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