  By studying young magnetically active late-type stars, i.e. analogues to the
young Sun, one can draw conclusions on the evolution of the solar dynamo. We
determine the topology of the surface magnetic field and study the relation
between the magnetic field and cool photospheric spots in three young late-type
stars. High-resolution spectropolarimetry of the targets were obtained with the
HARPSpol instrument mounted at the ESO 3.6 m telescope. The signal-to-noise
ratio of the Stokes IV measurements were boosted by combining the signal from a
large number of spectroscopic absorption lines through the least squares
deconvolution technique. Surface brightness and magnetic field maps were
calculated using the Zeeman-Doppler imaging technique. All the three targets
show clear signs of both magnetic fields and cool spots. Only one of the
targets, namely V1358 Ori, shows evidence of the dominance of non-axisymmetric
modes. In two of the targets, the poloidal field is significantly stronger than
the toroidal one, indicative of an $\alpha^2$-type of a dynamo, in which
convective turbulence effects dominate over the weak differential rotation. In
two of the cases there is a slight anti-correlation between the cool spots and
the strength of the radial magnetic field. However, even in these cases the
correlation is much weaker than in the case of sunspots. The weak correlation
between the measured radial magnetic field and cool spots may indicate a more
complex magnetic field structure in the spots or spot groups involving mixed
magnetic polarities. Comparison with a previously published magnetic field map
shows that on one of the stars, HD 29615, the underlying magnetic field has
changed its polarity between 2009 and 2013.
