  We have studied a set of 41 magnetic clouds (MCs) measured by the ACE
spacecraft, using the discrete orthogonal wavelet transform (Daubechies wavelet
of order two) in three regions: Pre-MC (plasma sheath), MC and Post-MC. We have
used data from the IMF GSM-components with time resolution of 16 s. The
mathematical property chosen was the statistical mean of the wavelet
coefficients $(\langle Dd1 \rangle)$. The Daubechies wavelet coefficients have
been used because they represent the local regularity present in the signal
being studied. The results reproduced the well-known fact that the dynamics of
the sheath region is more than that of the MC region. This technique could be
useful to help a specialist to find events boundaries when working with IMF
datasets, i.e., a best form to visualize the data. The wavelet coefficients
have the advantage of helping to find some shocks that are not easy to see in
the IMF data by simple visual inspection. We can learn that fluctuations are
not low in all MCs, in some cases waves can penetrate from the sheath to the
MC. This methodology has not yet been tested to identify some specific
fluctuation patterns at IMF for any other geoeffective interplanetary events,
such as Co-rotating Interaction Regions (CIRs), Heliospheric Current Sheet
(HCS) or ICMEs without MC signatures. In our opinion, as is the first time that
this technique is applied to the IMF data with this purpose, the presentation
of this approach for the Space Physics Community is one of the contributions of
this work.
