MWA is a radio interferometer with a unique property – high surface brightness and high spacial resolution at the same time. This makes it an ideal instrument for studying the diffuse emission of galactic gas in radio recombination lines (RRL). This signal is faint and generally very difficult to observe. We have observed a wide field around the galactic centre with the highest frequency resolution available (10KHz) and very deep integration time (22 hours, over 900 observations). Due to the narrow spectral nature of the signal individual channels need to be imaged first and than integrated before the spectra can be obtained. This requires a massive amount of imaging that needs to be done – over 1.5 million images – before the signal can be detected.