A. Tohuvavohu (PSU), D.N. Burrows (PSU) and N.P.M. Kuin (UCL-MSSL) for the Swift team
At 12:43:49 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 180930A (trigger=864584) (Tohuvavohu et al. GCN Circ. 23279). Swift slewed immediately to the burst. At the time of the trigger, the initial BAT position was 106° from the Sun (7.3 hours West) and 44° from the 71%-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.
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. 23286),
the BAT ground-calculated position is RA, Dec = 76.894, -25.124 deg which is RA(J2000) = 0
The mask-weighted light curve (Figure 1) shows a single episode of weak emission from T-4 s to T+4 s with several peaks.
The time-averaged spectrum from T-3.24 to T+4.20 s is best fit by a simple power-law model.
The power law index of the time-averaged spectrum is 1.86 ± 0.28.
The fluence in the 15-150 keV band is 2.1 ± 0.4 x 1
The results of the batgrbproduct analysis are available at https://gcn.gsfc.nasa.gov/notices_s/864584/BA/.
Analysis of the initial XRT data was reported by Burrows et al. (GCN Circ. 23285).
We have analysed 2.6 ks of XRT data for GRB 180930A, from 212 s to 6.0 ks after the BAT trigger. The data comprise 47 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Osborne et al. (GCN Circ. 23280).
The light curve (Figure 2) can be modelled with a power-law decay with a decay index of α=2.04 ± 0.09.
A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.01 ± 0.15. The best-fitting absorption column is 7.2 (+3.7, -3.3) x 1
A summary of the PC-mode spectrum is thus:
Total column: 7.2 (+3.7, -3.3) x 1
Galactic foreground: 2.1 x 1
Excess significance: 2.6 σ
Photon index: 2.01 ± 0.15
The results of the XRT team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00864584.
The Swift/UVOT began settled observations of the field of GRB 180930A 212 s after the BAT trigger
(Kuin and Tohuvavohu GCN Circ. 23283).
No optical afterglow consistent with the XRT position (Evans GCN Circ. 23280) 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 |
-25°07'01.0" | 1.7" | XRT-final | UKSSDC |
0 |
-25°07'01.0" | 1.7" | XRT-enhanced | Osborne et al. GCN Circ. 23282 |
0 |
-25°07'25.6" | 2.2' | BAT-refined | Barthelmy et al. GCN Circ. 23286 |
Band | Authors | GCN Circ. | Subject | Observatory | Notes |
---|---|---|---|---|---|
Optical | Zheng and Filippenko | 23281 | KAIT Optical Upper Limit | KAIT | upper limits |
Optical | Malesani and Sagues | 23284 | NOT optical upper limits | NOT | upper limits |
Optical | Mazaeva et al. | 23302 | TSHAO optical upper limit | Zeiss-1000 | upper limits |
Filter | Exp(s) | Mag | ||
---|---|---|---|---|
whit |
212 | 362 | 147 | >21.2 |
white | 212 | 2818 | 602 | >21.1 |
v | 517 | 2620 | 226 | >20.1 |
b | 443 | 2718 | 240 | >20.7 |
u | 418 | 2693 | 245 | >19.7 |
w1 | 394 | 2669 | 253 | >20.8 |
m2 | 369 | 2644 | 233 | >19.3 |
w2 | 659 | 2595 | 194 | >19.9 |
Table 3. UVOT observations reported by Kuin and Tohuvavohu (GCN Circ. 23283). The start and stop times of the exposures are given in seconds since the BAT trigger. The preliminary 3-σ upper limits are given. No correction has been made for extinction in the Milky Way.
October 4, 2018