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We present the characterization of 5 new short-period low-mass eclipsingbinaries from the WFCAM Transit Survey. The analysis was performed by using thephotometric WFCAM J-mag data and additional low- and intermediate-resolutionspectroscopic data to obtain both orbital and physical properties of thestudied sample. The light curves and the measured radial velocity curves weremodeled simultaneously with the JKTEBOP code, with Markov chain Monte Carlosimulations for the error estimates. The best-model fit have revealed that theinvestigated detached binaries are in very close orbits, with orbitalseparations of $2.9 \leq a \leq 6.7$ $R_{\odot}$ and short periods of $0.59\leq P_{\rm orb} \leq 1.72$ d, approximately. We have derived stellar massesbetween $0.24$ and $0.72$ $M_{\odot}$ and radii ranging from $0.42$ to $0.67$$R_{\odot}$. The great majority of the LMEBs in our sample has an estimatedradius far from the predicted values according to evolutionary models. Thecomponents with derived masses of $M < 0.6$ $M_{\odot}$ present a radiusinflation of $\sim$$9\%$ or more. This general behavior follows the trend ofinflation for partially-radiative stars proposed previously. These systems addto the increasing sample of low-mass stellar radii that are not well-reproducedby stellar models. They further highlight the need to understand the magneticactivity and physical state of small stars. Missions like TESS will providemany such systems to perform high-precision radius measurements to tightlyconstrain low-mass stellar evolution models.

Low-mass eclipsing binaries in the WFCAM Transit Survey: the persistence of the M-dwarf radius inflation problem