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H II regions and high-mass starless clump candidates: II. Fragmentation and induced star formation at similar to 0.025 pc scale: an ALMA continuum study
Zhang, S.1; Zavagno, A.1,2; Lopez-Sepulcre, A.3,4; Liu, H.5,6,7; Louvet, F.8; Figueira, M.9; Russeil, D.1; Wu, Y.10; Yuan, J.11; Pillai, T. G. S.12,13
2021-02-05
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN0004-6361
Volume646Pages:28
AbstractContext. The ionization feedback from HII regions modifies the properties of high-mass starless clumps (HMSCs, of several hundred to a few thousand solar masses with a typical size of 0.1-1 pc), such as dust temperature and turbulence, on the clump scale. The question of whether the presence of HII regions modifies the core-scale (similar to 0.025 pc) fragmentation and star formation in HMSCs remains to be explored. Aims. We aim to investigate the difference of 0.025 pc-scale fragmentation between candidate HMSCs that are strongly impacted by HII regions and less disturbed ones. We also search for evidence of mass shaping and induced star formation in the impacted candidate HMSCs. Methods. Using the ALMA 1.3 mm continuum, with a typical angular resolution of 1.3 '', we imaged eight candidate HMSCs, including four impacted by HII regions and another four situated in the quiet environment. The less-impacted candidate HMSCs are selected on the basis of their similar mass and distance compared to the impacted ones to avoid any possible bias linked to these parameters. We carried out a comparison between the two types of candidate HMSCs. We used multi-wavelength data to analyze the interaction between HII regions and the impacted candidate HMSCs. Results. A total of 51 cores were detected in eight clumps, with three to nine cores for each clump. Within our limited sample, we did not find a clear difference in the similar to 0.025 pc-scale fragmentation between impacted and non-impacted candidate HMSCs, even though HII regions seem to affect the spatial distribution of the fragmented cores. Both types of candidate HMSCs present a thermal fragmentation with two-level hierarchical features at the clump thermal Jeans length lambda(th)(J,clump) and 0.3 lambda(th)(J,clump). The ALMA emission morphology of the impacted candidate HMSCs AGAL010.214-00.306 and AGAL018.931-00.029 sheds light on the capacities of HII regions to shape gas and dust in their surroundings and possibly to trigger star formation at similar to 0.025 pc-scale in candidate HMSCs. Conclusions. The fragmentation at similar to 0.025 pc scale for both types of candidate HMSCs is likely to be thermal-dominant, meanwhile HII regions probably have the capacity to assist in the formation of dense structures in the impacted candidate HMSCs. Future ALMA imaging surveys covering a large number of impacted candidate HMSCs with high turbulence levels are needed to confirm the trend of fragmentation indicated in this study.
Keywordstars: formation stars: massive HII regions ISM: structure submillimeter: ISM techniques: interferometric
Funding OrganizationALMA Region Center Grenoble ; ALMA Region Center Grenoble ; IRAM ; IRAM ; Institut Universitaire de France ; Institut Universitaire de France ; National Science Foundation ; National Science Foundation ; ASI (Agenzia Spaziale Italiana) ; ASI (Agenzia Spaziale Italiana) ; ALMA Region Center Grenoble ; ALMA Region Center Grenoble ; IRAM ; IRAM ; Institut Universitaire de France ; Institut Universitaire de France ; National Science Foundation ; National Science Foundation ; ASI (Agenzia Spaziale Italiana) ; ASI (Agenzia Spaziale Italiana) ; ALMA Region Center Grenoble ; ALMA Region Center Grenoble ; IRAM ; IRAM ; Institut Universitaire de France ; Institut Universitaire de France ; National Science Foundation ; National Science Foundation ; ASI (Agenzia Spaziale Italiana) ; ASI (Agenzia Spaziale Italiana) ; ALMA Region Center Grenoble ; ALMA Region Center Grenoble ; IRAM ; IRAM ; Institut Universitaire de France ; Institut Universitaire de France ; National Science Foundation ; National Science Foundation ; ASI (Agenzia Spaziale Italiana) ; ASI (Agenzia Spaziale Italiana)
DOI10.1051/0004-6361/202038421
WOS KeywordM QUIET CLUMPS ; GALACTIC PLANE ; MOLECULAR CLOUD ; COLUMN-DENSITY ; EVOLUTION ; GRAVITY ; MOTIONS ; DRIVEN ; CORES ; GAL
Language英语
Funding ProjectALMA Region Center Grenoble ; IRAM ; Institut Universitaire de France ; National Science Foundation[AST-2009842] ; ASI (Agenzia Spaziale Italiana)[I/038/080/0] ; ASI (Agenzia Spaziale Italiana)[I/029/12/0]
Funding OrganizationALMA Region Center Grenoble ; ALMA Region Center Grenoble ; IRAM ; IRAM ; Institut Universitaire de France ; Institut Universitaire de France ; National Science Foundation ; National Science Foundation ; ASI (Agenzia Spaziale Italiana) ; ASI (Agenzia Spaziale Italiana) ; ALMA Region Center Grenoble ; ALMA Region Center Grenoble ; IRAM ; IRAM ; Institut Universitaire de France ; Institut Universitaire de France ; National Science Foundation ; National Science Foundation ; ASI (Agenzia Spaziale Italiana) ; ASI (Agenzia Spaziale Italiana) ; ALMA Region Center Grenoble ; ALMA Region Center Grenoble ; IRAM ; IRAM ; Institut Universitaire de France ; Institut Universitaire de France ; National Science Foundation ; National Science Foundation ; ASI (Agenzia Spaziale Italiana) ; ASI (Agenzia Spaziale Italiana) ; ALMA Region Center Grenoble ; ALMA Region Center Grenoble ; IRAM ; IRAM ; Institut Universitaire de France ; Institut Universitaire de France ; National Science Foundation ; National Science Foundation ; ASI (Agenzia Spaziale Italiana) ; ASI (Agenzia Spaziale Italiana)
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000617516400001
PublisherEDP SCIENCES S A
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/79223
Collection中国科学院国家天文台
Corresponding AuthorZhang, S.
Affiliation1.Aix Marseille Univ, LAM, CNES, CNRS, Marseille, France
2.Inst Univ France IUF, Paris, France
3.Univ Grenoble Alpes, Inst Planetol & Astrophys Grenoble IPAG, CNRS, F-38000 Grenoble, France
4.Inst Radioastron Millimetr IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France
5.Yunnan Univ, Dept Astron, Kunming 650091, Yunnan, Peoples R China
6.China Chile Joint Ctr Astron, CASSACA, Camino El Observ 1515, Santiago, Chile
7.Univ Concepcion, Dept Astron, Av Esteban Iturra S-N,Dist Univ 160-C, Concepcion, Chile
8.Univ Chile, Dept Astron Chile, Santiago, Chile
9.Natl Ctr Nucl Res, Ul Pasteura 7, PL-02093 Warsaw, Poland
10.Peking Univ, Dept Astron, Beijing 100871, Peoples R China
11.Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China
12.Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA
13.Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany
Recommended Citation
GB/T 7714
Zhang, S.,Zavagno, A.,Lopez-Sepulcre, A.,et al. H II regions and high-mass starless clump candidates: II. Fragmentation and induced star formation at similar to 0.025 pc scale: an ALMA continuum study[J]. ASTRONOMY & ASTROPHYSICS,2021,646:28.
APA Zhang, S..,Zavagno, A..,Lopez-Sepulcre, A..,Liu, H..,Louvet, F..,...&Pillai, T. G. S..(2021).H II regions and high-mass starless clump candidates: II. Fragmentation and induced star formation at similar to 0.025 pc scale: an ALMA continuum study.ASTRONOMY & ASTROPHYSICS,646,28.
MLA Zhang, S.,et al."H II regions and high-mass starless clump candidates: II. Fragmentation and induced star formation at similar to 0.025 pc scale: an ALMA continuum study".ASTRONOMY & ASTROPHYSICS 646(2021):28.
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