Searching for signs of jet-driven negative feedback in the nearby radio
  galaxy UGC 05771
  Hydrodynamical simulations predict that the jets of young radio sources can
inhibit star formation in their host galaxies by injecting heat and turbulence
into the interstellar medium (ISM). To investigate jet-ISM interactions in a
galaxy with a young radio source, we have carried out a multi-wavelength study
of the $z = 0.025$ Compact Steep Spectrum radio source hosted by the early-type
galaxy UGC 05771. Using Keck/OSIRIS observations, we detected
H\textsubscript{2} 1--0 S(1) and [Fe \textsc{ii}] emission at radii of 100s of
pc, which traces shocked molecular and ionised gas being accelerated outwards
by the jets to low velocities, creating a `stalling wind'. At kpc radii, we
detected shocked ionised gas using observations from the CALIFA survey,
covering an area much larger than the pc-scale radio source. We found that
existing interferometric radio observations fail to recover a large fraction of
the source's total flux, indicating the likely existence of jet plasma on kpc
scales, which is consistent with the extent of shocked gas in the host galaxy.
To investigate the star formation efficiency in UGC 05771, we obtained IRAM CO
observations to analyse the molecular gas properties. We found that UGC 05771
sits below the Kennicutt-Schmidt relation, although we were unable to
definitively conclude if direct interactions from the jets are inhibiting star
formation. This result shows that jets may be important in regulating star
formation in the host galaxies of compact radio sources.
