  The generation of large-scale magnetic fields ($\overline{\mathbf{B}}$) in
astrophysical systems is driven by the mean turbulent electromotive force
($\overline{{\cal E}}$), the cross correlation between local fluctuations of
velocity and magnetic fields. This can depend non-locally on
$\overline{\mathbf{B}}$ through a convolution kernel $K_{ij}$. In a new
approach to find $K_{ij}$, we directly fit the time series data of
$\overline{{\cal E}}$ versus $\overline{\mathbf{B}}$ from a galactic dynamo
simulation using singular value decomposition. We calculate the usual turbulent
transport coefficients as moments of $K_{ij}$, show the importance of including
non-locality over eddy length scales to fully capture their amplitudes and that
higher order corrections to the standard transport coefficients are small in
the present case.
