  This article presents the first direct "observation" of the global-scale, 3D
coronal magnetic fields of Carrington Rotation (CR) Cycle 2112 using vector
tomographic inversion techniques. The Vector tomographic inversion uses
observational measurements of the Fe {\sc{xiii}} 10747 \AA\ Hanle effect
polarization signals by the Coronal Multichannel Polarimeter (CoMP) and coronal
density and temperature structures derived from scalar tomographic inversion of
STEREO/EUVI coronal emission lines (CELs) intensity images as inputs to derive
a coronal magnetic field model that best reproduces the observed polarization
signals. While independent verifications of the vector tomography results
cannot be performed, we compared the tomography inverted coronal magnetic
fields with those constructed by MagnetoHydroDynamic (MHD) simulation based on
observed photospheric magnetic fields of CR 2112 and 2113. We found that the
MHD model for CR 2112 is qualitatively consistent with the tomography inverted
result for most of the reconstruction domain except for a couple of regions.
Particularly for one of the most noticeable exception region, we found that the
MHD simulation for CR 2113 predicted a model that more closely resemble the
vector tomography inverted magnetic fields. We discuss the utilities and
limitations of the tomographic inversion technique, and present ideas for
future developments.
