  A Coronal Mass Ejection (CME) is an inhomogeneous structure consisting of
different features which evolve differently with the propagation of the CME.
Simultaneous heliospheric tracking of different observed features of a CME can
improve our understanding about relative forces acting on them. It also helps
to estimate accurately their arrival times at the Earth and identify them in
in- situ data. This also enables to find association between remotely observed
features and in-situ observations near the Earth. In this paper, we attempt to
continuously track two density enhanced features, one at the front and another
at the rear edge of the 6 October 2010 CME. This is achieved by using
time-elongation maps constructed from STEREO/SECCHI observations. We derive the
kinematics of the tracked features using various reconstruction methods. The
estimated kinematics are used as inputs in the Drag Based Model (DBM) to
estimate the arrival time of the tracked features of the CME at L1. On
comparing the estimated kinematics as well as the arrival times of the remotely
observed features with in-situ observations by ACE and Wind, we find that the
tracked bright feature in the J-map at the rear edge of 6 October 2010 CME
corresponds most probably to the enhanced density structure after the magnetic
cloud detected by ACE and Wind. In-situ plasma and compositional parameters
provide evidence that the rear edge density structure may correspond to a
filament associated with the CME while the density enhancement at the front
corresponds to the leading edge of the CME. Based on this single event study,
we discuss the relevance and significance of heliospheric imager (HI)
observations in identification of the three-part structure of the CME.
