  Signature from Pop III massive stars of $140$--$260\,{\rm M_\odot}$ that end
their lives as pair-instability supernovae (PISNe) are expected to be seen in
very metal-poor (VMP) stars of ${\rm [Fe/H]}\leq -2$. Although thousands of VMP
stars have been discovered, the identification of a VMP star with a PISN
signature has been elusive. Recently, the VMP star LAMOST J1010+2358 was
claimed to be the first star with a clear PISN signature. A subsequent study
showed that ejecta from low-mass core-collapse supernovae (CCSNe) can also fit
the abundance pattern equally well and additional elements such as C and Al are
required to differentiate the two sources. Follow-up observations of LAMOST
J1010+2358 by two independent groups were able to detect both C and Al.
Additionally, key odd elements such as Na and Sc were also detected whose
abundances were found to be higher than the upper limits found in the original
detection. We perform a detailed analysis of the newly observed abundance
patterns by exploring various possible formation channels for VMP stars. We
find that purely low-mass CCSN ejecta as well as the combination of CCSN and
Type 1a SN ejecta can provide an excellent fit to the newly observed abundance
pattern. Our results confirm earlier analysis that the newly observed abundance
pattern is peculiar but has no signatures of PISN.
