Clues to the photosphere emission origin of gamma-ray burst polarization

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Table 1.

Correlation between α and the polarization degree.

GRB Name	α	Polarization degree
POLAR:
GRB 161218A	−0.54 ± 0.07	9.0 $_{- 7.0}^{+ 10.7} %$ $_{-7.0}^{+10.7} \%$
GRB 170114A	−0.68 ± 0.09	4.0 $_{- 4.0}^{+ 10.5} %$ $_{-4.0}^{+10.5} \%$
GRB 170127C	0.25 ± 0.12	11.0 $_{- 8.4}^{+ 19.3} %$ $_{-8.4}^{+19.3} \%$
GRB 170206A	−0.49 ± 0.04	10.0 $_{- 8.6}^{+ 7.4} %$ $_{-8.6}^{+7.4} \%$

AstroSAT:
GRB 160106A	−0.53 ± 0.07	69 ± 24 %
GRB 160325A	−0.71 ± 0.07	59 ± 28 %
GRB 160802A	−0.61 ± 0.04	85 ± 30 %
GRB 160821A	−0.97 ± 0.01	54 ± 16 %
GRB 160910A	−0.36 ± 0.03	94 ± 32 %

Notes. We show the distribution of the low-energy spectral index α and the polarization degree for four POLAR bursts (adopted from Zhang et al. 2019) and five AstroSAT bursts (adopted from Chattopadhyay et al. 2019). We did not adopt GRB 170101A in POLAR or 160131A in AstroSAT due to the lack of Fermi/GBM detection. The low-energy spectral index α from Swift/BAT or Konus/Wind could have a relatively large error. The errors of PD for POLAR were taken from Kole et al. (2020).

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