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We characterize the bulge, disk, and halo subcomponents in the Andromedagalaxy (M31) over the radial range 0.4 < R < 225 kpc. The cospatial nature ofthese subcomponents renders them difficult to disentangle using surfacebrightness (SB) information alone, especially interior to ~20 kpc. Our newdecomposition technique combines information from the luminosity function (LF)of over 1.5 million bright (20 < I < 22) stars from the Panchromatic HubbleAndromeda Treasury (PHAT) survey, radial velocities of over 5000 red giantbranch stars in the same magnitude range from the Spectroscopic and PhotometricLandscape of Andromeda's Stellar Halo (SPLASH) survey, and integrated I-band SBprofiles from various sources. We use an affine-invariant Markov chain MonteCarlo algorithm to fit an appropriate toy model to these three data sets. Thebulge, disk, and halo SB profiles are modeled as a Sersic, exponential, andcored power-law, respectively, and the LFs are modeled as broken power-laws. Wefind that the number of stars with a disk-like LF is ~5% larger than the numberin the dynamically cold component, suggesting that some stars born in the diskhave been dynamically heated to the point that they are kinematicallyindistinguishable from halo members. This is the first kinematical evidence fora "kicked-up disk" population in the stellar halo of M31. The fraction ofkicked-up disk stars is consistent with that found in simulations. See Dormanet al. (2013, submitted) for more information.

A New Approach to Detailed Structural Decomposition: Kicked-up Disk Stars in Andromeda's Halo?