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We have observed four low‐luminosity active galactic nuclei (AGNs) classified as type 1 Low‐Ionization Nuclear Emission‐Line Regions (LINERs) with the X‐Ray Telescope (XRT) and the Ultraviolet–Optical Telescope (UVOT) onboard  Swift , in an attempt to clarify the main powering mechanism of this class of nearby sources. Among our targets, we detect X‐ray variability in NGC 3998 for the first time. The light curves of this object reveal variations of up to 30 per cent amplitude in half a day, with no significant spectral variability on this time‐scale. We also observe a decrease of ∼30 per cent over 9 d, with significant spectral softening. Moreover, the X‐ray flux is ∼40 per cent lower than observed in previous years. Variability is detected in M81 as well, at levels comparable to those reported previously: a flux increase in the hard X‐rays (1–10 keV) of 30 per cent in ∼3 h and variations by up to a factor of 2 within a few years. This X‐ray behaviour is similar to that of higher luminosity, Seyfert‐type objects. Using previous high‐angular‐resolution imaging data from the  Hubble Space Telescope  ( HST ), we evaluate the diffuse UV emission due to the host galaxy and isolate the nuclear flux in our UVOT observations. All sources are detected in the UV band, at levels similar to those of the previous observations with  HST . The XRT (0.2–10 keV) spectra are well described by single power laws and the UV‐to‐X‐ray flux ratios are again consistent with those of Seyferts and radio‐loud AGNs of higher luminosity. The similarity in X‐ray variability and broad‐band energy distributions suggests the presence of similar accretion and radiation processes in low‐ and high‐luminosity AGNs.

Variability and spectral energy distributions of low‐luminosity active galactic nuclei: a simultaneous X‐ray/UV look with Swift