Extragalactic magnetar giant flare GRB 231115A: Insights from Fermi/GBM observations

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Volume 694 (February 2025)

A&A, 694 (2025) A323

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Table 1.

Time-resolved spectral analysis using BBs.

Interval #	Time	E_p	α	Energy Flux (ℱ)	L_iso	E_iso
	(ms)	(keV)		(×10⁻⁶ ergs s⁻¹ cm⁻²)	(×10⁴⁵ erg⋅ s⁻¹)	(×10⁴⁴ erg)
GRB 231115A
(1)	−34:−17	$400_{- 200}^{+ 200}$ $400^{+200}_{-200}$	$0 . 3_{- 1.4}^{+ 3.8}$ $0.3 ^{+3.8}_{-1.4}$	$1 . 2_{- 0.5}^{+ 0.5}$ $1.2 ^{+0.5}_{-0.5}$	$1 . 8_{- 0.3}^{+ 0.7}$ $1.8 ^{+0.7}_{-0.3}$	$0 . 4_{- 0.1}^{+ 0.1}$ $0.4 ^{+0.1}_{-0.1}$
(2)	−17:−8	$520_{- 70}^{+ 70}$ $520^{+70}_{-70}$	$0 . 5_{- 0.5}^{+ 0.5}$ $0.5 ^{+0.5}_{-0.5}$	$20_{- 2}^{+ 2}$ $20 ^{+2}_{-2}$	$28 . 6_{- 1.3}^{+ 2.2}$ $28.6 ^{+2.2}_{-1.3}$	$2 . 75_{- 0.13}^{+ 0.19}$ $2.75 ^{+0.19}_{-0.13}$
(3)	−8:−5	$450_{- 100}^{+ 110}$ $450^{+110}_{-100}$	$1 . 2_{- 1.7}^{+ 1.5}$ $1.2 ^{+1.5}_{-1.7}$	$11_{- 7}^{+ 3}$ $11 ^{+3}_{-7}$	$16_{- 2}^{+ 4}$ $16 ^{+4}_{-2}$	$0 . 58_{- 0.07}^{+ 0.11}$ $0.58 ^{+0.11}_{-0.07}$
(4)	−5:0	$900_{- 200}^{+ 300}$ $900^{+300}_{-200}$	$- 0 . 1_{- 0.4}^{+ 0.4}$ $-0.1 ^{+0.4}_{-0.4}$	$35_{- 3}^{+ 3}$ $35 ^{+3}_{-3}$	$51_{- 2}^{+ 3}$ $51 ^{+3}_{-2}$	$2 . 7_{- 0.1}^{+ 0.2}$ $2.7 ^{+0.2}_{-0.1}$
(5)	0:23	$510_{- 50}^{+ 50}$ $510^{+50}_{-50}$	$0 . 8_{- 0.5}^{+ 0.5}$ $0.8 ^{+0.5}_{-0.5}$	$10 . 3_{- 1.1}^{+ 1.0}$ $10.3 ^{+1.0}_{-1.1}$	$15_{- 1}^{+ 1}$ $15 ^{+1}_{-1}$	$3 . 7_{- 0.2}^{+ 0.3}$ $3.7 ^{+0.3}_{-0.2}$
(6)	23:40	$600_{- 300}^{+ 400}$ $600^{+400}_{-300}$	$- 0 . 3_{- 0.6}^{+ 0.7}$ $-0.3 ^{+0.7}_{-0.6}$	$4 . 4_{- 1.1}^{+ 1.2}$ $4.4 ^{+1.2}_{-1.1}$	$6 . 4_{- 0.9}^{+ 1.3}$ $6.4 ^{+1.3}_{-0.9}$	$1 . 3_{- 0.2}^{+ 0.3}$ $1.3 ^{+0.3}_{-0.2}$
(7)	40:63	$220_{- 120}^{+ 220}$ $220^{+220}_{-120}$	$- 0 . 5_{- 0.6}^{+ 1.5}$ $-0.5 ^{+1.5}_{-0.6}$	$0 . 7_{- 0.4}^{+ 0.8}$ $0.7 ^{+0.8}_{-0.4}$	$1 . 0_{- 0.6}^{+ 0.9}$ $1.0 ^{+0.9}_{-0.6}$	$0 . 41_{- 0.12}^{+ 0.23}$ $0.41 ^{+0.23}_{-0.12}$

T_BB duration (97):	−34:63	$600_{- 60}^{+ 60}$ $600^{+60}_{-60}$	$0 . 14_{- 0.25}^{+ 0.24}$ $0.14^{+0.24}_{-0.25}$	$7 . 8_{- 0.5}^{+ 0.5}$ $7.8^{+0.5}_{-0.5}$	$11 . 4_{- 0.4}^{+ 0.6}$ $11.4 ^{+0.6}_{-0.4}$	$11 . 5_{- 0.3}^{+ 0.4}$ $11.5 ^{+0.4}_{-0.3}$

GRB 051103
(1*)	−8:−2	$2, 100_{- 1300}^{+ 7900}$ $2,100^{+7900}_{-1300}$	$- 0 . 5_{- 0.3}^{+ 0.5}$ $-0.5 ^{+0.5}_{-0.3}$	$200_{- 110}^{+ 450}$ $200 ^{+450}_{-110}$	$300_{- 200}^{+ 700}$ $300 ^{+700}_{-200}$	$17_{- 9}^{+ 39}$ $17 ^{+39}_{-9}$
(2)	−2:4	$1, 700_{- 500}^{+ 1200}$ $1,700^{+1200}_{-500}$	$- 0 . 2_{- 0.2}^{+ 0.2}$ $-0.2 ^{+0.2}_{-0.2}$	$1, 300_{- 400}^{+ 1000}$ $1,300 ^{+1000}_{-400}$	$1, 900_{- 600}^{+ 1400}$ $1,900 ^{+1400}_{-600}$	$120_{- 30}^{+ 90}$ $120 ^{+90}_{-30}$
(3**)	4:10	$10, 000_{- 7000}^{+ 0}$ $10,000^{+0}_{-7000}$	$- 0 . 36_{- 0.08}^{+ 0.20}$ $-0.36 ^{+0.20}_{-0.08}$	$2, 600_{- 1500}^{+ 200}$ $2,600 ^{+200}_{-1500}$	$3, 900_{- 2000}^{+ 500}$ $3,900 ^{+500}_{-2000}$	$230_{- 130}^{+ 20}$ $230 ^{+20}_{-130}$
(4*)	10:22	$7, 000_{- 5000}^{+ 3000}$ $7,000^{+3000}_{-5000}$	$- 0 . 39_{- 0.11}^{+ 0.28}$ $-0.39 ^{+0.28}_{-0.11}$	$1, 400_{- 900}^{+ 500}$ $1,400 ^{+500}_{-900}$	$2, 000_{- 1300}^{+ 800}$ $2,000 ^{+800}_{-1300}$	$240_{- 180}^{+ 80}$ $240 ^{+80}_{-180}$
(5*)	22:34	$1, 700_{- 800}^{+ 8000}$ $1,700^{+8000}_{-800}$	$0 . 2_{- 0.5}^{+ 0.9}$ $0.2 ^{+0.9}_{-0.5}$	$280_{- 140}^{+ 960}$ $280 ^{+960}_{-140}$	$400_{- 300}^{+ 1400}$ $400 ^{+1400}_{-300}$	$50_{- 20}^{+ 170}$ $50 ^{+170}_{-20}$
(6)	34:74	$1, 000_{- 200}^{+ 400}$ $1,000^{+400}_{-200}$	$0 . 4_{- 0.3}^{+ 0.5}$ $0.4 ^{+0.5}_{-0.3}$	$100_{- 20}^{+ 40}$ $100 ^{+40}_{-20}$	$150_{- 30}^{+ 50}$ $150 ^{+50}_{-30}$	$60_{- 11}^{+ 21}$ $60 ^{+21}_{-11}$
(7)	74:106	$670_{- 130}^{+ 240}$ $670^{+240}_{-130}$	$0 . 1_{- 0.3}^{+ 0.4}$ $0.1 ^{+0.4}_{-0.3}$	$35_{- 6}^{+ 9}$ $35 ^{+9}_{-6}$	$52_{- 9}^{+ 13}$ $52 ^{+13}_{-9}$	$16_{- 3}^{4}$ $16 ^{4}_{-3}$

T_BB duration (114):	−8:106	$1700_{- 300}^{+ 500}$ $1700^{+500}_{-300}$	$- 0 . 1_{- 0.11}^{+ 0.12}$ $-0.1^{+0.12}_{-0.11}$	$250_{- 40}^{+ 80}$ $250^{+80}_{-40}$	$360_{- 60}^{+ 80}$ $360^{+80}_{-60}$	$490_{- 60}^{+ 110}$ $490^{+110}_{-60}$

Notes. The BB interval, time-resolved fluence is from fitting the spectrum with a COMPT over a combined Fermi/GBM (NaI and BGO detectors) spectral range of 8 keV–40 MeV. For GRB 051103 the fits were made using the WIND/KONUS three-channel spectra (20–1200 keV), which typically poorly constrain E_p outside this band. The L_iso and E_iso values were calculated over the standardized bolometric energy range of 1 keV to 10 MeV. For intervals marked with (**) the E_p is not constrained (i.e., > 10 MeV). For intervals marked with (*) the E_p positive error is not constrained.

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