A study of Kepler supernova remnant: angular power spectrum estimation
  from radio frequency data
  Supernova remnants (SNRs) have a variety of overall morphology as well as
rich structures over a wide range of scales. Quantitative study of these
structures can potentially reveal fluctuations of density and magnetic field
originating from the interaction with ambient medium and turbulence in the
expanding ejecta. We have used $1.5$GHz (L band) and $5$GHz (C band) VLA data
to estimate the angular power spectrum $C_{\ell}$ of the synchrotron emission
fluctuations of the Kepler SNR. This is done using the novel, visibility based,
Tapered Gridded Estimator of $C_{\ell}$. We have found that, for $\ell = (1.9 -
6.9) \times 10^{4}$, the power spectrum is a broken power law with a break at
$\ell = 3.3 \times 10^{4}$, and power law index of $-2.84\pm 0.07$ and
$-4.39\pm 0.04$ before and after the break respectively. The slope $-2.84$ is
consistent with 2D Kolmogorov turbulence and earlier measurements for the Tycho
SNR. We interpret the break to be related to the shell thickness of the SNR
($0.35 $ pc) which approximately matches $\ell = 3.3 \times 10^{4}$ (i.e.,
$0.48$ pc). However, for $\ell > 6.9 \times 10^{4}$, the estimated $C_{\ell}$
of L band is likely to have dominant contribution from the foregrounds while
for C band the power law slope $-3.07\pm 0.02$ is roughly consistent with $3$D
Kolmogorov turbulence like that observed at large $\ell$ for Cas A and Crab
SNRs.
