Simultaneous Evidence of Edge Collapse and Hub-filament Configurations: A Rare Case Study of a Giant Molecular Filament, G45.3+0.1

Bhadari, N. K.; Dewangan, L. K.; Ojha, D. K.; Pirogov, L. E.; Maity, A. K.

doi:10.3847/1538-4357/ac65e9

Cited by 15 publications

(8 citation statements)

References 84 publications

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“…The algorithm disintegrates the astronomical image into its structural components (i.e., sources and filaments) and splits these components from each other and their backgrounds. One can find more details of the algorithm in Menʼshchikov (2021) (see also Bhadari et al 2022). The algorithm needs a single user-defined input, which is the maximum size of the structure to be extracted (for both filaments and sources).…”

Section: Hub-filament Systems In W31mentioning

confidence: 99%

Unraveling the Observational Signatures of Cloud–Cloud Collision and Hub-filament Systems in W31

Maity

Dewangan

Sano

et al. 2022

ApJ

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To understand the formation process of massive stars, we present a multiscale and multiwavelength study of the W31 complex hosting two extended H ii regions (i.e., G10.30-0.15 (hereafter, W31-N) and G10.15-0.34 (hereafter, W31-S)) powered by a cluster of O-type stars. Several Class i protostars and a total of 49 ATLASGAL 870 μm dust clumps (at d = 3.55 kpc) are found toward the H ii regions where some of the clumps are associated with the molecular outflow activity. These results confirm the existence of a single physical system hosting the early phases of star formation. The Herschel 250 μm continuum map shows the presence of a hub-filament system (HFS) toward both W31-N and W31-S. The central hubs harbor H ii regions and they are depicted with extended structures (with T d ∼ 25–32 K) in the Herschel temperature map. In the direction of W31-S, an analysis of the NANTEN2 12CO(J = 1−0) and SEDIGISM 13CO(J = 2−1) line data supports the presence of two cloud components around 8 and 16 km s−1, and their connection in velocity space. A spatial complementary distribution between the two cloud components is also investigated toward W31-S, where the signposts of star formation, including massive O-type stars, are concentrated. These findings favor the applicability of cloud–cloud collision (CCC) around ∼2 Myr ago in W31-S. Overall, our observational findings support the theoretical scenario of CCC in W31, which explains the formation of massive stars and the existence of HFSs.

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Section: Hub-filament Systems In W31mentioning

confidence: 99%

Unraveling the Observational Signatures of Cloud–Cloud Collision and Hub-filament Systems in W31

Maity

Dewangan

Sano

et al. 2022

ApJ

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“…The role of the filaments in the star formation processes is yet to be known. The zones where filaments either merge or collide with each other, are considered as appropriate environment for the formation of star clusters (André et al 2010(André et al , 2014Nakamura et al 2012Nakamura et al , 2014Henshaw et al 2013;Dewan-gan et al 2017Dewan-gan et al , 2019Bhadari et al 2022;Maity et al 2022). These zones are known as 'hub' and such system is known as 'hub-filamentary system' (HFS).…”

Section: Introductionmentioning

confidence: 99%

“…This scenario is of interest for many recent investigation which is possible after the availability of high quality Herschel data along with velocity information from the CO maps (Goicoechea et al 2015;Dewangan et al 2016Dewangan et al , 2022bWang & Hwang 2020). But, till now, such process has been reported in a few starforming sites (for e.g., Dewangan et al , 2019Bhadari et al 2020Bhadari et al , 2022.…”

Section: Introductionmentioning

confidence: 99%

Kronberger 55: A Candidate for End-dominated Collapse Scenario

Verma¹,

Sharma²,

Dewangan³

et al. 2023

Preprint

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Using optical photometric observations from 1.3m Devasthal Fast Optical Telescope and deep near-infrared (NIR) photometric observations from TANSPEC mounted on 3.6m Devasthal Optical Telescope, along with the multi-wavelength archival data, we present our study of open cluster Kronberger 55 to understand the star formation scenario in the region. The distance, extinction and age of the cluster Kronberger 55 are estimated as ∼3.5 kpc, E(B − V) ∼1.0 mag and 5 Myr, respectively. We identified Young Stellar Objects (YSOs) based on their excess infrared (IR) emission using the two-color diagrams (TCDs). The mid-infrared (MIR) images reveal the presence of extended structure of dust and gas emission along with the outflow activities in the region with two peaks, one at the location of cluster Kronberger 55 and another at 5 .35 southwards to it. The association of radio continuum emission with the southern peak, hints towards the formation of massive star/s. The Herschel sub-millimeter maps reveal the presence of two clumps connected with a filamentary strcuture in this region, and such configuration is also evident in the 12 CO(1 − 0) emission map. Our study suggests that this region might be a hub-filament system undergoing star formation due to the 'end-dominated collapse scenario'.

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“…In SFRs, a system of filaments converging to a central hub, which is referred to as a hub-filament system (HFS; Myers 2009), is a commonly observed feature, where young stellar objects (YSOs) and massive OB-stars (M 8 M ⊙ ) are born. Furthermore, researchers have also iden-Corresponding author: L. K. Dewangan Email: lokeshd@prl.res.in tified isolated filaments undergoing end-dominated collapse (EDC) or edge-collapse (Bastien 1983;Pon et al 2012;Clarke & Whitworth 2015), and observational evidence of such EDC filaments is gradually increasing in the literature (e.g., NGC 6334 (Zernickel et al 2013), Sh 2-242 (or S242; Dewangan et al 2019;Yuan et al 2020), IC 5146 (Wang et al 2019;Chung et al 2022), Monoceros R1 (or Mon R1; Bhadari et al 2020), G341.244-00.265 (Yu et al 2019), and G45.3+0.1 (Bhadari et al 2022)). Using multi-wavelength approach, a few SFRs are identified and reported, where the edge-collapse and the HFSs are simultaneously investigated (e.g., G45.3+0.1 (Bhadari et al 2022); IC 5146 dark Streamer (Wang et al 2019;Chung et al 2022)).…”

Section: Introductionmentioning

confidence: 99%

“…Furthermore, researchers have also iden-Corresponding author: L. K. Dewangan Email: lokeshd@prl.res.in tified isolated filaments undergoing end-dominated collapse (EDC) or edge-collapse (Bastien 1983;Pon et al 2012;Clarke & Whitworth 2015), and observational evidence of such EDC filaments is gradually increasing in the literature (e.g., NGC 6334 (Zernickel et al 2013), Sh 2-242 (or S242; Dewangan et al 2019;Yuan et al 2020), IC 5146 (Wang et al 2019;Chung et al 2022), Monoceros R1 (or Mon R1; Bhadari et al 2020), G341.244-00.265 (Yu et al 2019), and G45.3+0.1 (Bhadari et al 2022)). Using multi-wavelength approach, a few SFRs are identified and reported, where the edge-collapse and the HFSs are simultaneously investigated (e.g., G45.3+0.1 (Bhadari et al 2022); IC 5146 dark Streamer (Wang et al 2019;Chung et al 2022)). In such cases, an HFS is observed toward each edge of the EDC filament.…”

Section: Introductionmentioning

confidence: 99%

IC 5146 Dark Streamer: The First Reliable Candidate of Edge Collapse, Hub-filament Systems, and Intertwined Sub-filaments

Dewangan

Bhadari

Chung

et al. 2023

ApJ

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The paper presents an analysis of multiwavelength data of a nearby star-forming site, the IC 5146 dark streamer (d ∼ 600 pc), which has been treated as a single and long filament, fl. Two hub-filament systems (HFSs) are known to exist toward the eastern and the western ends of fl. Earlier published results favor simultaneous evidence of HFSs and end-dominated collapse (EDC) in fl. A Herschel column density map (resolution ∼13.″5) reveals two intertwined sub-filaments (i.e., fl-A and fl-B) toward fl, displaying a nearly double helix-like structure. This picture is also supported by the C18O(3–2) emission. The fray and fragment scenario may explain the origin of intertwined sub-filaments. In the direction of fl, two cloud components around 2 and 4 km s−1 are depicted using 13CO(1–0) and C18O(1–0) emission and are connected in velocity space. The HFSs are spatially found at the overlapping areas of these cloud components and can be explained by the cloud–cloud collision scenario. Nonthermal gas motion in fl with a larger Mach number is found. The magnetic field position angle measured from the filament’s long axis shows a linear trend along the filament. This signature is confirmed in the other nearby EDC filaments, presenting a more quantitative confirmation of the EDC scenario. Based on our observational outcomes, we witness multiple processes operational in the IC 5146 streamer. Overall, the streamer can be recognized as the first reliable candidate for edge collapse, HFSs, and intertwined sub-filaments.

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Simultaneous Evidence of Edge Collapse and Hub-filament Configurations: A Rare Case Study of a Giant Molecular Filament, G45.3+0.1

Cited by 15 publications

References 84 publications

Unraveling the Observational Signatures of Cloud–Cloud Collision and Hub-filament Systems in W31

Unraveling the Observational Signatures of Cloud–Cloud Collision and Hub-filament Systems in W31

Kronberger 55: A Candidate for End-dominated Collapse Scenario

IC 5146 Dark Streamer: The First Reliable Candidate of Edge Collapse, Hub-filament Systems, and Intertwined Sub-filaments

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