We present a comprehensive analysis ( photometric and kinematical ) of poorly studied open cluster NGC 4337 using 2MASS , WISE , APASS , and Gaia DR2 database .
By determining the membership probabilities of stars , we identified 624 most probable members with membership probability higher than 50 \% by using proper motion and parallax data taken from Gaia DR2 .
The mean proper motion of the cluster is obtained as \mu _ { x } = -8.83 \pm 0.01 and \mu _ { y } = 1.49 \pm 0.006 mas yr ^ { -1 } .
We find the normal interstellar extinction towards the cluster region .
The radial distribution of members provides a cluster radius of 7.75 arcmin ( 5.63 pc ) .
The estimated age of 1600 \pm 180 Myr indicates that NGC 4337 is an old open cluster with a bunch of red giant stars .
The overall mass function slope for main-sequence stars is found as 1.46 \pm 0.18 within the mass range 0.75 - 2.0 M _ { \odot } , which is in fair agreement with Salpeter ’ s value ( x=1.35 ) within uncertainty .
The present study demonstrates that NGC 4337 is a dynamically relaxed open cluster .
Using the Galactic potential model , Galactic orbits are obtained for NGC 4337 .
We found that this object follows a circular path around the Galactic center .
Under the kinematical analysis , we compute the apex coordinates ( A,D ) by using two methods : ( i ) the classical convergent point method and ( ii ) the AD-diagram method .
The obtained coordinates are : ( A _ { conv } ,D _ { conv } ) = ( 96 ^ { \textrm { o } } .27 \pm 0 ^ { \textrm { o } } .10 , 13 ^ { \textrm { o } } .14 \pm 0 ^ { \textrm { o } } .27 ) \& ( A _ { \circ } ,D _ { \circ } ) = ( 100 ^ { \textrm { o } } .282 \pm 0 ^ { \textrm { o } } .10 , 9 ^ { \textrm { o } } .577 \pm 0 ^ { \textrm { o } } .323 ) respectively .
We also computed the Velocity Ellipsoid Parameters ( VEPs ) , matrix elements ( \mu _ { ij } ) , direction cosines ( l _ { j } , m _ { j } , n _ { j } ) and the Galactic longitude of the vertex ( l _ { 2 } ) .