We identify new structures in the halo of the Milky Way Galaxy from positions , colors and magnitudes of five million stars detected in the Sloan Digital Sky Survey .
Most of these stars are within 1.26 ^ { \circ } of the celestial equator .
We present color-magnitude diagrams ( CMDs ) for stars in two previously discovered , tidally disrupted structures .
The CMDs and turnoff colors are consistent with those of the Sagittarius dwarf galaxy , as had been predicted .
In one direction , we are even able to detect a clump of red stars , similar to that of the Sagittarius dwarf , from stars spread across 110 square degrees of sky .
Focusing on stars with the colors of F turnoff objects , we identify at least five additional overdensities of stars .

Four of these may be pieces of the same halo structure , which would cover a region of the sky at least 40 ^ { \circ } in diameter , at a distance of 11 kpc from the Sun ( 18 kpc from the center of the Galaxy ) .
The turnoff is significantly bluer than that of thick disk stars , and closer to the Galactic plane than a power-law spheroid .
We suggest two models to explain this new structure .
One possibility is that this new structure could be a new dwarf satellite of the Milky Way , hidden in the Galactic plane , and in the process of being tidally disrupted .
The other possibility is that it could be part of a disk-like distribution of stars which is metal-poor , with a scale height of approximately 2 kpc and a scale length of approximately 10 kpc .

The fifth overdensity , which is 20 kpc away , is some distance from the Sagittarius dwarf streamer orbit and is not associated with any known structure in the Galactic plane .
We have tentatively identified a sixth overdensity in the halo .
If this sixth structure is instead part of a smooth distribution of halo stars ( the spheroid ) , then the spheroid must be very flattened , with axial ratio q = 0.5 .
It is likely that there are many smaller streams of stars in the Galactic halo .