A 500 pc filamentary gas wisp in the disk of the Milky Way

Li, Guangxing; Wyrowski, F.; Menten, K. M.; Беллоче, А.

doi:10.1051/0004-6361/201322411

Cited by 58 publications

(75 citation statements)

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“…the 500 pc filamentary gas wisp from Li et al (2013) and the bubble N39 from Deharveng et al (2010). In addition, the secondary bubble N131-A (see Sect.…”

Section: How To Form Bubble N131?mentioning

confidence: 97%

“…Filamentary structures in molecular clouds are ubiquitous in the Milky Way, and have been identified from subparsec to kpc scale (Wang et al 2011;Jackson et al 2010;Li et al 2013;Peretto et al 2014;Ragan et al 2014;Goodman et al 2014). On the molecular cloud scale, filaments may form through converging flows (Csengeri et al 2011), shear (Smith et al 2014), the collision of shocked sheets (Padoan et al 2001 , and 4.5 μm (blue).…”

Section: Introductionmentioning

confidence: 99%

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N131: A dust bubble born from the disruption of a gas filament

Zhang

Wyrowski

et al. 2016

A&A

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Context. OB-type stars have strong ionizing radiation and drive energetic winds. The ultraviolet radiation from ionizing stars may heat dust and ionize gas to sweep up an expanding bubble shell. This shell may be the result of feedback leading to a new generation of stars. Aims. N131 is an infrared dust bubble residing in a molecular filament. We study the formation and fragmentation of this bubble with multiwavelength dust and gas observations. Methods. Towards the bubble N131, we analysed archival multiwavelength observations including 3.6, 4. 5, 5.8, 8.0, 24, 70, 160, 250, 350, 500 μm, 1.1 mm, and 21 cm. In addition, we performed new observations of CO (2-1), CO (1-0), and 13 CO (1-0) with the IRAM 30 m telescope. Results. Multiwavelength dust and gas observations reveal a ring-like shell with compact fragments, two filamentary structures, and the secondary bubble N131-A. Bubble N131 is a rare object with a large hole at 24 μm and 21 cm in the direction of its centre. The dust and gas clumps are compact and might have been compressed at the inner edge of the ring-like shell, while they are extended and might be pre-existing at the outer edge. The column density, excitation temperature, and velocity show a potentially hierarchical distribution from the inner to outer edge of the ring-like shell. We also detected the front and back sides of the secondary bubble N131-A in the direction of its centre. The derived Lyman-continuum ionizing photon flux within N131-A is equivalent to an O9.5 star. Based on the above, we suggest that the bubble N131 might be triggered by the strong stellar winds from a group of massive stars inside the bubble. Conclusions. We propose a scenario in which the bubble N131 forms from the disruption of a gas filament by the expansion of the H II region, strong stellar winds, and fragments under self-gravity.

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“…the 500 pc filamentary gas wisp from Li et al (2013) and the bubble N39 from Deharveng et al (2010). In addition, the secondary bubble N131-A (see Sect.…”

Section: How To Form Bubble N131?mentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

N131: A dust bubble born from the disruption of a gas filament

Zhang

Wyrowski

et al. 2016

A&A

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“…IRDC 18223 - Tackenberg et al 2014;G351 -Leurini et al 2011, both of which appear in our catalogue). However, there have also been a number of much larger and more massive filamentary structures recently reported in the literature; these can be several hundreds of parsecs in length and have masses ∼10 5 M (Ragan et al 2014;Jackson et al 2010;Battersby et al 2014;Li et al 2013;Wang et al 2014). Many of these have been initially found from visual inspection of mid-infrared images with the aim of identifying coherent filamentary patterns Tables 2 and 3 presented by Ragan et al (2014) and includes a few similar structures reported in the literature.…”

Section: Filamentary Structures In the Galaxymentioning

confidence: 99%

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

Urquhart

Leurini

et al. 2016

A&A

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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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“…Similarly we can observe features such as shells and interstellar filaments on scales of 10's pcs, again lying between the scales of star formation and galaxies typically adopted for simulations. These appear to be ubiquitous across the ISM, but recent observations have highlighted the existence of extremely long, > 100 E-mail: dobbs@astro.ex.ac.uk pc thin filaments along spiral arms and inter-arm regions (Li et al 2013;Ragan et al 2014;Wang et al 2014;Goodman et al 2014).…”

Section: Introductionmentioning

confidence: 99%

The interstellar medium and star formation on kpc size scales

Dobbs

2015

Monthly Notices of the Royal Astronomical Society

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By resimulating a region of a global disc simulation at higher resolution, we resolve and study the properties of molecular clouds with a range of masses from a few 100's M to 10 6 M . The purpose of our paper is twofold, i) to compare the ISM and GMCs at much higher resolution compared to previous global simulations, and ii) to investigate smaller clouds and characteristics such as the internal properties of GMCs which cannot be resolved in galactic simulations. We confirm the robustness of cloud properties seen in previous galactic simulations, and that these properties extend to lower mass clouds, though we caution that velocity dispersions may not be measured correctly in poorly resolved clouds. We find that the properties of the clouds and ISM are only weakly dependent on the details of local stellar feedback, although stellar feedback is important to produce realistic star formation rates and agreement with the Schmidt-Kennicutt relation. We study internal properties of GMCs resolved by 10 4 − 10 5 particles. The clouds are highly structured, but we find clouds have a velocity dispersion radius relationship which overall agrees with the Larson relation. The GMCs show evidence of multiple episodes of star formation, with holes corresponding to previous feedback events and dense regions likely to imminently form stars. Our simulations show clearly long filaments, which are seen predominantly in the inter-arm regions, and shells.

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A 500 pc filamentary gas wisp in the disk of the Milky Way

Cited by 58 publications

References 61 publications

N131: A dust bubble born from the disruption of a gas filament

N131: A dust bubble born from the disruption of a gas filament

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

The interstellar medium and star formation on kpc size scales

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