Synchrotron polarization with a partially random magnetic field: General approach and application to X-ray polarization from supernova remnants

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Volume 689 (September 2024)

A&A, 689 (2024) A137

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Table B.1.

Best-fit coefficients (a, b, c, d, e), to adopt for the function $X_{F}^{appr} (s, β, x_{cut})$ $X_{F}^{\mathrm{appr}}(s,{\beta},x_{\mathrm{cut}})$ , in order to approximate the function X_F(s, β, x_cut), for various choices of the parameters s and β. The last column gives the maximum deviation, in absolute value, of the approximation.

s	β	a	b	c	d	e	Max.Dev.
1.9	1.0	6.02774	0.5619608	1.90225	0.3330766	0.99241	0.0024

1.9	1.5	7.11761	0.7251578	1.99772	0.4280908	0.95624	0.0062

1.9	2.0	4.70687	0.7723972	2.02137	0.4993386	1.19300	0.0079

2.0	1.0	5.01121	0.5586867	1.90537	0.3329990	1.01129	0.0019

2.0	1.5	6.03545	0.7317618	1.99846	0.4280685	0.95430	0.0072

2.0	2.0	4.42475	0.7957342	2.02102	0.4993466	1.13191	0.0083

2.1	1.0	4.23132	0.5548417	1.90750	0.3329464	1.03592	0.0016

2.1	1.5	5.17683	0.7359420	1.99879	0.4280585	0.95770	0.0069

2.1	2.0	4.27174	0.8200959	2.02095	0.4993476	1.06808	0.0060

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