We continue our study of rich Galactic clusters by presenting deep CCD observations of both NGC 2168 ( M35 ) and NGC 2323 ( M50 ) .
Both clusters are found to be rich ( NGC 2168 contains at least 1000 stars brighter than V = 22 and NGC 2323 contains \sim 2100 stars brighter than our photometric limit of V \sim 23 ) and young ( age of NGC 2168 = 180 Myrs , age of NGC 2323 = 130 Myrs ) .
The color-magnitude diagrams for the clusters exhibit clear main sequences stretching over 14 magnitudes in the V , B { - } V plane .
Comparing these long main sequences with those of earlier clusters in the survey , as well as with the Hyades , has allowed for accurate distances to be established for each cluster ( d of NGC 2168 = 912 \pm ^ { 70 } _ { 65 } pc , d of NGC 2323 = 1000 \pm ^ { 81 } _ { 75 } pc ) .
Analysis of the luminosity and mass functions suggest that despite their young ages , both clusters are somewhat dynamically relaxed exhibiting signs of mass-segregation .
This is especially interesting in the case of NGC 2323 , which has an age of only 1.3 times the dynamical relaxation time .
The present photometry is also deep enough to detect all of the white dwarfs in both clusters .
We discuss some interesting candidates which may be the remnants of quite massive ( M \geq 5 M _ { \odot } ) progenitor stars .
The white dwarf cooling age of NGC 2168 is found to be in good agreement with the main-sequence turn-off age .
These objects are potentially very important for setting constraints on the white dwarf initial-final mass relationship and upper mass limit for white dwarf production .