We measure the spatial density of F turnoff stars in the Sagittarius dwarf tidal stream , from Sloan Digital Sky Survey ( SDSS ) data , using statistical photometric parallax .
We find a set of continuous , consistent parameters that describe the leading Sgr stream ’ s position , direction , and width for 15 stripes in the North Galactic Cap , and 3 stripes in the South Galactic Cap .
We produce a catalog of stars that has the density characteristics of the dominant leading Sgr tidal stream that can be compared with simulations .
We find that the width of the leading ( North ) tidal tail is consistent with recent triaxial and axisymmetric halo model simulations .
The density along the stream is roughly consistent common disruption models in the North , but possibly not in the South .
We explore the possibility that one or more of the dominant Sgr streams has been mis-identified , and that one or more of the ‘ bifurcated ’ pieces is the real Sgr tidal tail , but we do not reach definite conclusions .
If two dwarf progenitors are assumed , fits to the planes of the dominant and ‘ bifurcated ’ tidal tails favor an association of the Sgr dwarf spheroidal galaxy with the dominant Southern stream and the ‘ bifurcated ’ stream in the North .
In the North Galactic Cap , the best fit Hernquist density profile for the smooth component of the stellar halo is oblate , with a flattening parameter q = 0.53 , and a scale length of r _ { 0 } = 6.73 .
The Southern data for both the tidal debris and the smooth component of the stellar halo do not match the model fits to the North , although the stellar halo is still overwhelmingly oblate .
Finally , we verify that we can reproduce the parameter fits on the asynchronous Milkyway @ home volunteer computing platform .