  The ejecta kinematics of supernova remnants (SNRs) is one of crucial clues to
understand the explosion mechanism of type Ia supernovae (SNe). In particular,
the kinematic asymmetry of iron-peak elements provides the key to understanding
physical processes taking place in the core of the exploding white dwarfs (WDs)
although it has been poorly understood by observations. In this paper, we show
for the first time the asymmetric expansion structure in the line-of-sight
direction of Fe ejecta in Kepler's SNR revealed by spectral and imaging
analysis using the Chandra archival data. We found that the K$\alpha$ line
centroid energy and line width is relatively lower ($<$ 6.4 keV) and narrower
($\sim$80 eV) around the center of the remnant, which implies that the majority
of the Fe ejecta in the central region is red-shifted. At the outer regions, we
identify bright blue-shifted structures as it might have been ejected as high
velocity dense clumps. Taking into account the broad population of the Fe
charge states, we estimate the red-shifted velocity of ~2,000 km/s and the
blue-shifted velocity of ~3,000 km/s for each velocity structure. We also
present a possibility that a portion of the Fe ejecta near the center are
interacting with the dense circumstellar medium (CSM) on the near side of the
remnant. As the origin of the asymmetric motion of the Fe ejecta, we suggest
three scenarios, (1) the asymmetric distribution of the CSM, (2) the "shadow"
in Fe cast by the companion star, and (3) the asymmetric explosion.
