2019MNRAS.489.5866S

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_l of the synchrotron emission fluctuations of the Kepler SNR. This is done using the novel, visibility-based, Tapered Gridded Estimator of C_l. We have found that, for l = (1.9-6.9) x 10⁴, the power spectrum is a broken power law with a break at l = 3.3 x 10⁴, and power-law index of -2.84 ± 0.07 and -4.39 ± 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 l = 3.3 x 10⁴ (i.e. 0.48 pc). However, for l > 6.9 x 10⁴, the estimated C_l of L band is likely to have dominant contribution from the foregrounds while for C band the power-law slope -3.07 ± 0.02 is roughly consistent with 3D Kolmogorov turbulence like that observed at large l for Cas A and Crab SNRs.