SIMBAD references

What determines the nuclear radio emission in local galaxies? To address this question, we combine optical [O III] line emission, robust black hole (BH) mass estimates, and high-resolution e-MERLIN 1.5-GHz data, from the LeMMINGs survey, of a statistically complete sample of 280 nearby optically active (LINER and Seyfert) and inactive [H II and absorption line galaxies (ALGs)] galaxies. Using [O III] luminosity (L_[O III]_) as a proxy for the accretion power, local galaxies follow distinct sequences in the optical-radio planes of BH activity, which suggest different origins of the nuclear radio emission for the optical classes. The 1.5-GHz radio luminosity of their parsec-scale cores (L_core) is found to scale with BH mass (M_BH) and [O III] luminosity. Below M_BH ∼ 10^6.5 M_☉, stellar processes from non-jetted H II galaxies dominate with L_core ∝M_BH^0.61±0.33^ and L_core ∝L_[O III]_^0.79±0.30^. Above M_BH ∼ 10^6.5 M_☉, accretion-driven processes dominate with L_core ∝M_BH^1.5–1.65 and L_core ∝L_[O III]_^0.99–1.31 for active galaxies: radio-quiet/loud LINERs, Seyferts, and jetted H II galaxies always display (although low) signatures of radio-emitting BH activity, with L_1.5 GHz_ ≳10^19.8 W Hz^–1 and M_BH >= 10⁷ M_☉, on a broad range of Eddington-scaled accretion rates ({dot}m). Radio-quiet and radio-loud LINERs are powered by low-{dot}m discs launching sub-relativistic and relativistic jets, respectively. Low-power slow jets and disc/corona winds from moderately high to high-{dot}m discs account for the compact and edge-brightened jets of Seyferts, respectively. Jetted H II galaxies may host weakly active BHs. Fuel-starved BHs and recurrent activity account for ALG properties. In conclusion, specific accretion-ejection states of active BHs determine the radio production and the optical classification of local active galaxies.