Radio haloes in nearby galaxies modelled with 1D cosmic-ray transport
  using SPINNAKER
  We present radio continuum maps of 12 nearby ($D\leq 27~\rm Mpc$), edge-on
($i\geq 76^{\circ}$), late-type spiral galaxies mostly at $1.4$ and 5 GHz,
observed with the Australia Telescope Compact Array, Very Large Array,
Westerbork Synthesis Radio Telescope, Effelsberg 100-m and Parkes 64-m
telescopes. All galaxies show clear evidence of radio haloes, including the
first detection in the Magellanic-type galaxy NGC 55. In 11 galaxies, we find a
thin and a thick disc that can be better fitted by exponential rather than
Gaussian functions. We fit our SPINNAKER (SPectral INdex Numerical Analysis of
K(c)osmic-ray Electron Radio-emission) 1D cosmic-ray transport models to the
vertical model profiles of the non-thermal intensity and to the non-thermal
radio spectral index in the halo. We simultaneously fit for the advection speed
(or diffusion coefficient) and magnetic field scale height. In the thick disc,
the magnetic field scale heights range from 2 to 8 kpc with an average across
the sample of $3.0\pm 1.7~\rm kpc$; they show no correlation with either
star-formation rate (SFR), SFR surface density ($\Sigma_{\rm SFR}$) or rotation
speed ($V_{\rm rot}$). The advection speeds range from 100 to $700~\rm
km\,s^{-1}$ and display correlations of $V\propto \rm SFR^{0.36\pm 0.06}$ and
$V\propto \Sigma_{\rm SFR}^{0.39\pm 0.09}$; they agree remarkably well with the
escape velocities ($0.5\leq V/V_{\rm esc}\leq 2$), which can be explained by
cosmic-ray driven winds. Radio haloes show the presence of disc winds in
galaxies with $\Sigma_{\rm SFR} > 10^{-3}~\rm M_{\odot}\,yr^{-1}\,kpc^{-2}$
that extend over several kpc and are driven by processes related to the
distributed star formation in the disc.
