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Filamentary structures are ubiquitous in high-mass star-forming molecularclouds. Their relation with high-mass star formation is still to be understood.Here we report interferometric observations toward 8 filamentary high-massstar-forming clouds. A total of 50 dense cores are identified in these clouds,most of which present signatures of high-mass star formation. Five of them arenot associated with any star formation indicators, hence are prestellar corecandidates. Evolutionary phases of these cores and their linewidths,temperatures, NH$_3$ abundances, and virial parameters are found to becorrelated. In a sub-sample of 4 morphologically well-defined filaments, wefind that their fragmentation can not be solely explained by thermal orturbulence pressure support. We also investigate distributions of gastemperatures and non-thermal motions along the filaments, and find a spatialcorrelation between non-thermal linewidths and star formation activities. Wefind evidence of gas flows along these filaments, and derive an accretion ratealong filaments of $\sim$10$^{-4}$ M$_\odot$ yr$^{-1}$. These results suggest astrong relationship between massive filaments and high-mass star formation,through i) filamentary fragmentation in very early evolutionary phases to formdense cores, ii) accretion flows along filaments that are important for thegrowth of dense cores and protostars, and iii) enhancement of non-thermalmotion in the filaments by the feedback or accretion during star formation.

Filamentary Fragmentation and Accretion in High-Mass Star-Forming Molecular Clouds