  We present observations of $J$=1-0 transition lines of ${ }^{12}
\mathrm{CO}$, ${ }^{13} \mathrm{CO}$, and $\mathrm{C}^{18} \mathrm{O}$ towards
the Galactic region of $153.60^{\circ} \leqslant l \leqslant 156.50^{\circ}$
and $1.85^{\circ} \leqslant b \leqslant 3.50^{\circ}$, using the Purple
Mountain Observatory (PMO) 13.7 m millimeter telescope. Based on the \tht data,
one main filament and five sub-filaments are found together as a network
structure in the velocity interval of $[-42.5, -30.0] \,\mathrm{km}
\mathrm{\,s}^{-1}$. The kinematic distance of this molecular cloud (MC) is
estimated to be $\sim4.5 \mathrm{\,kpc}$. The median length, width, excitation
temperature, line mass of these filaments are $\sim49 \mathrm{\,pc}$, $\sim2.9
\mathrm{\,pc}$, $\sim8.9 \mathrm{\,K}$, and $\sim39 \,M_{\odot}
\mathrm{pc}^{-1}$, respectively. The velocity structures along these filaments
exhibit oscillatory patterns, which are likely caused by the fragmentation or
accretion process along these filaments. The maximum accretion rate is
estimated to be as high as $\sim700 \,M_{\odot} \mathrm{pc}^{-1}$. A total of
$\sim162$ \tht clumps and $\sim 103$ young stellar objects (YSOs) are
identified in this region. Most of the clumps are in gravitationally bound
states. Three \hii regions (G154.359+2.606, SH2-211, SH2-212) are found to be
located in the apexes of the filaments. Intense star forming activities are
found along the entire filamentary cloud. The observed results may help us to
better understand the link between filaments and massive star formation.
