Deep V and I CCD photometry of young star cluster NGC 1893 with the 3.6m
  DOT
  Young star clusters consisting of massive stars are the ideal sites to study
the star formation processes and influence of massive stars on the subsequent
star formation. NGC 1893 is a young star cluster associated with the HII region
Sh2-236. It contains about five `O'-type stars and several early `B'-type
stars. It is located at a distance of $\sim$3.25 kpc and has a reddening,
E(B-V)$\sim$0.4 mag. To characterize the young low-mass stellar population in
the central portion of the cluster, we carried out deep VI band observations of
the region using the 4K$\times$4K CCD IMAGER mounted on the 3.6-m DOT. Our
analysis shows that the present data are deep enough to detect stars below
$\sim$24 mag. We found optical counterparts of $\sim$220 candidate members,
including young stars and unclassified cluster members from Caramazza et al.
(2008). We estimated the membership probabilities of the Gaia sources (mostly
bright stars with G$<$19 mag) located within the cluster radius using the Gaia
EDR3. Toward the fainter end, we used the optical color-magnitude diagram (CMD)
to select the cluster members from a sample of young stars. The unclassified
member candidates and X-ray sources from Caramazza et al. (2012) are also found
to be young low-mass stars. In total, we identified $\sim$425 young stars with
age$<$10 Myr, and 110 of these are new. Most of these stars appear kinematic
members of the cluster. By examining the CMD for the stars in the cluster
region, we suggest that the cluster has insignificant contamination due to
field stars in the pre-main sequence zone of the CMD. The slope of the mass
function in the mass range 0.2$\le$M/M$\odot$$\le$2.5 is found to be $\Gamma$ =
-1.43 $\pm$ 0.15, consistent with those of other star-forming complexes. The
spatial distribution of the young stars as a function of mass suggests that
toward the cluster center, most of the stars are massive.
