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NGC 4473 is a so--called double sigma (2$\sigma$) galaxy, i.e. a galaxy withrare, double peaks in its 2D stellar velocity dispersion. Here, we present theglobular cluster (GC) kinematics in NGC 4473 out to $\sim10\,R_e$ (effectiveradii) using data from combined HST/ACS and Subaru/Suprime--Cam imaging andKeck/DEIMOS spectroscopy. We find that the 2$\sigma$ nature of NGC 4473persists up to 3 $R_e$, though it becomes misaligned to the photometric majoraxis. We also observe a significant offset between the stellar and GC rotationamplitudes. This offset can be understood as a co--addition ofcounter--rotating stars producing little net stellar rotation. We identify asharp radial transition in the GC kinematics at $\sim4\,R_e$ suggesting a welldefined kinematically distinct halo. In the inner region ($<4\,R_e$), the blueGCs rotate along the photometric major axis, but in an opposite direction tothe galaxy stars and red GCs. In the outer region ($>4\,R_e$), the red GCsrotate in an opposite direction compared to the inner region red GCs, along thephotometric major axis, while the blue GCs rotate along an axis intermediatebetween the major and minor photometric axes. We also find a kinematicallydistinct population of very red GCs in the inner region with elevated rotationamplitude and velocity dispersion. The multiple kinematic components in NGC4473 highlight the complex formation and evolutionary history of this 2$\sigma$galaxy, as well as a distinct transition between the inner and outercomponents.

The SLUGGS Survey: Globular cluster kinematics in a "double sigma" galaxy - NGC 4473