  Outlined is the discovery of a very faint, diffuse, low surface-brightness
(0.5 \mJybeam, 1.4 \mJyarcminsq on average) structure around the radio source
B2 0258+35 hosted by an HI-rich early-type galaxy (NGC 1167). Since B2 0258+35
is a young Compact Steep Spectrum (CSS) source, the newly discovered structure
could represent a remnant from an earlier stage of AGN activity.
  We go on by explaining in detail all the possibilities for triggering the
radio activity in B2 0258+35 regarding gas accretion in a recurrent AGN
activity framework.
  NGC 1167 hosts a very regular, extended and massive \HI\ disc that has been
studied in great detail. Previous studies of the \HI\ closer to the core seem
to go against the assumption of a circum-nuclear disc of \HI\ as the source of
the accreting gas.
  We consider the cooling of gas from the hot, X-ray halo as a possible
alternative option for the fueling of the AGN, as suggested in the case of
other sources of similar radio power as B2 0258+35.
  Estimates are given for the age of the faint diffuse emission as well as for
the current accretion rate, which are in good agreement with literature values.
  If our assumptions about the accretion mechanism are correct, similar
large-scale, relic-like structures should be more commonly found around
early-type galaxies and this will be hopefully confirmed by the next generation
of sensitive, low-frequency radio surveys.
