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The feeble radiative efficiency characteristic of Low-Luminosity ActiveGalactic Nuclei (LLAGN) is ascribed to a sub-Eddington accretion rate,typically at $\log(L_{\rm bol}/L_{\rm edd}) \lesssim -3$. At the finest angularresolutions that are attainable nowadays using mid-infrared (mid-IR)interferometry, the prototypical LLAGN in NGC 1052 remains unresolved down to$< 5\, \rm{mas}$ ($0.5\, \rm{pc}$). This is in line with non-thermal emissionfrom a compact jet, a scenario further supported by a number of evidences: thebroken power-law shape of the continuum distribution in the radio-to-UV range;the $\sim 4\%$ degree of polarisation measured in the nuclear mid-IR continuum,together with the mild optical extinction ($A_V \sim 1\, \rm{mag}$); and the"harder when brighter" behaviour of the X-ray spectrum, indicative ofself-Compton synchrotron radiation. A remarkable feature is the steepness ofthe IR-to-UV core continuum, characterised by a power-law index of $\sim 2.6$,as compared to the canonical value of $0.7$. Alternatively, to explain theinterferometric data by thermal emission would require an exceptionally compactdust distribution when compared to those observed in nearby AGN, with $A_V\gtrsim 2.8\, \rm{mag}$ to account for the IR polarisation. This is in contrastwith several observational evidences against a high extinction along the lineof sight, including the detection of the nucleus in the UV range and the welldefined shape of the power-law continuum. The case of NGC 1052 shows thatcompact jets can dominate the nuclear emission in LLAGN across the wholeelectromagnetic spectrum, a scenario that might be common among this class ofactive nuclei.

A Compact Jet at the Infrared Heart of the Prototypical Low-Luminosity AGN in NGC 1052