Mapping the Kinematically Decoupled Core in NGC 1407 with MUSE
  Studies of the kinematics of NGC 1407 have revealed complex kinematical
structure, consisting of the outer galaxy, an embedded disc within a radius of
$\sim60$ arcsec, and a kinematically decoupled core (KDC) with a radius of less
than 30arcsec. However, the size of the KDC and the amplitude of the kinematic
misalignment it induces have not yet been determined. In this paper, we explore
the properties of the KDC using observations from the MUSE Integral Field
Spectrograph to map out the kinematics in the central arcminute of NGC 1407.
Velocity and kinemetry maps of the galaxy reveal a twist of $\sim$148 degree in
the central $10$ arcseconds of the galaxy, and the higher-order moments of the
kinematics reveal that within the same region, this slowly-rotating galaxy
displays no net rotation. Analysis of the stellar populations across the galaxy
found no evidence of younger stellar populations in the region of the KDC,
instead finding uniform age and super-solar $\alpha$-enhancement across the
galaxy, and a smoothly decreasing metallicity gradient with radius. We
therefore conclude that NGC 1407 contains a triaxial, kiloparsec-scale KDC with
distinct kinematics relative to the rest of the galaxy, and which is likely to
have formed through either a major merger or a series of minor mergers early in
the lifetime of the galaxy. With a radius of $\sim$5 arcseconds or $\sim0.6$
kpc, NGC 1407 contains the smallest KDC mapped by MUSE to date in terms of both
its physical and angular size.
