We present a comprehensive multi-wavelength study of the star-forming region NGC 1893 to explore the effects of massive stars on low-mass star formation .
Using near-infrared colours , slitless spectroscopy and narrow-band H \alpha photometry in the cluster region we have identified candidate young stellar objects ( YSOs ) distributed in a pattern from the cluster to one of the nearby nebulae Sim 129 .
The V, ( V - I ) colour-magnitude diagram of the YSOs indicates that majority of these objects have ages between 1 to 5 Myr .
The spread in the ages of the YSOs may indicate a non-coeval star formation in the cluster .
The slope of the KLF for the cluster is estimated to be 0.34 \pm 0.07 , which agrees well with the average value ( \sim 0.4 ) reported for young clusters .
For the entire observed mass range 0.6 < M / M _ { \odot } \leq 17.7 the value of the slope of the initial mass function , ` \Gamma ’ , comes out to be -1.27 \pm 0.08 , which is in agreement with the Salpeter value of -1.35 in the solar neighborhood .
However , the value of ` \Gamma ’ for PMS phase stars ( mass range 0.6 < M / M _ { \odot } \leq 2.0 ) is found to be -0.88 \pm 0.09 which is shallower than the value ( -1.71 \pm 0.20 ) obtained for MS stars having mass range 2.5 < M / M _ { \odot } \leq 17.7 indicating a break in the slope of the mass function at \sim 2 M _ { \odot } .
Estimated ` \Gamma ’ values indicate an effect of mass segregation for main-sequence stars , in the sense that massive stars are preferentially located towards the cluster center .
The estimated dynamical evolution time is found to be greater than the age of the cluster , therefore the observed mass segregation in the cluster may be the imprint of the star formation process .
There is evidence for triggered star formation in the region , which seems to govern initial morphology of the cluster .