Co Observations and Investigation of Triggered Star Formation Toward the N10 Infrared Bubble and Surroundings

Gama, Diana Renata Gonçalves; Lépine, J. R. D.; Mendoza, Edgar; Wu, Yuefang; Yuan, Jinghua

doi:10.3847/0004-637x/830/2/57

Cited by 8 publications

(4 citation statements)

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“…Proposed examples of triggered star formation abound in the literature over a variety of scales. In particular, the high quality infrared observations from the Spitzer and Herschel space observatories over the last decade and a half have provided abundant support for the actual existence of triggered star formation along the edges of bubble-like HII regions (Deharveng & Zavagno 2011;Samal et al 2014;Liu et al 2016;Gama et al 2016;Cichowolski et al 2018). Examples at larger scales where star formation appears to have been caused by expanding supershells seen in HI in the disk of our Galaxy also exist (Megeath et al 2003;Oey et al 2005;Arnal & Corti 2007;Lee & Chen 2009), although the evidence is more elusive, largely due to confusion and crowdedness along the line of sight.…”

Section: Discussionmentioning

confidence: 99%

The possible common origin of M 16 and M 17

Comerón

Torra

2018

A&A

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Context. It has been suggested that the well-studied giant HII regions M16 and M17 may have had a common origin, being an example of large-scale triggered star formation. While some features of the distribution of the interstellar medium in the region support this interpretation, no definitive detection of an earlier population of massive stars responsible for the triggering has been made thus far. Aims. We have carried out observations looking for red supergiants in the area covered by a giant shell seen in HI and CO centered on galactic coordinates l ∼ 14 • 5, b ∼ +1 • that peaks near the same radial velocity as the bulk of the emission from both giant HII regions, which are located along the shell. Red supergiants have ages in the range expected for the parent association whose most massive members could have triggered the formation of the shell and of the giant HII regions along its rim. Methods. We have obtained spectroscopy in the visible of a sample of red stars selected on the basis of their infrared colors, whose magnitudes are consistent with them being red supergiants if they are located at the distance of M16 and M17. Spectroscopy is needed to distinguish red supergiants from AGB stars and RGB stars, which are expected to be abundant along the line of sight.Results. Out of a sample of 37 bright red stars, we identify four red supergiants that confirm the existence of massive stars in the age range between ∼ 10 and ∼ 30 Myr in the area. At least three of them have Gaia DR2 parallaxes consistent with them being at the same distance as M16 and M17. Conclusions. The evidence of past massive star formation within the area of the gaseous shell lends support to the idea that it was formed by the combined action of stellar winds and ionizing radiation of the precursors of the current red supergiants. These could be the remnants of a richer population, whose most massive members have exploded already as core-collapse supernovae. The expansion of the shell against the surrounding medium, perhaps combined with the overrun of preexisting clouds, is thus a plausible trigger of the formation of a second generation of stars currently responsible for the ionization of M16 and M17.F. Comerón and J. Torra: On the possible common origin of M16 and M17 selection criteria and our findings, through which we produce a crude estimate of the overall massive star content of the association and the mechanical energy deposited in the bubble, which suggest that the scenario of triggered formation of M16 and M17 is indeed plausible.

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Section: Discussionmentioning

confidence: 99%

The possible common origin of M 16 and M 17

Comerón

Torra

2018

A&A

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“…To validate the reliability of the workflow, we selected a subregion within 10° l 20°& −5°.25 b 5°. 25 from the MWISP as experimental data, which includes some active high-mass star-forming regions (hereafter HSRs), such as M16 (Hill et al 2012;Tremblin et al 2014), M17 (Felli et al 1984;Chen et al 2021;Yin et al 2022), W31 (Beuther et al 2011;Gama et al 2016;Maity et al 2022), W33 (Messineo et al 2015;Tursun et al 2022), andW39 (Kerton et al 2013). At the same time, the infrared dust clumps of Herschel (Elia et al 2017) also cover the HSR, providing us with an opportunity to validate the Facet-SS-3D-Clump using data from different wavelength bands.…”

Section: Introductionmentioning

confidence: 99%

A Catalog of ¹³CO Clumps from the MWISP in l = 10°–20°

Luo,

Zheng,

Jiang

et al. 2024

Res. Astron. Astrophys.

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In this study, we comprehensively validate the effectiveness of a molecular clump detection workflow using 13CO data from the Milky Way Image Scroll Painting (MWISP) project, covering the inner Milky Way within the longitude range 10° ≤ l ≤ 20° and a latitude strip of |b| ≤ 5:25°. The workflow, namely Facet-SS-3D-Clump, initially employs FacetClumps to identify molecular clumps. Subsequently, high-confidence clumps are obtained by cross-matching with the clumps detected by other algorithms, such as Dendrogram. Then, these high-confidence clumps are used as prior knowledge to train a semi-supervised deep clustering approach, SS-3D-Clump, which is applied to verify candidate clumps detected by FacetClumps, providing confidence levels for the molecular clumps. Finally, a catalogue comprising 18,757 molecular clumps extracted from 13CO (J = 1 - 0) emission data was obtained using the workflow. By matching with Herschel infrared dust clumps, we found that 82.3% of the dust clumps correspond to 13CO clumps, which confirmed the accuracy of the workflow. The catalogue is 90% complete above 37 K km s-1. We observe a significant deviation of the mean Galactic latitude for clumps within|b| ≤ 2° from the midplane, with b = -0.110°. In the future, Facet-SS-3D-Clump will be applied to detect 13CO clumps in the entire MWISP data.In this study, we present a catalogue of molecular clumps extracted from 13CO (J = 1 - 0) emission data of the Milky Way Image Scroll Painting (MWISP) project. The data covers the inner MilkyWay within the longitude range 10° ≤ l ≤ 20° and the latitude strip of |b| ≤ 5:25°. The clumps extraction of workflow, namely Facet-SS-3D-Clump, consists of two parts: the identification of clumps candidates and their verification. First, Facet-SS-3D-Clump employs FacetClumps to identify clumps candidates. Subsequently, high-confidence clumps are obtained by cross-matching with the clumps detected by other algorithms, such as Dendrogram. Second, these high-confidence clumps are used as prior knowledge to train a semi-supervised deep clustering approach, SS-3D-Clump, which is applied to verify clumps candidates detected by FacetClumps, providing confidence levels for the molecular clumps. Finally, the catalogue comprising 18,757 molecular clumps was obtained using Facet-SS-3D-Clump, and the catalogue is 90% complete above 37 K km s-1. We observe a significant deviation of the mean Galactic latitude for clumps within |b| ≤ 2° from the midplane, with b = -0.110°. We found that 82.3% of the dust clumps correspond to 13CO clumps by matching with Herschel infrared dust clumps. In the future, Facet-SS-3D-Clump will be applied to detect 13CO clumps in the entire MWISP data.

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“…证据. 例如, 2016 年, Yan等人 [11] 利用 12 CO, 13 CO, [25] , N10 [26] , N14 [27] , N22 [27,28] , N46 [29] , N49 [1,30,31] , N65 [32] , N68 [33] , N74 [27] , N131 [34,35] , S24 [36] , S51 [37] , CN20 [38] , CN107 [39] , CN109 [39] , CN148 [40] , RCW120 [41] , G24.136+00.436 [42] 等做了相关的研究工作. 压缩到一起, 形成一致密的壳层结构.…”

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