radio-quiet Seyferts, whose origin is under debate [@panessa2019 and references therein]. In general, a coronal origin for the radio emission is suggested by the observed relation between the radio luminosity at 5 GHz $L_R$ and the X-ray (0.2–20 keV) luminosity $L_X$, with $L_R/L_X={10^{-5}}$ like in coronally active stars . Another hint is the presence of a mm-wave excess with respect to the spectral slope extrapolated from low frequencies [@behar2015; @behar2018]. [NGC 4388]{} has a complex radio structure [@falcke1998; @mundell2000], with a faint core having a flux density of 1.3 mJy at 1.6 GHz and $<0.55$ mJy at 5 GHz [@gp2009]. This source exhibits a mm excess [@behar2018], but it also has a $L_R/L_X$ ratio $< {10^{-7}}$ [from the upper limit to the 5-GHz luminosity reported by @gp2009]. [NGC 2110]{} shows an S-shaped jet-counterjet radio structure, with a relatively bright core having a flux density of 100 mJy at 5 GHz [@ulv1983; @mundell2000]. [@beckmann2010] argue that this object is borderline between a radio-quiet Seyfert and a radio-loud galaxy with a [@fr1974] type I morphology. No mm excess is found in [NGC 2110]{}, whose radio and mm emission is consistent with originating from the jet [@behar2018]. We conclude that the radio emission 