can produce surface spots, so that in order to maintain its luminosity, an object has to increase in size. This results in the object having a lower surface gravity than it would have without any magnetic activity. An investigation of magnetic activity in field M dwarfs has suggested that activity peaks around M7, with significant activity continuing into later spectral types [@hawley00]. Magnetic activity could be even greater among younger objects. A recent paper has suggested that the temperature reversal observed in 2MASS 0535$-$0546 could be due to magnetic fields inhibiting convection [@mohanty12].

While age spreads could explain the scatter in pEW values, our small sample size and the magnitude of the uncertainties on our data do not allow us to infer age spreads in young clusters. For example, the spread in data values could be due to observational scatter or may arise from differing formation mechanisms and accretion histories (B12). To settle the question of age spreads, we would need a sufficiently large sample of objects in order to undertake a rigorous statistical analysis.

  ---------------------------------- ------------------------ --------- ----------------------- ---------------
                Object                Previous Spectral Type             Revised Spectral Type  
                                                                 WK               QK            
        2MASS 0345$+$25$^{1}$                   L0               $-$              $-$                 $-$
        BRI 0021$-$0214$^{1}$                  M9.5              $-$              $-$                 