//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9400 SUBJECT: GRB 090519: Swift detection of a burst DATE: 09/05/19 21:22:46 GMT FROM: Scott Barthelmy at NASA/GSFC M. Perri (ASDC), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), C. Gronwall (PSU), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester), C. Pagani (PSU), D. M. Palmer (LANL), A. Rowlinson (U Leicester), M. H. Siegel (PSU), M. Stamatikos (NASA/ORAU) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 21:08:56 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090519 (trigger=352648). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 142.293, +0.183 which is RA(J2000) = 09h 29m 10s Dec(J2000) = +00d 10' 58" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows several overlapping peaks with a duration of about 40 sec. The peak count rate was ~1300 counts/sec (15-350 keV), at ~3 sec after the trigger. The XRT began observing the field at 21:10:51.3 UT, 114.9 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 142.27902, 0.17925 which is equivalent to: RA(J2000) = 09h 29m 6.96s Dec(J2000) = +00d 10' 45.3" with an uncertainty of 3.7 arcseconds (radius, 90% containment). This location is 52 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at http://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (2.96e+20 cm^-2, Kalberla et al. 2005), with an excess column of 1.9 (+2.14/-1.86) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 5.77e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 123 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 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 0.04. Burst Advocate for this burst is M. Perri (perri AT asdc.asi.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.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9401 SUBJECT: GRB 090519: TAROT Calern observatory optical observations DATE: 09/05/19 21:51:16 GMT FROM: Alain Klotz at CESR-CNRS Klotz, A. (CESR-OMP), Gendre, B. (LAM-OAMP), Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report: We imaged the field of GRB 090519 detected by SWIFT (trigger 352648) with the TAROT robotic telescope (D=25cm) located at the Calern observatory, France. The observations started 76.0s after the GRB trigger (6.6s after the notice). The elevation of the field decreased from 21 degrees above horizon and weather conditions were good. The date of trigger : t0 = 2009-05-19T21:08:56.5 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 any OT at the XRT position mentionned by Perri et al. 2009 (GCNC 9400) with a limiting magnitude of: t0+76.0s to t0+136.0s : R > 16.8 The second image is 30.0s exposure in tracking mode: t0+142.8s to t0+172.8s : R > 17.5 We co-added a series of exposures: t0+142.8s to t0+319.6s : R > 18.5 Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. N.B. Galactic coordinates are lon=233.3028 lat=+34.5244 and the galactic extinction in R band is 0.1 magnitude estimated from D. Schlegel et al. 1998ApJ...500..525S. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9402 SUBJECT: GRB 090519: FARO Chante Perdrix Observatory optical observations DATE: 09/05/19 22:13:56 GMT FROM: Alain Klotz at CESR-CNRS Klotz, A. (CESR-OMP), Kugel, F. (Obs. Chanteperdrix) report: We imaged the field of GRB 090519 detected by SWIFT (trigger 352648) with the FARO robotic telescope (D=20cm) located at the Chante Perdrix Observatory, Banon, France. FARO stands for Francois & Alain Robotic Observatory: http://chanteperdrix.dyndns.org The observations started 122.4s after the GRB trigger (53.0s after the notice). The elevation of the field decreased from 22 degrees above horizon and weather conditions were good. The date of trigger : t0 = 2009-05-19T21:08:56.5 The first image is 60.0s exposure in tracking mode. We do not detect any OT at the XRT position mentionned by Perri et al. 2009 (GCNC 9400) with a limiting magnitude of: t0+122.4s to t0+182.4s : R > 15.7 Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9403 SUBJECT: GRB 090519: NOT afterglow candidate DATE: 09/05/19 22:32:39 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst C.C. Thoene (INAF/Brera), D. Malesani (DARK/NBI), A.J. Levan (Univ. Warwick), P. Jakobsson (Univ. Iceland), J. Hjorth (DARK/NBI), N.R. Tanvir (Univ. Leicerster), report on behalf of a larger collaboration We observed the field of GRB 090519 (Perri et al., GCN 9400) with the NOT equipped with ALFOSC. At the edge of the XRT error circle, we detect a fading source at coordinates (J2000): RA = 09:29:07.0 Dec = +00:10:49.1 with an error of ~0.5". The source faded by ~0.3 +- 0.10 mag between 19.8 and 44.4 min after the GRB, suggesting that this is indeed the afterglow of GRB 090519. A (fainter) object is seen at the position of the candidate in the SDSS, which may be a bright host galaxy. On May 19.897 UT, the source had R ~ 21.6. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9404 SUBJECT: GRB 090519: Limits from BOOTES-1B DATE: 09/05/19 23:59:23 GMT FROM: Martin Jelinek at Inst.Astrophys.Andalucia,Granada Martin Jelinek (IAA Granada) and Petr Kubanek (IPL Valencia) on behalf of the BOOTES team. report We observed the errorbox of the GRB 090519 (Perri et al, GCN9400) with the 30cm robotic telescope BOOTES-1B in Spain. The observation started 99s after the GRB trigger. In our unfiltered images we do not detect any new object within the BAT or XRT errorbox with the following limits: Tstart-Tgrb exposure limit 99s 3.5s 15.1 108s 30s 16.5 108s 23x30s 17.6 This message may be cited //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9405 SUBJECT: GRB 090519: Enhanced Swift-XRT position DATE: 09/05/20 01:25:47 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 2178 s of XRT Photon Counting mode data and 1 UVOT images for GRB 090519, 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 = 142.27878, +0.18020 which is equivalent to: RA (J2000): 09h 29m 6.91s Dec (J2000): +00d 10' 48.7" with an uncertainty of 1.8 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, arXiv:0812.3662). This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9406 SUBJECT: GRB 090519, Swift-BAT refined analysis DATE: 09/05/20 02:30:23 GMT FROM: Jay R. Cummings at NASA/GSFC/Swift H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC), M. Perri (ASDC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-119 to T+276 sec from the recent telemetry downlink, we report further analysis of BAT GRB 090519 (trigger #352648) (Perri, et al., GCN Circ. 9400). The BAT ground-calculated position is RA, Dec = 142.317, 0.190 deg which is RA(J2000) = 09h 29m 16.2s Dec(J2000) = +00d 11' 23.9" with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment). This is 0.8 arcmin from the enhanced XRT afterglow position (Goad et al. GCN Circ #9405). The partial coding was 57%. The mask-weighted lightcurve shows multiple overlapping peaks starting at about T-17 sec and ending about T+95 sec. T90 (15-350 keV) is 64 +- 10 sec (estimated error including systematics). The time-averaged spectrum from T-12.4 to T+60.4 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.02 +- 0.20. The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10-06 erg/cm2. The 1-sec peak photon flux measured from T-10 sec in the 15-150 keV band is 0.6 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/352648/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9407 SUBJECT: GRB 090519: Swift/UVOT Upper Limits DATE: 09/05/20 03:27:00 GMT FROM: Stefan Immler at NASA/GSFC S. Immler (NASA/CRESST/GSFC) and M. Perri (ASDC) report on behalf of the Swift/UVOT team: The Swift/UVOT observed the field of GRB 090519 starting 106 s after the BAT trigger (Perri et al., GCN Circ. 9400). No optical afterglow is detected in the initial UVOT exposures at the enhanced position of the X-ray afterglow (Goad et al., GCN Circ. 9405) or the position of the NOT afterglow candidate (Thoene et al. GCN Circ. 9403). Three-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) are: Filter T_start(s) T_stop(s) Exp(s) Mag white 123 7430 862 >21.5 v 106 7841 597 >19.8 b 536 7224 568 >20.6 u 281 7019 617 >20.4 uvw1 662 8131 469 >20.3 uvm2 637 8046 587 >20.4 uvw2 588 7636 549 >20.6 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.04 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9408 SUBJECT: GRB 090519: GROND observation DATE: 09/05/20 08:02:04 GMT FROM: Jochen Greiner at MPI A. Rossi (Tautenburg), T. Kruehler, J. Greiner and A. Yoldas (all MPE Garching) report on behalf of the GROND team: We observed the field of GRB 090519 (Swift trigger 352648, M. Perri et al., GCN #9400) simultaneously in g'r'i'z'JHK with GROND mounted at the 2.2m ESO/MPI telescope at La Silla Observatory (Chile). Observations started on 19 May 2009 at 23:44 UT, 2.5 h after the burst, under challenging sky conditions with cirrus. We detect the afterglow at a position consistent with the enhanced XRT error circle and NOT (Thoene et al., GCN #9403). With an exposure time of 40min in JHK and 49min in griz, preliminary photometry yields the following AB magnitudes: g =25.0 +-0.4 r =23.5 +-0.2 i =23.5 +-0.3 z >23.6 J >21.9 H >20.7 K >19.9 calibrated using SDSS and 2MASS field stars. The quoted magnitudes are not corrected for the galactic foreground extinction corresponding to a reddening of E_(B-V)=0.04. The large g-i color as compared to r-i indicates that the Lyman break may be located in the g' band. Fitting the SED with Hyper-Z results in a preliminary photometric redshift of z = 3.9+0.4-0.7, assuming no intrinsic extinction. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9409 SUBJECT: GRB 090519: VLT spectroscopic redshift DATE: 09/05/20 08:54:17 GMT FROM: Paolo D'Avanzo at INAF-OAB A. J. Levan (Univ. Warwick), P. Jakobsson (U. Iceland), C. C. Thoene (INAF/OAB), P. D'Avanzo (U. Bicocca & INAF/OAB), A. De Cia (U. Iceland), J. P. U. Fynbo, J. Hjorth, D. Malesani (DARK/NBI), D. Fugazza (INAF/OAB), N. R. Tanvir (U. Leicester) report on behalf of a larger collaboration: Using FORS2 on the ESO Very Large Telescope, we have obtained low-resolution spectra (3 x 30 min) of the optical afterglow of GRB 090519 (Perri et al., GCN 9400; Thoene et al., GCN 9403) with the grism 300V, covering the wavelength range 3500-9200 AA. In the acquisition image the afterglow has a magnitude of R ~ 23.5. The first spectrum was taken approximately 4 hours after the burst. In a preliminary analysis we detect a break around 4400 AA and strong absorption features around 5000 AA and 5900 AA. We interpret these features as the Lyman limit, Lyman-beta and Lyman-alpha at a redshift of z = 3.85. This is in agreement with the photometric redshift reported by Rossi et al. (GCN 9408). We thank the Paranal staff for excellent support, in particular Gianni Marconi, Kieran O'Brien and Patricia Guajardo. [GCN OPS NOTE(20may09): Per the original first-author's (CCT) request, the author list was changed.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9410 SUBJECT: GRB 090519: NOT refined analysis DATE: 09/05/20 14:53:33 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst D. Malesani (DARK/NBI), C.C. Thoene (INAF/Brera), P. Jakobsson (Univ. Iceland), A.J. Levan (Univ. Warwick) J.P.U. Fynbo, B. Milvang-Jensen (DARK/NBI), report on behalf of a larger collaboration. We provide further analysis of the photometric data on the afterglow of GRB 090519 (Perri et al., GCN 9400) taken at the NOT and VLT (Thoene et al., GCN 9403; Levan et al., GCN 9409). Calibration of the field based on archival VLT zeropoints yields a significantly fainter magnitude for the afterglow with respect to our previous GCN 9403, which was based on USNO stars. The new calibration is consistent with SDSS stars and with the value reported by Rossi et al. (GCN 9408). We find for the afterglow R = 22.8 on 2009 May 19.897 UT (0.33 hr after the GRB). The decay of the afterglow is well described by a power law with index alpha = 0.44 +- 0.03 between 0.33 and 3.6 hr after the GRB. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9411 SUBJECT: GRB 090519: Swift-XRT refined analysis DATE: 09/05/20 15:17:58 GMT FROM: Matteo Perri at ISAC/ASDC M. Perri, V. D'Elia, G. Stratta (ASDC) report on behalf of the Swift-XRT team: We have analysed the first 17 ks of XRT data for GRB 090519 (Perri et al., GCN Circ. 9400), from 121 s to 37 ks after the BAT trigger. The first 41 seconds of data are in Windowed Timing (WT) mode and at later times in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN. Circ. 9405). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=2.8 (+/-0.2). At around T+580 s the decay flattens to an alpha of 0.6 (+/-0.3) before breaking again at about T+2 ks to a final decay with index alpha=1.4 (+0.3)(-0.2). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.5 (+/-0.2). The best-fitting intrinsic absorption column at z=3.85 (Thoene et al., GCN Circ. 9409) is 1.9(+1.7,-1.6)e22 cm^-2, in excess of the Galactic value of 3.0e20 cm^-2 (Kalberla et al. 2005). The counts-to-observed (-unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.9e-11 (5.4e-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 1.4, the count rate at T+24 hours will be 3e-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5e-14 (1.6e-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00352648. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9412 SUBJECT: GRB 090519B: Fermi GBM detection DATE: 09/05/20 15:32:50 GMT FROM: Andreas von Kienlin at MPE A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: "At 11:05:27.54 UT on 19 May 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090519B (trigger 264423929 / 090519462). The on-ground calculated location, using the GBM trigger data, is RA = 105.9, DEC = -56.7 (J2000 degrees, equivalent to 07h 04m, 56d 42'), with an uncertainty of 3.9 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 18 degrees. The GBM light curve shows a single peak lasting about 4 seconds superimposed on a lower-level continuum. The burst duration (T90) is about 87 s (8-1000 keV). The time-averaged spectrum from T0-2.432 s to T0+1.152 s is well fit by a simple power law function with index -1.63 +/- 0.05 (chi squared 822 for 720 d.o.f.). The event fluence (8-1000 keV) in this time interval is (1.40 +/- 0.01)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0-0.640 s in the 8-1000 keV band is 5.02 +/- 0.14 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."