M.G. Bernardini (INAF-OAB), K.L. Page (U. Leicester) and N.P.M. Kuin (UCL-MSSL) for the Swift team
At 07:14:48 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 190511A (trigger=903158) (Bernardini et al. GCN Circ. 24472). Swift slewed immediately to the burst. At the time of the trigger, the initial BAT position was 86° from the Sun (5.3 hours East) and 40° from the 42%-illuminated Moon. Table 1 contains the best reported positions from Swift, and the latest XRT position can be viewed at http://www.swift.ac.uk/xrt_positions.
Malesani et al. (GCN Circ. 24492) reported the position from NOT for the optical afterglow of this GRB. Kuin et al. (GCN Circ. 24494) reported the detection with UVOT of an optical afterglow. Table 2 is a summary of GCN Circulars about this GRB from observatories other than Swift.
Standard analysis products for this burst are available at https://gcn.gsfc.nasa.gov/swift_gnd_ana.html.
As reported by Barthelmy et al. (GCN Circ. 24502),
the BAT ground-calculated position is RA, Dec = 126.443, -20.252 deg which is RA(J2000) = 0
The mask-weighted light curve (Figure 1) shows a complex, multi-peaked structure, starting at about T-25 s, peaking at T+0 s and declining to background by T+10 s.
The spacecraft slewed away from the burst position by T+475 s.
The time-averaged spectrum from T-24.27 to T+6.88 s is best fit by a simple power-law model.
The power law index of the time-averaged spectrum is 1.19 ± 0.10.
The fluence in the 15-150 keV band is 7.4 ± 0.5 x 1
The results of the batgrbproduct analysis are available at https://gcn.gsfc.nasa.gov/notices_s/903158/BA/.
Analysis of the initial XRT data was reported by Page et al. (GCN Circ. 24498). We have analysed 19 ks of XRT data for GRB 190511A, from 129 s to 366.2 ks after the BAT trigger. The data comprise 175 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN Circ. 24481).
The light curve (Figure 2) can be modelled with an initial power-law decay with an index of α=1.15 (+0.04, -0.03), followed by a break at T+23.2 ks to an α of 2.2 (+0.5, -0.3).
A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.07 (+0.08, -0.07). The best-fitting absorption column is consistent with the Galactic value of 1.1 x 1
A summary of the PC-mode spectrum is thus:
Total column: 1.6 (+0.7, -0.5) x 1
Galactic foreground: 1.1 x 1
Excess significance: <1.6 σ
Photon index: 2.12 (+0.24, -0.23)
The results of the XRT team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00903158.
The Swift/UVOT began settled observations of the field of GRB 190511A 131 s after the BAT trigger
(Kuin et al. GCN Circ. 24494).
A source consistent with the XRT position (Goad et al. GCN Circ. 24481) is detected in the initial UVOT exposures.
Table 3 gives preliminary
magnitudes using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc., 1358, 373).
No correction has been made for the expected extinction in the Milky Way
corresponding to a reddening of
Figure 1. The BAT
mask-weighted light curve in the four individual and total
energy bands. The units are counts
Figure 2. The XRT light curve.
Any data from a crosshatched region are not included in the fit.
RA (J2000) | Dec (J2000) | Error | Note | Reference |
---|---|---|---|---|
0 |
-20°15'33.6" | 0.42" | UVOT-refined | Kuin et al. GCN Circ. 24494 |
0 |
-20°15'34.1" | 1.6" | XRT-final | UKSSDC |
0 |
-20°15'33.7" | 2.0" | XRT-enhanced | Goad et al. GCN Circ. 24481 |
0 |
-20°15'05.6" | 1.5' | BAT-refined | Barthelmy et al. GCN Circ. 24502 |
Band | Authors | GCN Circ. | Subject | Observatory | Notes |
---|---|---|---|---|---|
Optical | Malesani et al. | 24492 | NOT optical afterglow | NOT | detection |
Gamma-ray | Fermi | 24471 | Fermi GBM Final Real-time Localization | Fermi GBM | |
Gamma-ray | von Kienlin | 24482 | Fermi GBM observation | Fermi GBM | Fluence=2.21±0.05x1 (8 |
Gamma-ray | Axelsson et al. | 24483 | Fermi-LAT detection | Fermi LAT | |
Gamma-ray | Kozlova et al. | 24534 | Konus-Wind observation | Konus-Wind | Duration=~31.8 seconds Fluence=1.93(-0.11,+0.12)x1 |
Other | Alberto | 24499 | en |
Filter | Exp(s) | Mag | ||
---|---|---|---|---|
white | 131 | 281 | 147 | 16.0 ± 0.1 |
b | 5684 | 5884 | 197 | 21.6 ± 0.3 |
Table 3. UVOT observations reported by Kuin et al. (GCN Circ. 24494). The start and stop times of the exposures are given in seconds since the BAT trigger. The preliminary detections and 3-σ upper limits are given. No correction has been made for extinction in the Milky Way.
May 18, 2019