Multi-epoch Low Radio Frequency Surveys of the Kepler K2 Mission Campaign Fields 3, 4, and 5 with the Murchison Widefield Array. (arXiv:1905.09392v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tingay_S/0/1/0/all/0/1">S.J. Tingay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hancock_P/0/1/0/all/0/1">P.J Hancock</a>
We present Murchison Widefield Array (MWA) monitoring of the Kepler K2
mission Fields 3, 4, and 5 at frequencies of 155 and 186 MHz, from observations
contemporaneous with the K2 observations. This work follows from previous MWA
and GMRT surveys of Field 1, with the current work benefiting from a range of
improvements in the data processing and analysis. We continue to build a body
of systematic low frequency blind surveys overlapping with transient/variable
survey fields at other wavelengths, providing multi-wavelength data for object
classes such as flare stars. From the current work, we detect no variable
objects at a surface density above 2e-4 per square degree, at flux densities of
~500 mJy, and observation cadence of days to weeks, representing almost an
order of magnitude decrease in measured upper limits compared to previous
results in this part of observational parameter space. This continues to show
that radio transients at metre and centimetre wavelengths are rare.
We present Murchison Widefield Array (MWA) monitoring of the Kepler K2
mission Fields 3, 4, and 5 at frequencies of 155 and 186 MHz, from observations
contemporaneous with the K2 observations. This work follows from previous MWA
and GMRT surveys of Field 1, with the current work benefiting from a range of
improvements in the data processing and analysis. We continue to build a body
of systematic low frequency blind surveys overlapping with transient/variable
survey fields at other wavelengths, providing multi-wavelength data for object
classes such as flare stars. From the current work, we detect no variable
objects at a surface density above 2e-4 per square degree, at flux densities of
~500 mJy, and observation cadence of days to weeks, representing almost an
order of magnitude decrease in measured upper limits compared to previous
results in this part of observational parameter space. This continues to show
that radio transients at metre and centimetre wavelengths are rare.
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