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Aims. We aim to infer information about the magnetic field in the low solarcorona from coronal rain clumps using high-resolution spectropolarimetricobservations in the Ca ii 8542 A line obtained with the Swedish 1-m SolarTelescope. Methods. The weak-field approximation (WFA) provides a simple toolto obtain the line-of-sight component of the magnetic field fromspectropolarimetric observations. We adapted a method developed in a previouspaper in order to assess the different conditions that must be satisfied inorder to properly use the WFA for the data at hand. We also made use ofvelocity measurements in order to estimate the plane-of-the-sky magnetic fieldcomponent, so that the magnetic field vector could be inferred. Results. Wehave inferred the magnetic field vector from a data set totalling 100 spectralscans in the Ca ii 8542 A line, containing an off-limb view of the lowerportion of catastrophically cooled coronal loops in an active region. Ourresults, albeit limited by the cadence and signal-to-noise ratio of the data,suggest that magnetic field strengths of hundreds of Gauss, even reaching up to1000 G, are omnipresent at coronal heights below 9 Mm from the visible limb.Our results are also compatible with the presence of larger magnetic fieldvalues such as those reported by previous works. However, for large magneticfields, the Doppler width from coronal rain is not that much larger than theZeeman width, thwarting the application of the WFA. Furthermore, we havedetermined the temperature, T , and microturbulent velocity, $\xi$, of coronalrain clumps and off-limb spicules present in the same data set, and we havefound that the former ones have narrower T and $\xi$ distributions, theiraverage temperature is similar, and coronal rain has microturbulent velocitiessmaller than those of spicules

Magnetic field inference in active region coronal loops using coronal rain clumps