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High-mass stars and star clusters commonly form within hub-filament systems.Monoceros R2, harbors one of the closest such systems, making it an excellenttarget for case studies. We investigate the morphology, stability and dynamicalproperties of the hub-filament system on basis of 13CO and C18O observationsobtained with the IRAM-30m telescope and H2 column density maps derived fromHerschel dust emission observations. We identified the filamentary network andcharacterized the individual filaments as either main (converging into the hub)or secondary (converging to a main filament) filaments. The main filaments haveline masses of 30-100 Msun/pc and show signs of fragmentation. The secondaryfilaments have line masses of 12-60 Msun/pc and show fragmentation onlysporadically. In the context of Ostriker's hydrostatic filament model, the mainfilaments are thermally super-critical. If non-thermal motions are included,most of them are trans-critical. Most of the secondary filaments are roughlytrans-critical regardless of whether non-thermal motions are included or not.From the main filaments, we estimate a mass accretion rate of 10(-4)-10(-3)Msun/pc into the hub. The secondary filaments accrete into the main filamentswith a rate of 0.1-0.4x10(-4) Msun/pc. The main filaments extend into the hub.Their velocity gradients increase towards the hub, suggesting acceleration ofthe gas. We estimate that with the observed infall velocity, the mass-doublingtime of the hub is ~2.5 Myr, ten times larger than the free-fall time,suggesting a dynamically old region. These timescales are comparable with thechemical age of the HII region. Inside the hub, the main filaments show a ring-or a spiral-like morphology that exhibits rotation and infall motions. Onepossible explanation for the morphology is that gas is falling into the centralcluster following a spiral-like pattern.

Dynamics of cluster-forming hub-filament systems: The case of the high-mass star-forming complex Monoceros R2