The nature of LOFAR rotation measures and new constraints on magnetic fields in cosmic filaments and on magnetogenesis scenarios

Open Access

Table B.1.

As for Table 3 except the magnetic field is dependent on the gas density as B_f ∝ ρ_g^2/3.

model	α	$B_{f, 0}^{10}$ $B_{f,0}^{10}$	A_rrm	β
		[nG]	[rad m⁻²]
stochastic α_s = -1.0	2.7 ± 0.4	4.0 ± 1.0	1.30 ± 0.08	0.7 ± 0.4
stochastic α_s = 0.0	2.5 ± 0.7	4.5 ± 2.3	1.30 ± 0.10	0.5 ± 0.7
stochastic α_s = 1.0	2.6 ± 0.5	4.2 ± 1.2	1.28 ± 0.09	0.6 ± 0.5
stochastic α_s = 2.0	2.3 ± 0.8	5.1 ± 2.4	1.28 ± 0.12	0.3 ± 0.8
astroph	2.1 ± 0.5	7.9 ± 2.2	1.15 ± 0.11	0.1 ± 0.5
astroph 2	2.0 ± 0.6	9.7 ± 3.2	1.11 ± 0.12	0.0 ± 0.6
astroph 2 + stochastic α_s = -1.0	2.2 ± 0.6	7.5 ± 2.4	1.23 ± 0.11	0.2 ± 0.6
uniform	2.2 ± 1.0	5.3 ± 4.1	1.26 ± 0.13	0.2 ± 1.0

Notes. Columns are the same except $B_{f, 0}^{10}$ $B_{f,0}^{10}$ is the filament field strength at z = 0 and gas density contrast δ_g = 10. A local component term as A_rrm/(1 + z)² is also used.

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