Filament coalescence and hub structure in Mon R2

Here we study the MonR2 star forming region, which has a rich network of filaments joining in cluster hub, aiming at understanding hub structure and to examine mass fraction residing filaments, is key factor that influences massive formation. We conducted multi-scale, multi-component analysis Herschel column density maps (resolution 18.2" or $\sim$0.07 pc 830 pc) region using newly developed algorithm "getsf" identify structural components, namely, extended cloud, sources. find cascades lower coalesce form higher eventually merging inside (0.8 radius). As opposed previous view as clump with $\sim$1 radius, it be short high-density filaments. The total reservoir HFS (5 $\times$ 5 split between (54%), cloud (37%) sources (9%). M/L increase from $\sim$ 10 Msun/pc 1.5pc 100 its centre, while number per annulus 0.2pc width decreases 20 2 same range. observed radial (filament component only) displays power-law dependence $N_{\mathrm{H}_2} \propto r^{-2.17}$ up radius $\sim$2.5 central resembling global collapse HFS. present scenario where can supported by magnetic fields interact, merge reorganize themselves coalesce. In new suggest only stars located benefit longitudinal flows gas become massive, may explain reason for formation many low-mass centres.