Swift Observations of GRB 210419A

S. Laha (GSFC/UMBC/CRESST), A.P. Beardmore (U. Leicester) and M.H. Siegel (PSU) for the Swift team

1. Introduction

At 06:53:41 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 210419A (trigger=1044032) (Laha et al. GCN Circ. 29828). Swift slewed immediately to the burst. At the time of the trigger, the initial BAT position was 88° from the Sun (4.0 hours East) and 93° from the 40%-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.

2. BAT Observations and Analysis

As reported by Palmer et al. (GCN Circ. 29838), the BAT ground-calculated position is RA, Dec = 86.912, -65.452 deg which is RA(J2000) = 05h47m38.9s Dec(J2000) = -65°27'07.2" with an uncertainty of 2.7 arcmin, (radius, sys+stat, 90% containment). The partial coding was 61%.

The BAT light curve (Figure 1) showed a complex structure with a duration of about ~100 s. T90 (15-350 keV) is 64.43 ± 11.69 s (estimated error including systematics).

The time-averaged spectrum from T+21.92 to T+95.01 s is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.17 ± 0.24. The fluence in the 15-150 keV band is 7.8 ± 1.2 x 10-7 erg cm-2. This fluence is larger than that of 32% of the long GRBs in the Second BAT GRB Catalog (Sakamoto et al. 2011). The 1-s peak photon flux measured from T+41.82 s in the 15-150 keV band is 0.6 ± 0.2 ph cm-2 s-1. All the quoted errors are at the 90% confidence level.

3. XRT Observations and Analysis

Analysis of the initial XRT data was reported by Beardmore et al. (GCN Circ. 29835). We have analysed 8.7 ks of XRT data for GRB 210419A, from 134 s to 126.7 ks after the BAT trigger. The data comprise 143 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. 29830).

The late-time light curve (Figure 2) (from T0+5.5 ks) can be modelled with a power-law decay with a decay index of α=0.88 ± 0.21.

A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.71 (+0.11, -0.10). The best-fitting absorption column is 1.4 (+0.4, -0.3) x 1021 cm-2, in excess of the Galactic value of 7.8 x 1020 cm-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.60 (+0.29, -0.27) and a best-fitting absorption column of 1.9 (+0.7, -0.6) x 1021 cm-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 2.6 x 10-11 (4.8 x 10-11) erg cm-2 count-1.

A summary of the PC-mode spectrum is thus:
Total column: 1.9 (+0.7, -0.6) x 1021 cm-2
Galactic foreground: 7.8 x 1020 cm-2
Excess significance: 2.9 σ
Photon index: 2.60 (+0.29, -0.27)

The results of the XRT team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01044032.

4. UVOT Observations and Analysis

The Swift/UVOT began settled observations of the field of GRB 210419A 136 s after the BAT trigger (Siegel and Laha GCN Circ. 29841). No optical afterglow consistent with the XRT position (Osborne et al., GCN Circ. 29830) 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 EB-V of 0.075 mag. in the direction of the GRB (Schlegel et al. 1998).

BAT light curve

Figure 1. The BAT mask-weighted light curve in the four individual and total energy bands. The units are counts s-1 illuminated-detector-1. The vertical green dash-dotted lines show the T50 interval, the vertical black dashed lines show the T90 interval, and vertical blue (orange) solid lines show the start (stop) of slews.

XRT light curve

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
05h47m24.16s -65°30'08.1" 2.0" XRT-final UKSSDC
05h47m24.23s -65°30'09.0" 2.0" XRT-enhanced Osborne et al. GCN Circ. 29830
05h47m38.9s -65°27'07.2" 2.7' BAT-refined Palmer et al. GCN Circ. 29838

Table 1. Positions from the Swift instruments.

Band Authors GCN Circ. Subject Observatory Notes
Optical Strausbaugh and Cucchiara 29829 LCO Optical Upper Limit LCO upper limits
Optical Lipunov et al. 29832 Swift GRB 210419A: Global MASTER-Net
observations report 		MASTER
Optical Lipunov et al. 29836 Swift GRB210419.98: Global MASTER-Net
observations report 		MASTER

Table 2. Summary of GCN Circulars from other observatories sorted by band and then circular number.

Filter Tstart(s) Tstop(s) Exp(s) Mag
whiteFC 136 286 147 >18.1
uFC 294 544 246 >17.9
white 136 1027 333 >18.1
v 627 1079 58 >17.5
b 550 746 39 >17.7
u 294 721 265 >17.9
w1 677 871 39 >17.8
m2 651 1103 58 >18.3
w2 119 1053 67 >19.3

Table 3. UVOT observations reported by Siegel and Laha (GCN Circ. 29841). 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.

April 21, 2021