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tokens: in Figure 2 . The black solid curves in panel (a) are the same isochrones as used in Figure 2 , but for a distance of 29 kpc. For the Sgr Stream, solid blue lines are used in panel (a) instead of dashed blue lines to represent the Sgr bright arm, and the distance of 23 kpc was adopted for these isochrones. In panel (b), we also show the Law Majewski ( 2010 ) N -body model particles in right- (leading) or left-facing (trailing) triangles. These particles are color coded following Law Majewski ( 2010 ), such that different colors represent the time at which a given debris particle became unbound from the Sgr dSph: magenta for 1.5–3 Gyr ago; and cyan for 3–5 Gyr ago. The gray cross is the same as in Figure 2 . An expectation value of 3 MW halo stars is predicted within the area spanned by the gray cross. The ORPH-F2 field is located on the main Sgr Stream (or the bright arm) at Λ ⊙ = 2264, and we expect Sgr Stream stars to be present in this field. We have overlaid the same age+metallicity isochrones used in the ORPH-F1 field for identifying Sgr stream stars, but at a distance of 22 kpc based on Figure 4 of Belokurov et al. ( 2014 ). Among the stars consistent with these isochrones, seven are easily identified as a conspicuous clump in the PM diagram. These are plotted in blue circles in Figure 4 . For comparison, we also plot the Law Majewski ( 2010 ) N -body model particles that are within 15 in both right ascension and declination from the center of our HST field. The observed PM clump is very close to the model particles as expected, and similar to the findings for Sgr FIELD 4 in Sohn et al. ( 2015 ) at Λ ⊙ = 2511. Beyond these, no other significant excess has been found in the PM diagram. 3.3. ORPH-F3 Figure 5 shows the CMD and PM diagram for the ORPH-F3 field. If present, Orphan Stream stars should be at a distance of 24 kpc. We used the fiducial isochrones to identify Orphan Stream stars, and found four stars consistent with the isochrones within their photometric errors. However, all of these stars are far away from the PM prediction of Newberg et al. ( 2010 ). There is only one star (22) that is close enough to the model prediction to be considered a member of the Orphan Stream, but its color ( F 606 W − F 775 W ≃ 0.8) is too red for its brightness to be considered an Orphan Stream star. We conclude that there is no star associated with the Orphan Stream in this field. Given that this field is about 12 away in the orthogonal direction from the densest part of the Orphan Stream, and given that the Orphan Stream is a thin stellar stream, it is unsurprising to find no star in a small HST ACS field. Figure 5. Selection of stars associated with stellar streams in the ORPH-F3 field. The panels and symbols are similar to those in Figure 2 . The black solid curves in panel (a) are the same isochrones as used in Figure 2 , but for a distance of 24 kpc. The dashed green curve is a fiducial isochrone for a population with an age of 12 Gyr and a