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We present observations of $J$=1-0 transition lines of ${ }^{12}\mathrm{CO}$, ${ }^{13} \mathrm{CO}$, and $\mathrm{C}^{18} \mathrm{O}$ towardsthe Galactic region of $153.60^{\circ} \leqslant l \leqslant 156.50^{\circ}$and $1.85^{\circ} \leqslant b \leqslant 3.50^{\circ}$, using the PurpleMountain Observatory (PMO) 13.7 m millimeter telescope. Based on the \tht data,one main filament and five sub-filaments are found together as a networkstructure in the velocity interval of $[-42.5, -30.0] \,\mathrm{km}\mathrm{\,s}^{-1}$. The kinematic distance of this molecular cloud (MC) isestimated to be $\sim4.5 \mathrm{\,kpc}$. The median length, width, excitationtemperature, 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 filamentsexhibit oscillatory patterns, which are likely caused by the fragmentation oraccretion process along these filaments. The maximum accretion rate isestimated to be as high as $\sim700 \,M_{\odot} \mathrm{pc}^{-1}$. A total of$\sim162$ \tht clumps and $\sim 103$ young stellar objects (YSOs) areidentified in this region. Most of the clumps are in gravitationally boundstates. Three \hii regions (G154.359+2.606, SH2-211, SH2-212) are found to belocated in the apexes of the filaments. Intense star forming activities arefound along the entire filamentary cloud. The observed results may help us tobetter understand the link between filaments and massive star formation.

CO(J = 1-0) Observations toward the Filamentary Cloud in the Galactic  Region of $153.60^{\circ} \leqslant l \leqslant 156.50^{\circ}$ and  $1.85^{\circ} \leqslant b \leqslant 3.50^{\circ}$