//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1325 SUBJECT: IPN localization of GRB020405 DATE: 02/04/05 17:18:58 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley and T. Cline, on behalf of the Ulysses GRB team, F. Frontera, C. Guidorzi, and E. Montanari, on behalf of the BeppoSAX GRBM team, I. Mitrofanov, D. Anfimov and M. Litvak on behalf on HEND/Odyssey GRB team, and W. Boynton, C. Fellows, K. Harshman, and C. Shinohara, on behalf of the GRS/Odyssey GRB team, report: Ulysses, Mars Odyssey - HEND, and BeppoSAX observed this GRB at 02486 s. As observed by Ulysses, it had a duration of ~40 seconds, a 25-100 keV fluence of ~3x10^-5 erg/cm2, and a peak flux of ~10^-6 erg/cm2 s over 0.5 s. We have triangulated it to a preliminary, 3 sigma error box with approximate area 75 square arcminutes whose coordinates are: ERROR BOX CENTER: 209.543 -31.388 ERROR BOX CORNER: 209.216 -31.393 ERROR BOX CORNER: 209.594 -31.350 ERROR BOX CORNER: 209.491 -31.425 ERROR BOX CORNER: 209.873 -31.381 This error box can be improved. With this burst, we announce the resumption of IPN activities with the Mars Odyssey spacecraft. We had intended to announce this with a GCN message prior to the localization of our first burst; that announcement will now be sent sometime next week. [GCN OPS NOTE (06apr02): The "name" of the GRB in the Subject-line was changed from 050402 to 020405 as per the normal naming convention.] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1326 SUBJECT: GRB 020405: Optical afterglow candidate DATE: 02/04/06 01:36:12 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price, B.P. Schmidt (RSAA, ANU) and T.S. Axelrod (Arizona) report: We have observed the error box of GRB 020405 with the robotic MSO 50-inch telescope + MACHO imager at 2002 Apr 05.75 UT (approximately 17.5 hours after the GRB). Upon visual inspection of the images, we find a source that is not present on the second Digitised Sky Survey. The source is R ~ 18.5 mag and is located at coordinates: RA: 13:58:03.12 Dec: -31:22:22.2 J2000 with error approximately 0.3 arcsec in each coordinate. A finding chart is available from: http://darkalf.caltech.edu/~pap/grb020405finder.ps This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1327 SUBJECT: GRB 020405, U-band observations DATE: 02/04/06 04:53:03 GMT FROM: Alberto Castro-Tirado at Inst.de Astro. de Andalucia GRB 020405, U-band observations --------------------------- A. J. Castro-Tirado, J. Gorosabel (Instituto de Astrofísica de Andalucía, IAA-CSIC, Granada), T. Augusteijn (Isaac Newton Group of Telescopes) and José María Castro Cerón (ROA,San Fernando) report: We have observed the central region of the GRB 020405 error box (Hurley et al., GCN Circ. 1325) with the Prime Focus Camera at the 4.2-m William HerschelTelescope at the ORM in La Palma, providing a 16'.2 square field of view. A comparison of the U- and R-band images obtained on Apr 6.104-6.122 UT reveals an extremely blue object at the position of the optical candidate proposed by Price et al. (GCN Circ. 1326) thus supporting the relationship with the GRB. This U-band detection would imply that the redshift is < 2.1 . This message can be cited. [GCN OPS NOTE (20jul02): The affiliation for JMCC was changed from "IAA-CSIC and ROA, San Fernando" to "ROA, San Fernando".] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1328 SUBJECT: V band observations of GRB020405 DATE: 02/04/06 07:57:06 GMT FROM: Elena Pian at ITESRE-CNR,Bologna E. Palazzi, N. Masetti (IASF-CNR, Bologna), E. Pian (INAF, OA Trieste), J. Licandro (TNG), R. Maiolino (INAF, OA Arcetri), P. Saracco (INAF, OA Brera), F. Fiore (INAF, OA Roma), on behalf of a large collaboration, report: "We have observed the central portion of the error box of GRB020405 (GCN 1325) at TNG with Dolores and V filter for 10 minutes, starting 2002 April 6, 01:34 UT. The seeing was 1.6". From a preliminary analysis of the images we detect the source reported by Price et al. (GCN 1326) with a magnitude V = 20.2 +- 0.3, assuming V=18.5 and V=17.6 for the comparison USNO-A2.0 stars 0525-16813005 and 0525-16815468, respectively. This message may be cited." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1329 SUBJECT: Fading Optical Afterglow and Possible Host Galaxy of GRB 020405 DATE: 02/04/06 11:50:11 GMT FROM: Jens Hjorth at U.Copenhagen Fading Optical Afterglow and Possible Host Galaxy of GRB 020405 J. Hjorth (U. Copenhagen), J. Fynbo (ESO), E. Pian (INAF, OA Trieste), A. Delsanti (ESO), B. L. Jensen (U. Copenhagen), J. Gorosabel (IAA, Granada), H. Pedersen (U. Copenhagen), and M. I. Andersen (U. Oulu) report: Optical images of the candidate afterglow (Price et al., GCN #1326) of GRB 020405 (Hurley et al., GCN #1325) were obtained at the Danish 1.5-m telescope on La Silla as follows: Date Filter Exp. time 6 April 2002 UT (sec) 03:16 R 600 05:04 R 600 05:16 V 600 05:37 B 1200 05:56 Gunn i 900 Calibrating our photometry to the reference star USNO525_16813005 (for which we assume B = 19.3 and R = 17.8) we find R = 20.9 and B - R = 0.0. In addition, comparison between the two R-band images indicates that the afterglow faded with 0.099 +- 0.040 mag between the two epochs, thus supporting the interpretation that the source is indeed the afterglow of GRB 020405. A color image (based on the BVi images) posted at http://www.astro.ku.dk/~jens/grb020405_color.gif shows the very blue color of the afterglow (see also Castro-Tirado et al., GCN #1327). In addition, the R-band images posted at http://www.astro.ku.dk/~jens/grb020405_host1.gif http://www.astro.ku.dk/~jens/grb020405_host2.gif reveal a bright galaxy located ~ 2" to the south-west of the afterglow. If this is the host galaxy, then the redshift of GRB 020405 may be fairly low, making it a good candidate for a search of an underlying supernova. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1330 SUBJECT: GRB020405: VLT spectroscopy DATE: 02/04/06 18:27:39 GMT FROM: Elena Pian at ITESRE-CNR,Bologna N. Masetti, E. Palazzi (IASF-CNR, Bologna), E. Pian (INAF, OA Trieste), J. Hjorth (U. Copenhagen), A. Castro-Tirado (IAA-CSIC, Granada), H. Boehnhardt (ESO), P. Price (RSAA, ANU), on behalf of the GRACE collaboration, report: "On 2002 April 6.213 UT we have taken a 30 min spectrum of the candidate afterglow of GRB020405 (GCN 1326) with the VLT equipped with FORS1 and low resolution grating 150I+OG590. After a preliminary analysis of the spectrum, narrow emission lines, likely from the host galaxy, are seen which may be identified with [O II], [O III] and Hbeta at a redshift of 0.695 +- 0.005. At the same redshift we also detect the Ca II doublet in absorption. This message may be cited." //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1331 SUBJECT: GRB020405, Radio Observations DATE: 02/04/06 21:08:02 GMT FROM: Edo Berger at Caltech E. Berger, S. R. Kulkarni (Caltech), and D. A. Frail (NRAO) report on behalf of the Caltech-NRAO-CARA GRB collaboration: "On 2002, April 6.22 UT we observed a field centered on the position of the optical afterglow candidate reported by Price et al. (GCN #1326) with the VLA at 8.46 GHz. We detect a 490 microJy radio source coincident with the position of the optical source at (J2000): RA=13 58 03.125, DEC=-31 22 21.90 with an uncertainty of 0.03 arcsec in both coordinates. Further observations with the VLA are in progress, and we strongly urge millimeter and submillimeter observations to determine the density and profile of the circumburst environment." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1333 SUBJECT: GRB 020405: Decay index DATE: 02/04/07 02:46:33 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price, B.P. Schmidt (RSAA, ANU) and T.S. Axelrod (Arizona) report: We have re-observed the afterglow candidate (GCN #1326) with the robotic MSO 50-inch telescope + MACHO imager at 2002 Apr 6.43. The afterglow candidate has faded by approximately 1 magnitude since the observations of Apr 5.75 (GCN #1326), from which we derive an optical decay index of alpha ~ 1.26. Using the reference star of Hjorth et al. (GCN #1329), we find that R ~ 19.9 mag at Apr 6.43. This value does not appear to be consistent with that of Hjorth et al., which might be explained by the filter mis-match and use of different apertures. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1335 SUBJECT: GRB020405: OT observations DATE: 02/04/07 12:26:43 GMT FROM: Eran Ofek at Tel Aviv U. A. Gal-Yam, E. O. Ofek and Y. Lipkin (Wise Observatory, TAU) report: We have observed the center of the error box of GRB 020405 using the Wise Observatory 1m telescope + Tek CCD camera at 2002 Apr 05.95 UT. Three 900 s R-band images were obtained. We identify the candidate OT proposed by Price et al. (GCN 1326) for which we measure an R-band magnitude of 18.8 +/- 0.14 mag, using the R=17.8 mag reference star from Hjorth et al. (GCN 1329). Our measured value seems to agree better with those of Price et al. (GCN 1333) than those of Hjorth et al. (GCN 1329). //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1336 SUBJECT: Revised Photometry of the Optical Afterglow of GRB 020405 DATE: 02/04/07 13:07:51 GMT FROM: Jens Hjorth at U.Copenhagen Revised Photometry of the Optical Afterglow of GRB 020405 J. Hjorth (U. Copenhagen) reports: The calibration of the PSF photometry reported in GCN #1329 relied on a misidentification of the USNO A2.0 star 0525_16813005 with 0525_16812476. Calibration to 0525_16813005 yields R = 19.8 and B - R = 1.0 at April 6.21 UT, consistent with the reports of Palazzi et al. (GCN #1328), Price et al. (GCN #1333), and Gal-Yam et al. (GCN #1335). The systematic error in these values is of the order of +- 0.3 mag. I apologize for the impact this error may have had on follow-up strategies and thank Javier Gorosabel and Paul Price for pointing out the problem. Additional data taken with the DK1.5m between Apr 7.13 and Apr 7.37 confirm the continued fading of the source. A careful analysis of these data is in progress! //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1337 SUBJECT: GRB020405: VLT optical observations DATE: 02/04/07 21:12:03 GMT FROM: Stefano Covino at Brera Astronomical Observatory S. Covino, G. Ghisellini, P. Saracco, G. Tagliaferri, F. Zerbi (Observ. of Brera, Milan, Italy); S. Di Serego, A. Cimatti, Della Valle (Observ. of Arcetri, Florence, Italy); F. Fiore, G.L. Israel, L. Stella (Observ. of Monte Porzio, Rome, Italy); M. Vietri (Univ. Rome 3, I); N. Kawai (RICHEN, Japan); D. Lazzati (IoA, Cambridge, UK); S. Ortolani (Univ. of Padua, Italy); L. Pasquini (ESO, Germany); G. Ricker (MIT, USA); E. Le Floch, P. Goldoni, F. Mirabel (CEA, F), H. Boehnhardt (on behalf of the Melipal team, ESO, Paranal, Chile) report: On 2002 April 7.14 we observed the optical counterpart of GRB 020405 reported by Price et al. (GCN 1326). The observations were performed with the ESO VLT-3 (Melipal) telescope equipped with FORS1 with a V filter in the imaging polarimetry mode. The transient source is clearly detected and the acquisition image allowed to derive the Bessel V magnitude of the transient, V=21.45 +/- 0.1, assuming V=18.5 and V=17.6 for the comparison USNO-A2.0 stars 0525-16813005 and 0525-16815468, respectively, as reported in Palazzi et al. (GCN 1328). This message is citeable. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1340 SUBJECT: GRB 020405: Moderate-resolution spectroscopy DATE: 02/04/08 19:25:15 GMT FROM: Paul Price at RSAA, ANU at CIT P.A. Price (Caltech), M. Pettini (Cambridge), N. Reddy, C. Steidel and S.R. Kulkarni (Caltech) report on behalf of the REACT GRB collaboration: We have observed the afterglow of GRB 020405 (GCN #1326) with the Keck II telescope + ESI. Observations consisted of 2x1800 sec exposures in the eschellete mode. In this mode we are able to resolve the sky lines, which is particularly important since at the reported redshift of z = 0.695 (Masetti et al., GCN #1330) the [O II] line is coincident with a strong atmospheric line. A preliminary reduction of the spectra reveals emission lines of [O II], Hbeta, and [O III], at a mean redshift of z = 0.6898 +/- 0.0005. In particular, we resolve the [O II] doublet and thus we consider the redshift to be secure. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1345 SUBJECT: GRB020405: VLT optical observations and V band decay slope DATE: 02/04/09 12:52:29 GMT FROM: Stefano Covino at Brera Astronomical Observatory S. Covino, G. Ghisellini, P. Saracco, G. Tagliaferri, F. Zerbi (Observ. of Brera, Milan, Italy); S. Di Serego, A. Cimatti, Della Valle (Observ. of Arcetri, Florence, Italy); F. Fiore, G.L. Israel, L. Stella (Observ. of Monte Porzio, Rome, Italy); M. Vietri (Univ. Rome 3, I); N. Kawai (RICHEN, Japan); D. Lazzati (IoA, Cambridge, UK); S. Ortolani (Univ. of Padua, Italy); L. Pasquini (ESO, Germany); G. Ricker (MIT, USA); E. Le Floch, P. Goldoni, F. Mirabel (CEA, F), H. Boehnhardt (on behalf of the Melipal team, ESO, Paranal, Chile) report: On 2002 April 8.164 we observed the optical counterpart of GRB 020405 reported by Price et al. (GCN 1326). The observations were performed with the ESO VLT-3 (Melipal) telescope equipped with FORS1 with a V filter in the imaging polarimetry mode. The transient source is clearly detected and the acquisition image allowed to derive the Bessel V magnitude of the transient, V=22.0 +/- 0.1, assuming V=18.5 and V=17.6 for the comparison USNO-A2.0 stars 0525-16813005 and 0525-16815468, respectively, as reported in Palazzi et al. (GCN 1328). Relative photometry between our V band observations of April 7.143 and 8.164 shows that the OT decayed by 0.60 +- 0.05 magnitudes, implying a decay slope of 1.52 +- 0.12, also consistent with the previous V mesurement by Palazzi et al (GCN 1328). This message is citeable. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1369 SUBJECT: GRB020405: predicted break DATE: 02/04/13 16:03:45 GMT FROM: Daniele Malesani at Obs.Astro. di Brera D. Malesani, G. Ghisellini, S. Covino (Brera Observ., Milan) and D. Lazzati (IoA Cambridge, UK) report: According to the idea of Frail et al. (2001, ApJ, 562, L55) that the jet energies of GRBs are universal, an achromatic jet break in the afterglow lightcurve is predicted for all bursts at the time t_jet = 20.4 (1+z) / (E_gamma/1e52) days, where E_gamma is the observed (i.e. isotropic) energy of the prompt emission. This result is independent of the unknown efficiency and circumburst density. For GRB020405, with z=0.69 (GCN 1330 and GCN 1340) and E_gamma>4.3e52 erg (assuming H_0=65, Omega_m=0.3, Omega_Lambda=0.7 and taking the fluence to be larger than the reported value in the 25-100 keV band: 3e-5 erg/cm2, GCN 1325), we have t_jet<8 days. Hence the break should have occured before April 13. Our V-band data (GCN 1337, 1345) connect very well with a previous measurement by Palazzi et al. (GCN 1328), who use the same calibration stars. The decay slope is hence very well defined (1.52+-0.04), making easier the possible detection of the predicted break (see the lightcurve at: http://www.merate.mi.astro.it/~gabriele/020405.html ). Since both the detection or the non-detection of the break would be very important to constrain Frail et al. idea, we urge photometric observations of the afterglow of this burst. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1375 SUBJECT: GRB020405: VLT observations of the OT environment DATE: 02/04/18 14:18:16 GMT FROM: Nicola Masetti at ITeSRE,CNR,Bologna N. Masetti, E. Palazzi (IASF/CNR, Bologna), E. Maiorano, A. Simoncelli (U. Bologna), E. Pian (INAF, OA Trieste), A. Castro-Tirado (IAA-CSIC, Granada), A. Fruchter (STScI, Baltimore), J. Greiner (MPE Garching and AI Potsdam), J. Hjorth (U. Copenhagen), L. Kaper, E. van den Heuvel (U. Amsterdam), R. Cabanac, A. Kaufer (ESO), on behalf of the GRACE Collaboration, report: "We have obtained an R-band image (2 x 3 minutes integration) of GRB020405 from VLT-UT3 (Melipal) plus FORS1 on 2002 Apr. 15.244 under a seeing of 0.65 arcsec. We find that the OT is located within a complex environment composed of at least four extended objects, one of which is underlying the OT and showing a bright knot (possibly a star-forming region, or alternatively the host nucleus) ~1 arcsec south of the OT itself. Also, the presumed host galaxy indicated by Hjorth et al. (GCN #1329) and located ~2 arcsec southwest of the OT seems not to be the actual host but a galaxy which is likely interacting with it. Indeed, a spectrum of this galaxy taken with Melipal+FORS1 on 2002 April 7.310 shows that it is at the same redshift of the OT (GCNs #1330, #1340). This finding strengthens the suggestion that GRBs are sometimes associated with interacting galaxies possibly displaying substantial star formation, as seen e.g. for GRB001007 (Castro Ceron et al. 2002, A&A, in press [astro-ph/0110049]). No suggestion of a break in the light curve (see GCN #1369) is apparent up to ~10 days after the GRB. However, in the VLT image reported above, the OT brightness is already substantially contamined by the host emission. For this reason it would be quite difficult to see any future possible break in the OT light curve with ground-based observations. A close-up of the VLT R-band field around the OT can be found at: http://tonno.tesre.bo.cnr.it/~masetti/grb020405.html This message can be cited.". //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1388 SUBJECT: GRB020405 field photometry at ESO DATE: 02/05/10 16:25:52 GMT FROM: Nicola Masetti at ITeSRE,CNR,Bologna A. Simoncelli, E. Maiorano (U. Bologna), E. Palazzi, N. Masetti (IASF/CNR, Bologna), E. Pian (INAF, OA Trieste), J. Hjorth (U. Copenhagen), A. Castro-Tirado (IAA-CSIC, Granada), A. Fruchter (STScI, Baltimore), J. Greiner (MPE Garching and AI Potsdam), L. Kaper, E. van den Heuvel (U. Amsterdam), A. Delsanti, M. Billeres (ESO), on behalf of the GRACE Collaboration, report: "We have acquired BVRcIc photometry of the field of GRB020405 with the Danish 1.54m and NTT 3.58m ESO telescopes at La Silla, Chile. We placed the photometric data of 6 selected stars, together with an R-band image of the field on which the stars are marked, at the URL: http://tonno.tesre.bo.cnr.it/~masetti/grb020405_phot.html The current photometry has a potential external zero-point error of about three percent that needs to be added in quadrature to the Poisson errors given for the magnitude uncertainties of the selected stars. Specifically, the magnitudes of the USNO-A2.0 stars 0525-16813005 and 0525-16815468 (Palazzi et al., GCN #1328; Hjorth et al., GCN # 1329), which are labeled as stars # 2 and # 5 of our sample, are V = 19.01 +- 0.01, R = 18.48 +- 0.01 for the first one and V = 17.92 +- 0.01 for the second.". This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1431 SUBJECT: GRB020405: polarimetric observations DATE: 02/06/19 10:15:48 GMT FROM: Stefano Covino at Brera Astronomical Observatory S. Covino, G. Ghisellini, D. Malesani, P. Saracco, G. Tagliaferri, F. Zerbi (Observ. of Brera, Milan, Italy); S. Di Serego, A. Cimatti, M. Della Valle (Observ. of Arcetri, Florence, Italy); F. Fiore, G.L. Israel, L. Stella (Observ. of Monte Porzio, Rome, Italy); M. Vietri (Univ. Rome 3, I); N. Kawai (Tokyo Tech, Japan); D. Lazzati (IoA, Cambridge, UK); S. Ortolani (Univ. of Padua, Italy); L. Pasquini (ESO, Germany); G. Ricker (MIT, USA); E. Le Floch, P. Goldoni, F. Mirabel (CEA, F) report: On 2002 April 7.21 and April 8.26 we observed the optical counterpart to GRB020405. The observations were performed with the ESO VLT-3 (Melipal) telescope equipped with FORS1 with a Bessel V band filter in the imaging polarimetry mode. The transient source is clearly detected superposed to a bright galaxy. The acquisition images allowed us to derive the magnitude of the transient as reported in GCN 1337 and GCN 1345 (Covino et al.). On April 7.21 (2.1 days after the GRB) we found linear polarization at the level of 1.93 +/- 0.33 per cent with position angle 154 +/- 5 degrees while on April 8.26 (3.2 days after the GRB) we found linear polarization at the level of 1.23 +/- 0.43 per cent with position angle 168 +/- 9 degrees. Polarization measurements were corrected for any instrumental effect or measurement bias and the reported polarization degrees and position angles are derived from Stokes parameters normalized to the average of the field stars. This message is citeable. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 1458 SUBJECT: GRB 020405: HST observations reveal red bump DATE: 02/07/23 07:15:10 GMT FROM: Paul Price at RSAA, ANU P.A. Price (RSAA, ANU), S.R. Kulkarni, D.W. Fox and J.S. Bloom (Caltech) report on behalf of the larger Caltech-NRAO-CARA GRB collaboration: We observed the afterglow of GRB 020405 (GCN #1326) with HST+WFPC2 at several epochs spanning 19-31 days after the GRB in F555W, F702W and F814W, with additional observations approximately two months after the GRB to remove host contamination. These observations formed part of our large Cycle 10 program to search for SNe underlying low redshift GRBs. We have performed Novicki-Tonry photometry (see astro-ph/0207187) on both ground-based and HST imaging. The resultant light curve, including data from Bersier et al. (astro-ph/0206465), is at http://www.mso.anu.edu.au/~pap/grb020405/ . An excess of flux is evident in the HST images, compared to an extrapolation of the light-curve from early times. Based on the red colour and the time of peak emission, we identify this excess as a SN associated with GRB 020405. We have plotted the light-curve of SN 1998bw at z=0.695 (Masetti et al., GCN #1330) and dimmed by 0.5 mag as a comparison. This SN appears to be red relative to SN 1998bw, but this is sensitive to the amount of flux in the afterglow at the final available HST images. Further HST observations to measure the host galaxy and remove this ambiguity are planned for August. This message may be cited.