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The properties of a stellar grouping that is ~ 3.5 kpc to the north east ofthe center of M31 is examined. This structure has (1) a surface brightness thatis lower than the surrounding disk, (2) a more-or-less round appearance, (3) asize of ~ 300 arcsec (~ 1 kpc), and (4) an integrated brightness M_K = 6.5. Itis populated by stars with ages > 100 Myr and J-K colors that tend to be bluerthan those of stars in the surrounding disk. Comparisons with model luminosityfunctions suggest that the star formation rate in this object has changed twicein the past few hundred Myr. Fitting a Sersic function to the light profilereveals a power-law index and effective surface brightness that are similar tothose of dwarf galaxies with the same integrated brightness. Two possibleorigins for this object are considered: (1) it is a heretofore undiscoveredsatellite of M31 that is seen against/in/through the M31 disk, or (2) it is afossil star-forming region in the M31 disk.

A Large Group of Asymptotic Giant Branch Stars in the Disk of M31: A Missing Piece of the Puzzle?