We present the results of a wide-field camera survey of the stars in the Monoceros Ring , thought to be an additional structure in the Milky Way of unknown origin .
Lying roughly in the plane of the Milky Way , this may represent a unique equatorial accretion event which is contributing to the Thick Disk of the Galaxy .
Alternatively , the Monoceros Ring may be a natural part of the Disk formation process .
With ten pointings in symmetric pairs above and below the plane of the Galaxy , this survey spans 90 degrees about the Milky Way ’ s equator .
Signatures of the stream of stars were detected in three fields , ( l , b ) = ( 118 , +16 ) ^ { \circ } and ( 150 , +15 ) ^ { \circ } plus a more tentative detection at ( 150 , -15 ) ^ { \circ } .
Galactocentric distance estimates to these structures gave \sim 17 , \sim 17 , and \sim 13 kpc respectively .
The Monoceros Ring seems to be present on both sides of the Galactic plane , in a form different to that of the Galactic warp , suggestive of a tidal origin with streams multiply wrapping the Galaxy .
A new model of the stream has shown a strong coincidence with our results and has also provided the opportunity to make several more detections in fields in which the stream is less significant .
The confirmed detection at ( l , b ) = ( 123 , -19 ) ^ { \circ } at \sim 14 , kpc from the Galactic centre allows a re-examination revealing a tentative new detection with a Galactocentric distance of \sim 21 kpc .
These detections also lie very close to the newly discovered structure in Triangulum-Andromedae hinting of a link between the two .
The remaining six fields are apparently non-detections although in light of these new models , closer inspection reveals tentative structure .
With the overdensity of M-giant stars in Canis Major being claimed both as a progenitor to the Monoceros Ring and alternatively a manifestation of the Milky Way warp , much is still unknown about this structure and its connection to the Monoceros Ring .
Further constraints are needed for the numerical simulations to adequately resolve the increasingly complex view of this structure .