  The Einstein Telescope (ET) is the future third generation gravitational wave
detector consisting of three independent interferometers arranged in a
triangular configuration, with the sensitivity large enough to be able to
detect stellar mass black holes even beyond the redshift of 10. In this paper,
we analyze the capabilities of ET as a standalone instrument and not part of a
network. We show that the analysis of detection of binary coalescences in the
three individual interferometers of the ET allow us to weakly constrain the sky
location of the source. We present the analysis that leads to the constraints
on the redshift and source frame chirp mass of detected binaries. We show that
these values can be estimated with the accuracy comparable to the one expected
from networks of gravitational wave interferometers. Thus, we show that the ET
as a single instrument is able to break the redshift - chirp mass degeneracy
and is therefore a valuable tool to explore properties of populations of
merging compact object binaries.
