SUBJECT: GRB 080229: Deep Gemini/GMOS optical observations DATE: 08/03/01 07:53:03 GMT FROM: Edo Berger at Princton U E. Berger (Princeton/Carnegie) reports on behalf of a larger collaboration: "We observed the refined BAT error circle of GRB 080229 (GCN #7338) with GMOS on the Gemini-South telescope starting on 2008 Mar 1.26 UT (13.1 hours after the burst). We obtained a total of 5x120 sec in g,r,i,z is 0.8" seeing. We do not detect any sources within the XRT error circle (GCN #7343) to the following 3-sigma magnitude limits: g>26.0, r>25.9, i>25.6, z>25.3." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7345 SUBJECT: GRB 080229: TNG NIR observations DATE: 08/03/01 08:00:00 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, C. Guidorzi (INAF-OAB) on behalf of the CIBO collaboration and G. Andreuzzi and Noemi Pinilla Alonso (FGG-INAF, TNG) report: We observed the field of the GRB 080229 (Cannizzo et al., GCN 7335) with the Italian 3.6m TNG telescope located at Canary Islands on March 01.259 UT (about 13.1 hours after the burst). Observations have been carried out with the NICS NIR camera in imaging mode under good (1.1") seeing conditions. We do not detect any afterglow candidate inside the enhanced XRT error box (Beardmore et al., GCN 7343) down to the following limiting magnitudes (3sigma c.l., calibrated against the 2MASS catalog): J > 20.9 H > 20.1 K > 19.5 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7346 SUBJECT: GRB080229: Swift XRT refined analysis DATE: 08/03/01 12:39:34 GMT FROM: Jirong Mao at INAF-OAB GRB080229: Swift XRT refined analysis J.Mao, (INAF-OAB), A. Moretti (INAF-OAB), J. Canizzo (NASA/UMBC), C. Guidorzi (Univ. Bicocca & INAF-OAB), A, Beardmore (U Leicester) P. Evans (U Leicester) report on behalf of the Swift-XRT team: We have analysed the first 2 orbits of Swift-XRT data obtained for BAT GRB 080229 (trigger #304379, Cannizzo, et al., GCN Circ. 7335). The data consist of 149 s in Windowed Timing (WT) mode, starting 90 s after the BAT trigger and 8.34 ks in Photon Counting (PC) mode. The astrometrically corrected X-ray position is given in Beardomre et al. GCN 7324. The XRT light-curve shows a flare peaking few seconds after the beginning of the observation (103+/-2 s). The descending part of the flare can be fit by a power law with a slope of alpha1=4.45+/-0.09 up to a break at t1=192.4+/- 2.5 s, which is followed by a flat decay with a slope of alpha2=0.18+/-0.01. A second break is present at 2700+/-1000 s with alpha3=0.8+/-0.5 The spectrum formed from all the WT data can be modeled with a power-law of photon index Gamma = 2.88 ± 0.09, with an absorbing column of NH = (3.1 ± 0.2)e21 cm^-2 (in excess with respect to the Galactic value of 8.97e20 cm^-2). The spectrum formed from the PC data can be modeled with a power-law of photon index Gamma = 1.99 ± 0.07, with an absorbing column of NH = (3.1 ± 0.2)e21 cm^-2, which is in agreement with the WT one. If the light-curve continues to decay with a slope of 0.8, the afterglow at 24 hour will be still bright with an expected count rate of 0.3 count s^-1. This corresponds to an observed (unabsorbed) flux of 1.41E-11(2.2e-11) erg cm-2 s-1. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7347 SUBJECT: GRB 080229: VLT NIR observations DATE: 08/03/01 18:28:34 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo and G. Tagliaferri (INAF-OAB) on behalf of the MISTICI collaboration report: We observed the field of the GRB 080229 (Cannizzo et al., GCN 7335) with the ESO-VLT on March 01.411 UT (about 16.8 hours after the burst). Observations have been carried out in J-band with the ISAAC NIR camera in imaging mode under very good (0.7") seeing conditions. We do not detect any afterglow candidate inside the enhanced XRT error box (Beardmore et al., GCN 7343) down to J > 21.6 (3sigma c.l., calibrated against the 2MASS catalog). We acknowledge support from the ESO staff, in particular Thomas Szeifert. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7348 SUBJECT: GRB 080229: I-band observations from OSN DATE: 08/03/01 18:54:39 GMT FROM: Antonio Deugarte at IAA-CSIC A. de Ugarte Postigo (ESO, Chile), F. Aceituno, A.J. Castro-Tirado (IAA-CSIC, Spain) on behalf of a larger colaboration report, We have observed the field of GRB 080229 (Cannizzo et al. GCN 7335) with the 1.5m telescope at Sierra Nevada Observatory (OSN, Granada). The observations were obtained in I-band and range between March 1.1681 and March 1.2638 UT (mean exposure 0.5042 days after the burst). We do not detect any new source in the error box of Swift/XRT (Beardmore et al. GCN 7343) down to a 3-sigma limiting magnitude of I~22.0. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7354 SUBJECT: GRB080229B: Swift XRT afterglow observation DATE: 08/03/03 11:53:47 GMT FROM: Alberto Moretti at Obs Brera Merate A. Moretti (INAF-OAB), J. Mao (INAF-OAB), C. Guidorzi (Univ. Bicocca & INAF-OAB) report on behalf of the Swift-XRT team: We have analysed the Swift-XRT observation of GRB 080229B detected by SuperAgile (Evangelista et al. GCN Circ). The data consist of 13.4 ks in Photon Counting (PC) mode starting 27 hours after the SuperAGILE trigger and ending at 48 hours. We found a fading, uncatalogued X-ray source at the position: RA:199.25169 Dec:-64.86239 which is equivalent to: RA(J2000) = 13h 17m 00.40s Dec(J2000) = -64d 51' 44.6" with an uncertainty of 3.9 arcseconds (radius, 90% containment). This location is 73 arcseconds from the SuperAGILE position. The afterglow is decaying with a power-law slope of 0.9+/-0.5. The spectral parameters are poorly constrained due to the paucity of the statistics (~100 photons). The spectrum can be modelled with a power-law of photon index Gamma = 2.8 +/- 1.0, with an absorbing column of NH = (1.4 +/- 0.7)e22 cm^-2 (consistent with the Galactic value of 8.9e21 cm^-2). If the light-curve continues to decay with a slope of 0.9, the afterglow at 3 days (March 4th) will have an expected count rate of 0.0085 count s-1. This corresponds to an observed (unabsorbed) flux of 5.8E-13 (2.2e-12) ergs cm-2 s-1. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7355 SUBJECT: Swift UVOT observations of GRB080229B DATE: 08/03/03 13:45:48 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 observed the field of 080229B, detected by SuperAgile (Evangelista et al. GCN CIRC 7340), starting 76.3 Ks after the trigger. Exposures were taken in the v band. No optical afterglow is detected at the position of the refined XRT position (Moretti et al. GCN CIRC 7354) in the first 5 summed exposures. The following 3-sigma upper limit (in the UVOT photometric system, Breeveld et al., GCN Circ. 6614) was determined at the XRT position (RA=13:17:00.4 DEC= -64:51:44.6 J2000): Filter Tstart(Ks) Tstop(Ks) Exp(s) Mag v 76.27 104.73 816 >19.8 We note that this field is very crowded and it suffers from a high Galactic reddening E(B-V) = 1.9. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7361 SUBJECT: VLA possible radio detection of GRB 080229 DATE: 08/03/04 13:46:24 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 080229 (GCN 7335) at a frequency of 8.46 GHz on 2008 March 01.50 UT. We detect a radio source of flux density of 635 +/- 44 uJy at a position of RA(J2000) 15 12 52.21984, DEC(J2000) -14 42 15.3000. This is 2.82" away from the X-ray afterglow position determined by Swift-XRT (GCN 7343). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7377 SUBJECT: GRB080229, optical upper limit DATE: 08/03/08 07:30:06 GMT FROM: Ryuuji Hara at U of Miyazaki R. Hara, H.hayasi, N.Ohmori, K.Kono H. Tanaka, M.Yamauchi, E.Sonoda, (University of Miyazaki) We have observed the field covering the error circle of GRB080229 (GCN 7338, C. Markwardt et al.) with the unfiltered CCD camera on the 30-cm telescope at University of Miyazaki. The observation was started 17:05:03 UT, ~225 min after the Swift trigger time. We have compared our data of 30 sec exposures with the USNO-A2.0 catalog,there is no new source at the reported position. the upper limits are as follows: -------------------------------------------------------------- Start(UT) End(UT) Num. of frames Limit (mag.) -------------------------------------------------------------- 19:33:57 19:34:27 1 ~16.06 19:33:57 20:39:37 20 ~16.79 --------------------------------------------------------------- //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7380 SUBJECT: GRB080229, optical upper limit (Correction) DATE: 08/03/10 08:25:57 GMT FROM: Ryuuji Hara at U of Miyazaki R.Hara notes: I stated in GCN7337$B!!(Bas "The observation was started 17:05:03 UT, ~225 min after the Swift trigger time." but the correct one is "The observation was started 19:30:40 UT, about 146 min after the Swift trigger time." We apologize for any inconvenience this may have caused. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7404 SUBJECT: GRB 080229: NIR upper limit DATE: 08/03/11 03:23:10 GMT FROM: Takeo Minezaki at U.of Tokyo/Astro T. Minezaki (IoA, Tokyo), P.A. Price (IfA, Hawaii), Y. Yoshii (IoA, Tokyo), L. Cowie (IfA, Hawaii) and Y. Kakazu (IfA, Hawaii) report: We observed the localisation of GRB 080229 with the MAGNUM telescope + MIP dual-beam imager. We do not find any afterglow in the RIYJHK images within the XRT error circle (GCN #7343). We estimated the upper limits in JHK based on flux calibration with a nearby 2MASS star as follows: Filter t - t_GRB (hour) Limit (mag) J +19.8 20.5 H +20.7 20.0 K +20.4 19.4 This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7407 SUBJECT: GRB 080229A: GAO 150cm telescope Optical Observation DATE: 08/03/11 11:18:46 GMT FROM: Kenzo Kinugasa at Gunma Astro. Obs/Japan K. Kinugasa (Gunma Astronomical Observatory) report: The field of GRB 080229A (Cannizzo et al. GCN 7335) was observed with the 150 cm telescope of the Gunma Astronomical Observatory. Starting at 18:19 UT (1.25 hours after the burst), Rc, and Ic frames were acquired for 5 x 3-min exposures under a poor seeing (~3.5arcsec) condition. The enhaunced XRT position (Beardmore et al. GCN 7343) is close to a bright star, so the field are strongly contaminated with the light from this star. We do not identify the optical counterpart reported by Yoshida et al. (GCN 7341) to 3-sigma limiting magnitudes of Rc=19.3 and Ic=18.7 relative to USNO-B1.0 magnitudes. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8453 SUBJECT: Radio observation of GRB 080229b with ATCA DATE: 08/10/31 17:40:33 GMT FROM: Aquib Moin at CIRA/ATNF Aquib Moin (Curtin Institute of Radio Astronomy / Australia Telescope National Facility), Steven Tingay (Curtin Institute of Radio Astronomy), Chris Phillips (Australia Telescope National Facility), Gregory Taylor (University of New Mexico), Mark Wieringa (Australia Telescope National Facility) and Ralph Martin (Perth Observatory) report: We observed the SWIFT-XRT X-ray afterglow position of the GRB 080229b (GCN 7354) at 4.8 and 8.456 GHz with the Australia Telescope Compact Array (ATCA) on May 31, 2008 between 04:39:45 UT and 12:09:05 UT. We did not detect a radio source at the XRT position of the GRB 080229b afterglow (GCN 7354). The radio flux density at the GRB X-ray afterglow position is -0.704 +/- 0.422 mJy at 4.8 GHz, and -0.012 +/- 0.255 mJy at 8.6 GHz (1-sigma). The Australia Telescope Compact Array (/ Parkes telescope / Mopra telescope / Long Baseline Array) is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. See field image at: http://astronomy.ivec.org/dokuwiki/doku.php/grb/grb_080229b_field_image //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8465 SUBJECT: Radio observation of GRB 080229a with ATCA DATE: 08/11/03 01:29:59 GMT FROM: Aquib Moin at CIRA/ATNF Aquib Moin (Curtin Institute of Radio Astronomy / Australia Telescope National Facility), Steven Tingay (Curtin Institute of Radio Astronomy), Chris Phillips (Australia Telescope National Facility), Gregory Taylor (University of New Mexico), Mark Wieringa (Australia Telescope National Facility) and Ralph Martin (Perth Observatory) report: We observed the BAT refined position of the GRB 080229a (GCN 7338) at 4.8 and 8.456 GHz with the Australia Telescope Compact Array (ATCA) on May 31, 2008 between 08:18:55 UT and 13:38:25 UT. We did not detect a radio source at the BAT position of the GRB 080229a (GCN 7338). The radio flux density at the GRB position is -0.053 +/- 0.175 mJy at 4.8 GHz, and -0.383 +/- 0.356 mJy at 8.6 GHz (1-sigma). The Australia Telescope Compact Array (/ Parkes telescope / Mopra telescope / Long Baseline Array) is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. See field image at: http://cira.ivec.org/dokuwiki/doku.php/grb/grb_080229a_field_image Please note: http://astronomy.ivec.org is now http://cira.ivec.org