Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites

By T. Hill, Fr'ed'erique Motte, P. Didelon, S. Bontemps, V. Minier, M. Hennemann, N. Schneider, P. Andre', A. Men’shchikov, L. Anderson and 22 more. 2011

197 citations recorded by the source corpus.

We present the first Herschel PACS and SPIRE results of the Vela C molecular complex in the far-infrared and submillimetre regimes at 70, 160, 250, 350, and 500 um, spanning the peak of emission of cold prestellar or protostellar cores. Column density and multi-resolution analysis (MRA) differentiates the Vela C complex into five distinct sub-regions. Each sub-region displays differences in their column density and temperature probability distribution functions (PDFs), in particular, the PDFs of the 'Centre-Ridge' and 'South-Nest' sub-regions appear in stark contrast to each other. The Centre-Ridge displays a bimodal temperature PDF representative of hot gas surrounding the HII region RCW 36 and the cold neighbouring filaments, whilst the South-Nest is dominated by cold filamentary structure. The column density PDF of the Centre-Ridge is flatter than the South-Nest, with a high column density tail, consistent with formation through large-scale flows, and regulation by self-gravity. At small to intermediate scales MRA indicates the Centre-Ridge to be twice as concentrated as the South-Nest, whilst on larger scales, a greater portion of the gas in the South-Nest is dominated by turbulence than in the Centre-Ridge. In Vela C, high-mass stars appear to be preferentially forming in ridges, i.e., dominant high column density filaments.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/78d8604e4dcea4dce7ee3a5c2bd414ca036853c8

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Citations in the corpus

An ALMA study of the Orion Integral Filament: I. Evidence for narrow fibers in a massive cloud (2018, background): “Typically located at kpc distances, most of these massive filaments are found in hub-like associations (Myers 2009) forming dense ridges of gas (Galván-Madrid et al. 2010; Schneider et al. 2010; Henning et al. 2010; Hill et al. 2011; Hennemann et al. 2012; Peretto et al. 2013).”
ON THE STAR FORMATION EFFICIENCY OF TURBULENT MAGNETIZED CLOUDS (2012, background): “…an isothermal equation of state, which is a reasonable approximation for dense, molecular gas of solar metallicity, over a wide range of densities (Wolfire et al. 1995; Omukai et al. 2005; Pavlovski et al. 2006; Glover & Mac Low 2007a,b; Glover et al. 2010; Hill et al. 2011; Hennemann et al. 2012).”
WHAT DETERMINES THE DENSITY STRUCTURE OF MOLECULAR CLOUDS? A CASE STUDY OF ORION B WITH HERSCHEL (2013, background): “Solenoidal forcing arises from galactic rotation and magneto-rotational instabilities. global gravitational collapse of larger spatial areas like filaments and ridges (see, e.g., Schneider et al. (2010), Hill et al. (2011), Palmeirim et al. (2013) for observational examples).”
The spine of the swan: a Herschel study of the DR21 ridge and filaments in Cygnus X (2012, methodology): “Studying the Vela C region, Hill et al. (2011) suggested that “ridges”, i.e., massive, gravitationally unstable filamentary structures of high column density (NH2 > 10 23 cm−2) that dominate their environment could be preferential sites of high-mass star formation (cf. Nguyen Luong et al. 2011).”
THE STAR FORMATION RATE OF TURBULENT MAGNETIZED CLOUDS: COMPARING THEORY, SIMULATIONS, AND OBSERVATIONS (2012, methodology): “This is a reasonable approximation for dense, molecular gas of solar metallicity, over a wide range of densities (Wolfire et al. 1995; Omukai et al. 2005; Pavlovski et al. 2006; Glover & Mac Low 2007a,b; Glover et al. 2010; Hill et al. 2011; Hennemann et al. 2012).”
LOW VIRIAL PARAMETERS IN MOLECULAR CLOUDS: IMPLICATIONS FOR HIGH-MASS STAR FORMATION AND MAGNETIC FIELDS (2013, background): “For starless cores, such work typically finds temperatures in the range 10–15 K. Direct estimates of dust temperatures from continuum emission yield similar values for regions not in the immediate vicinity of HMSF (e.g., Hill et al. 2011).”
Cluster-formation in the Rosette molecular cloud at the junctions of filaments (2012, unknown): “, the PDFs of other high-mass SF clouds are more complex and show several breaks in the PDFs (Hill et al. 2011, Csengeri et al., in prep.).”
A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey (2015, methodology): “…2010; Miville-Deschênes et al. 2010) and other imaging surveys such as HiGAL (Molinari et al. 2010; Schisano et al. 2014), HOBYS (Motte et al. 2010; Hill et al. 2011), and EPoS (Henning et al. 2010) now demonstrate that these filaments are truly ubiquitous in the cold ISM, present a high degree…”
On the universality of interstellar filaments: theory meets simulations and observations (2015, background): “…recently attracted much attention, especially since the Herschel satellite revealed a wealth of filamentary structures in both star-forming and quiescent clouds (André et al. 2010; Men’shchikov et al. 2010; MivilleDeschênes et al. 2010; Arzoumanian et al. 2011; Hill et al. 2011; Roy et al. 2015).”