Conn, BlairNoel, Noelia E. D.Rix, Hans-WalterLane, R RLewis, Geraint FrancisIrwin, Mike J.Martin, Nicolas FIbata, Rodrigo A.Dolphin, AndrewChapman, Scott2018-11-292018-11-290004-637Xhttp://hdl.handle.net/1885/152178We derive distance, density, and metallicity distribution of the stellar Monoceros Overdensity (MO) in the outer Milky Way, based on deep imaging with the Subaru Telescope. We applied color-magnitude diagram fitting techniques in three stripes at galactic longitudes, l 130°, 150°, 170°, and galactic latitudes, +15° ≤ b ≤ +25°. The MO appears as a wall of stars at a heliocentric distance of 10.1 ± 0.5kpc across the observed longitude range with no distance change. The MO stars are more metal-rich ([Fe/H] -1.0) than the nearby stars at the same latitude. These data are used to test three different models for the origin of the MO: a perturbed disk model, which predicts a significant drop in density adjacent to the MO that is not seen; a basic flared disk model, which can give a good match to the density profile but the MO metallicity implies the disk is too metal-rich to source the MO stars; and a tidal stream model, which, from the literature, brackets the distances and densities we derive for the MO, suggesting that a model can be found that would fully fit the MO data. Further data and modeling will be required to confirm or rule out the MO feature as a stream or as a flaring of the diskapplication/pdf201210.1088/0004-637X/754/2/1012018-11-29