Resolving the Vela C ridge with P-ArTéMiS and<i>Herschel</i>

Hill, T.; André, Ph.; Arzoumanian, D.; Motte, F.; Minier, V.; Men’shchikov, A.; Didelon, P.; Hennemann, M.; Könyves, V.; Nguyen-Luong, Q.; Palmeirim, P.; Peretto, N.; Schneider, N.; Bontemps, Sylvain; Louvet, F.; Elia, D.; Giannini, T.; Revéret, V.; Pennec, J. Le; Rodríguez, L. F.; Boulade, O.; Doumayrou, E.; Dubreuil, Didier; Gallais, P.; Lortholary, M.; Martignac, J.; Talvard, M.; Breuck, C. De

doi:10.1051/0004-6361/201220504

Cited by 37 publications

(50 citation statements)

References 27 publications

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“…Inutsuka & Miyama 1992;Kawachi & Hanawa 1998). The shape of their radial column density profiles with a high degree of symmetry about the filament major axis and a well-defined power law regime at large radii, approximately consistent with a radial density structure ρ ∝ r −2 Palmeirim et al 2013;Hill et al 2012), is consistent with a theoretical model of a nearly isothermal collapsing cylinder (Kawachi & Hanawa 1998;Palmeirim et al 2013), and therefore also suggestive of gravitational contraction. If supercritical filaments are indeed contracting, then their central column density is expected to increase with time (cf.…”

Section: An Evolutionary Scenario For Interstellar Filaments?supporting

confidence: 78%

Formation and evolution of interstellar filaments

Arzoumanian

André

Peretto

et al. 2013

A&A

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152

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We investigate the gas velocity dispersions of a sample of filaments recently detected as part of the Herschel Gould Belt Survey in the IC 5146, Aquila, and Polaris interstellar clouds. To measure these velocity dispersions, we use 13 CO, C 18 O, and N 2 H + line observations obtained with the IRAM 30 m telescope. Correlating our velocity dispersion measurements with the filament column densities derived from Herschel data, we show that interstellar filaments can be divided into two regimes: thermally subcritical filaments, which have transonic velocity dispersions (c s < ∼ σ tot < 2 c s ) independent of column density and are gravitationally unbound; and thermally supercritical filaments, which have higher velocity dispersions scaling roughly as the square root of column density (σ tot ∝ Σ 0 0.5 ) and which are self-gravitating. The higher velocity dispersions of supercritical filaments may not directly arise from supersonic interstellar turbulence but may be driven by gravitational contraction/accretion. Based on our observational results, we propose an evolutionary scenario whereby supercritical filaments undergo gravitational contraction and increase in mass per unit length through accretion of background material, while remaining in rough virial balance. We further suggest that this accretion process allows supercritical filaments to keep their approximately constant inner widths (∼0.1 pc) while contracting.

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Section: An Evolutionary Scenario For Interstellar Filaments?supporting

confidence: 78%

Formation and evolution of interstellar filaments

Arzoumanian

André

Peretto

et al. 2013

A&A

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152

201

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“…The median width is ∼0.5 pc, which is significantly larger than the widths measured from the Herschel Gould Belt Survey (André et al 2014) where filament inner widths of ∼0.1 pc are typically reported for nearby clouds (e.g. Arzoumanian et al 2011;Hill et al 2012), and we have made no attempt to separate out the contribution from a possible 6-3 pc) for a sample of 9 large-scale filaments. However, we note that the values calculated here show a distance-dependence, i.e.…”

Section: Lengths and Widthsmentioning

confidence: 58%

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

Urquhart

Leurini

et al. 2016

A&A

111

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Context. Filamentary structures are ubiquitous in the interstellar medium. Investigating their connection to the large-scale structure of the Galaxy and their role in star formation is leading to a paradigm shift in our understanding of star formation. Aims. We study the properties of filamentary structures from the ATLASGAL survey, which is the largest and most sensitive systematic ground-based survey of the inner Galactic plane at submillimeter wavelengths. Methods. We use the DisPerSE algorithm to identify spatially coherent structures located across the inner-Galaxy (300• < < 60• and |b| < 1.5). As a result we produce a catalogue of ∼1800 structures; these were then independently classified by the five lead authors into one of the following types: marginally resolved, elongated structures, filaments, network of filaments and complexes. This resulted in the identification of 517 filamentary structures. We determine their physical properties and investigate their overall Galactic distribution.Results. We find that almost 70% of the total 870 µm flux associated with these structures resides in filaments and networks of filaments and we estimate that they are likely to be associated with a similar fraction of the mass. Correlating these structures with tracers of massive star formation we also find that a similar fraction of the massive star forming clumps are associated with filaments and networks of filaments, which highlights the importance of these types of structures to star formation in the Galaxy. We have determined distances, masses and physical sizes for 241 of the filamentary structures. We find a median distance of 3.8 kpc, a mean mass of a few 10 3 M , a mean length of ∼6 pc and a mass-to-length ratio of (M/L) ∼200-2000 M pc −1 . We also find that these filamentary structures are tightly correlated with the spiral arms in longitude and velocity, and that their semi-major axis is preferentially aligned parallel to the Galactic mid-plane and therefore with the direction of large-scale Galactic magnetic field. We find many examples where the dense filaments identified in ATLASGAL are associated with larger scale filamentary structures (∼100 pc), and argue that this is likely to be common, and as such these may indicate a connection between large-scale Galactic dynamics and star formation. Conclusions. We have produced a large and Galaxy-wide catalogue of dense filamentary structures that are representative of a particular size and mass range not previously well studied in the literature. Analyses of the properties and distribution of these filaments reveals that they are correlated with the spiral arms and make a significant contribution to star formation in the Galaxy. Massive star formation is ongoing within ∼20% of the filaments and is strongly correlated with the filaments with the largest mass-tolength ratios. The luminosity of the embedded sources has a similar distribution to the Galactic-wide samples of young massive stars and can therefore be considered to be representative.

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“…The above studies have also provided new clues as to the role of filaments in the onset of star formation for lowand high-mass stars (e.g., Arzoumanian et al 2011;Hill et al 2012). Latest results point towards a scenario in which prestellar cores form by gravitational fragmentation of unstable filaments ) with a quasi-constant width of ∼0.1 pc in the solar neighbourhood (Arzoumanian et al 2011), although with possible variations at farther distances (Schisano et al 2014).…”

Section: Introductionmentioning

confidence: 84%

Galactic cold cores

Rivera-Ingraham

Ristorcelli

Juvela

et al. 2016

A&A

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Context. The association of filaments with protostellar objects has made these structures a priority target in star formation studies. However, little is known about the link between filament properties and their local environment. Aims. The datasets from the Herschel Galactic Cold cores key programme allow for a statistical study of filaments with a wide range of intrinsic and environmental characteristics. Characterisation of this sample can therefore be used to identify key physical parameters and quantify the role of the environment in the formation of supercritical filaments. These results are necessary to constrain theoretical models of filament formation and evolution. Methods. Filaments were extracted from fields at distance D < 500 pc with the getfilaments algorithm and characterised according to their column density profiles and intrinsic properties. Each profile was fitted with a beam-convolved Plummer-like function, and the filament structure was quantified based on the relative contributions from the filament "core", represented by a Gaussian, and "wing" component, dominated by the power-law behaviour of the Plummer-like function. These filament parameters were examined for populations associated with different background levels. Results. Filaments increase their core (M line,core ) and wing (M line,wing ) contributions while increasing their total linear mass density (M line,tot ). Both components appear to be linked to the local environment, with filaments in higher backgrounds having systematically more massive M line,core and M line,wing . This dependence on the environment supports an accretion-based model of filament evolution in the local neighbourhood (D ≤ 500 pc). Structures located in the highest backgrounds develop the highest central A V , M line,core , and M line,wing as M line,tot increases with time, favoured by the local availability of material and the enhanced gravitational potential. Our results indicate that filaments acquiring a significantly massive central region with M line,core > ∼ M crit /2 may become supercritical and form stars. This translates into a need for filaments to become at least moderately self-gravitating to undergo localised star formation or become star-forming filaments.

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Resolving the Vela C ridge with P-ArTéMiS andHerschel

Cited by 37 publications

References 27 publications

Formation and evolution of interstellar filaments

Formation and evolution of interstellar filaments

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

Galactic cold cores

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