The solar dynamo is responsible for the tangled magnetic structure of the Sun. One of the key elements for maintaining the Sun’s dynamo is the Sun’s differential rotation, which is measured using three principal methods: helioseismology, spectroscopy, and tracking the movement of solar structures (the tracer method). Sunspots have the advantage of long-term observations and data records compared to other tracers. Many observatories retain databases with patterns of sunspots on the solar disc, and among those with a long tradition is the Kanzelhöhe Observatory for Solar and Environmental Research (KSO). In this paper, the differential rotation of the Sun is analyzed using Kanzelhöhe drawings of the solar disc for the solar cycle No. 19 (years 1954 - 1964), with a focus on determining the parameters (A, B) of the differential rotation and evaluating the asymmetry in the Sun’s rotation around the equator. The realization of this aim was achieved through a simple procedure consisting of four steps. In the first step, the positions of sunspots and sunspot groups were identified manually. The synodic velocities were calculated from the positions of the sunspot groups using two different methods: the daily shift method (DS method) and the robust least squares method (rLSQ method). The synodic rotation velocity was then converted to the sidereal rotation velocity using a specific correction factor that accounts for the relative motion of theEarth and the Sun at a given moment. At the end, the parameters of differential rotation, A and B, were determined by fitting the expression ω = A + B sin^2 (b) to the sidereal velocity ω depending on the corresponding squares of the sine of the heliographic latitude sin^2(b). The qualitative description of the Sun’s rotation for the solar cycle No. 19 (years 1954 - 1964) is consistent with the standard model of differential rotation. In particular, the angular velocity of the Sun’s rotation decreases from the equator toward the poles, symmetrically in both hemispheres (N and S), with a specific quantitative profile of rotation: ωsid = (14.39 ± 0.02) ◦/dan − (2.70 ± 0.15) sin^2(b) ◦ /dan ωsid = (14.33 ± 0.02) ◦/dan − (2.31 ± 0.12) sin^2(b) ◦ /dan for the rLSQ and DS method, respectively.