A significant asymmetry in the distribution of faint blue stars in the inner Galaxy , Quadrant 1 ( l = 20 \arcdeg - 45 \arcdeg ) compared to Quadrant 4 was first reported by ( 21 ) .
Parker et al ( 2003 , 2004 ) greatly expanded the survey to determine its spatial extent and shape and the kinematics of the affected stars .
This excess in the star counts was subsequently confirmed by ( 18 ) using SDSS data .
Possible explanations for the asymmetry include a merger remnant , a triaxial Thick Disk , and a possible interaction with the bar in the Disk .
In this paper we describe our program of wide field photometry to map the asymmetry to fainter magnitudes and therefore larger distances .
To search for the signature of triaxiality , we extended our survey to higher Galactic longitudes .
We find no evidence for an excess of faint blue stars at l \geq 55 \arcdeg including the faintest magnitude interval .
The asymmetry and star count excess in Quadrant 1 is thus not due to a triaxial Thick Disk .