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Spectropolarimetry using IR wavelength of 1075 nm has been provedto be a powerful tool for directly mapping solar coronal magneticfields including transverse component directions and line-of-sightcomponent intensities. Solar tomography, or stereoscopy based on EUVobservations, can supply 3-D information for some magnetic fieldlines in bright EUV loops. In a previous paper citep{liu08} thelocations of the IR emission sources in the 3-D coordinate systemwere inferred from the comparison between the polarization data andthe potential-field-source-surface (PFSS) model, for one of fivewest limb regions in the corona (Lin et al., 2004). The paper shows thatthe region with the loop system in the active region over thephotospheric area with strong magnetic field intensity is the regionwith a dominant contribution to the observed Stokes signals. So, theinversion of the measured Stokes parameters could be done assumingthat most of the signals come from a relatively thin layer over thearea with a large photospheric magnetic field strength. Here, thefive limb coronal regions are studied together in order to study thespatial correlation between the bright EUV loop features and theinferred IR emission sources. It is found that, for the coronalregions above the stronger photospheric magnetic fields, thelocations of the IR emission sources are closer to or moreconsistent with the bright EUV loop locations than those aboveweaker photospheric fields. This result suggests that the structuresof the coronal magnetic fields observed at IR and EUV wavelengthsmay be different when weak magnetic fields present there

Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations