THIS FILE CHANGES WITH TIME -- HIT THE RELOAD BUTTON NOW! ///////////////////////////////////////////////////////////////////// GRB 980519 12:20:10 UT SOD=44410 sec TJD=10952 DOY=139 BATSE Trigger Number is 6764. The BATSE lightcurve shows a duration ~30sec. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 74 SUBJECT: GRB980519, BeppoSAX-WFC position DATE: 98/05/19 17:02:00 GMT FROM: Luigi Piro at IAS/CNR Frascati Luigi Piro on behalf of the BeppoSAX team report: GB980519 (BATSE trigger n.6764) has been detected by the GRBM of BeppoSAX and by the WFC at about 12:20:00 UT of May 19. A preliminary position by the WFC is: RA(2000)=350.54 Dec(2000)=77.293 with an error radius of 5'. A BeppoSAX follow up with the NFI is being planned. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 75 SUBJECT: GRB980519, BeppoSAX-WFC updated position DATE: 98/05/19 17:19:24 GMT FROM: Luigi Piro at IAS/CNR Frascati Luigi Piro on behalf of the BeppoSAX team report: GB980519 (BATSE trigger n.6764) was detected by the GRBM of BeppoSAX and by the WFC at about 12:20:00 UT of May 19. Refined position from the WFC are: RA(2000)=350.561 Dec(2000)=+77.255 with an error radius of 3'. This is 2' from the preliminary position. [GCN Operator's Note: Due to an unfortunate and rare scheduling conflict at the GCN end, the original position notice was closely spaced in time with this updated position notice.] ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 78 SUBJECT: GRB980519 optical observations DATE: 98/05/20 02:46:49 GMT FROM: Jens Hjorth at NORDITA The Nordic Optical Telescope GRB team (A. O. Jaunsen, J. Hjorth, M. I. Andersen, K. Kjernsmo, H. Pedersen, E. Palazzi) reports the detection at the 2.5-m NOT of an unresolved (in seeing of 1.5"-2"), variable object located within the BeppoSAX error box of GRB 980519 (GCN #75). The coordinates (+- 0.5") are RA(2000) = 23 22 21.46 Dec(2000) = +77 15 43.0 The object had an I magnitude of about 19.5 on May 19.87 UTC but is not detected in the DSS while objects of similar magnitude are. The OT had faded by about 0.6 mag in V and I on May 20.0 UTC. These observations suggest that the OT is the optical counterpart of GRB 980519. Preliminary Cousins I photometry (+-0.1 mag, not corrected for extinction) of 4 nearby reference stars yields RA(2000) Dec(2000) I A 23 22 17.74 +77 15 51.2 19.04 B 23 22 27.29 +77 15 43.5 19.49 C 23 22 28.50 +77 15 25.4 18.52 D 23 22 47.14 +77 16 23.5 15.69 On this system the OT had I=20.08 on May 20.00 UTC Finding charts, images and updates will be posted at http://www.uio.no/~ajaunsen/grb980519 This note can be cited. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 79 SUBJECT: GRB 980519 Optical Observations DATE: 98/05/20 12:35:45 GMT FROM: George Djorgovski at Caltech/Palomar GRB980519 Optical Observations S. G. Djorgovski, R. R. Gal, S. R. Kulkarni, J. S. Bloom, and A. Kelly, on behalf of the Caltech GRB Collaboration, report: "We obtained multicolor (BVRri) CCD images of the field of GRB 980519 (see GCN Circ. 75), using Palomar Observatory 200-inch and 60-inch telescopes, on UT May 20. We confirm the optical transient (OT) discovered by Jaunsen et al. (GCN Circ. 78). The object is continuing to fade. Using the magnitudes of stars B and C of Jaunsen et al. (their star A gives discrepant results) to tie in the instrumental magnitude systems, we derive for the OT: I = 21.46 (+- 0.1) in this magnitude system, on UT May 20.436 (mean epoch). Comparing with the value of I = 20.08 mag in the same system on UT May 20.00 from Jaunsen et al., we derive the power-law decline slope of -1.98 for the I-band light curve. This is fully consistent with the relative V-band light curve given at http://www.uio.no/~ajaunsen/grb980519. These measurements are preliminary. A more detailed analysis of the data is in progress. This note can be cited." ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 80 SUBJECT: GRB980519 Optical Observations DATE: 98/05/20 15:11:30 GMT FROM: Jules Halpern at Columbia U. The MDM Observatory GRB team (J. Kemp, J. Halpern) reports followup photometry of the variable optical candidate discovered by Jaunsen et al. (GCN #78) in the BeppoSAX error box of GRB 980519. In a series of CCD images taken with the MDM 1.3m telescope, centered around May 20.31 UT, the candidate had I=20.1+/-0.3, R=20.9+/-0.2. These magnitudes were measured differentially with respect to stars A, B, and C of Jaunsen et al., which we recalibrated using Landolt standards. Preliminary photometry of those reference stars is as follows: RA(2000) Dec(2000) R I A 23 22 17.74 +77 15 51.2 17.93 17.28 B 23 22 27.29 +77 15 43.5 (19.26) (18.56) C 23 22 28.50 +77 15 25.4 18.15 17.43 Parentheses indicate values that are less certain. Note the large discrepancy between our I-band measurements and those of Jaunsen et al.; the latter may instead refer to the V band. MDM images will be posted at http://cba.phys.columbia.edu/jonathan/grb/. This note can be cited. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 81 SUBJECT: GRB980519 IPN POSITION DATE: 98/05/20 17:01:26 GMT FROM: Kevin Hurley at UCBerkeley/SSL The position of this burst has been obtained by triangulation using Ulysses and BATSE preliminary data. It is described by an annulus centered at RA(2000)=329.485, Dec(2000)=-11.873, whose radius is 89.981 degrees, and whose total width is 4.9 arcminutes. This annulus intersects the refined SAX WFC error circle (BeppoSAX GRB Mail No. 98/16) and is consistent with the position of the optical transient reported by J. Hjorth (GCN 78). A figure may be found at http://ssl.berkeley.edu/ipn3/980519. Processing with the final data is expected to improve this position. This message is citeable. ///////////////////////////////////////////////////////////////////// Circular No. 6910 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) BMARSDEN@CFA.HARVARD.EDU or DGREEN@CFA.HARVARD.EDU (science) URL http://cfa-www.harvard.edu/iau/cbat.html Phone 617-495-7244/7440/7444 (for emergency use only) GRB 980519 J. M. Muller, BeppoSAX Science Data Center, Rome, and Space Research Organization of the Netherlands (SRON), Utrecht; J. Heise, SRON; C. Butler, Agenzia Spaziale Italiana, Rome; F. Frontera, Istituto Tecnologie e Studio Radiazioni Extraterrestri (ITESRE), Bologna; L. Di Ciolo, G. Gandolfi and A. Coletta, BeppoSAX Science Operation Center, Telespazio, Rome; and P. Soffitta, Istituto Astrofisica Spaziale (IAS), CNR, Frascati, communicate on behalf of the BeppoSAX team: "On May 19.51410 UT, a gamma-ray burst (Bacodine trigger 6764) was detected by the Gamma-Ray Burst Monitor onboard BeppoSAX. A preliminary analysis shows a complex burst lasting 30 s with a peak intensity of about 1500 counts/s (40-700 keV). An x-ray counterpart of this burst was detected by the Wide Field Camera WFC2 having a duration of 190 s and a peak flux of about 2.5 Crab (2-28 keV). The position derived from the WFC2 image is R.A. = 23h22m15s, Decl. = +77o15'.0 (equinox 2000.0; error radius 3'). A BeppoSAX follow-up observation is in progress." (C) Copyright 1998 CBAT 1998 May 20 (6910) Daniel W. E. Green ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 82 SUBJECT: GRB980519 Optical Observations DATE: 98/05/20 19:55:36 GMT FROM: Eric Deutsch at U.Washington On behalf of the Apache Point Observatory GRB team, A. Diercks & C. Stubbs observed with the APO 3.5m telescope the optical transient (OT) discovered by Jaunsen et al. (GCN #78) in the BeppoSAX error box of GRB 980519. Conditions were mostly cloudy with roughly 1.8 arcsec seeing. Photometry by E. Deutsch & A. Diercks on a 1 hr series of images centered around May 20.44 UT yields the following magnitudes and relative uncertainties for the OT and reference stars: ID R mag RelErr -- ----- ----- OT 21.20 0.03 A 17.93 0.01 B 19.31 0.01 C 18.06 0.01 Absolute calibration is based only on R magnitudes of reference stars reported by Kemp & Halpern (GCN #80). No independent calibration was possible due to heavy clouds. Our measurement is 0.3 mag fainter than the earlier observations of Kemp & Halpern (GCN #80). Images are posted at: http://www.astro.washington.edu/deutsch/grb/grb980519/ This note can be cited. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 83 SUBJECT: GRB980519 Optical Observations DATE: 98/05/20 23:16:27 GMT FROM: Fredrick J Vrba at USNO GRB980519 Optical Observations The U. S. Naval Observatory GRB team (F. J. Vrba, B. Canzian, S. E. Levine, H. H. Guetter, A. A. Henden, C. B. Luginbuhl, J. A. Munn), D. H. Hartmann (Clemson Univ.), and M. C. Jennings (IGPP, UCR visitor) report follow up optical photometry of the variable object found by Jaunsen et al. (GCN Report 78) within the BeppoSAX error circle of GRB980519 (see GCN Report 75). Observations were obtained with the USNO Flagstaff Station 40-inch telescope between UT 1998 May 20.143 and 20.328 under the pole and again between UT 1998 May 20.426 and 20.464 when the field could be re-acquired at large hour angle. Four sets of observations were obtained in the Cousins R filter, two in the Cousins I filter, and one in the Johnson/Cousins V filter. Each set of observations consisted of three co-added and dithered images of 10 minutes each. The observations were obtained through variable cirrus clouds and haze. Preliminary reductions of the R-filter data by comparing with the magnitudes of stars A, B, and C as given in GCN Report 80 yield: UT Date R (mag) 1998 May 20.163 20.39 +/- 0.12 20.229 20.77 +/- 0.15 20.287 20.87 +/- 0.13 20.445 21.15 +/- 0.13 The uncertainties reflect both the internal photometry errors and the scatter in the magnitude offsets to stars A, B, and C. These data are consistent with the single R magnitudes from the MDM telescope (GCN Report 80) and the APO 3.5-m telescope (GCN Report 82). The lightcurve derived from these combined datapoints can be found on our web site at: http://psyche.usno.navy.mil/nofs/grb/grb980519.html. During this time interval the data do not appear to be consistent with a simple power law decrease in brightness. In a more detailed analysis we plan to also reduce these data with respect to two TYCHO stars within our CCD FOV and to analyze the V and I data to investigate colors. For further information contact F. J. Vrba at fjv@nofs.navy.mil or by telephone at (520) 779-5132. This GCN note can be cited. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 84 SUBJECT: GRB980519 optical observations DATE: 98/05/21 09:17:17 GMT FROM: Jens Hjorth at NORDITA GRB 980519 Optical Observations On behalf of the Nordic Optical Telescope GRB team J. Hjorth, A. O. Jaunsen, K. Kjernsmo, and H. Pedersen report updated as well as new photometry of the optical transient (Jaunsen et al., GCN #78) believed to be related to GRB 980519. As indicated by Djorgovski et al. (GCN #79) and Kemp & Halpern (GCN #80) the photometry reported in GCN #78 was incorrect. This was due to the strongly variable, non-photometric conditions prevailing at the time of observations. Adopting the Kemp & Halpern (GCN #80) zero point the updated photometry of the OT yields I=18.48+-0.1 on May 19.88 UT and I=19.05+-0.03 on May 20.00 UT. In the same photometric system we report the following measurements: May 20.98 UT I=21.64+-0.2 May 21.17 UT I=21.64+-0.1 These measurements are uncertain as the OT is close to the detection limit in our images. Thus, the rapid decay has continued during May 20 UT. Our last measurements provide marginal evidence that the decay has leveled off. If confirmed, this may be due to non-trivial intrinsic variability of the source or to an extra source of light along the line of sight to the OT, eg. the host galaxy. The above findings are preliminary. A more detailed analysis of the data is in progress. This note can be cited. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 85 SUBJECT: GRB970519, optical follow-up at Schmidt Calern DATE: 98/05/21 14:56:00 GMT FROM: Michel Boer at CESR-CNRS Alain Maury (OCA), D. albanese (OCA), and Michel Boer (CESR/CNRS) report: "We obtained images of the localization of GRB 980519 (GCN circ 75) as reported by BeppoSAX team, on May 19 and 20 using the 90cm Schmidt telescope of the Observatoire de la Cote d'Azur. The optical transient reported by Jaunsen et al. (GCN Circ. 78) is clearly detected and fading on images taken at UT May 19.862556, 20.076519, 20.964261 on unfiltered exposures. The corresponding magnitudes are May 19.862556 19.06 +- 0.26 May 20.076519 19.81 +- 0.37 May 20.964261 22.06 +- 0.76 The power-law slope decline is roughly 2.0, which, given the uncertainties is consistent with the value reported by Djorgovski et al. (GCN circ. 79) The images, the light curve and a small GIF animation is given at http://wwwrc.obs-azur.fr/schmidt/980519.html This notice is citable ================================================================================ Michel Boer Tel.: (33) (0) 5 61 55 66 40 Centre d'Etude Spatiale des Rayonnements fax: (33) (0) 5 61 55 67 01 (CESR - CNRS) Internet: boer@cesr.fr 9, ave. du Colonel Roche BP 4346 31028 Toulouse Cedex 4 ================================================================================ ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 86 SUBJECT: GRB980519 BATSE Observations DATE: 98/05/21 18:33:07 GMT FROM: Valerie Connaughton at MSFC V. Connaughton (National Research Council and NASA Marshall Space Flight Center) reports on behalf of the BATSE GRB team: GRB980519 (GCN 74) was detected by BATSE on May 19.51403 as trigger 6764. The event lasted about 60 seconds and was seen as a series of spikes riding on a single pulse for the first 20 seconds, followed by a gradual decay. A peak flux of 6.94 +/- 0.25 photons cm^-2 s^-1 between 50 and 300 keV, integrated over 64 ms, places it in the brightest 12% of BATSE bursts. The fluence above 25 keV is 2.54 +/- 0.41 x 10^-5 erg cm^-2. The location is consistent with the BeppoSAX-WFC position in GCN 74 & 75. A light curve of the event can currently be obtained by e-mail from me at vc@msfc.nasa.gov, or will be available next week at http://www.batse.msfc.nasa.gov/~kippen/batserbr/ when the BATSE Web server is back in operation. This message is citeable. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 87 SUBJECT: GRB 980519 Optical Observations DATE: 98/05/22 00:47:18 GMT FROM: Josh Bloom at CIT GRB 980519 Optical Observations J. S. Bloom, S. G. Djorgovski, R. R. Gal, S. R. Kulkarni, and A. Kelly, on behalf of the Caltech GRB Collaboration, report: "We obtained CCD images of the field of GRB 980519 using COSMIC on the Palomar Observatory 200-inch on UT May 20. In particular, we imaged the GRB field for 500 s (Cousins R) and 600 s (Gunn i). We photometrically calibrated our Gunn i-band and Cousins R-band images against standard Landolt 1992 (AJ 104, 340) stars (in SA 113). We accounted for atmosphere extinction and included a color correction term in the fit to account for the fact that Landolt reports magnitudes in a different R and I band system. Derived magnitudes of the following 10 secondary stars are thus in the Londolt RI system (we kept the naming the convention of Jansen et al. GCN 78): Object RA DEC I_landolt err R_landolt err A 23:22:20.0 +77:15:52 17.34 +/- 0.05 17.94 +/- 0.05 B 29.6 44 18.64 +/- 0.05 19.41 +/- 0.05 C 28.7 26 17.57 +/- 0.05 18.10 +/- 0.05 E 20.6 24 18.85 +/- 0.05 20.19 +/- 0.06 F 31.8 45 18.48 +/- 0.05 19.91 +/- 0.06 G 33.2 +77:14:59 17.25 +/- 0.05 19.02 +/- 0.05 H 20.7 14:55 18.13 +/- 0.05 19.44 +/- 0.05 I 09.2 +77:15:51 19.27 +/- 0.06 19.80 +/- 0.06 J 07.6 +77:16:01 19.05 +/- 0.06 20.08 +/- 0.06 L 35.0 16:15 18.57 +/- 0.05 19.21 +/- 0.05 Uncertainty in optimum aperture size for each star is the dominate source of statistical error. There is an overall zero-point systematic error (not included above) in each band which amounts to 0.150 mag (I) and 0.151 (R). The approximate RA and DEC are measured in J2000 from the Digital Sky Survey (DSS). We note our derivation for A,B, and C magnitudes are highly discrepant from that of Jansen et al. GCN #78, but agree quite well with that of Kemp and Halpern (GCN #80) and Diercks et al. (GCN #82). At the time of observations we find the OT has magnitudes of May 20.43 UT, I_landolt = 20.86 +/- 0.11; May 20.48 UT, R_landolt = 21.57 +/- 0.09. A finding chart with the secondary stars noted may be found at http://astro.caltech.edu/~jsb/grb980519.ps This message may be cited." ///////////////////////////////////////////////////////////////////// TITLE: GCN/IPN/HUNTSVILLE LOCALIZATION NOTICE_TYPE: Final (based on the Huntsville AD Report location) NOTICE_DATE: Thu May 21 01:09:02 GMT 1998 TRIGGER_NUM: 6764 GRB_DATE: 98/05/19 GRB_TIME: 12:20:12.64 UT BACO_RA: 54.58d {+03h 38m 18s} (J2000) BACO_DEC: +64.84d {+64d 50' 07"} HUNT_RA: 356.78d {+23h 47m 07s} (J2000) HUNT_DEC: 76.34d {+76d 20' 10"} HUNT_ERR: 1.94 [degees radius, statistical only] B_H_DELTA: 21.09 [deg] HUNT_SC_AZ: 6.10 [deg] HUNT_SC_EL: 35.40 [deg] {Zen_angle=54.60} SUN_POSTN: 56.08d {+03h 44m 19s} +19.79d {+19d 47' 14"} (Current) SUN_B_DIST: 45.05 [deg] MOON_POSTN: 334.25d {+22h 17m 01s} -10.39d {-10d 23' 11"} (Current) MOON_B_DIST: 95.31 [deg] ANNULUS_RA: 329.4854d {+21h 57m 56s} (J2000) ANNULUS_DEC: -11.8727d {-11d 52' 21"} ANNULUS_RADIUS: 89.964 [deg] ANNULUS_WIDTH: 0.104 [deg] (Total width) COMMENTS: GRB. LOTS OF STRUCTURE. DURATION APPROX. = 60 SEC. VISIBLE ABOVE 300KEV. This IPN localization is preliminary. The "total width" of the annulus was selected to include all known uncertainties and systematics. The final analysis will reduce this width. All follow-up queries should be addressed to Kevin Hurley (UC Berkeley, khurley@sunspot.ssl.berkeley.edu). The center of the IPN annulus is tabulated below along the segment that intersects the Huntsville error circle. The Distance column is the sky-angle distance between the Huntville location and the sampled position on the arc segment. The position of maximum probability plus the 1-, 2-, & 3-sigma containment probabilities (statistical+systematic) are marked. A detailed description of the format, content, and meaning of this document is given in the URL: http://gcn.gsfc.nasa.gov/gcn/ipn.html (J2000) RA DEC Distance 15.277 73.171 5.77 <=== +3-sigma probability 15.111 73.218 5.70 14.945 73.265 5.63 14.778 73.311 5.57 14.612 73.357 5.50 14.446 73.403 5.43 14.280 73.448 5.37 14.113 73.493 5.30 13.947 73.537 5.24 13.781 73.582 5.17 13.614 73.625 5.11 13.448 73.669 5.05 13.281 73.712 4.98 13.115 73.755 4.92 12.948 73.797 4.86 12.782 73.840 4.79 12.615 73.881 4.73 12.449 73.923 4.67 12.282 73.964 4.61 12.115 74.005 4.55 11.949 74.045 4.49 11.782 74.085 4.43 11.615 74.125 4.36 11.449 74.165 4.30 11.282 74.204 4.24 11.115 74.243 4.19 10.949 74.281 4.13 10.782 74.320 4.07 10.615 74.358 4.01 10.448 74.395 3.95 10.282 74.433 3.89 10.115 74.470 3.83 <=== +2-sigma probability 9.948 74.507 3.78 9.782 74.543 3.72 9.615 74.579 3.66 9.448 74.615 3.60 9.282 74.651 3.55 9.115 74.686 3.49 8.948 74.721 3.44 8.782 74.756 3.38 8.615 74.790 3.32 8.449 74.824 3.27 8.282 74.858 3.21 8.115 74.892 3.16 7.949 74.925 3.11 7.782 74.958 3.05 7.616 74.991 3.00 7.450 75.024 2.94 7.283 75.056 2.89 7.117 75.088 2.84 6.950 75.120 2.78 6.784 75.151 2.73 6.618 75.183 2.68 6.451 75.214 2.63 6.285 75.244 2.57 6.119 75.275 2.52 5.953 75.305 2.47 5.787 75.335 2.42 5.620 75.365 2.37 5.454 75.394 2.32 5.288 75.424 2.27 5.122 75.453 2.22 4.956 75.482 2.17 4.790 75.510 2.12 4.625 75.539 2.07 4.459 75.567 2.02 4.293 75.595 1.97 4.127 75.622 1.92 <=== +1-sigma probability 3.961 75.650 1.87 3.796 75.677 1.82 3.630 75.704 1.77 3.464 75.731 1.72 3.299 75.757 1.68 3.133 75.784 1.63 2.968 75.810 1.58 2.803 75.836 1.53 2.637 75.861 1.49 2.472 75.887 1.44 2.307 75.912 1.39 2.142 75.937 1.35 1.976 75.962 1.30 1.811 75.987 1.25 1.646 76.011 1.21 1.481 76.035 1.16 1.316 76.059 1.12 1.151 76.083 1.07 0.987 76.107 1.03 0.822 76.130 0.98 0.657 76.153 0.94 0.492 76.177 0.90 0.328 76.199 0.85 0.163 76.222 0.81 359.999 76.245 0.77 359.834 76.267 0.73 359.670 76.289 0.69 359.506 76.311 0.64 359.341 76.333 0.61 359.177 76.354 0.57 359.013 76.376 0.53 358.849 76.397 0.49 358.685 76.418 0.46 358.521 76.439 0.42 358.357 76.459 0.39 358.193 76.480 0.36 358.029 76.500 0.33 357.865 76.520 0.31 357.702 76.540 0.29 357.538 76.560 0.28 357.374 76.580 0.28 <=== Max probability 357.211 76.599 0.28 357.047 76.618 0.29 356.884 76.638 0.30 356.721 76.656 0.32 356.557 76.675 0.34 356.394 76.694 0.37 356.231 76.712 0.39 356.068 76.731 0.42 355.905 76.749 0.46 355.742 76.767 0.49 355.579 76.785 0.53 355.416 76.802 0.56 355.253 76.820 0.60 355.090 76.837 0.63 354.928 76.855 0.67 354.765 76.872 0.71 354.602 76.889 0.74 354.440 76.905 0.78 354.277 76.922 0.82 354.115 76.938 0.86 353.953 76.955 0.90 353.790 76.971 0.93 353.628 76.987 0.97 353.466 77.003 1.01 353.304 77.018 1.05 353.142 77.034 1.09 352.980 77.049 1.13 352.818 77.065 1.16 352.656 77.080 1.20 352.494 77.095 1.24 352.332 77.110 1.28 352.171 77.125 1.32 352.009 77.139 1.35 351.847 77.154 1.39 351.686 77.168 1.43 351.524 77.182 1.47 351.363 77.196 1.51 351.201 77.210 1.54 351.040 77.224 1.58 350.879 77.238 1.62 350.718 77.251 1.66 350.557 77.265 1.69 350.396 77.278 1.73 350.234 77.291 1.77 350.074 77.304 1.81 349.913 77.317 1.84 349.752 77.330 1.88 349.591 77.343 1.92 349.430 77.355 1.95 <=== -1-sigma probability 349.269 77.367 1.99 349.109 77.380 2.03 348.948 77.392 2.06 348.788 77.404 2.10 348.627 77.416 2.14 348.467 77.428 2.17 348.306 77.439 2.21 348.146 77.451 2.25 347.986 77.462 2.28 347.826 77.474 2.32 347.665 77.485 2.36 347.505 77.496 2.39 347.345 77.507 2.43 347.185 77.518 2.46 347.025 77.528 2.50 346.865 77.539 2.54 346.705 77.549 2.57 346.546 77.560 2.61 346.386 77.570 2.64 346.226 77.580 2.68 346.066 77.590 2.72 345.907 77.600 2.75 345.747 77.610 2.79 345.588 77.620 2.82 345.428 77.629 2.86 345.269 77.639 2.89 345.109 77.648 2.93 344.950 77.657 2.96 344.791 77.666 3.00 344.631 77.676 3.03 344.472 77.684 3.07 344.313 77.693 3.10 344.154 77.702 3.14 343.995 77.711 3.17 343.836 77.719 3.21 343.677 77.728 3.24 343.518 77.736 3.28 343.359 77.744 3.31 343.200 77.752 3.35 343.041 77.760 3.38 342.882 77.768 3.41 342.724 77.776 3.45 342.565 77.783 3.48 342.406 77.791 3.52 342.248 77.799 3.55 342.089 77.806 3.59 341.930 77.813 3.62 341.772 77.820 3.65 341.613 77.827 3.69 341.455 77.834 3.72 341.296 77.841 3.76 341.138 77.848 3.79 340.980 77.855 3.82 340.821 77.861 3.86 340.663 77.868 3.89 <=== -2-sigma probability 340.505 77.874 3.93 340.347 77.880 3.96 340.189 77.887 3.99 340.030 77.893 4.03 339.872 77.899 4.06 339.714 77.905 4.09 339.556 77.910 4.13 339.398 77.916 4.16 339.240 77.922 4.19 339.082 77.927 4.23 338.924 77.933 4.26 338.766 77.938 4.29 338.609 77.943 4.33 338.451 77.948 4.36 338.293 77.953 4.39 338.135 77.958 4.43 337.977 77.963 4.46 337.820 77.968 4.49 337.662 77.973 4.53 337.504 77.977 4.56 337.347 77.982 4.59 337.189 77.986 4.63 337.031 77.990 4.66 336.874 77.994 4.69 336.716 77.999 4.73 336.559 78.003 4.76 336.401 78.007 4.79 336.244 78.010 4.82 336.086 78.014 4.86 335.929 78.018 4.89 335.771 78.021 4.92 335.614 78.025 4.96 335.457 78.028 4.99 335.299 78.032 5.02 335.142 78.035 5.05 334.985 78.038 5.09 334.827 78.041 5.12 334.670 78.044 5.15 334.513 78.047 5.18 334.355 78.049 5.22 334.198 78.052 5.25 334.041 78.055 5.28 333.884 78.057 5.31 333.726 78.060 5.35 333.569 78.062 5.38 333.412 78.064 5.41 333.255 78.066 5.45 333.098 78.068 5.48 332.941 78.070 5.51 332.784 78.072 5.54 332.626 78.074 5.58 332.469 78.076 5.61 332.312 78.077 5.64 332.155 78.079 5.67 331.998 78.080 5.71 331.841 78.082 5.74 331.684 78.083 5.77 331.527 78.084 5.80 331.370 78.085 5.83 <=== -3-sigma probability -------------------------------- THE END -------------------------------- ////////////////////////////////////////////////////////////// Circular No. 6912 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) BMARSDEN@CFA.HARVARD.EDU or DGREEN@CFA.HARVARD.EDU (science) URL http://cfa-www.harvard.edu/iau/cbat.html Phone 617-495-7244/7440/7444 (for emergency use only) GRB 980519 L. Nicastro, Istituto di Fisica Cosmica ed Applicazioni all'Informatica, CNR, Palermo; L. A. Antonelli, BeppoSAX Science Data Center, Rome; G. Celidonio, M. R. Daniele, C. De Libero, and G. Spoliti, BeppoSAX Science Operation Center, Rome; L. Piro, Istituto Astrofisica Spaziale, CNR, Rome; and E. Pian, Istituto di Tecnologie e Studio delle Radiazioni Extraterrestri, CNR, Bologna, on behalf of the BeppoSAX team, report: "The BeppoSAX Wide Field Camera error box of GRB 980519 (IAUC 6910) was observed with the BeppoSAX Narrow Field Instruments starting on May 19.920 UT (9.7 hr after the burst). A previously unknown x-ray source, 1SAX J2322.3+7716, was detected by the LECS and MECS instruments (units 2 and 3) at R.A. = 23h22m22s, Decl. = +77o16'.1 (equinox 2000.0; error radius 50"). This position is 1'.2 from the centroid of the WFC position and is compatible with the optical transient detected by Jaunsen et al. (GCN 78; R.A. = 23h22m21s.46, Decl. = +77o15'43".0, equinox 2000.0; I about 19.5 on May 19.87). The source exhibits a non-monotonic decay, steeper during the first 4-5 hr of the 1.2-day observation. The average count rate of the first 4 hr is 0.007 +/- 0.001 counts/s (2-10 keV) in the two MECS units, corresponding to (3.8 +/- 0.6) x 10E-13 erg cmE-2 sE-1 (assuming a Crab-like energy spectrum). At the end of the observation, the source had faded by a factor of about 4. These results strongly suggest that 1SAX J2322.3+7716 is the x-ray afterglow of GRB 980519." (C) Copyright 1998 CBAT 1998 May 22 (6912) Daniel W. E. Green ///////////////////////////////////////////////////////////////////// Circular No. 6913 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) BMARSDEN@CFA.HARVARD.EDU or DGREEN@CFA.HARVARD.EDU (science) URL http://cfa-www.harvard.edu/iau/cbat.html Phone 617-495-7244/7440/7444 (for emergency use only) GRB 980519 A. Maury and D. Albanese, Observatoire de la Cote d'Azur (OCA); M. Boer, Centre d'Etude Spatiale des Rayonnements, CNRS; and M. Feroci, Istituto Astrofisica Spaziale, CNR, report: "We obtained images of the field of GRB 980519 (IAUC 6909, 6910, 6912) on May 19 and 20 with the OCA 0.90-m Schmidt telescope. The optical transient reported by Jaunsen et al. (GCN 78) is clearly detected and fading on unfitered exposures taken on May 19.86256, 20.07652, and 20.96426 UT, at which time we measure magnitudes 19.06 +/- 0.26, 19.81 +/- 0.37, and 22.06 +/- 0.76, respectively. The power- law slope decline is roughly 2.0, which, given the uncertainties, is consistent with the value reported by Djorgovski et al. (GCN 79). The images and the light curve are available at http://wwwrc.obs-azur.fr/schmidt/980519.html." (C) Copyright 1998 CBAT 1998 May 22 (6913) Daniel W. E. Green ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 88 SUBJECT: GRB980519 optical observations DATE: 98/05/22 22:19:07 GMT FROM: Roy Gal at CalTech GRB980519 Optical Observations with Keck and Palomar R. R. Gal, J. S. Bloom, C. Steidel, K. L. Adelberger, S. G. Djorgovski, and S. R. Kulkarni, on behalf of the Caltech GRB Collaboration, report: "We have obtained additional photometric CCD images of the field of GRB 980519. C. Steidel and K. Adelberberger have obtained 11 minutes of R-band data using the W.M. Keck Observatory 10-m, and R. Gal has obtained 800 sec. of i band data and 750 sec. of R band data with the Palomar Observatory 5-m on UT May 21. We measured magnitudes for the OT using the Landolt magnitude system derived by Bloom et al.(GCN #87) for the nearby stars. The OT is no longer visible in our i-band data, with an upper limit of I > 21.6 +/- 0.7, at UT May 21.43. The OT is still seen in the R band with R = 23.48 +/- 0.2 at UT May 21.469 (Palomar) and R = 23.10 +/- 0.13 at UT May 21.6 (Keck). The fainter Palomar magnitude at the earlier epoch is likely due to poor seeing conditions (>2") which place the object close to our detection limit. C. Steidel and K. Adelberger also report that in seeing conditions of 0.75" at Keck the OT is not distinguishable from a point source. We note that these observations place an upper limit on the magnitude of the OT host galaxy of not brighter than R ~ 24 mag. Our R-band magnitudes are consistent with the source still fading with a slope of approximately 2.0, while the I-band data do not provide additional constraints on the slope. This message may be cited." ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 89 SUBJECT: GRB 980519 DATE: 98/05/22 22:21:24 GMT FROM: Dale A Frail at NRAO D. A. Frail, G. B. Taylor (NRAO), S. R. Kulkarni (Caltech), and the BeppoSAX GRB team report: Beginning on May 19.8, May 20.6 and May 22.3 UT we observed the field containing the fading X-ray source 1SAX J2322.3+7716 (Nicastro et al. IAUC 6912) with the VLA at 8.3 GHz. The May 22.3 UT observations detected a 102+/-19 microJy radio source coincident with the optical transient first seen by Jaunsen et al. (GCN 78). The radio source VLA J2322+7715 is at ra = 23h22m21.49s dec = +77d15'43.2" (equinox J2000) with a conservative error of 0.1 arcsec in each coordinate. Re-examining this location for the data taken on May 19.8 UT and May 20.6 UT we measure a flux density of 38+/-28 and 68+/-27 microJy, respectively. We propose that VLA J2322+7715 is the radio afterglow from GRB 980519. Additional radio observations are in progress to look for significant variability. This message may be cited. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 90 SUBJECT: GRB980519 I-band observations DATE: 98/05/22 22:23:30 GMT FROM: Francisco J Castander at UChicago GRB980519 I-band observations F. J. Castander, R. Evans, D. E. Reichart, D. Q. Lamb and W. Wild, University of Chicago, report: "We made I-band observations of the BeppoSAX WFC error circle for GRB980519 (GCN #75) on May 21.34 - 21.36 UT and May 22.27 - 22.38 UT, using the 41-inch telescope at Yerkes Observatory. On May 21.35, we detected the optical transient reported by Jaunsen et al. (GCN #78) at about I = 21.9 mag, near the limiting magnitude of the image. On May 22.33, we did not detect the optical transient down to an image limiting magnituide of I = 21.0 mag. These magnitudes are tied to the Bloom et al. (GCN #87) calibration standards. This report may be cited." /////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 91 SUBJECT: GRB980519 optical observations DATE: 98/05/22 23:19:18 GMT FROM: Alan Diercks at U.Washington On behalf of the Manastash Ridge Observatory GRB team, A. Diercks & J. Morgan observed with the MRO 0.76m telescope the optical transient (OT) discovered by Jaunsen et al. (GCN #78) in the BeppoSAX error box of GRB 980519. Conditions were cloudy with roughly 3 arcsec seeing. Photometry by E. Deutsch & A. Diercks on a 12,000s series of images centered around May 20.4 UT yields the following magnitudes and uncertainties for the OT and reference objects: ID R mag RelErr -- ----- ----- OT 21.07 0.25 A 17.93 0.05 B 19.36 0.08 C 18.06 0.05 Absolute calibration is based only on R magnitudes of reference stars reported by Bloom et al. (GCN #87). No independent calibration was possible due to thick clouds. Our measurement is consistent with the nearly simultaneous R magnitudes reported in GCN #80 and GCN #82. This note can be cited. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 92 SUBJECT: GRB 980519 Optical Observations DATE: 98/05/25 23:58:13 GMT FROM: Roy Gal at CalTech GRB 980519 Optical Observations R. R. Gal, J. S. Bloom, S. G. Djorgovski, and S. R. Kulkarni on behalf of the Caltech GRB Collaboration, report: "In addition to the I and R photometry reported by Bloom et al. (GCN #87), we have photometered the B and V Palomar 200inch images of the field of GRB 980519. Derived magnitudes of the following 7 secondary stars are in the Landolt BV system (see GCN #87 for details): Star B err(B) V err(V) A 19.51 0.13 18.31 0.12 B 21.74 0.34 20.05 0.09 C 19.27 0.11 18.35 0.08 E 22.88 0.11 21.07 0.24 F 22.61 0.17 20.83 0.13 G 21.51 0.19 19.74 0.10 H 21.94 0.29 20.26 0.13 The derived magnitudes of the OT are: May 20.4485 UT, B = 22.53 +/- .14 May 20.466 UT, V = 21.74 +/- .16 May 21.448 UT, B > 22.9 (3-sigma upper limit) May 21.476 UT, V > 22.0 (3-sigma upper limit) The non-detection on May 21 is consistent with the power-law decline slope of beta = -1.98 reported in Djorgovski et al. (GCN #79). Moreover, broadband colors circa May 20.4 (BV reported herein; RI reported in Bloom #87) suggest a spectral index of alpha = -1.26 +/- 0.3. This is also consistent with the simple blastwave model (eg. Wijers, Rees and Meszaros MNRAS 288, L51.) prediction that alpha = (2/3) beta. The V-band point is somewhat higher (~3 sigma) than the extrapolated spectrum, suggesting the spectrum of the transient may not have been a pure power-law. Lastly, given the general consistency of spectral slope with flux time decay, we note the absence of strong extinction in the OT (in contrast to GRB 980329). This report may be cited." ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 96 SUBJECT: GRB980519 Secondary Standards DATE: 98/06/05 00:37:19 GMT FROM: Arne A Henden at USNO/USRA The U. S. Naval Observatory GRB team (A. A. Henden, F. J. Vrba, C. B. Luginbuhl, B. Canzian, S. E. Levine, H. H. Guetter, J. A. Munn) report follow up optical photometry of the secondary standards (see Jaunsen, et. al. GCN 78 and Bloom, et. al. GCN 87) in the field of GRB980519. The observations were made on two photometric nights during the past week with the USNO 1.0m telescope. Johnson BV and Cousins RI filters were used, with an average of 32 Landolt standards of wide color range and extinction observed on each night. The transformations are accurate to 0.01-0.02mag per single observation. DAOPHOT psf fitting was used in the GRB field, with magnitude corrections to adjust the photometry to a standard aperture diameter. Given below is the photometry, with errors based on the variance between the two nights. More detail, including coordinates and comparisons between other published values for these stars, can be found on our Web site at: http://psyche.usno.navy.mil/nofs/grb/grb980519.html For further information contact A. A. Henden at aah@nofs.navy.mil or by telephone at (520) 779-5132. This GCN note can be cited. ID B Berr V Verr R Rerr I Ierr -------------------------------------------------------------- A 19.661 0.114 18.558 0.018 17.914 0.005 17.338 0.027 B 20.218 0.061 19.318 0.027 18.477 0.001 C 19.313 0.060 18.549 0.027 18.029 0.004 17.525 0.004 D 16.433 0.003 15.614 0.005 15.139 0.000 14.686 0.004 E 21.230 0.146 19.998 0.030 18.767 0.022 F 21.174 0.226 19.900 0.109 18.578 0.289 G 19.915 0.006 18.867 0.004 17.999 0.054 H 20.574 0.062 19.432 0.044 17.990 0.050 I 20.054 0.021 19.645 0.042 19.138 0.007 J 20.907 0.036 20.001 0.011 19.148 0.011 ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 124 SUBJECT: GRB980519 observation report DATE: 98/07/06 11:22:28 GMT FROM: Elia Leibowitz at Wise Obs, Tel Aviv U Elia Leibowitz and Peter Ibbetson, Wise Observatory, Tel Aviv University, Israel report: Using the Wise Observatory 1-m telescope and the observatory Tectronix CCD camera, we obtained on May 20 a 1800 sec exposure of GRB980519, through a B filter. The time of mid-exposure is 01:22:11 UT. The image of the optical counterpart is at the limit of detectability. Applying the DAOPHOT photometry package we measured the instrumental magnitude of the counterpart and of nearby stars. Based on the B calibration of stars C and D of Henden et al. (GCN Circ. #96), we estimate the B magnitude of the optical counterpart as 20.95 +/- 0.25 mag. This message is quotable in publications. ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 148 SUBJECT: GRB980519, Optical Observations DATE: 98/07/29 16:15:36 GMT FROM: Vladimir Sokolov at SAO RAS The faintest GRB host galaxy? V. Sokolov, S. Zharikov (SAO-RAS), E. Palazzi (ITeSRE-CNR), L. Nicastro (IFCAI-CNR) and the SAX-GRB team report: "On 1998 July 23.85 UT and 24.96 UT we obtained a deep Rc band image of the field of the GRB 980519 optical transient (Jaunsen et al. GCN #78) with the 6-m BTA telescope of SAO-RAS. The total observing time was 9600 s with 600 s per exposure. Conditions were photometric with an average seeing of 1.20 arcsec. A faint extended source is clearly detected at the position of the OT. Due to the faintness of the object, we are not able to check if between the two nights there was any luminosity variation. The object magnitude was the same within the errors, and the photometry of the GRB 980519 OT in 2.5 arcsec diameter aperture was made by two observational nights and gave Rc = 26.05 +/- 0.22. For photometric calibration we used the secondary standards from Henden et al. (GCN #96). From the time of optical observations of GRB980519 OT with Keck and Palomar (GCN #88) in the R band the assumed power-law decline slope of -1.98 (GCN #79) would make the OT undetectable at the epoch of our observations. So, we conclude that the OT has stopped its power law decay a long time ago, and the observable now extended object is the host galaxy of GRB 980519 and it could be the faintest among those known up today. Images of the field will be posted at http://www.sao.ru/~zhar/home/GRB/980519.html This message can be cited." ///////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 149 SUBJECT: Optical Observations of the Host Galaxy of GRB 980519 DATE: 98/08/03 17:26:21 GMT FROM: Josh Bloom at CIT J. S. Bloom, S. R. Kulkarni, S. G. Djorgovski, R. R. Gal, A. Eichelberger, D. A. Frail report on behalf of the Caltech/NRAO GRB collaboration: "Data were obtained on the Keck II telescope on July 18, 1998 UT by Kulkarni and P. Groot (U. of Amsterdam) using the LRIS instrument. We confirm the existence of a faint object with R_c= 26.1 +/- 0.3 (July 18.516) at the position of the optical transient of GRB 980519 (GCN #78) and noted recently by Sokolov et al. (GCN 148). The exposure time was 1500 s. Despite excellent seeing conditions (0.6 arcsec, full width at half maximum) we see little evidence for extension of the source, the presumed host of the GRB. In addition, we note the non-detection (Gunn-i > 24.5) of the host on July 29.396 1998 (2400 sec exp; 1.5 arcsec seeing) with COSMIC on the 200-inch Telescope at Palomar. The Keck image of the host of GRB 980519 and secondary standard stars (GCN #87) may be obtained at http://astro.caltech.edu/~jsb/host_grb980519.ps" This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 698 SUBJECT: GRB980519, HST/STIS observations of the host galaxy DATE: 00/06/13 14:23:51 GMT FROM: Stephen Holland at IFA, U of Aarhus Stephen Holland, Johan Fynbo, Bjarne Thomsen (University of Aarhus), Michael Andersen (University of Oulu), Gunnlaugur Bjornsson (University of Iceland), Jens Hjorth (University of Copenhagen), Andreas Jaunsen (University of Oslo), Priya Natarajan (Univeristy of Cambridge, & Yale), and Nial Tanvir (University of Hertfordshire) We have initiated a survey of the host galaxies of gamma-ray bursts (GRBs) using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. The data will consist of deep images of the host galaxies of eleven GRBs taken at least one year after the GRB occurred. We have waived the normal one-year proprietary period for this data, and we will make drizzled images available to the astronomical community. The web site for the Survey of the Host Galaxies of Gamma-Ray Bursts is "http://www.ifa.au.dk/~hst/grb_hosts/index.html". We have obtained 8983 seconds of STIS images taken with the 50CCD (clear) aperture of GRB 980519. A combined image is now available at "http://www.ifa.au.dk/~hst/grb_hosts/data/index.html". This data was taken approximately 750 days after the burst. We find two small galaxies within approximately 1.5 arcseconds of the GRB. The bright galaxy has an AB magnitude of 27.0 +/- 0.1 in the STIS 50CCD (clear) aperture while the fainter galaxy, which we presume to be the host, has an AB magnitude of 28.0 +/- 0.3. The total flux from both objects agrees with the Kron-Cousins R-band magnitudes measured by Hjorth et al. (1999, A&AS, 138, 461), Sokolov et al. (1998, GCNC 148), and Bloom et al. (1998, GCNC 149) if the combined colour of the two galaxies is V-R = 0.8 +/- 0.4. The GRB occurred approximately 0.7 arcseconds to the north of the centre of the faint galaxy. The bright galaxy shows some signs of a barred spiral structure. The central regions have a full-width at half-maximum (after correcting for the point spread function) of ~0.06 arcseconds. The faint galaxy is elongated with an ellipticity of ~0.3 and a major axis of ~1 arcsecond.