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We report on the young massive clump (G35.20w) in W48 that previous molecularline and dust observations have revealed to be in the very early stages of starformation. Based on virial analysis, we find that a strong field of ~1640microG is required to keep the clump in pressure equilibrium. We performed adeep Zeeman effect measurement of the 113 GHz CN (1-0) line towards this clumpwith the IRAM 30 m telescope. We combine simultaneous fitting of all CNhyperfines with Monte Carlo simulations for a large range in realization of themagnetic field to obtain a constraint on the line-of-sight field strength of-687 +/- 420 microG. We also analyze archival dust polarization observationstowards G35.20w. A strong magnetic field is implied by the remarkably orderedfield orientation that is perpendicular to the longest axis of the clump. Basedon this, we also estimate the plane-of-sky component of the magnetic field tobe ~740 microG. This allows for a unique comparison of the two orthogonalmeasurements of magnetic field strength of the same region and at similarspatial scales. The expected total field strength shows no significant conflictbetween the observed field and that required for pressure equilibrium. Byproducing a probability distribution for a large range in field geometries, weshow that plane-of-sky projections are much closer to the true field strengthsthan line-of-sight projections. This can present a significant challenge forZeeman measurements of magnetized structures, even with ALMA. We also show thatCN molecule does not suffer from depletion on the observed scales in thepredominantly cold and highly deuterated core in an early stage of high-massstar formation and is thus a good tracer of the dense gas.

CN Zeeman and dust polarization in a high-mass cold clump