Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/29106
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Sokolov, Vlas | en_US |
dc.contributor.author | Wang, Ke | en_US |
dc.contributor.author | Pineda, Jaime E. | en_US |
dc.contributor.author | Caselli, Paola | en_US |
dc.contributor.author | Henshaw, Jonathan D. | en_US |
dc.contributor.author | Barnes, Ashley T. | en_US |
dc.contributor.author | Tan, Jonathan C. | en_US |
dc.contributor.author | FONTANI, FRANCESCO | en_US |
dc.contributor.author | Jiménez-Serra, Izaskun | en_US |
dc.date.accessioned | 2020-12-22T15:20:53Z | - |
dc.date.available | 2020-12-22T15:20:53Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29106 | - |
dc.description.abstract | To probe the initial conditions for high-mass star and cluster formation, we investigate the properties of dense filaments within the infrared dark cloud (IRDC) G035.39-00.33 (G035.39) in a combined Very Large Array and Green Bank Telescope mosaic tracing the NH<SUB>3</SUB> (1, 1) and (2, 2) emission down to 0.08 pc scales. Using agglomerative hierarchical clustering on multiple line-of-sight velocity component fitting results, we identify seven extended velocity-coherent components in our data, likely representing spatially coherent physical structures, some exhibiting complex gas motions. The velocity gradient magnitude distribution peaks at its mode of 0.35 and has a long tail extending into higher values of 1.5-2 , and it is generally consistent with those found toward the same cloud in other molecular tracers and with the values found toward nearby low-mass dense cloud cores at the same scales. Contrary to observational and theoretical expectations, we find the nonthermal ammonia line widths to be systematically narrower (by about 20%) than those of N<SUB>2</SUB>H<SUP>+</SUP> (1-0) line transition observed with similar resolution. If the observed ordered velocity gradients represent the core envelope solid-body rotation, we estimate the specific angular momentum to be about 2 × 10<SUP>21</SUP> cm<SUP>2</SUP> s<SUP>-1</SUP>, similar to the low-mass star-forming cores. Together with the previous finding of subsonic motions in G035.39, our results demonstrate high levels of similarity between kinematics of a high-mass star-forming IRDC and the low-mass star formation regime. | en_US |
dc.language.iso | eng | en_US |
dc.title | Multicomponent Kinematics in a Massive Filamentary Infrared Dark Cloud | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/aafaff | en_US |
dc.identifier.scopus | 2-s2.0-85062006030 | en_US |
dc.identifier.isi | 000458126700008 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/aafaff | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 872 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 30 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 9 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2019ApJ...872...30S | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0003-0348-3418 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
1812.09581.pdf | preprint | 5.42 MB | Adobe PDF | View/Open |
Sokolov_2019_ApJ_872_30.pdf | pdf editoriale | 17.34 MB | Adobe PDF | View/Open |
29106-Sokolov_2019_ApJ_872_30_P01.pdf | Miur | 9.58 MB | Adobe PDF | |
29106-Sokolov_2019_ApJ_872_30_P02.pdf | Miur | 7.82 MB | Adobe PDF |
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