  The phase of in-spiral of double compact objects (DCOs: NS+WD, NS+NS, BH+NS,
and BH+BH binaries) in the disk field population of the Galaxy provides a
potential source in the frequency range from $10^{-4}$ to 0.1 Hz, which can be
detected by the European New Gravitational Observatory (NGO: eLISA is derived
from the previous LISA proposal) project. In this frequency range, much
stronger gravitational wave (GW) radiation can be obtained from DCO sources
because they possess more mass than other compact binaries (e.g., close double
white dwarfs). In this study, we aim to calculate the gravitational wave
signals from the resolvable DCO sources in the Galaxy using a binary population
synthesis approach, and to carry out physical properties of these binaries
using Monte Carlo simulations. Combining the sensitivity curve of the eLISA
detector and a confusion-limited noise floor of close double white dwarfs, we
find that only a handful of DCO sources can be detected by the eLISA detector.
The detectable number of DCO sources reaches 160, in the context of
low-frequency eLISA observations we find that the number of NS+WD, NS+NS,
BH+NS, and BH+BH are 132, 16, 3, and 6, respectively.
