The spatial distribution of the evolved stars in Be 64 and Be 69, shown in Figs. 15 (click here) and 16 (click here), manifests that evolved stars have preferential distribution in the outskirts of the clusters. Hawarden (1975) has also found that giant branch clump stars in old open clusters are in general less centrally concentrated than the brightest stars remaining on the upper MS.
Adopting a value of 
, the galactocentric distance
for the clusters has been calculated. The [Fe/H] value has been obtained by
using the relation log Z= 0.977 
from Bertelli et
al. (1994). The various parameters obtained are given in Table 4. The
metallicity of these two clusters is in accordance with the radial gradient obtained
by Friel & Janes (1993) and Carraro & Chiosi (1994).
The z distance of Be 69 (
below the formal galactic
plane) and Be 64 (
above the formal galactic plane)
suggests that Be 69 is situated in the anticenter direction of the thin
disk whereas the cluster Be 64 may be located in the thick disk. The
value of the metallicity for Be 64 (
) is also
close to the average value (
) of the metallicity
for the thick disk population (Sandage & Fouts 1987).
(1) We present photometry for two previously unstudied open clusters.
Overall morphology of the CMDs of both clusters indicates that clusters are of
intermediate age.
(2) The reddening for Be 64 and Be 69 comes out to be 
and 
. From mapping
of interstellar reddening done by Pandey & Mahra (1987), values of
and 
have been obtained towards the Be 64 and Be
69 direction, respectively, which are in good agreement with the values
obtained in the present study.
(3) The estimated metallicity for the clusters (Z = 0.008, 
), and the galactocentric distance of the clusters follow the
radial gradient in metallicity obtained by Friel & Janes (1993) and
Carraro & Chiosi (1994). The location of Be 69 puts the cluster in the
thin disk towards the anticenter direction, whereas the location of Be 64 suggests
that the cluster may be a member of the thick disk.
(4) The evolved stars appear to be concentrated in the outskirts of
the clusters.
Table 1: Details of observation
Table 4: Galactic coordinates and estimated parameters of open clusters
analysed in the paper
Acknowledgements
This work is partly supported by the Department of Science and Technology (India) under the grant SP/S2/O -07/93. Authors are thankful to the referee Dr. G. Carraro for useful comments.
