Table 3.
Best-fit parameters of the filament magnetic field strength and evolution with redshift to the measured RRM rms at 144-MHz of the sample filtered with GRMth = 14 rad m−2 and in case of an astrophysical component term of shape Arrm/(1 + z)2.
| Model | α | Bf, 0 | Arrm | β |
|---|---|---|---|---|
| [nG] | [rad m−2] | |||
| stochastic αs = −1.0 | 2.1 ± 0.4 | 20 ± 4 | 1.14 ± 0.10 | 0.1 ± 0.4 |
| stochastic αs = 0.0 | 1.9 ± 0.4 | 24 ± 5 | 1.12 ± 0.10 | −0.1 ± 0.4 |
| stochastic αs = 1.0 | 1.8 ± 0.4 | 24 ± 5 | 1.10 ± 0.11 | −0.2 ± 0.4 |
| stochastic αs = 2.0 | 1.8 ± 0.4 | 25 ± 5 | 1.11 ± 0.11 | −0.2 ± 0.4 |
| astroph | 1.8 ± 0.4 | 27 ± 6 | 1.06 ± 0.12 | −0.2 ± 0.4 |
| astroph 2 | 1.9 ± 0.4 | 24 ± 5 | 1.02 ± 0.11 | −0.1 ± 0.4 |
| astroph 2 + stochastic αs = −1.0 | 1.7 ± 0.4 | 27 ± 6 | 1.13 ± 0.10 | −0.3 ± 0.4 |
| uniform | 1.9 ± 0.5 | 24 ± 6 | 1.12 ± 0.11 | −0.1 ± 0.5 |
Notes. The case with density taken from simulations and constant magnetic field strength is reported. Columns are the magnetogenesis model studied (astroph and astroph 2 are the first and second astrophysical models discussed in Section 3) and the fit parameters: the slope α of the filament magnetic field behaviour as a function of redshift; the strength Bf, 0 of the filament magnetic field at z = 0; the astrophysical component term Arrm; the slope β of the comoving magnetic field. All cases are fit to the RRM rms computed in 20-source redshift bins.
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