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The recent data collected by {\it Herschel} have confirmed that interstellarstructures with filamentary shape are ubiquitously present in the Milky Way.Filaments are thought to be formed by several physical mechanisms acting fromthe large Galactic scales down to the sub-pc fractions of molecular clouds, andthey might represent a possible link between star formation and the large-scalestructure of the Galaxy. In order to study this potential link, a statisticallysignificant sample of filaments spread throughout the Galaxy is required. Inthis work we present the first catalogue of $32,059$ candidate filamentsautomatically identified in the Hi-GAL survey of the entire Galactic Plane. Forthese objects we determined morphological (length, $l^{a}$, and geometricalshape) and physical (average column density, $N_{\rm H_{2}}$, and averagetemperature, $T$) properties. We identified filaments with a wide range ofproperties: 2$'$\,$\leq l^{a}\leq$\, 100$'$, $10^{20} \leq N_{\rm H_{2}} \leq10^{23}$\,cm$^{-2}$ and $10 \leq T\leq$ 35\,K. We discuss their associationwith the Hi-GAL compact sources, finding that the most tenuous (and stable)structures do not host any major condensation and we also assign a distance to$\sim 18,400$ filaments for which we determine mass, physical size, stabilityconditions and Galactic distribution. When compared to the spiral armsstructure, we find no significant difference between the physical properties ofon-arm and inter-arm filaments. We compared our sample with previous studies,finding that our Hi-GAL filament catalogue represents a significant extensionin terms of Galactic coverage and sensitivity. This catalogue represents anunique and important tool for future studies devoted to understanding thefilament life-cycle.

The Hi-GAL catalogue of dusty filamentary structures in the Galactic Plane