THE NORTHERN WRAPS OF THE SAGITTARIUS STREAM AS TRACED BY RED CLUMP STARS: DISTANCES, INTRINSIC WIDTHS, AND STELLAR DENSITIES

We trace the tidal Stream of the Sagittarius dwarf spheroidal galaxy (Sgr dSph) using Red Clump (RC) stars from the catalog of the Sloan Digital Sky Survey-Data Release 6, in the range 150 degrees less than or similar to R.A. less than or similar to 220 degrees, corresponding to the range of orbital azimuth 220 degrees less than or similar to Lambda less than or similar to 290 degrees. Substructures along the line of sight (los) are identified as significant peaks in the differential star count profiles (SCPs) of candidate RC stars. A proper modeling of the SCPs allows us to obtain (1) <= 10% accurate, purely differential distances with respect to the main body of Sgr, (2) estimates of the FWHM along the los, and (3) estimates of the local density, for each detected substructure. In the range 255 degrees less than or similar to Lambda less than or similar to 290 degrees 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 similar or equal to 43 kpc at Lambda similar or equal to 290 degrees to d similar or equal to 30 kpc at Lambda similar or equal to 255 degrees, and a more nearby coherent series of detections lying at a constant distance d similar or equal to 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 los. For Lambda less than or similar to 255 degrees the detected structures are more complex and less easily interpreted. We are confident of being able to trace the continuation of the leading arm down to Lambda similar or equal to 220 degrees and d similar or equal to 20 kpc; the trailing arm is seen up to Lambda less than or similar to 240 degrees 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.