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Supernova remnants (SNRs) have a variety of overall morphology as well asrich structures over a wide range of scales. Quantitative study of thesestructures can potentially reveal fluctuations of density and magnetic fieldoriginating from the interaction with ambient medium and turbulence in theexpanding ejecta. We have used $1.5$GHz (L band) and $5$GHz (C band) VLA datato estimate the angular power spectrum $C_{\ell}$ of the synchrotron emissionfluctuations 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 $-2.84$ isconsistent with 2D Kolmogorov turbulence and earlier measurements for the TychoSNR. 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 whilefor C band the power law slope $-3.07\pm 0.02$ is roughly consistent with $3$DKolmogorov turbulence like that observed at large $\ell$ for Cas A and CrabSNRs.

A study of Kepler supernova remnant: angular power spectrum estimation from radio frequency data