Table 5.
Properties of cosmic ray diffusion.
| Galaxy | B0 | Urad/UB | E1 | E2 | τ1 | τ2 | lCRE1 | lCRE2 | D1 | D2 |
|---|---|---|---|---|---|---|---|---|---|---|
| (μG) | (GeV) | (Myr) | (kpc) | (1028 cm2 s−1) | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
| NGC 3184 | 8.1 | 0.16 | 1.15 | 3.57 | 124 ± 31 | 40 ± 10 | 4.8 ± 0.3 | 3.4 ± 0.2 | 5.5 ± 1.6 | 8.9 ± 2.5 |
| NGC 4736 | 10.3 | 0.56 | 1.01 | 3.17 | 74 ± 19 | 24 ± 6 | 1.3 ± 0.1 | 1.0 ± 0.1 | 0.6 ± 0.2 | 1.4 ± 0.5 |
| NGC 5055 | 9.6 | 0.22 | 1.07 | 3.29 | 105 ± 26 | 34 ± 9 | N/A | N/A | N/A | N/A |
| NGC 5194 | 12.2 | 0.25 | 0.95 | 2.92 | 70 ± 18 | 23 ± 6 | 3.8 ± 0.1 | 2.1 ± 0.1 | 5.9 ± 1.6 | 5.8 ± 1.7 |
Notes. Entries with subscripts “1” and “2” are at observing frequencies ν1 ≈ 140 MHz and ν2 = 1365 MHz, respectively. Columns: (1) galaxy name; (2) magnetic field strength in the disc estimated using BFIELD from Beck & Krause (2005). We assumed a path-length of 1 kpc, a proton-to-electron ratio of K = 100, and non-thermal radio spectral index of −0.8, and energy equipartiton; (3) ratio of radiation energy density to magnetic field energy density. The first was estimated from the total infrared luminosities of Galametz et al. (2013), including a contribution from the stellar population and the cosmic ray microwave background (see (Heesen et al. 2018a); (4,5) CRE energies from Eq. (7); (6,7) CRE lifetimes from Eq. (8); (8,9) CRE diffusion lengths (Eq. (5)); analytic estimate of the CRE diffusion coefficients as defined in Eq. (6).
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