-The results of the complex study of galactic open cluster Trumpler 2 are presented.The positions of approximately 3000 stars up to the limit magnitude B \sim 16.25 mag in the area 80 \arcmin \times 80 \arcmin around the cluster were measured in order to obtain the proper motions .
Measurements of star positions on 6 plates with the maximal epoch difference of 63 years were taken by means of the automated measuring complex ” Fantasy ” .
The root-mean error of the relative proper motions is 4.2 mas yr ^ { -1 } .
The catalogue of BV magnitudes of all the stars in the investigated area was compiled .
Astrometric selection of the cluster members within the region of R < 16 \arcmin from the center of the cluster was made by means of the W.Sanders method ( 1971 ) .
In that field 192 stars were found to have the individual membership probability greater then 85 \% , 148 of them are situated within the \pm 3 \sigma _ { B - V } band around the main sequence ( MS ) of the cluster .
They are considered to be cluster members by two criteria .
The U-B \sim B-V diagram plotted for the astrometrical cluster members by the data taken from the Washington catalogue of the UBV photometry in the galactic cluster fields ( Hoag et al .
1961 ) has made it possible to redefine the value of the color excess E ( B-V ) = 0. ^ { m } 40 instead of previously published values ranged from 0 . ^ { m } 30 to 0 . ^ { m } 34 .
The superposition of the MS of the cluster with the ZAMS Schmidt-Kaler ( 1965 ) for thus accepted E ( B-V ) leads to the coincidence at the value of the apparent distance module ( V - M _ { V } ) = 10.50 which corresponds to the distance r = 725 pc .
The luminosity and mass functions of the Trumpler 2 were constructed and the value of the slope ( \Gamma = - 1.90 \pm 0.22 ) was determined .
The cluster age of 8.913 \times 10 ^ { 7 } yr was determined on the base of Girardi et al .
( 2000 ) isochrone grid .
Correspondent to this age the turn-off point of the MS is ( B-V ) _ { 0 } = -0. ^ { m } 16 .
It is shown that the red giant on the late stage of the evolution ( st N.1095 ) belongs to cluster and indicated the brightness variability .
The possibility that the number of both known and recently discovered variables are cluster members was considered .
The catalogues of the proper motions and of the photometry of stars are appended . Tables 2,3,3A,5 will be only available in electronic form at the CDS