Andromeda chained to the Box -- Dynamical Models for M31: Bulge & Bar
  Andromeda is our nearest neighbouring disk galaxy and a prime target for
detailed modelling of the evolutionary processes that shape galaxies. We
analyse the nature of M31's triaxial bulge with an extensive set of N-body
models, which include Box/Peanut (B/P) bulges as well as initial classical
bulges (ICBs). Comparing with IRAC 3.6$\mu m$ data, only one model matches
simultaneously all the morphological properties of M31's bulge, and requires an
ICB and a B/P bulge with 1/3 and 2/3 of the total bulge mass respectively. We
find that our pure B/P bulge models do not show concentrations high enough to
match the S\'ersic index ($n$) and the effective radius of M31's bulge.
Instead, the best model requires an ICB component with mass $M^{\rm
ICB}=1.1\times10^{10}{\rm M_{\odot}}$ and three-dimensional half-mass radius
$r_{\rm half}^{\rm ICB}$=0.53 kpc (140 arcsec). The B/P bulge component has a
mass of $M^{\rm B/P}=2.2\times10^{10}{\rm M_{\odot}}$ and a half-mass radius of
$r_{\rm half}^{\rm B/P}$=1.3 kpc (340 arcsec). The model's B/P bulge extends to
$r^{\rm B/P}$=3.2 kpc (840 arcsec) in the plane of the disk, as does M31's
bulge. In this composite bulge model, the ICB component explains the velocity
dispersion drop observed in the centre within $R<$190 pc (50 arcsec), while the
B/P bulge component reproduces the observed rapid rotation and the kinematic
twist of the observed zero velocity line. This model's pattern speed is
$\Omega_p$=38 km/s/kpc, placing corotation at $r_{\rm cor}$=5.8 kpc (1500
arcsec). The outer Lindblad resonance (OLR) is then at $r_{\rm OLR}$=10.4kpc,
near the 10kpc-ring of M31, suggesting that this structure may be related to
the bar's OLR. By comparison with an earlier snapshot, we estimate that M31's
thin bar extends to $r_{\rm bar}^{\rm thin}\sim$4.0 kpc (1000 arcsec) in the
disk plane, and in projection extends to $R_{\rm bar}^{\rm thin}\sim$2.3 kpc
(600 arcsec).
