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dc.contributor.author
Dewangan, L. K.
dc.contributor.author
Ojha, D. K.
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Sharma, Saurabh
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del Palacio, Santiago
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Bhadari, N. K.
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Das, A.
dc.date.available
2021-08-19T12:52:39Z
dc.date.issued
2020-11
dc.identifier.citation
Dewangan, L. K.; Ojha, D. K.; Sharma, Saurabh; del Palacio, Santiago; Bhadari, N. K.; et al.; New Insights into the HII Region G18.88-0.49: Hub-Filament System and Accreting Filaments; IOP Publishing; Astrophysical Journal; 903; 1; 11-2020
dc.identifier.issn
0004-637X
dc.identifier.uri
http://hdl.handle.net/11336/138510
dc.description.abstract
We present an analysis of multiwavelength observations of an area of 0.°27 × 0.°27 around the Galactic H ii region G18.88-0.49, which is powered by an O-type star (age ∼ 105 yr). The Herschel column density map reveals a shell-like feature of extension ∼12 pc × 7 pc and mass ∼2.9 × 104 M o˙ around the H ii region; its existence is further confirmed by the distribution of molecular (12CO, 13CO, C18O, and NH3) gas at [60, 70] km s-1. Four subregions are studied toward this shell-like feature and show a mass range of ∼0.8-10.5 × 103 M o˙. These subregions associated with dense gas are dominated by nonthermal pressure and supersonic nonthermal motions. The shell-like feature is associated with the H ii region, Class I protostars, and a massive protostar candidate, illustrating the ongoing early phases of star formation (including massive stars). The massive protostar is found toward the position of the 6.7 GHz methanol maser, and is associated with outflow activity. Five parsec-scale filaments are identified in the column density and molecular maps and appear to be radially directed to the dense parts of the shell-like feature. This configuration is referred to as a "hub-filament"system. Significant velocity gradients (0.8-1.8 km s-1 pc-1) are observed along each filament, suggesting that the molecular gas flows toward the central hub along the filaments. Overall, our observational findings favor a global nonisotropic collapse scenario as discussed in Motte et al., which can explain the observed morphology and star formation in and around G18.88-0.49.
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application/pdf
dc.language.iso
eng
dc.publisher
IOP Publishing
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
H II regions
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Interstellar medium
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Star formation
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Pre-main sequence stars
dc.subject.classification
Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
New Insights into the HII Region G18.88-0.49: Hub-Filament System and Accreting Filaments
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2021-08-17T15:53:06Z
dc.journal.volume
903
dc.journal.number
1
dc.journal.pais
Reino Unido
dc.description.fil
Fil: Dewangan, L. K.. Physical Research Laboratory India; India
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Fil: Ojha, D. K.. International Centre Of Theoretical Science. Tata Institute Of Fundamental Research; España
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Fil: Sharma, Saurabh. Aryabhatta Research Institute Of Observational Sciences; India
dc.description.fil
Fil: del Palacio, Santiago. Universidad Nacional de La Plata; Argentina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
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Fil: Bhadari, N. K.. Indian Institute Of Technology Gandhinagar; India. Physical Research Laboratory India; India
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Fil: Das, A.. University Of Hyderabad; India
dc.journal.title
Astrophysical Journal
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.3847/1538-4357/abb827
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abb827
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