We trace the tidal Stream of the Sagittarius dwarf spheroidal galaxy ( Sgr dSph ) using Red Clump stars from the catalog of the Sloan Digital Sky Survey - Data Release 6 , in the range 150 \arcdeg \lesssim RA \lesssim 220 \arcdeg , corresponding to the range of orbital azimuth 220 \arcdeg \lesssim \Lambda \lesssim 290 \arcdeg .
Substructures along the line of sight are identified as significant peaks in the differential star count profiles ( SCP ) of candidate Red Clump stars .
A proper modeling of the SCPs allows us to obtain : ( a ) \leq 10 % accurate , purely differential distances with respect to the main body of Sgr , ( b ) estimates of the FWHM along the line of sight , and ( c ) estimates of the local density , for each detected substructure .
In the range 255 \arcdeg \lesssim \Lambda \lesssim 290 \arcdeg we cleanly and continuously trace various coherent structures that can be ascribed to the Stream , in particular : the well known northern portion of the leading arm , running from d \simeq 43 kpc at \Lambda \simeq 290 \arcdeg to d \simeq 30 kpc at \Lambda \simeq 255 \arcdeg , and a more nearby coherent series of detections lying at constant distance d \simeq 25 kpc , that can be identified with a wrap of the trailing arm .
The latter structure , predicted by several models of the disruption of Sgr dSph , was never traced before ; comparison with existing models indicates that the difference in distance between these portions of the leading and trailing arms may provide a powerful tool to discriminate between theoretical models assuming different shapes of the Galactic potential .
A further , more distant wrap in the same portion of the sky is detected only along a couple of lines of sight .
For \Lambda \lesssim 255 \arcdeg the detected structures are more complex and less easily interpreted .
We are confident to be able to trace the continuation of the leading arm down to \Lambda \simeq 220 \arcdeg and d \simeq 20 kpc ; the trailing arm is seen up to \Lambda \simeq 240 \arcdeg where it is replaced by more distant structures .
Possible detections of more nearby wraps and of the Virgo Stellar Stream are also discussed .
These measured properties provide a coherent set of observational constraints for the next generation of theoretical models of the disruption of Sgr .