  We report on the coronal hole (CH) influence on the 54 magnetic cloud (MC)
and non-MC associated coronal mass ejections (CMEs) selected for studies during
the Coordinated Data Analysis Workshops (CDAWs) focusing on the question if all
CMEs are flux ropes. All selected CMEs originated from source regions located
between longitudes 15E-15W. Xie, Gopalswamy, and St, Cyr (2013, Solar Phys.,
doi:10.1007/s11207-012-0209-0) found that these MC and non-MC associated CMEs
are on average deflected towards and away from the Sun-Earth line respectively.
We used a CH influence parameter (CHIP) that depends on the CH area, average
magnetic field strength, and distance from the CME source region to describe
the influence of all on-disk CHs on the erupting CME. We found that for CHIP
values larger than 2.6 G the MC and non-MC events separate into two distinct
groups where MCs (non-MCs) are deflected towards (away) from the disk center.
Division into two groups was also observed when the distance to the nearest CH
was less than 3.2x10^5 km. At CHIP values less than 2.6 G or at distances of
the nearest CH larger than 3.2x10^5 km the deflection distributions of the MC
and non-MCs started to overlap, indicating diminishing CH influence. These
results give support to the idea that all CMEs are flux ropes, but those
observed to be non-MCs at 1 AU could be deflected away from the Sun-Earth line
by nearby CHs, making their flux rope structure unobservable at 1 AU.
