CO(J=1-0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50

We present observations of the J = 1 - 0 transition lines of (CO)-C-12, (CO)-C-13, and (CO)-O-18 toward the Galactic region of 153.degrees 60 <= l <= 156.degrees 50 and 1.degrees 85 <= b <= 3.degrees 50, using the Purple Mountain Observatory 13.7 m millimeter telescope. Based on the (CO)-C-13 data, one main filament and five subfilaments are found together as a network structure in the velocity interval of [-42.5, -30.0] km s(-1). The kinematic distance of this molecular cloud is estimated to be similar to 4.5 kpc. The median length, width, excitation temperature, and line mass of these filaments are similar to 49 pc, similar to 2.9 pc, similar to 8.9 K, and similar to 39 M (circle dot) 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 similar to 700 M (circle dot) pc(-1). A total of similar to 162 (CO)-C-13 clumps and similar to 103 young stellar objects are identified in this region. Most of the clumps are in gravitationally bound states. Three H ii regions (G154.359+2.606, SH2-211, and SH2-212) are found to be located in the apexes of the filaments. Intense star-forming activity is found along the entire filamentary cloud. The observed results may help us to better understand the link between filaments and massive star formation.

Automated summary

Observations of a specific region in the Galaxy reveal the presence of filamentary structures, along with their estimated kinematic distance and various parameters. The velocity structures along these filaments exhibit oscillatory patterns, possibly due to fragmentation or accretion processes. Numerous clumps and young stellar objects are also identified in this region, most of which are in gravitationally bound states. Therefore, these observational results are of significant importance in enhancing our understanding of the connection between filamentary structures and massive star formation.