  We present an analysis of the galaxy merger rate in the redshift range
$4.0<z<9.0$ (i.e. about 1.5 to 0.5 Gyr after the Big Bang) based on visually
identified galaxy mergers from morphological parameter analysis. Our dataset is
based on high-resolution NIRCam JWST data (F150W and F2000W broad-band filters)
in the low-to-moderate magnification ($\mu<2$) regions of the Abell 2744
cluster field. From a parent set of 675 galaxies $(M_{UV}\in[-26.6,-17.9])$, we
identify 64 merger candidates from the Gini, $M_{20}$ and Asymmetry
morphological parameters, leading to a merger fraction $f_m=0.11\pm0.04$. There
is no evidence of redshift evolution of $f_m$ even at the highest redshift
considered, thus extending well into the epoch of reionization the constant
trend seen previously at $z\lesssim 6$. Furthermore, we investigate any
potential redshift dependent differences in the specific star formation rates
between mergers and non-mergers. Our analysis reveals no significant
correlation in this regard, with deviations in the studied redshift range
typically falling within $0.25$ dex (logarithmic scale) that can be attributed
to sample variance and measurement errors. Finally, we also demonstrate that
the classification of a merging system is robust with respect to the observed
(and equivalently rest-frame) wavelength of the high-quality JWST broad-band
images used. This preliminary study highlights the potential for progress in
quantifying galaxy assembly through mergers during the epoch of reionization,
with significant sample size growth expected from upcoming large JWST infrared
imaging datasets.
