Astronomy & Astrophysics

All Tables

Table 1: Observational parameters of VLA observations.
Table 2: Weights and rms noise values of total intensity $\sigma _{I}$ and of polarized intensity $\sigma _{Q,U}$ (for Stokes parameters Q and U) (in $\mu$ Jy/beam) in the final maps.
Table 3: Properties of the radio ridges in the bars of NGC 1097 and NGC 1365 from the $\lambda 6.2$ cm data. I is the total intensity, P the polarized intensity. $\epsilon _I$ and $\epsilon _{\rm P}$ are the contrasts in I and P between the ridges and the surrounding regions. $\alpha$ is the spectral index between $\lambda 6.2$ cm and $\lambda 3.5$ cm, $f_{\rm th}$ is the thermal fraction of I, $I_{\rm s}=I(1-f_{\rm th})$ is the synchrotron intensity, and $p=P/I_{\rm s}$ is the fractional polarization of the synchrotron emission. B_I and $B_{\rm P}$ are the equipartition strengths of the total and regular + anisotropic random magnetic fields derived from $I_{\rm s}$ and P (see Sect. 3.6). The distance along the NGC 1097 ridge is measured from the galaxy's centre. For NGC 1365, average values along the ridges are given.
Table 4: Properties of the central parts of NGC 1097 ( $r<1~{\rm kpc}$ ) and NGC 1365 ( $r<2~{\rm kpc}$ ) from the $\lambda 3.5$ cm data. The locations of the regions are described in the text. The thermal fractions were determined with the assumption of a synchrotron spectral index of $\alpha _{\rm s}=-1.0$ .
Table A.1: Parameters of fitted model for NGC 1097, with notation as in Eq. (B.1).
Table A.2: Parameters of fitted model for NGC 1365, with notation as in Eq. (B.1) and ring width $1.75~{\rm kpc}$ .