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The Monoceros Ring (also known as the Galactic Anticenter Stellar Structure)and A13 are stellar overdensities at estimated heliocentric distances of $d\sim 11$ kpc and 15 kpc observed at low Galactic latitudes towards theanticenter of our Galaxy. While these overdensities were initially thought tobe remnants of a tidally-disrupted satellite galaxy, an alternate scenario isthat they are composed of stars from the Milky Way (MW) disk kicked out totheir current location due to interactions between a satellite galaxy and thedisk. To test this scenario, we study the stellar populations of the MonocerosRing and A13 by measuring the number of RR Lyrae and M giant stars associatedwith these overdensities. We obtain low-resolution spectroscopy for RR Lyraestars in the two structures and measure radial velocities to compare withpreviously measured velocities for M giant stars in the regions of theMonoceros Ring and A13, to assess the fraction of RR Lyrae to M giant stars($f_{RR:MG}$) in A13 and Mon/GASS. We perform velocity modeling on 153 RR Lyraestars (116 in the Monoceros Ring and 37 in A13) and find that both structureshave very low $f_{RR:MG}$. The results support a scenario in which stars in A13and Mon/GASS formed in the MW disk. We discuss a possible association betweenMon/GASS, A13, and the Triangulum-Andromeda overdensity based on their similarvelocity distributions and $f_{RR:MG}$.

A Disk Origin for the Monoceros Ring and A13 Stellar Overdensities