Deep 230-470 MHz VLA Observations of the mini-halo in the Perseus
  Cluster
  We present a low-frequency view of the Perseus cluster with new observations
from the Karl G. Jansky Very Large Array (JVLA) at 230-470 MHz. The data reveal
a multitude of new structures associated with the mini-halo. The mini-halo
seems to be influenced both by the AGN activity as well as by the sloshing
motion of the cool core cluster's gas. In addition, it has a filamentary
structure similar to that seen in radio relics found in merging clusters. We
present a detailed description of the data reduction and imaging process of the
dataset. The depth and resolution of the observations allow us to conduct for
the first time a detailed comparison of the mini-halo structure with the X-ray
structure as seen in the Chandra X-ray images. The resulting image shows very
clearly that the mini-halo emission is mostly contained behind the cold fronts,
similar to that predicted by simulations of gas sloshing in galaxy clusters.
However, due to the proximity of the Perseus cluster, as well as the quality of
the data at low radio frequencies and at X-ray wavelengths, we also find
evidence of fine structure. This structure includes several radial radio
filaments extending in different directions, a concave radio structure
associated with the southern X-ray bay and sharp edges that correlate with
X-ray edges. Mini-halos are therefore not simply diffuse, uniform radio
sources, but are rather filled with a rich variety of complex structures. These
results illustrate the high-quality images that can be obtained with the new
JVLA at low radio-frequencies, as well as the necessity to obtain deeper,
higher-fidelity radio images of mini-halos and halos in clusters to further
understand their origin.
