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Only in the late 1940s the connection between cosmic radio waves and synchrotron emission could be established. Synchrotron emissions of AGN is due to the presence of magnetic fields. This emission is observable as polarized emission. Cosmic objects emit intense radio waves through the synchrotron emission. It is widely held that radio sources in the cosmic universe emit by the synchrotron process, especially at the lower radio frequencies in the metre and cm wavelength range. This range is detected by the FIRST survey. (http://www.ugr.es/~battaner/escritos/granada_paper.pdf)  \subsection{Results from previous publications. - this secton is incomplete}  \subsection{My aim/focus}  I will use large-area optical and radio surveys (SDSS and FIRST) to systematically measure the enhanced radio emission in merging galaxies in the low redshift Universe (z < 0.4). Through the use of statistical techniques on a catalogue of all the optically-selected SDSS quasar pairs for which there is a radio detection (in FIRST) within 3 arc seconds (which is roughly half the angular resolution of the radio maps in FIRST), I will make aggregated radio detections of the population of galaxy mergers that do not have individual radio detections. This is done because existing radio surveys are not as sensitive as their optical/IR counterparts. The statistically analysed data will be combined with a sample of "post-merger" (clearly disrupted, but individual) galaxies with the aim of investigating the nature of this enhanced emission as a function of galaxy separation.  The sample of “post-merger” galaxies lists the optically-selected SDSS quasar pairs that aren't detected in the FIRST radio maps. In other words, for these pairs, no radio source was detected within 3 arc seconds of the optical position. As non-radio-detected SDSS quasar pair images are stacked up (add) the radio maps of the non-detections later on and get a statistical radio detection. We aim to observe and analyse these detections. 
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