Observations of the region of M 31 have been made at Cambridge at 408 and 1407 MHz with resolutions of 80#>c 120 and 23 X 35 respectively. A catalogue of 213 discrete sources with flux densities S408> 12 X io-5 W m-2 Hz-' has been prepared, although very few of these appear to be related to M 31. New techniques have been used to examine the large-scale distribution of radiation from the nebula itself; the results presented here show that the disk component of the continuum radiation is largely non-thermal at 408 MHz and originates almost entirely in the nucleus and the H II spiral arms. Its distribution suggests that the particle acceleration processes or magnetic field are closely linked with stur formation and the presence of ionized gas. Two possible spur' features may be associated with the companion galaxies M 32 and NGC 205, but the spurs previously reported have not been confirmed. A brief comparison of the radio emission from M 31 and the Galaxy is made.