  The first Large-Sized Telescope (LST-1) proposed for the forthcoming
Cherenkov Telescope Array (CTA) has started to operate in 2019 in La Palma. The
large structure of LST-1 - with a 23 m mirror dish diameter - imposes a strict
control of its deformations that could affect the pointing accuracy and its
overall performance. According to CTA specifications that are conceived to
resolve e.g. the fine structure of galactic sources, the LST post-calibration
pointing accuracy should be better than 14 arcseconds. To fulfill this
requirement, the telescope pointing precision is monitored with two dedicated
CCD cameras located at the dish center. The analysis of their images allows us
to disentangle different systematic deformations of the structure. In this
work, we investigate a complementary approach that offers the possibility to
monitor the pointing of the telescope during the acquisition of sky data. After
properly cleaning the events from the Cherenkov showers, the reconstructed
positions of the stars imaged in the camera field of view are compared to their
nominal expected positions in catalogues. This provides a direct measurement of
the telescope pointing, that can be used to cross-check the other methods and
as a real-time monitoring of the optical properties of the telescope and of the
pointing corrections applied by the bending models. Additionally, this method
benefits from not relying on specific hardware or dedicated observations. In
this contribution we will illustrate this analysis and show results based on
simulations of LST-1.
