  We present the first high-resolution spectroscopic study on the Orphan Stream
for five stream candidates, observed with the Magellan Inamori Kyocera Echelle
(MIKE) spectrograph on the Magellan Clay telescope. The targets were selected
from the low-resolution catalog of Casey et al (2013a): 3 high-probability
members, 1 medium and 1 low-probability stream candidate were observed. Our
analysis indicates the low and medium-probability target are metal-rich field
stars. The remaining three high-probability targets range over $\sim$1 dex in
metallicity, and are chemically distinct compared to the other 2 targets and
all standard stars: low [$\alpha$/Fe] abundance ratios are observed, and lower
limits are ascertained for [Ba/Y], which sit well above the Milky Way trend.
These chemical signatures demonstrate that the undiscovered parent system is
unequivocally a dwarf spheroidal galaxy, consistent with dynamical constraints
inferred from the stream width and arc. As such, we firmly exclude the proposed
association between NGC 2419 and the Orphan stream. A wide range in
metallicities adds to the similarities between the Orphan stream and Segue 1,
although low [$\alpha$/Fe] abundance ratios in the Orphan stream are in tension
with high [$\alpha$/Fe] values observed in Segue 1. Open questions remain
before Segue 1 could possibly be claimed as the `parent' of the Orphan stream.
The parent system could well remain undiscovered in the southern sky.
