  The origin of a new kinematically identified metal-poor stellar stream, the
KFR08 stream, has not been established. We present stellar parameters, stellar
ages, and detailed elemental abundances for Na, Mg, Al, Si, Ca, Sc, Ti, Cr, Ni,
Zn, Sr, Y, Zr, Ba, La, and Eu for 16 KFR08 stream members based on analysis of
high resolution spectra. Based on the abundance ratios of 14 elements, we use
the chemical tagging method to identify the stars which have the same chemical
composition, and thus, might have a common birthplace, such as a cluster.
Although three stars were tagged with similar elemental abundances ratios, we
find that, statistically, it is not certain that they originate from a
dissolved star cluster. This conclusion is consistent with the large dispersion
of [Fe/H] ($\sigma_{\rm{[Fe/H]}} = 0.29$) among the 16 stream members. We find
that our stars are $\alpha$ enhanced and that the abundance patterns of the
stream members are well matched to the thick disk. In addition, most of the
stream stars have estimated stellar ages larger than 11 Gyr. These results,
together with the hot kinematics of the stream stars, suggest that the KFR08
stream is originated from the thick disk population which was perturbed by a
massive merger in the early universe.
