//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20819 SUBJECT: GRB 170306A: Swift detection of a burst DATE: 17/03/06 07:26:32 GMT FROM: Jamie A. Kennea at PSU/Swift-XRT C. B. Markwardt (NASA/GSFC), V. D'Elia (ASDC), J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC), A. Melandri (INAF-OAB) and K. L. Page (U Leicester) report on behalf of the Swift Team: At 07:06:12 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 170306A (trigger=741220). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 263.082, -44.747 which is RA(J2000) = 17h 32m 20s Dec(J2000) = -44d 44' 50" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of about 20 sec. The peak count rate was ~1000 counts/sec (15-350 keV), at ~5 sec after the trigger. The XRT began observing the field at 07:08:26.0 UT, 133.5 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source located at RA, Dec 263.06892, -44.74808 which is equivalent to: RA(J2000) = 17h 32m 16.54s Dec(J2000) = -44d 44' 53.1" with an uncertainty of 3.7 arcseconds (radius, 90% containment). This location is 33 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 consistent with the Galactic value of 3.82 x 10^21 cm^-2 (Willingale et al. 2013). UVOT took a finding chart exposure of 150 seconds with the White filter starting 139 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. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the sub-image. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the region. No correction has been made for the expected extinction corresponding to E(B-V) of 0.41. Burst Advocate for this burst is C. B. Markwardt (Craig.Markwardt AT 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: 20820 SUBJECT: GRB 170306A: LCO Cerro Tololo observations DATE: 17/03/06 09:02:26 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), A. Gomboc (U. Nova Gorica), C.G. Mundell (U. Bath) on behalf of a large collaboration report: We observed Swift GRB 170306A (Markwardt et al. GCN 20819) on March 6, 07:26:06 UT (~20 minutes since the GRB trigger time) with the 1-m LCO unit in Cerro Tololo with SDSS r and i filters. Within the Swift XRT error circle we detect an uncatalogued source at the following position: RA(J2000) = 17:32:16.76 Dec(J2000)= -44:44:53.7 with an error radius of 1". We find the following magnitude values as calibrated against nearby USNOB-1 objects (R2 and I values): Mid Time Exposure Filter Magnitude (AB) (min) (s) ------------------------------------------------------- 24 5x60 SDSS-I 18.5 +- 0.2 34 5x60 SDSS-R 19.0 +- 0.2 ------------------------------------------------------- At the moment we cannot make any statement on the temporal behaviour of the source. The expected Galactic dust extinction is A_r=1~mag, A_i=0.7 mag (from Schlafly et al. 2011). Given the crowded field, we caution that the source might be unrelated to the GRB. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20822 SUBJECT: GRB 170306A: GROND observations DATE: 17/03/06 15:17:58 GMT FROM: Patricia Schady at MPE/Swift Patricia Schady, Phil Wiseman (both MPE) and Jan Bolmer (ESO, Santiago) report: We observed the field of GRB 170306A (Swift trigger 741220; Markwardt et al., GCN #20819) simultaneously in g’r’i’z’JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile). Observations started at 07:20 UT on 2017-03-06, 14 minutes after the GRB trigger, and they continued for ~2 hours, until the start of astronomical twilight. They were performed at an average seeing of 1.3" and at an average airmass of 1.5. Within the 3.7" XRT error circle (Markwardt et al., GCN #20819) we detect two uncatalogued sources in addition to the source reported by Guidorzi et al. (GCN #20820). These two newly identified sources have AB magnitudes r’~20.0 mag and r’~20.3 mag calibrated against GROND zeropoints and uncorrected for the significant Galactic foreground extinction along the line of sight. None of the sources within the XRT error circle show any significant variability during the 2 hours of GROND observations. We acknowledge the excellent support provided by the Chilean observer at the telescope, and the support astronomer, Angela Hempel, in obtaining these data. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20823 SUBJECT: GRB 170306A: Swift/UVOT Upper Limits DATE: 17/03/06 18:52:02 GMT FROM: Sam Emery at MSSL-UCL S.W.K. Emery (UCL-MSSL) and C. B. Markwardt (NASA/GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 170306A 140 s after the BAT trigger (Markwardt et al., GCN Circ. 20819). No optical afterglow consistent with the XRT position (Markwardt et al., GCN Circ. 20819) and the optical positions (Guidorzi et al., GCN Circ. 20820; Schady et al., GCN Circ. 20822) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 140 290 147 >20.0 u_FC 299 548 246 >18.9 white 140 771 186 >20.4 v 629 821 39 >18.1 b 554 747 39 >18.6 u 299 722 265 >19.0 w1 678 870 39 >18.1 m2 653 846 39 >19.0 w2 604 796 39 >18.1 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.41 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20825 SUBJECT: GRB 170306B: Tiled Swift observations DATE: 17/03/06 18:58:17 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a series of observations, tiled on the sky, of the Fermi/LAT GRB 170306B. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00065 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20826 SUBJECT: GRB 170306B: Fermi-LAT detection DATE: 17/03/06 18:58:37 GMT FROM: Nicola Omodei at Stanford U. N. Omodei (Stanford U.), G, Vianello (Stanford U.), D. Tak(U. of Maryland) and F. Longo (University and INFN Trieste) report on behalf of the Fermi-LAT team: At 14:07:22.27 on March 06, 2017, Fermi-LAT detected high-energy emission from GRB 170306B, which was also detected by Fermi-GBM (trigger 510502047). The best LAT on-ground location is found to be RA, Dec 154.62, 51.59 (degrees, J2000) with an error radius of 0.61 deg (90% containment, statistical error only). This was 55 deg from the LAT boresight at the time of the trigger and triggered an autonomous repoint of the spacecraft. The data from the Fermi-LAT show a significant increase in the event rate within 4.3 degree of the GBM location after the GBM trigger that is temporally correlated with the GBM emission with high significance. More than 10 photons above 100 MeV are observed within 300 seconds. The highest-energy photon is a 500 MeV event which is observed 46 seconds after the GBM trigger. A Swift ToO has been requested for this burst. The Fermi-LAT point of contact for this burst is Nicola Omodei (nicola.omodei@stanford.edu). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20827 SUBJECT: GRB 170306B: Fermi GBM detection DATE: 17/03/06 19:32:55 GMT FROM: Peter Veres at UAH P. Veres (UAH), C. Meegan (UAH) and A. von Kienlin (MPE) report on behalf of the Fermi GBM Team: "At 14:07:22.27 UT on 6 March 2017, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 170306B (trigger 510502047 / 170306588), which was also detected by Fermi/LAT (Omodei et al., GCN 20826). The GBM on-ground location is consistent with the LAT position. The trigger resulted in an Autonomous Repoint Request (ARR) by the GBM Flight Software owing to the high peak flux of the GRB. This ARR was accepted and the spacecraft slewed to the GBM in-flight location. The GBM light curve shows multiple overlapping pulses with a duration (T90) of about 18.7 s (50-300 keV). The time-averaged spectrum from T0-3.8 s to T0+26.9 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.73 +/- 0.03 and the cutoff energy, parameterized as Epeak, is 289 +/- 10 keV. The event fluence (10-1000 keV) in this time interval is (3.07 +/- 0.06)E-5 erg/cm^2. The 1-sec peak photon flux measured starting from T0+8.7 s in the 10-1000 keV band is 12.4 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20828 SUBJECT: GRB 170306A: Swift-XRT refined Analysis DATE: 17/03/06 21:36:26 GMT FROM: Phil Evans at U of Leicester P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester) and report on behalf of the Swift-XRT team: report on behalf of the Swift-XRT team: We have analysed 6.7 ks of XRT data for GRB 170306A, from 119 s to 28.8 ks after the BAT trigger. The data comprise 29 s in Windowed Timing (WT) mode (the first 8 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The refined XRT position is RA, Dec = 263.0690, -44.7482 which is equivalent to: RA (J2000): 17 32 16.56 Dec(J2000): -44 44 53.5 with an uncertainty of 3.6 arcsec (radius, 90% confidence). The light curve can be modelled with an initial power-law decay with an index of alpha=3.25 (+0.28, -0.21), followed by a break at T+559 s to an alpha of 0.36 (+0.10, -0.26). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.05 (+0.30, -0.19). The best-fitting absorption column is 3.98 (+1.64, -0.16) x 10^21 cm^-2, consistent with the Galactic value of 3.8 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.8 x 10^-11 (6.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.98 (+1.64, -0.16) x 10^21 cm^-2 Galactic foreground: 3.8 x 10^21 cm^-2 Excess significance: <1.6 sigma Photon index: 2.05 (+0.30, -0.19) If the light curve continues to decay with a power-law decay index of 0.36, the count rate at T+24 hours will be 0.011 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x 10^-13 (6.9 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00741220. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20829 SUBJECT: GRB 170306A, Swift-BAT refined analysis DATE: 17/03/07 02:59:37 GMT FROM: Amy Lien at GSFC T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), N. Gehrels (GSFC), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 170306A (trigger #741220) (Markwardt et al., GCN Circ. 20819). The BAT ground-calculated position is RA, Dec = 263.087, -44.765 deg which is RA(J2000) = 17h 32m 20.9s Dec(J2000) = -44d 45' 52.5" with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 29%. The mask-weighted light curve shows a pulse that starts at ~T-7 s and ends at ~T+20 s. In addition, there is a hint of some weak emissions from ~T-100 s to ~T-80 s. T90 (15-350 keV) is 17.8 +- 6.7 sec (estimated error including systematics). The time-averaged spectrum from T-7.1 to T+19.7 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.98 +- 0.28. The fluence in the 15-150 keV band is 8.3 +- 1.4 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+10.93 sec in the 15-150 keV band is 1.3 +- 0.4 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/741220/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20830 SUBJECT: GRB 170306B: Swift-XRT observations DATE: 17/03/07 11:32:04 GMT FROM: Andrea Melandri at INAF-OAB V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), A. Cholden-Brown (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), B. Mingo (U. Leicester), A. Melandri (INAF-OAB) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 170306B in a series of observations tiled on the sky. The total exposure time is 4.5 ks, distributed over 8 tiles; the maximum exposure at a single sky location was 1.4 ks. The data were collected between T0+17.4 ks and T0+29.9 ks, and are entirely in Photon Counting (PC) mode. No uncatalogued X-ray sources have been detected. The 3-sigma upper limit in the field (not including the regions where the tiles overlap) ranges from ~0.007 to ~0.021 ct s^-1, corresponding to a 0.3-10 keV observed flux of 2.9e-13 to 8.5e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum). Four previously-catalogued X-ray sources have been detected, however their status as catalogued objects makes them unlikely to be the afterglow. The results of the XRT-team automatic analysis of the tiled XRT observations, including a position-specific upper limit calculator, are available at http://www.swift.ac.uk/xrt_products/TILED_GRB00065. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20831 SUBJECT: Konus-Wind observation of GRB 170306B DATE: 17/03/07 11:39:11 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline, on behalf of the Konus-Wind team, report: The long GRB 170306B (Fermi-LAT detection: Omodei et al., GCN 20826; Fermi-GBM detection: Veres et al., GCN 20827) triggered Konus-Wind at T0=50850.920 s UT (14:07:30.920) The light curve shows a multi-peaked structure with a total duration of ~25 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of (3.4 ± 0.4)x10^-5 erg/cm2 and a 64-ms peak energy flux, measured from T0+3.712, of (4.1 ± 0.6)x10^-6 erg/cm2 (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+22.528 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.58 (-0.13,+0.16), the high energy photon index beta = -2.62 (-0.61,+0.28), the peak energy Ep = 237 (-27,+27) keV, chi2 = 105/97 dof. The spectrum near the peak count rate (measured from T0 to T0+6.912 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.40 (-0.11,+0.12), the high energy photon index beta = -2.70 (-0.84,+0.29), the peak energy Ep = 214 (-24,+30) keV, chi2 = 120/97 dof. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB170306_T50850/ All the quoted errors are estimated at the 90% confidence level. All the presented results are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20839 SUBJECT: GRB 170306B: POLAR observation DATE: 17/03/08 14:02:46 GMT FROM: Haulin Xiao at PSI/POLAR H.L. Xiao (PSI), R. Marcinkowski (PSI) and W. Hajdas (PSI) report on behalf of the POLAR collaboration: At 2017-03-06 14:07:20.0 UT(T0), during a routine on-ground search of data, POLAR detected GRB 170306B, which was also observed by Fermi-GBM (trigger # 510502047), Fermi-LAT (trigger #170306588) and SPI ACS at 2017-03-06 14:07:25. The POLAR light curve consists of multiple peaks with duration (T90) of 25.0 +/- 1.0 s measured from T0. The 1.00 s peak flux at T0 + 11.50 s is equal to 2380 +/- 100 counts/sec. POLAR recorded 31640 events from the burst. Above measurements are in the energy range of about 15 - 300 keV. LC_URL: http://polar.psi.ch/triggers/GRB_170306B_raw.png or http://polar.psi.ch/pub/lc.php?event=GRB+170306B Using the best location from Fermi-LAT, which is (J2000): RA : 154.650 [deg] Dec: 51.630 [deg] Err: 39.00 [arcmin] the incident angle in the POLAR coordinate at T0 is: Theta: 87.0 [deg] Phi: 98.4 [deg] The analysis results presented above are preliminary. POLAR is a dedicated Gamma-Ray Burst polarimeter which was launched on-board the Chinese space laboratory Tiangong-2 (TG-2) on Sep 15, 2016. More information about POLAR can be found at http://polar.psi.ch/pub , http://polar.ihep.ac.cn/en/ and http://isdc.unige.ch/polar/ . This message is quotable in publications. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20843 SUBJECT: GRB 170306A: GROND afterglow detection DATE: 17/03/10 13:15:22 GMT FROM: Patricia Schady at MPE/Swift Patricia Schady (MPE Garching) reports: Following on from the GROND (Greiner et al. 2008, PASP 120, 405) observations of GRB 170306A on the 2017-03-06 (Schady et al., GCN #20819), I re-observed the field simultaneously in g'r'i'z'JHK with GROND at on 2017-03-10, 4 days after the GRB trigger. Observations were performed at an average seeing of 1.4" and at an average airmass of 1.7. One of the three sources detected with GROND (Schady et al., GCN #20819) within the refined XRT error circle (D’Avanzo et al., GCN #20828) is no longer seen in the latest GROND observations down to the following 3 sigma limiting magnitudes (all in AB system): g’ > 22.6 mag r’ > 23.5 mag i’ > 22.3 mag z’ > 22.4 mag J > 20.4 mag H > 19.9 mag K > 18.9 mag This source is therefore the likely optical/NIR afterglow of GRB 170306A. The position of the afterglow candidate is RA (J2000) = 17:32:16.69 Dec (J2000) = -44:44:55.5 with a positional uncertainty of 0.3" in both coordinates. Based on combined images with 36 min of total integration time in g'r'i'z' and 30 min in JHK at a mid-time of 09:33 UT on 2017-03-06, the afterglow candidate had the following preliminary magnitudes (all in AB system): g' = 21.6 +/- 0.1 mag r’ = 20.4 +/- 0.1 mag i’ = 20.0 +/- 0.1 mag z' = 19.9 +/- 0.1 mag J = 19.1 +/- 0.1 mag H = 18.4 +/- 0.1 mag K = 18.5 +/- 0.2 mag The given magnitudes are derived based on images calibrated against GROND zero points in the optical and 2MASS field stars in the NIR bands. They are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)= 0.36 in the direction of the burst (Schlafly & Finkbeiner 2011). I acknowledge the excellent support provided by the Chilean observer at the telescope, and the support astronomer, Sam Kim, in obtaining these data. I also thank David Buckley for some useful email exchanges that in part led to the second epoch of GROND observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 20844 SUBJECT: GRB170306A: SALT observations DATE: 17/03/10 20:05:16 GMT FROM: Soebur Razzaque at U of Johannesburg D.A.H. Buckley (SAAO/SALT), A, Martin-Carrillo (U. College Dublin), S. Razzaque (U. Johannesburg) and R. Skelton (SAAO/SALT) report on behalf of a larger collaboration. We observed the nominal position of GRB 170306A (Markwardt et al. GCN 20819 and Guidorzi et al. GCN 20820) on 2017-03-07 at 01:22:42 UTC using the Southern African Large Telescope (SALT) in Sutherland, South Africa, 18.61 h after the Swift GRB trigger. A 20 sec r'-band image was obtained using SALTICAM just prior to the commencement of attempted low resolution (R ~ 355 at 660 nm) spectroscopy. Two stellar objects at r’ ~ 19 and 20 were seen, with FWHM of 1.7 arcsec, near the GRB position and long slit spectroscopy was attempted of both. Only the brighter one provided a detection, which was noisy and showed no obvious spectral features. Subsequent information provided by P. Schady on possible optical candidates from the first GROND observation (Schady et al. GCN 20822) was used to confirm the identification of the r’ = 20.4 object identified by Schady (GCN 20843) as the optical counterpart. The SALT image shows a very weak detection of this object, barely above the background, with an estimated brightness of r’= 21.4 +/- 0.3, having dimmed approximately one magnitude since detection. We thank Patricia Schady and Christiano Guidorzi for providing information to assist in the identification of the optical counterpart. ________________________________ This email and all contents are subject to the following disclaimer: http://disclaimer.uj.ac.za