Abstract
In the past decade filaments have been recognised as a major structural element of the interstellar medium, the densest of these filaments hosting the formation of most stars. In some star-forming molecular clouds converging networks of filaments, also known as hub filament systems, can be found. These hubs are believed to be preferentially associated to massive star formation. As of today, there are no metrics that allow the systematic quantification of a filament network convergence. Here, we used the IRAM 30m NIKA2 observations of the Galactic plane from the GASTON large programme to systematically identify filaments and produce a filament convergence parameter map. We use such a map to show that: i. hub filaments represent a small fraction of the global filament population; ii. hubs host, in proportion, more massive and more luminous compact sources that non-hubs; iii. hub-hosting clumps are more evolved that non-hubs; iv. no discontinuities are observed in the properties of compact sources as a function of convergence parameter. We propose that the rapid global collapse of clumps is responsible for (re)organising filament networks into hubs and, in parallel, enhancing the mass growth of compact sources.
Highlights
The existence of interstellar filaments has been known for more than four decades [1]
We propose that the rapid global collapse of clumps is responsible fororganising filament networks into hubs and, in parallel, enhancing the mass growth of compact sources
In order to do this, we first need to build the skeleton of the filament network within the GASTON 1.15mm image of the = 24o region
Summary
The existence of interstellar filaments has been known for more than four decades [1]. Since filaments are front and centre of a large fraction of star formation research, and numerous breakthroughs have been made. It has been shown, for instance, that the majority of prestellar cores, and, by extension, the majority of stars form as the result of the fragmentation of individual 0.1pc-wide self-gravitating filaments [e.g. 4, 5]. Massive star-forming cores, on the other hand, seem to preferentially find themselves at the centre of converging networks of filaments, or hubs [e.g. 6, 7]. This raises a number of questions on the physical relationship between filament convergence and the evolution of star-forming clouds. In the study presented here, we use the very sensitive 1.15mm continuum data of the GASTON large programme on the IRAM 30m to determine the time evolution of compact millimetre sources as a function of the local filament network convergence
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
