Authors: Giuliana de Toma (NCAR/HAO), Joan Burkepile (NCAR/HAO), Mike Galloy (NCAR/HAO), Steve Tomczyk (Solar Scientific LLC), and Enrico Landi (Univ. of Michigan)

The UCoMP coronagraph at the Mauna Loa Solar Observatory (MLSO) is an imaging polarimeter that takes daily synoptic observations of the solar corona up to 2 solar radii with a spatial resolution of 3 arcsec/pixel. It can observe several coronal emission lines in the visible and IR from 530nm to 1083nm, including the FeXIII lines at 1074.7nm 1079.8nm with a formation temperature intermediate between the Fe XII 19.3nm and FeXIV 21.1nm lines observed by SDO/AIA. While not specifically designed to study CMEs, UCOMP has captured several coronal eruptions, including partial halos. We present examples of pre-eruptive and eruptive magnetic structures observed simultaneously by MLSO/UCoMP, MLSO/K-Cor, SDO/AIA and LASCO. We illustrate the uniqueness of the UCoMP spectro-polarimetric observations, which include line-of-sight velocity, line width, and linear polarization, and emphasize the synergy between UCOMP and current ground- and space-based instruments.