  It is well known that small-scale magnetism dominates the surface magnetic
field topologies of active late-type stars. However, little information is
available on the spatial distribution of this key magnetic field component.
Here, we take advantage of the recently developed magnetic field diagnostic
procedure relying on the magnetic intensification of iron atomic lines in the
optical. We extend this methodology from measuring a single average field
strength value to simultaneous Doppler imaging reconstruction of the
two-dimensional maps of temperature and magnetic field strength. We applied
this novel surface mapping approach to two spectroscopic data sets of the young
active Sun-like star LQ Hya. For both epochs, we found a fairly uniform field
strength distribution, apart from a latitudinal trend of the field strength
increasing from 1.5-2.0 kG at low latitudes to 3.0-3.5 kG, close to the
rotational poles. This distribution of the small-scale field does not display a
clear correlation with the locations of temperature spots or the global
magnetic field structure reconstructed for the same epochs.
