A STUDY OF THE NGC 1193 AND NGC 1798 OPEN CLUSTERS USING CCD UBV PHOTOMETRIC AND GAIA EDR3 DATA

We present photometric, astrometric, and kinematic studies of the old open star clusters NGC 1193 1798. Both are investigated by combining data sets from Gaia EDR3 CCD UBV observational data. Analysis radial distribution stars through cluster regions indicates that limit radii $r_{\rm lim}=8'$ for both clusters. determine membership probabilities considering proper motion trigonometric parallax data, resulting in 361 428 1798 being identified as most likely members, having greater than P>0.5. Mean components estimated ($\mu_{\alpha}\cos \delta$, $\mu_{\delta}) = (-0.207(0.009), -0.431(0.008)$) $\mu_{\delta})=(0.793(0.006), -0.373(0.005)$) mas/yr E(B-V) color excesses were derived $0.150(0.037)$ 0.505(0.100) mag use two-color diagrams. Photometric metallicities also determined diagrams with results [Fe/H] -0.30(0.06) dex [Fe/H]=-0.20(0.07) The isochrone fitting distance age 5562(381) pc 4.6(1) Gyr, respectively. For 1798, these parameters 4451(728) 1.3(0.2) Gyr. These ages indicate overall present-day mass function slopes main-sequence found 1.38(2.16) 1.30(0.21) which fair agreement value Salpeter (1955). Kinematic dynamic orbital calculations belong to thick-disk thin-disk populations, In addition, born outside solar circle, orbit metal-poor region Galactic disk.