OGHReS: Large-scale filaments in the outer Galaxy

Colombo, D.; König, C.; Urquhart, J. S.; Wyrowski, F.; Mattern, M.; Menten, K. M.; Lee, M.-Y.; Brand, J.; Wienen, M.; Мазумдар, П.; Schüller, F.; Leurini, S.

doi:10.1051/0004-6361/202142182

Cited by 14 publications

(18 citation statements)

References 78 publications

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“…The interplay between gravity, magnetic fields, turbulence, radiation transport, chemistry and stellar feedback shapes the interstellar medium (ISM) into a complex web of structures with varying morphologies across multiple scales. Large-scale observational survey data have shown the prevalence of bubbles and ring-like structures associated with HII regions and super-shells seen in HI linked to multiple supernovae, as well as the connection between dense gas filaments and cores with the star formation process (McClure-Griffiths et al 2002;Churchwell et al 2006;Daigle, Joncas & Parizeau 2007;Molinari et al 2010;André et al 2010;Ehlerová & Palouš 2013;Schisano et al 2014;Li et al 2016;Rigby et al 2016;Arzoumanian et al 2019;Schisano et al 2020;Colombo et al 2021;Neralwar et al 2022). It is imperative for methods to readily identify and classify these features as it is only through understanding the formation of, connection between, and gas flows within these structures that a comprehensive picture of the ISM can be built (see Pineda et al 2022, for a recent review on the topic).…”

Section: Introductionmentioning

confidence: 99%

RJ-plots: An improved method to classify structures objectively

Clarke

Jaffa²,

Whitworth

2022

Monthly Notices of the Royal Astronomical Society

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The interstellar medium is highly structured, presenting a range of morphologies across spatial scales. The large data sets resulting from observational surveys and state-of-the-art simulations studying these hierarchical structures means that identification and classification must be done in an automated fashion to be efficient. Here we present RJ-plots, an improved version of the automated morphological classification technique J-plots developed by Jaffa et al. (2018). This method allows clear distinctions between quasi-circular/elongated structures and centrally over/under-dense structures. We use the recent morphological SEDIGISM catalogue of Neralwar et al. (2022) to show the improvement in classification resulting from RJ-plots, especially for ring-like and concentrated cloud types. We also find a strong correlation between the central concentration of a structure and its star formation efficiency and dense gas fraction, as well as a lack of correlation with elongation. Furthermore, we use the accreting filament simulations of Williams & Walch (2020) to highlight a multi-scale application of RJ-plots, finding that while spherical structures become more common at smaller scales they are never the dominant structure down to r ∼ 0.03 pc.

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Section: Introductionmentioning

confidence: 99%

RJ-plots: An improved method to classify structures objectively

Clarke

Jaffa²,

Whitworth

2022

Monthly Notices of the Royal Astronomical Society

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“…Surveys at multiwavelengths, e.g., infrared (IR) surveys (André et al 2010(André et al , 2014, high-resolution H I surveys (Soler et al 2020), and CO surveys (Colombo et al 2021;Yuan et al 2021), have revealed that filamentary structures are ubiquitous in the cold Galactic interstellar medium (ISM). The filaments are found to have lengths ranging from 0.1 pc to 1 kpc, containing gas mass of ∼10 3 -10 5 M e (Ragan et al 2014;Hacar et al 2018;Syed et al 2022).…”

Section: Introductionmentioning

confidence: 99%

CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50

Guo

Chen

Feng

et al. 2022

ApJ

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We present observations of the J = 1 – 0 transition lines of 12CO, 13CO, and C18O toward the Galactic region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50, using the Purple Mountain Observatory 13.7 m millimeter telescope. Based on the 13CO data, one main filament and five subfilaments are found together as a network structure in the velocity interval of [−42.5, −30.0] km s−1. The kinematic distance of this molecular cloud is estimated to be ∼4.5 kpc. The median length, width, excitation temperature, and line mass of these filaments are ∼49 pc, ∼2.9 pc, ∼8.9 K, and ∼39 M ⊙ pc−1, respectively. The velocity structures along these filaments exhibit oscillatory patterns, which are likely caused by the fragmentation or accretion process along these filaments. The maximum accretion rate is estimated to be ∼700 M ⊙ pc−1. A total of ∼162 13CO clumps and ∼103 young stellar objects are identified in this region. Most of the clumps are in gravitationally bound states. Three H ii regions (G154.359+2.606, SH2-211, and SH2-212) are found to be located in the apexes of the filaments. Intense star-forming activity is found along the entire filamentary cloud. The observed results may help us to better understand the link between filaments and massive star formation.

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“…The filamentary nature of molecular clouds is ubiquitous in the Galaxy and most of the star-forming clumps are situated in large scale filamentary structures (Schneider & Elmegreen 1979;Arzoumanian et al 2011;Polychroni et al 2013;Hacar et al 2013;Li et al 2016;Olmi et al 2016;Kainulainen et al 2017;Bresnahan et al 2018;Mattern et al 2018;Ballesteros-Paredes et al 2020;Arzoumanian et al 2022). The evolution of filaments is influenced by various mechanisms, e.g., ISM turbulence, shocked flows, supernovae feedback, galactic shear (Chen et al 2020;Colombo et al 2021). These filaments can be further classified into various types -e.g.…”

Section: Introductionmentioning

confidence: 99%

The SEDIGISM survey: Molecular cloud morphology

Neralwar

Colombo

Duarte-Cabral

et al. 2022

A&A

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The Structure, Excitation, and Dynamics of the Inner Galactic InterStellar Medium (SEDIGISM) survey has produced high (spatial and spectral) resolution 13 CO (2-1) maps of the Milky Way. It has allowed us to investigate the molecular interstellar medium in the inner Galaxy at an unprecedented level of detail and characterise it into molecular clouds. In a previous paper, we have classified the SEDIGISM clouds into four morphologies. However, how the properties of the clouds vary for these four morphologies is not well understood. Here, we use the morphological classification of SEDIGISM clouds to find connections between the cloud morphologies, their integrated properties, and their location on scaling relation diagrams. We observe that ring-like clouds show the most peculiar properties, having, on average, higher masses, sizes, aspect ratios and velocity dispersions compared to other morphologies. We speculate that this is related to the physical mechanisms that regulate their formation and evolution, for example, turbulence from stellar feedback can often results in the creation of bubble-like structures. We also see a trend of morphology with virial parameter whereby ring-like, elongated, clumpy and concentrated clouds have virial parameters in a decreasing order. Our findings provide a foundation for a better understanding of the molecular cloud behaviour based on their measurable properties.

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OGHReS: Large-scale filaments in the outer Galaxy

Cited by 14 publications

References 78 publications

RJ-plots: An improved method to classify structures objectively

RJ-plots: An improved method to classify structures objectively

CO(J = 1 – 0) Observations toward the Filamentary Cloud in the Galactic Region of 153.°60 ≤ l ≤ 156.°50 and 1.°85 ≤ b ≤ 3.°50

The SEDIGISM survey: Molecular cloud morphology

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