  We analyse and compare the clustering of young stars in Chamaeleon I and
Taurus. We compute the mean surface-density of companion stars \bar{N} as a
function of angular displacement \theta from each star. We then fit
\bar{N}(\theta) with two simultaneous power laws. For Chamaeleon I, the
exponents of the power laws are 1.97 and 0.28, with the elbow at ~0.011
degrees. For Taurus, we obtain 2.02 and 0.87, with the elbow at ~0.013 deg. For
both star clusters the observational data make quite large systematic
excursions from the best fitting curve in the binary regime. These excursions
may be attributable to evolutionary effects of the types discussed recently by
Nakajima et al. and Bate et al. In the clustering regime the data conform to
the best fitting curve very well. We also calculate the box-dimensions for the
two star clusters. However, the limited dynamic range makes these estimates
simply descriptors of the large-scale clustering, and not admissible evidence
for fractality. We also propose two algorithms for objectively generating maps
of constant stellar surface-density in young star clusters. Such maps are
useful for comparison with molecular-line and dust-continuum maps of
star-forming clouds, and with the results of numerical simulations. These maps
retain information which is suppressed in the evaluation of \bar{N}(\theta).
Analyzing such maps can be used to discriminate between fractal structure and
single-level clustering, and to determine the degree of central condensation in
small-N clusters. Algorithm I uses a universal smoothing length, and therefore
has a restricted dynamic range, but it is implicitly normalized. Algorithm II
uses a local smoothing length, which gives it much greater dynamic range, but
it has to be normalized explicitly.
