GCN Circular 24494
N. P. M. Kuin (UCL-MSSL), M. de Pasquale (U. of Istanbul) and M. G. Bernardini (INAF-OAB) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 190511A 131 s after the BAT trigger (Bernardini et al., GCN Circ. 24472). A source consistent with the XRT position (Goad et al. GCN Circ. 24481) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 08:25:46.44 = 126.44350 (deg.) Dec (J2000) = -20:15:33.6 = -20.25933 (deg.) with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence). There is a catalogued star at a distance of 1.3 arcsec. The extrapolated brightness using the SED from the Vizier photometry tool ( http://cdsportal.u-strasbg.fr/gadgets/ifr?url=http://cdsportal.unistra.fr/widgets/SED_plotter.xml&SED_plot_object=126.442680%2C%20-20.259685&SED_plot_radius=2 ) shows a brightness consistent with that of the white count rate seen at several ks after the trigger. We subtract here therefore the late time count rate in the following preliminary UVOT photometry of this GRB, knowing that this has to be refined using truely late time data. Where we did not have a late time measurement yet available, the photometry will be reported in due time. Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 131 281 147 16.0 +/- 0.1 b 5684 5884 197 21.6 +/- 0.3 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.09 in the direction of the burst (Schlegel et al. 1998). The afterglow was also discovered by NOT (Malasani et al. GCN Circ. 24492).