Radio data challenge the broadband modelling of GRB 160131A afterglow

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Table 2.

Best-fit parameters obtained by empirically fitting the radio SEDs of GRB 160131A from 0.8 to 44.8 days after the GRB trigger (see Fig. 4).

t_obs	0.8 d	2.7 d	5.8 d	12.7 d	44.8 d
Model	BPL	BPL	SPL	BPL	BPL
ν_b^(a)	8.9 ± 0.6	23.1 ± 0.5	–	6.6 ± 0.3	7.8 ± 0.3
F_b^(b)	0.32 ± 0.02	0.86 ± 0.10	–	0.32 ± 0.01	0.09 ± 0.01
β_pl	–	–	0.69 ± 0.04	–	–
β_1, bpl	2.2 ± 0.4	1.13 ± 0.03	–	2.39 ± 0.34	4.46 ± 1.90
β_2, bpl	0.50 ± 0.05	−0.75 ± 0.11	–	−0.52 ± 0.05	−0.55 ± 0.26
	0.79	1.60	1.27	0.74	0.88

Notes. “SPL” and “BPL” indicate a power-law (Eq. (2)) and a broken power-law model (Eq. (3)), respectively. ν_b is the break frequency and F_b the flux density at ν = ν_b; β_1, bpl and β_2, bpl are the two BPL spectral indices, while β_pl is the SPL index. The reduced chi square is denoted with .

^(a)

In units of GHz.

^(b)

In units of mJy.

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