A Radio Burst Detection Method Based on the Hough Transform. (arXiv:1904.11618v2 [astro-ph.IM] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Zuo_S/0/1/0/all/0/1">Shifan Zuo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_X/0/1/0/all/0/1">Xuelei Chen</a>

We present a simple and fast method for incoherent dedispersion and fast
radio burst (FRB) detection based on the Hough transform, which is widely used
for feature extraction in image analysis. The Hough transform maps a point in
the time-frequency data to a straight line in the parameter space, and points
on the same dispersed $f^{-2}$ curve to a bundle of lines all crossing at the
same point, thus the curve is transformed to a single point in the parameter
space, enabling an easier way for the detection of radio burst. By choosing an
appropriate truncation threshold, in a reasonably radio quiet environment, i.e.
with radio frequency interferences (RFIs) present but not dominant, the
computing speed of the method is very fast. Using simulation data of different
noise levels, we studied how the detected peak varies with different truncation
thresholds. We also tested the method with some real pulsar and FRB data.

We present a simple and fast method for incoherent dedispersion and fast
radio burst (FRB) detection based on the Hough transform, which is widely used
for feature extraction in image analysis. The Hough transform maps a point in
the time-frequency data to a straight line in the parameter space, and points
on the same dispersed $f^{-2}$ curve to a bundle of lines all crossing at the
same point, thus the curve is transformed to a single point in the parameter
space, enabling an easier way for the detection of radio burst. By choosing an
appropriate truncation threshold, in a reasonably radio quiet environment, i.e.
with radio frequency interferences (RFIs) present but not dominant, the
computing speed of the method is very fast. Using simulation data of different
noise levels, we studied how the detected peak varies with different truncation
thresholds. We also tested the method with some real pulsar and FRB data.

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