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The intermediate Helium subdwarf B star LS IV$-$14$^\circ$116 is a uniqueobject showing extremely peculiar atmospheric abundances as well as long-periodpulsations that cannot be explained in terms of the usual opacity mechanism.One hypothesis invoked was that a strong magnetic field may be responsible. Wediscredit this possibility on the basis of FORS2 spectro-polarimetry, whichallows us to rule out a mean longitudinal magnetic field down to 300 G.  Using the same data, we derive the atmospheric parameters for LSIV$-$14$^\circ$116 to be $T_{\rm eff}$ = 35,150$\pm$111 K, $\log{g}$ =5.88$\pm$0.02 and $\log{N(\rm He)/N(\rm H)}$ = $-$0.62$\pm$0.01. The highsurface gravity in particular is at odds with the theory that LSIV$-$14$^\circ$116 has not yet settled onto the Helium Main Sequence, and thatthe pulsations are excited by an $\epsilon$ mechanism acting on theHelium-burning shells present after the main Helium flash.  Archival UVES spectroscopy reveals LS IV$-$14$^\circ$116 to have a radialvelocity of 149.1$\pm$2.1 km/s. Running a full kinematic analysis, we find thatit is on a retrograde orbit around the Galactic centre, with a Galactic radialvelocity component $U$=13.23$\pm$8.28 km/s and a Galactic rotational velocitycomponent $V$=$-$55.56$\pm$22.13 km/s. This implies that LS IV$-$14$^\circ$116belongs to the halo population, an intriguing discovery.

The enigmatic He-sdB pulsator LS IV$-$14$^\circ$116: new insights from the VLT