FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN). III. Possible evidence for formation of NGC 6618 cluster in M 17 by cloud–cloud collision

Nishimura, Atsushi; Minamidani, Tetsuhiro; Umemoto, Tomofumi; Fujita, Shinji; Matsuo, Mitsuhiro; Hattori, Yusuke; Kohno, Mikito; Yamagishi, Masao; Tsuda, Yuichi; Kuriki, Mika; Kuno, Nario; Torii, Kazufumi; Tsutsumi, Daichi; Okawa, Kazuki; Sano, Hidetoshi; Tachihara, Kengo; Ohama, Akio; Fukui, Y.

doi:10.1093/pasj/psx149

Cited by 42 publications

(5 citation statements)

References 116 publications

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“…The two observational signatures-the complementary spatial distributions and bridging features between the colliding clouds-have been suggested as evidence (e.g., Fukui et al 2021). Such evidence was detected in CCC regions both in the Galactic (e.g., Furukawa et al 2009;Ohama et al 2010;Fukui et al 2014;Torii et al 2015;Fukui et al 2016;Fujita et al 2021a;Fukui et al 2017a;Torii et al 2017a;Torii et al 2017b;Enokiya et al 2018;Hayashi et al 2018;Kohno et al 2018;Nishimura et al 2018;Sano et al 2018;Fujita et al 2021b;Fujita et al 2019;Fukui et al 2019;Torii et al 2021;Torii et al 2018b;Fukui et al 2021;Fujita et al 2021c) and extragalactic (e.g., Tokuda et al 2019;Sano et al 2021) objects.…”

Section: Introductionmentioning

confidence: 96%

Massive star formation in the Carina nebula complex and Gum 31. I. the Carina nebula complex

Fujita

Sano

Enokiya

et al. 2020

Publications of the Astronomical Society of Japan

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Herein, we present results from observations of the 12CO (J = 1–0), 13CO (J = 1–0), and 12CO (J = 2–1) emission lines toward the Carina nebula complex (CNC) obtained with the Mopra and NANTEN2 telescopes. We focused on massive-star-forming regions associated with the CNC including the three star clusters Tr 14, Tr 15, and Tr 16, and the isolated WR-star HD 92740. We found that the molecular clouds in the CNC are separated into mainly four clouds at velocities −27, −20, −14, and −8 km s−1. Their masses are 0.7 × 104 M$\odot$, 5.0 × 104 M$\odot$, 1.6 × 104 M$\odot$, and 0.7 × 104 M$\odot$, respectively. Most are likely associated with the star clusters, because of their high 12CO (J = 2–1)/12CO (J = 1–0) intensity ratios and their correspondence to the Spitzer 8 μm distributions. In addition, these clouds show the observational signatures of cloud–cloud collisions. In particular, there is a V-shaped structure in the position–velocity diagram and a complementary spatial distribution between the −20 km s−1 cloud and the −14 km s−1 cloud. Furthermore, we found that SiO emission, which is a tracer of a shocked molecular gas, is enhanced between the colliding clouds by using ALMA archive data. Based on these observational signatures, we propose a scenario wherein the formation of massive stars in the clusters was triggered by a collision between the two clouds. By using the path length of the collision and the assumed velocity separation, we estimate the timescale of the collision to be ∼1 Myr. This is comparable to the ages of the clusters estimated in previous studies.

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Section: Introductionmentioning

confidence: 96%

Massive star formation in the Carina nebula complex and Gum 31. I. the Carina nebula complex

Fujita

Sano

Enokiya

et al. 2020

Publications of the Astronomical Society of Japan

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“…A clear observational evidence of the actual cloud-cloud collisions was first discovered by Hasegawa et al (1994) toward the Sgr B2 giant molecular cloud. More recently, a number of evidences of cloud-cloud collisions have been found in many massive star forming regions (e.g., Higuchi et al 2009;Torii et al 2011;Nakamura et al 2014;Fukui et al 2018;Nishimura et al 2018), suggesting that the cloud-cloud collisions can be one of the major triggers of massive star formation.…”

Section: Introductionmentioning

confidence: 99%

Cloud–cloud collision in the DR 21 cloud as a trigger of massive star formation

Dobashi

Shimoikura

Katakura

et al. 2019

Publications of the Astronomical Society of Japan

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We report on a possible cloud-cloud collision in the DR 21 region, which we found through molecular observations with the Nobeyama 45-m telescope. We mapped an area of ∼ 8 × 12 around the region with twenty molecular lines including the 12 CO(J = 1−0) and 13 CO(J = 1−0) emission lines, and sixteen of them were significantly detected. Based on the 12 CO and 13 CO data, we found five distinct velocity components in the observed region, and we call molecular gas associated with these components "−42","−22", "−3", "9", and "17" km s −1 clouds taking after their typical radial velocities. The −3 km s −1 cloud is the main filamentary cloud (∼ 31,000 M ) associated with young massive stars such as DR21 and DR21(OH), and the 9 km s −1 cloud is a smaller cloud (∼ 3, 400 M ) which may be an extension of the W75 region in the north. The other clouds are much smaller. We found a clear anticorrelation in the distributions of the −3 and 9 km s −1 clouds, and detected faint 12 CO emission having intermediate velocities bridging the two clouds at their intersection. These facts strongly indicate that the two clouds are colliding against each other. In addition, we found that DR21 and DR21(OH) are located in the periphery of the densest part of the 9 km s −1 cloud, which is consistent with results of recent numerical simulations of cloud-cloud collisions. We therefore suggest that the −3 and 9 km s −1 clouds are colliding, and that the collision induced the massive star formation in the DR21 cloud. The interaction of the −3 and 9 km s −1 clouds was previously suggested by Dickel, Dickel, and Wilson (1978), and our results strongly support their hypothesis of the interaction.

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“…If one traces the whole gravitational collapse initiating by low density like 1000 cm −3 , the initial condition assumed by the monolithic collapse model might be hardly realised with self-gravity alone. This reasoning may be supported by the scenarios of a cloud-cloud collision in a number of star forming regions by the recent observational works including well known H regions M20, M42 and M17 (Torii et al 2017;Fukui et al 2018;Nishimura et al 2018), giant molecular clouds with mini-starbursts W43, W51, and Carina (Kohno et al 2021;Fujita et al 2021a,b), the Galactic centre (Enokiya et al 2021a;Tsuboi et al 2021), the Magellanic Clouds (Fukui et al 2017;Tsuge et al 2019), M33 (Sano et al 2021;Tokuda et al 2020;Kondo et al 2021), and the Antennae galaxies (Tsuge et al 2021a,b) as well as theoretical results of colliding molecular gas flows (Inoue & Fukui 2013;Inoue et al 2018;Fukui et al 2020a). See also Fukui et al (2020b) for a review of the related observational and theoretical works.…”

Section: Introductionmentioning

confidence: 59%

Evidence for a Cloud-Cloud Collision in Sh2-233 Triggering the Formation of the High-mass Protostar Object IRAS 05358+3543

Yamada,

Fukui,

Sano

et al. 2021

Preprint

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We have carried out a new kinematical analysis of the molecular gas in the Sh2-233 region by using the CO = 2-1 data taken at ∼0.5 pc resolution. The molecular gas consists of a filamentary cloud of 5-pc length with 1.5-pc width where two dense cloud cores are embedded. The filament lies between two clouds, which have a velocity difference of 2.6 km s −1 and are extended over ∼5 pc. We frame a scenario that the two clouds are colliding with each other and compressed the gas between them to form the filament in ∼0.5 Myr which is perpendicular to the collision. It is likely that the collision formed not only the filamentary cloud but also the two dense cores. One of the dense cores is associated with the high-mass protostellar candidate IRAS 05358+3543, a representative high-mass protostar. In the monolithic collapse scheme of high mass star formation, a compact dense core of 100 ⊙ within a volume of 0.1 pc radius is assumed as the initial condition, whereas the formation of such a core remained unexplained in the previous works. We argue that the proposed collision is a step which efficiently collects the gas of 100 ⊙ into 0.1 pc radius. This lends support for that the cloud-cloud collision is an essential process in forming the compact high-mass dense core, IRAS 05358+3543.

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FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN). III. Possible evidence for formation of NGC 6618 cluster in M 17 by cloud–cloud collision

Cited by 42 publications

References 116 publications

Massive star formation in the Carina nebula complex and Gum 31. I. the Carina nebula complex

Massive star formation in the Carina nebula complex and Gum 31. I. the Carina nebula complex

Cloud–cloud collision in the DR 21 cloud as a trigger of massive star formation

Evidence for a Cloud-Cloud Collision in Sh2-233 Triggering the Formation of the High-mass Protostar Object IRAS 05358+3543

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