Recent observations with the Murchison Widefield Array at 185~MHz have serendipitously unveiled a heretofore unknown giant and relatively nearby ($z = 0.0178$) radio galaxy associated with NGC,1534. The diffuse emission presented here is the first in
dication that NGC,1534 is one of a rare class of objects (along with NGC,5128 and NGC,612) in which a galaxy with a prominent dust lane hosts radio emission on scales of $sim$700,kpc. We present details of the radio emission along with a detailed comparison with other radio galaxies with disks. NGC1534 is the lowest surface brightness radio galaxy known with an estimated scaled 1.4-GHz surface brightness of just 0.2,mJy,arcmin$^{-2}$. The radio lobes have one of the steepest spectral indices yet observed: $alpha=-2.1pm0.1$, and the core to lobe luminosity ratio is $<0.1$%. We estimate the space density of this low brightness (dying) phase of radio galaxy evolution as $7times10^{-7}$,Mpc$^{-3}$ and argue that normal AGN cannot spend more than 6% of their lifetime in this phase if they all go through the same cycle.
Lunar Cherenkov experiments aim to detect nanosecond pulses of Cherenkov emission produced during UHE cosmic ray or neutrino interactions in the lunar regolith. Pulses from these interactions are dispersed, and therefore reduced in amplitude, during
propagation through the Earths ionosphere. Pulse dispersion must therefore be corrected to maximise the received signal to noise ratio and subsequent chances of detection. The pulse dispersion characteristic may also provide a powerful signature to determine the lunar origin of a pulse and discriminate against pulses of terrestrial radio frequency interference (RFI). This characteristic is parameterised by the instantaneous Total Electron Content (TEC) of the ionosphere and therefore an accurate knowledge of the ionospheric TEC provides an experimental advantage for the detection and identification of lunar Cherenkov pulses. We present a new method to calibrate the dispersive effect of the ionosphere on lunar Cherenkov pulses using lunar Faraday rotation measurements combined with geomagnetic field models.
