Light-curve modelling constraints on the obliquities and aspect angles of the young Fermi pulsars

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Table 9

Best power-law fits to the distribution of E_cut and Γ as functions of the width of the acceleration gap for each model and RL or RQ pulsars.

		RQ			RL

		Power-law index	Intercept	R ²	Power-law index	Intercept	R ²

SG	E _cut	−0.59 ± 0.12	−0.14 ± 0.11	0.42	−0.46 ± 0.23	−0.14 ± 0.24	0.11
SG	Γ	−0.30 ± 0.07	−0.11 ± 0.06	0.39	−0.13 ± 0.07	0.05 ± 0.07	0.11

OG	E _cut	−0.41 ± 0.09	0.07 ± 0.07	0.42	−0.25 ± 0.15	0.11 ± 0.14	0.08
OG	Γ	−0.19 ± 0.05	0.01 ± 0.04	0.31	−0.06 ± 0.05	0.13 ± 0.04	0.04

OPC	E _cut	−0.29 ± 0.05	−0.01 ± 0.08	0.47	−0.21 ± 0.10	−0.03 ± 0.18	0.11
OPC	Γ	−0.15 ± 0.03	−0.04 ± 0.04	0.42	−0.09 ± 0.03	0.03 ± 0.06	0.26

Notes. The coefficient of determination R² relative to each fit is reported.

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