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Aims. We use high-resolution spectropolarimetric observations in the Ca ii8542 A line obtained with the SST to study the magnetic field in solarspicules. Methods. The equations that result from the application of the WeakField Approximation (WFA) to the radiative transfer equations are used to inferthe LOS component of the magnetic field (BLOS). Two restrictive conditions areimposed on the Stokes I and V profiles at each pixel before they can be used ina Bayesian inversion to compute its BLOS. Results. The LOS magnetic fieldcomponent has been inferred in six data sets totalling 448 spectral scans inthe Ca ii 8542 A line and containing both active region and quiet Sun areas,with values of hundreds of G being abundantly inferred. There seems to be nodifference, from the statistical point of view, between the magnetic fieldstrength of spicules in the quiet Sun or near an active region. On the otherhand, the BLOS distributions present smaller values on the disk than off-limb,a fact that can be explained by the effect of superposition on the chromosphereof on-disk structures. We find that spicules in the vicinity of a sunspot havea magnetic field polarity (i.e. north or south) equal to that of the sunspot.This paper also contains an analysis of the effect of off-limb overlappingstructures on the observed Stokes I and V parameters and the BLOS obtained fromthe WFA. It is found that this value is equal to or smaller than the largestLOS magnetic field components of the two structures. In addition, using randomBLOS, Doppler velocities and line intensities of these two structures leads in~ 50% of the cases to Stokes I and V parameters unsuitable to be used with theWFA. Conclusions. Our results present a scarcity of LOS magnetic fieldcomponents smaller than some 50 G, which must not be taken as evidence againstthe existence of these magnetic field strengths in spicules.

Ubiquitous hundred-Gauss magnetic fields in solar spicules