We present candidate K-giant members in the Orphan Stream which have been identified from low-resolution data taken with the AAOmega spectrograph on the Anglo-Australian Telescope .
From modest S/N spectra and independent cuts in photometry , kinematics , gravity and metallicity we yield self-consistent , highly probable stream members .
We find a revised stream distance of 22.5 \pm 2.0 kpc near the celestial equator , and our kinematic signature peaks at V _ { GSR } = 82.1 \pm 1.4 km s ^ { -1 } .
The observed velocity dispersion of our most probable members is consistent with arising from the velocity uncertainties alone .
This indicates that at least along this line-of-sight , the Orphan Stream is kinematically cold .
Our data indicates an overall stream metallicity of [ Fe/H ] = -1.63 \pm 0.19 dex which is more metal-rich than previously found and unbiased by spectral type .
Furthermore , the significant metallicity dispersion displayed by our most probable members , \sigma ( \mbox { [ Fe / H ] } ) = 0.56 dex , suggests that the unidentified Orphan Stream parent is a dSph satellite .
We highlight likely members for high-resolution spectroscopic follow-up .