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We analyze the kinematics of Andromeda's disk as a function of stellar age byusing photometry from the Panchromatic Hubble Andromeda Treasury (PHAT) surveyand spectroscopy from the Spectroscopic and Photometric Landscape ofAndromeda's Stellar Halo (SPLASH) survey. We use HI 21-cm and CO ($\rm J=1\rightarrow 0$) data to examine the difference between the deprojected rotationvelocity of the gas and that of the stars. We divide the stars into fourstellar age bins, from shortest lived to longest lived: massive main sequencestars (0.03 Gyr), more luminous intermediate mass asymptotic giant branch (AGB)stars (0.4 Gyr), less luminous intermediate mass AGB stars (2 Gyr), and lowmass red giant branch stars (4 Gyr). There is a clear correlation between theoffset of the stellar and the gas rotation velocity, or the asymmetric drift:the longer lived populations lag farther behind the gas than short livedpopulations. We also examine possible causes of the substructure in therotation curves and find that the most significant cause of scatter in therotation curves comes from the tilted ring model being an imperfect way toaccount for the multiple warps in Andromeda's disk.

Asymmetric Drift in the Andromeda Galaxy (M31) as a Function of Stellar Age