The Local Group dwarf elliptical galaxy M32 hosts one of the nearest and most under-luminous super-massive black holes ( SMBHs ) ever known , offering a rare opportunity to study the physics of accreting SMBHs at the most quiescent state . Recent Very Large Array ( VLA ) observations have detected a radio source at the nucleus of M32 , which is suggested to be the radio counterpart of the SMBH . To further investigate the radio properties of this nuclear source , we have conducted follow-up , high-resolution VLA observations in four epochs between 2015–2017 , each with dual frequencies . At 6 GHz , the nuclear source is resolved under an angular resolution of \sim 0 \farcs 4 , exhibiting a coreless , slightly lopsided morphology with a detectable extent of \sim 2 \arcsec ( \sim 8 parsec ) . No significant variability can be found among the four epochs . At 15 GHz , no significant emission can be detected within the same region , pointing to a steep intrinsic radio spectrum ( with a 3 \sigma upper limit of -1.46 for the spectral index ) . We discuss possible scenarios for the nature of this nuclear source and conclude that a stellar origin , in particular planetary nebulae , X-ray binaries , supernova remnants or diffuse ionized gas powered by massive stars , can be ruled out . Instead , the observed radio properties can be explained by synchrotron radiation from a hypothetical wind driven by the weakly accreting SMBH .