  Some of the accreting X-ray pulsars are reported to exhibit a peculiar
spectral feature at $\sim$10 keV, known as the "10 keV feature". The feature
has been characterized as either an emission line or an absorption line, and
its origin is unknown. It has been found in multiple observations of the same
source by different observatories, but not all the observations of any
particular source consistently showed the presence of it. In this work, we have
carried out a systematic investigation for the presence of the "10 keV feature"
using data from NuSTAR, a low background spectroscopic observatory having
uninterrupted wide band coverage on either side of 10 keV. We performed a
systematic spectral analysis on 58 archival NuSTAR observations of 30 bright
X-ray pulsars. The 3$-$79 keV spectral continua of these selected sources were
fitted with a model chosen on the basis of its fitting quality in 3$-$15 keV
and model simplicity, and then inspected for the presence of the "10 keV
feature". Our analysis indicates the presence of such a feature in 16 out of 58
the NuSTAR observations of 11 different sources and is fitted with a Gaussian
absorption model centered around 10 keV. Our analysis also suggests that such a
feature could be wrongly detected if flare data is not analyzed separately from
persistent emission.
