  We have searched for lines of the radioactive element technetium (Tc) in the
spectrum of Przybylski's star (HD101065). The nuclei of this chemical element
are formed in the slow process of capturing thermalized neutrons. The possible
lines of Tc~I are heavily blended. We have synthesized the profile of one
resonance line at 4297.06 \AA~, which is also a part of the complex blend, and
we arrived at a decision that it is not visible in the spectrum (as was first
noted by Ryabchikova), casting doubt on the existence of technetium in the
atmosphere of the Przybylski's star. Therefore, based on our calculated
combined profile, which has been adjusted to the observed blend profile at
~4297.2 A (that may possibly contain the resonance technetium line 4297.06 A),
we reduce the maximum technetium abundance to $\log\epsilon$(Tc/H) = 2.5. This
value can be considered only as an upper limit of the technetium abundance in
the Przybylski's star.
