The formation of filamentary bundles in turbulent molecular clouds


The classical picture of a star-forming filament is a near-equilibrium structure, with collapse dependent on its gravitational criticality. Recent observations have complicated this picture, revealing filaments as a mess of apparently interacting subfilaments, with transsonic internal velocity dispersions and mildly supersonic intra-subfilament dispersions. How structures like this form is unresolved. Here we study the velocity structure of filamentary regions in a simulation of a turbulent molecular cloud. We present two main findings: first, the observed complex velocity features in filaments arise naturally in self gravitating hydrodynamic simulations of turbulent clouds without the need for magnetic or other effects. Second, a region that is filamentary only in projection and is in fact made of spatially distinct features can displays these same velocity characteristics. The fact that these disjoint structures can masquerade as coherent filaments in both projection and velocity diagnostics highlights the need to continue developing sophisticated filamentary analysis techniques for star formation observations.


Observations with the Herschel satellite have revealed that the backbone of molecular clouds is a compex network of connecting and interacting filaments (citation not found: 2010A&A...518L.102A) (citation not found: 2010A&A...518L.100M) (citation not found: 2011A&A...529L...6A) (citation not found: 2012A&A...540L..11S). The dynamics of this web of dense molecular gas not only determines the evolution and stability of molecular clouds, but also regulates their condensation into stars. Molecular cloud cores and single low-mass stars are almost always found in filaments, often aligned like pearls on a string (Hartmann, 2002; Lada et al., 2008; (citation not found: 2010A&A...518L.102A). This can be interpreted as a result of the gravitational instability of a supercritical filamentary section (Inutsuka et al., 1997; (citation not found: 2011A&A...533A..34H). Where filaments intersect, more massive hubs form (Myers, 2009; Myers, 2013) that later on could become the progenitors of star clusters.

Lada et al. (2010) (see also e.g. Enoch et al., 2007) demonstrated that the fraction of gas in the dense molecular web is of order 10 percent of the total molecular mass. Interestingly, the mass fraction of protostars to dense (\(n > 10^4\) cm\(^{-3}\)) molecular gas is also a constant of the same order. Burkert et al. (2013) showed that this requires new filamentary segments to continuously form from the diffuse intra-filament medium on a gravitational collapse timescale.

Classically, gas filaments have been treated as cylinders of gas in hydrostatic equilibrium (Ostriker, 1964; (citation not found: 2012A&A...542A..77F) (citation not found: 2013A&A...558A..27R). It is not clear, however, how such quiescent structures could form in the turbulent environment of a molecular cloud (citation not found: 2010A&A...520A..17K) Heitsch, 2013). In addition, millimeter line studies indicate that filaments have intrinsic, super-thermal linewidths (citation not found: 2013A&A...553A.119A).

More recently, observations by (citation not found: 2013A&A...554A..55H) revealed that filaments are often compact bundles of thin spaghetti-like subfilaments. They presented observations of a prominent filamentary feature in Taurus, dominated by the L1495 cloud (Lynds, 1962) and several dark patches (Barnard, 1927). They observed the region in the moderate density tracer C\(^{18}\)O, obtaining spectra along a \(\sim 10\) pc length of the region. Analysing the richest \(\sim 3\) pc section of the filament in the resultant position–position–velocity space, they found the intriguing result that the gas along the ridge is organized in velocity-coherent filamentary structures, with typical lengths \(\sim0.5\) pc. Each filament is internally subsonic or transsonic, though the collection of filaments is characterised by a mildly supersonic interfilamentary dispersion of \(\sim 0.5\) km s\(^{-1}\). They describe the collection of velocity detections as “elongated groups that lie at different ‘heights’ (velocities) and present smooth and often oscillatory patterns”. Multiple velocity components along a single line of sight have also been observed in Serpens South (Tanaka et al., 2013); this feature may therefore be common for many young star forming sites.

The complexity of Hacar et al.’s position–position–velocity data, exemplified by their figure 9, invites theoretical and numerical exploration. In particular the apparent organization of filaments into bundles tends to bring to mind magnetic fields or other relatively complex physics. In this Letter we explore whether this velocity signal is present in simulated molecular clouds with a more minimal set of physics, including only gravity and hydrodynamic forces acting on the initial turbulence.