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The interstellar medium has a highly filamentary and hierarchical structure,which may play a significant role in star formation. A systematical study onthe large-scale filaments towards their physical parameters, distribution,structures and kinematics will inform us of what kind of filaments havepotential to form stars, how the material feed protostars through filaments,and the connection between star formation and Galactic spiral arms. Unlike thetraditional "by eyes" searches, we use a customized minimum spanning treealgorithm to identify filaments by linking Galactic clumps from the APEXTelescope Large Area Survey of the Galaxy catalogue. In the inner Galacticplane ($|l| < 60^\circ$), we identify 163 large-scale filaments with physicalproperties derived, including dense gas mass fraction, and compare them with anupdated spiral arm model in position-position-velocity space. Dense gas massfraction is found not to differ significantly in various Galactic position,neither does it in different spiral arms. We also find that most filaments areinter-arm filaments after adding a distance constraint, and filaments in armdiffer a little with those not in. One surprising result is that clumps on andoff filaments have no significant distinction in their mass at the same size.

A census of 163 large-scale (>=10 pc), velocity-coherent filaments in  inner Galactic plane: physical properties, dense gas fraction, and  association with spiral arms