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Faraday Rotation Measures (RM) should be interpreted with caution becausethere could be multiple magneto-ionized medium components that contribute tothe net Faraday rotation along sight-lines. We introduce a simple test usingGalactic diffuse polarised emission that evaluates whether structures evidentin RM observations are associated with distant circumgalactic medium (CGM) orforeground interstellar medium (ISM). We focus on the Magellanic Leading Armregion where a clear excess of RM was previously reported. There are twogaseous objects standing out in this direction: the distant Magellanic LeadingArm and the nearby Antlia supernova remnant (SNR). We recognized narrowdepolarised filaments in the $2.3\,\rm GHz$ S-band Polarization All Sky Survey(S-PASS) image that overlaps with the reported RM excess. We suggest that thereis a steep gradient in Faraday rotation in a foreground screen arising from theAntlia SNR. The estimated strength of the line-of-sight component of themagnetic field is $B_{\parallel}\sim 5\,\rm\mu G$, assuming that the excess ofRM is entirely an outcome of the magnetized supernova shell. Our analysisindicates that the overlap between the RM excess and the Magellanic Leading Armis only a remarkable coincidence. We suggest for future RM grid studies thatchecking Galactic diffuse polarisation maps is a convenient way to identifylocal Faraday screens.

Distant probes of RM structure -- Where is the Faraday Rotation towards the Magellanic Leading Arm?