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tokens: stripped from the progenitor within the last ∼5 Gyr (i.e., are part of the most recent leading debris tail). The model predicts that only the northeastern corner of the HiTS footprint should contain any Sgr debris. The mean distance of these model debris points is , with a spread of σ d ∼ 6 kpc. There are nine HiTS RRLs between 31 d H 49 kpc, of which four are in the region occupied by Sgr model debris (i.e., 170° 7R.A. 175°, −3° decl. 3°). Interestingly, these four stars are tightly clumped in distance, with a mean of and standard deviation of σ d ∼ 0.7 kpc. Nonetheless, given that these four stars are ∼165–20° from the center of the Sgr stream (using the Sgr-aligned coordinate system of Majewski et al. 2003 ), we consider their association with Sgr tentative at best. In conclusion, while there are likely stars from previously identified substructures in our sample of HiTS RRLs, it is unlikely that they have significantly biased our density profile fits, as each of the substructures would contribute only a small number of stars in our field of view. 7. Discussion and Summary We present the detection of 173 RRLs using observations from the 2014 campaign of the HiTS survey. The data cover ∼120 square degrees of the sky and include from 20 to 37 epochs in the g -band. The photometric depth of the HiTS data enables us to build a catalog that includes a significant number of stars that do not appear in previous public surveys overlapping the same sky region (such as the CRTS). Most of the additional RRLs we contribute have , corresponding to d H ≳ 60 kpc. The surveyed region overlaps with the position of currently known satellite galaxies of the Milky Way. We detect 65 RRLs members of the Sextans dSph, 46 of them being new discoveries. This number includes seven stars that were not classified as RRLs by other works, but were already considered as members of the dwarf. Two additional dwarf galaxies, Leo IV and Leo V, were found within our RRLs catalog. A more detailed analysis of the RRLs in Leo V has been presented in a companion paper (Medina et al. 2017 ). Regarding distant RRLs in our sample, we find 18 candidates with d H > 90 kpc, 11 of which are classified as ab -type, while seven are c -type. To understand the connection of this subsample with previously known/unknown systems, the period-amplitudes of the individual stars could play a major role. RRLs that are members of globular clusters are separated in the distincted Oosterhoff groups (Oo I and Oo II; Oosterhoff 1939 ). On the other hand, RRLs in ultra-faint dwarf galaxies are mostly Oo II (Clementini 2014 ), while the halo general population (within a radius of ∼80 kpc) presents stars in both locus, but the majority of them follow the locus of the Oo I group. This has been shown multiple times in the literature (e.g., Zinn et al. 2014 ; Catelan Smith 2015 ), and it is also clearly seen in Figure 4 . The distant sample of RRLs, however, does not follow the main trend of nearby field