The intermediate Helium subdwarf B star LS IV-14 ^ { \circ } 116 is a unique object showing extremely peculiar atmospheric abundances as well as long-period pulsations that can not be explained in terms of the usual opacity mechanism .
One hypothesis invoked was that a strong magnetic field may be responsible .
We discredit this possibility on the basis of FORS2 spectro-polarimetry , which allows us to rule out a mean longitudinal magnetic field down to 300 G .

Using the same data , we derive the atmospheric parameters for LS IV-14 ^ { \circ } 116 to be T _ { eff } = 35,150 \pm 111 K , \log { g } = 5.88 \pm 0.02 and \log { N ( He ) / N ( H ) } = - 0.62 \pm 0.01 .
The high surface gravity in particular is at odds with the theory that LS IV-14 ^ { \circ } 116 has not yet settled onto the Helium Main Sequence , and that the pulsations are excited by an \epsilon mechanism acting on the Helium-burning shells present after the main Helium flash .

Archival UVES spectroscopy reveals LS IV-14 ^ { \circ } 116 to have a radial velocity of 149.1 \pm 2.1 km/s .
Running a full kinematic analysis , we find that it is on a retrograde orbit around the Galactic centre , with a Galactic radial velocity component U =13.23 \pm 8.28 km/s and a Galactic rotational velocity component V = - 55.56 \pm 22.13 km/s .
This implies that LS IV-14 ^ { \circ } 116 belongs to the halo population , an intriguing discovery .