A comprehensive broadband analysis of the high-redshift GRB 240218A

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Table 4.

Spectral energy distribution modelling results.

Time interval	Data	Model	Parameters					p value
(from t₀)			Γ₁	Γ₂	E_b [keV]	E(B − V) [mag]	log(N_H) [cm⁻²]

160–170 s	BAT + XRT + REM	SBPL	$- 0 . 8_{- 0.3}^{+ 0.5}$ $-0.8^{+0.5}_{-0.3}$	$- 1 . 6_{- 0.05}^{+ 0.05}$ $-1.6^{+0.05}_{-0.05}$	0.06 $_{- 0.04}^{+ 0.19}$ $^{+0.19}_{-0.04}$	0.12^a	21.0^(a)	0.35
178–188 s	″	″	$- 1 . 39_{- 0.02}^{+ 0.02}$ $-1.39^{+0.02}_{-0.02}$	$- 2 . 9_{- 1.5}^{+ 0.9}$ $-2.9^{+0.9}_{-1.5}$	4.27 $_{- 1.64}^{+ 1.48}$ $^{+1.48}_{-1.64}$	0.12^a	21.0^(a)	0.05
195–205 s	BAT + XRT	″	$- 1 . 20_{- 0.07}^{+ 0.07}$ $-1.20^{+0.07}_{-0.07}$	$- 1 . 82_{- 0.22}^{+ 0.15}$ $-1.82^{+0.15}_{-0.22}$	7.76 $_{- 2.26}^{+ 4.26}$ $^{+4.26}_{-2.26}$	0.12^a	21.0^(a)	0.27
213–223 s	″	″	$- 1 . 30_{- 0.06}^{+ 0.05}$ $-1.30^{+0.05}_{-0.06}$	$- 2 . 8_{- 0.9}^{+ 0.5}$ $-2.8^{+0.5}_{-0.9}$	7.04 $_{- 1.21}^{+ 2.09}$ $^{+2.09}_{-1.21}$	0.12^a	21.0^(a)	0.27
230–240 s	″	″	$- 1 . 60_{- 0.07}^{+ 0.08}$ $-1.60^{+0.08}_{-0.07}$	$- 2 . 6_{- 1.6}^{+ 0.6}$ $-2.6^{+0.6}_{-1.6}$	10.0 $_{- 6.0}^{+ 29.8}$ $^{+29.8}_{-6.0}$	0.12^a	21.0^(a)	0.14
∼10³ s	XRT + REM	SBPL	$- 1 . 80_{- 0.04}^{+ 0.17}$ $-1.80^{+0.17}_{-0.04}$	$- 2 . 4_{- 1.0}^{+ 0.5}$ $-2.4^{+0.5}_{-1.0}$	$1 . 6_{- 1.6}^{+ 1.5}$ $1.6^{+1.5}_{-1.6}$	0.12 $_{- 0.01}^{+ 0.01}$ $^{+0.01}_{-0.01}$	20.6 $_{- 1.0}^{+ 0.6}$ $^{+0.6}_{-1.0}$	0.81
∼10³ s	XRT + REM	SBPL	$- 1 . 7_{- 0.1}^{+ 0.4}$ $-1.7^{+0.4}_{-0.1}$	$- 2 . 4_{- 0.4}^{+ 0.1}$ $-2.4^{+0.1}_{-0.4}$	$0 . 20_{- 0.17}^{+ 1.06}$ $0.20^{+1.06}_{-0.17}$	0.12^a	21.0^(a)	0.94
1.26–1.52 d	XRT + LBT (JHK)	PL	$- 1 . 99_{- 0.03}^{+ 0.02}$ $-1.99^{+0.02}_{-0.03}$	−	−	$0 . 12_{- 0.01}^{+ 0.01}$ $0.12^{+0.01}_{-0.01}$	$21 . 0_{- 0.4}^{+ 0.2}$ $21.0^{+0.2}_{-0.4}$	0.05
2.98–3.06 d	XRT + GTC (JHK)	PL	$- 1 . 99_{- 0.03}^{+ 0.02}$ $-1.99^{+0.02}_{-0.03}$	−	−	$0 . 12_{- 0.01}^{+ 0.01}$ $0.12^{+0.01}_{-0.01}$	$21 . 0_{- 0.4}^{+ 0.3}$ $21.0^{+0.3}_{-0.4}$	0.05

Notes. Spectral energy distribution analysis of GRB 240218A in different time intervals. The results coming from the best modelling are shown for each SED. The spectral slopes, Γ₁ and Γ₂, are reported as photon indices (Γ = β + 1). The Bayesian p values shown in the last column were computed according to Lucy (2016, 2018).

^(a)

Fixed parameter in the fit.

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