  The Indian Consortium of Cosmologists has proposed a cosmic microwave
background (CMB) space mission, Exploring Cosmic History and Origin (ECHO). A
major scientific goal of the mission is to detect the primordial B-mode signal
of CMB polarization. The detection of the targeted signal is very challenging
as it is deeply buried under the dominant astrophysical foreground emissions of
the thermal dust and the Galactic synchrotron. To facilitate the adequate
subtraction of thermal dust, the instrument design of ECHO has included nine
dust-dominated high-frequency bands over the frequency range of 220-850 GHz. In
this work, we closely reexamine the utility of the high-frequency ECHO bands in
foreground subtraction using the Needlet Internal Linear Combination component
separation method. We consider three dust models: a physical dust model, a dust
spectral energy distribution (SED) with a single modified black body (MBB)
emission law and a multilayer dust model with frequency-frequency
decorrelation. We consider eleven ECHO bands in the 28-190 GHz range as our
baseline configuration and investigate the changes in the level foreground and
noise residuals as subsequent dust-dominated high-frequency bands are added. We
find that adding the high-frequency bands leads to a consistent decrease in the
level of residual foreground and noise, and the sensitivity of r measurement
improves. Most of the reduction in both residual levels and enhancement in the
sensitivity is achieved in the 28-600 GHz frequency range. Negligible change in
residual levels is seen by extending the frequency range from 600 GHz to 850
GHz.
