  Due to the recent increase in the availability of photometric time-series
databases, the characterisation of low-mass eclipsing binaries for the study of
their orbital and physical parameters is now possible in large samples and with
good precision. We have identified and photometrically characterised a sample
of 230 detached close-orbiting eclipsing binaries with low-mass main-sequence
components in the Catalina Sky Survey. These low-mass stars have masses of $M
\leq 1.0\ M_{\odot}$ and orbital periods shorter than $2$ days. The adopted
method provided a robust estimate of stellar parameters (as mass and fractional
radius) by using only light curves and photometric colours, since no
spectroscopic information was available for these objects. A SDSS-2MASS
ten-colour grid of composite synthetic and observed colours and the K-Nearest
Neighbours method were employed to identify main-sequence stars and to estimate
their effective temperatures, typically of $T_{\rm eff}\leq 5720$ K. Each light
curve was modelled with the JKTEBOP code together with an asexual genetic
algorithm to obtain the most coherent values for the fitted parameters. The
present work provides an unprecedented number of homogeneous estimates of main
stellar parameters in short-period low-mass binary systems. The distribution of
the components of the investigated detached eclipsing binaries in the
mass-radius diagram supports a trend of radius inflation on low-mass
main-sequence stars. A relative increase of inflation for lower masses is also
found and our results suggest that the secondaries are more inflated, i.e. they
present larger radii than the primary components of same mass, when compared to
stellar evolutionary models.
