  Interplanetary coronal mass ejections (ICMEs) are magnetic structures
propagating from the Sun's corona to the interplanetary medium. With over 20
years of observations at the L1 libration point, ACE offers hundreds of ICMEs
detected at different times during several solar cycles and with different
features such as the propagation speed. We investigate a revisited catalog of
more than 400 ICMEs using the superposed epoch method on the mean, median, and
the most probable values of the distribution of magnetic and plasma parameters.
We also investigate the effects of the speed of ICMEs relative to the solar
wind, the solar cycle, and the existence of a magnetic cloud on the generic
ICME profile. We find that fast-propagating ICMEs (relatively to the solar wind
in front) still show signs of compression at 1 au, as seen by the compressed
sheath and the asymmetric profile of the magnetic field. While the solar cycle
evolution does not impact the generic features of ICMEs, there are more extreme
events during the active part of the cycle, widening the distributions of all
parameters. Finally, we find that ICMEs with or without a detected magnetic
cloud show similar profiles, which confirms the hypothesis that ICMEs with no
detected magnetic clouds are crossed further away from the flux rope core. Such
a study provides a generic understanding of processes that shape the overall
features of ICMEs in the solar wind and can be extended with future missions at
different locations in the solar system.
