G133.50+9.01: a likely cloud–cloud collision complex triggering the formation of filaments, cores, and a stellar cluster

Issac, Namitha; Tej, Anandmayee; Wu, Yuefang

doi:10.1093/mnras/staa3061

Cited by 6 publications

(10 citation statements)

References 53 publications

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“…While some proposed bridging features are remarkably similar to those in the Haworth et al (2015a) simulations (Torii et al 2011), others are much less clear-cut (e.g. Issac et al 2020, although we note that those authors present a significant quantity of other evidence in favour of a cloud collision).…”

supporting

confidence: 62%

Molecular line signatures of cloud–cloud collisions

Priestley

Whitworth

2021

Monthly Notices of the Royal Astronomical Society

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Collisions between interstellar gas clouds are potentially an important mechanism for triggering star formation. This is because they are able to rapidly generate large masses of dense gas. Observationally, cloud collisions are often identified in position-velocity (PV) space through bridging features between intensity peaks, usually of CO emission. Using a combination of hydrodynamical simulations, time-dependent chemistry, and radiative transfer, we produce synthetic molecular line observations of overlapping clouds that are genuinely colliding, and overlapping clouds that are just chance superpositions. Molecules tracing denser material than CO, such as NH3 and HCN, reach peak intensity ratios of 0.5 and 0.2 with respect to CO in the ‘bridging feature’ region of PV space for genuinely colliding clouds. For overlapping clouds that are just chance superpositions, the peak NH3 and HCN intensities are co-located with the CO intensity peaks. This represents a way of confirming cloud collisions observationally, and distinguishing them from chance alignments of unrelated material.

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supporting

confidence: 62%

Molecular line signatures of cloud–cloud collisions

Priestley

Whitworth

2021

Monthly Notices of the Royal Astronomical Society

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“…The first cluster to be identified as a possible collision object was Westerland 2, which harbors two associated clouds with a velocity difference of 20 km s −1 (Furukawa et al 2009;Ohama et al 2010) approximately. Other recent observations by Fukui et al (2014), Torii et al (2015), Baug et al (2016), Dewangan & Ojha (2017), Dewangan et al (2018Dewangan et al ( , 2019, Issac et al (2020) have also detected CCCs in the high-mass star forming regions.…”

Section: Introductionmentioning

confidence: 71%

Gas dynamics in the star forming region G18.148$-$0.283: Is it a manifestation of two colliding molecular clouds?

Dey,

Pandian,

Lal

2021

Preprint

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We report the results obtained from a multi-wavelength study of the HII region, G18.148−0.283, using the upgraded Giant Metre-wave Radio Telescope (uGMRT) at 1350 MHz along with other archival data. In addition to the radio continuum emission, we have detected the H169α and H170α radio recombination lines towards G18.148−0.283 using a correlator bandwidth of 100 MHz. The moment-1 map of the ionized gas reveals a velocity gradient of approximately 10 km s −1 across the radio continuum peaks. The 12 CO (J=3−2) molecular line data from the COHRS survey also shows the presence of two velocity components that are very close to the velocities detected in the ionized gas. The spectrum and position-velocity diagram from CO emission reveal molecular gas at an intermediate velocity range bridging the velocity components. We see mid-infrared absorption and far-infrared emission establishing the presence of a filamentary infrared dark cloud, the extent of which includes the targeted HII region. The magnetic field inferred from dust polarization is perpendicular to the filament within the HII region. We have also identified two O9 stars and 30 young stellar objects towards the target using data from the 2MASS, UKIDSS, and GLIMPSE surveys. Cumulatively, this suggests that the region is the site of a cloud-cloud collision that has triggered massive star formation and subsequent formation of an HII region.

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“…Simulations of Haworth et al (2015a,b) suggested that a broad intermediate-velocity feature that bridges between two colliding clouds will appear in a PV diagram. The bridge feature probes the turbulent motion of the gas enhanced by the collision and often appears at the spots of collisions (Issac et al 2020;Gong et al 2017). The increased velocity dispersion along the U-shape, especially at the bottom where the compressed layer formed (see the top right panel of Fig.…”

Section: Bridgementioning

confidence: 96%

“…First, we examined whether G323.18a and G323.18b are gravitationally bound as one structure. The virial mass was determined using the expression (Pillai et al 2011;Issac et al 2020)…”

Section: Signatures Of Cccsmentioning

confidence: 99%

“…The actual collision velocity might be higher because of projection effects. As pro-pounded by Issac et al (2020), Fukui (2013), andFukui et al (2015), independent of the angle of two colliding clouds, the isotropic turbulence is enhanced at the collision-shocked layer. This is consistent with the fact that the velocity dispersion increases greatly along the U-shape structure (see the top right panel of Fig.…”

Section: Complementary Distribution and U-shapementioning

confidence: 99%

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Cloud-cloud collision and star formation in G323.18+0.15

Zhou

Esimbek

et al. 2022

A&A

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We studied the cloud-cloud collision candidate G323.18+0.15 based on signatures of induced filaments, clumps, and star formation. We used archival molecular spectrum line data from the SEDIGISM 13 CO (J = 2-1) survey, from the Mopra southern Galactic plane CO survey, and infrared to radio data from the GLIMPSE, MIPS, Hi-GAL, and SGPS surveys. Our new result shows that the G323.18+0.15 complex is 3.55 kpc away from us and consists of three cloud components, G323.18a, G323.18b, and G323.18c. G323.18b shows a perfect U-shape structure, which can be fully complemented by G323.18a, suggesting a collision between G323.18a and the combined G323.18bc filamentary structure. One dense compressed layer (filament) is formed at the bottom of G323.18b, where we detect a greatly increased velocity dispersion. The bridge with an intermediate velocity in a position-velocity diagram appears between G323.18a and G323.18b, which corresponds to the compressed layer. G323.18a plus G323.18b as a whole are probably not gravitationally bound. This indicates that high-mass star formation in the compressed layer may have been caused by an accidental event. The column density in the compressed layer of about 1.36 × 10 22 cm −2 and most of the dense clumps and highmass stars are located there. The average surface density of class I and class II young stellar objects (YSOs) inside the G323.18+0.15 complex is much higher than the density in the surroundings. The timescale of the collision between G323.18a and G323.18b is 1.59 Myr. This is longer than the typical lifetime of class I YSOs and is comparable to the lifetime of class II YSOs.

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G133.50+9.01: a likely cloud–cloud collision complex triggering the formation of filaments, cores, and a stellar cluster

Cited by 6 publications

References 53 publications

Molecular line signatures of cloud–cloud collisions

Molecular line signatures of cloud–cloud collisions

Gas dynamics in the star forming region G18.148$-$0.283: Is it a manifestation of two colliding molecular clouds?

Cloud-cloud collision and star formation in G323.18+0.15

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