Resolving the Vela C ridge with P-ArTeMiS and Herschel
We present APEX/P-ArTéMiS 450\mu m continuum observations of RCW 36 and the adjacent ridge, a high-mass high-column density filamentary structure at the centre of the Vela C molecular cloud. These observations, at higher resolution than Herschel's SPIRE camera, reveal clear fragmentation of the...
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| creator | Hill, T Andre, Ph Arzoumanian, D Motte, F Minier, V Menshchikov, A Didelon, P Hennemann, M Konyves, V Nguyen-Luong, Q Palmeirim, P Peretto, N Schneider, N Bontemps, S Louvet, F Elia, D Giannini, T Reveret, V J Le Pennec Rodriguez, L Boulade, O Doumayrou, E Dubreuil, D Gallais, P Lortholary, M Martignac, J Talvard, M De Breuck, C |
| description | We present APEX/P-ArTéMiS 450\mu m continuum observations of RCW 36 and the adjacent ridge, a high-mass high-column density filamentary structure at the centre of the Vela C molecular cloud. These observations, at higher resolution than Herschel's SPIRE camera, reveal clear fragmentation of the central star-forming ridge. Combined with PACS far-infrared and SPIRE sub-millimetre observations from the Herschel HOBYS project we build a high resolution column density map of the region mapped with P-ArTéMiS. We extract the radial density profile of the Vela C ridge which with a ~ 0.1pc central width is consistent with that measured for low-mass star-forming filaments in the Herschel Gould Belt survey. Direct comparison with Serpens South, of the Gould Belt Aquila complex, reveals many similarities between the two regions. Despite likely different formation mechanisms and histories, the Vela C ridge and Serpens South filament share common characteristics, including their filament central widths. |
| doi_str_mv | 10.48550/arxiv.1211.0275 |
| format | Article |
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These observations, at higher resolution than Herschel's SPIRE camera, reveal clear fragmentation of the central star-forming ridge. Combined with PACS far-infrared and SPIRE sub-millimetre observations from the Herschel HOBYS project we build a high resolution column density map of the region mapped with P-ArTéMiS. We extract the radial density profile of the Vela C ridge which with a ~ 0.1pc central width is consistent with that measured for low-mass star-forming filaments in the Herschel Gould Belt survey. Direct comparison with Serpens South, of the Gould Belt Aquila complex, reveals many similarities between the two regions. 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Andre, Ph ; Arzoumanian, D ; Motte, F ; Minier, V ; Menshchikov, A ; Didelon, P ; Hennemann, M ; Konyves, V ; Nguyen-Luong, Q ; Palmeirim, P ; Peretto, N ; Schneider, N ; Bontemps, S ; Louvet, F ; Elia, D ; Giannini, T ; Reveret, V ; J Le Pennec ; Rodriguez, L ; Boulade, O ; Doumayrou, E ; Dubreuil, D ; Gallais, P ; Lortholary, M ; Martignac, J ; Talvard, M ; De Breuck, C</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a519-b014311fd7cdfc31c4268638853c51d478476697207f362bf3cb88f7ee85ee4f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2012</creationdate><topic>Columnar structure</topic><topic>Density</topic><topic>Filaments</topic><topic>Low mass stars</topic><topic>Molecular clouds</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Space telescopes</topic><topic>Star formation</topic><toplevel>online_resources</toplevel><creatorcontrib>Hill, T</creatorcontrib><creatorcontrib>Andre, Ph</creatorcontrib><creatorcontrib>Arzoumanian, D</creatorcontrib><creatorcontrib>Motte, F</creatorcontrib><creatorcontrib>Minier, V</creatorcontrib><creatorcontrib>Menshchikov, A</creatorcontrib><creatorcontrib>Didelon, P</creatorcontrib><creatorcontrib>Hennemann, M</creatorcontrib><creatorcontrib>Konyves, V</creatorcontrib><creatorcontrib>Nguyen-Luong, Q</creatorcontrib><creatorcontrib>Palmeirim, P</creatorcontrib><creatorcontrib>Peretto, N</creatorcontrib><creatorcontrib>Schneider, N</creatorcontrib><creatorcontrib>Bontemps, S</creatorcontrib><creatorcontrib>Louvet, F</creatorcontrib><creatorcontrib>Elia, D</creatorcontrib><creatorcontrib>Giannini, T</creatorcontrib><creatorcontrib>Reveret, V</creatorcontrib><creatorcontrib>J Le Pennec</creatorcontrib><creatorcontrib>Rodriguez, L</creatorcontrib><creatorcontrib>Boulade, O</creatorcontrib><creatorcontrib>Doumayrou, E</creatorcontrib><creatorcontrib>Dubreuil, D</creatorcontrib><creatorcontrib>Gallais, P</creatorcontrib><creatorcontrib>Lortholary, M</creatorcontrib><creatorcontrib>Martignac, J</creatorcontrib><creatorcontrib>Talvard, M</creatorcontrib><creatorcontrib>De Breuck, C</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Hill, T</au><au>Andre, Ph</au><au>Arzoumanian, D</au><au>Motte, F</au><au>Minier, V</au><au>Menshchikov, A</au><au>Didelon, P</au><au>Hennemann, M</au><au>Konyves, V</au><au>Nguyen-Luong, Q</au><au>Palmeirim, P</au><au>Peretto, N</au><au>Schneider, N</au><au>Bontemps, S</au><au>Louvet, F</au><au>Elia, D</au><au>Giannini, T</au><au>Reveret, V</au><au>J Le Pennec</au><au>Rodriguez, L</au><au>Boulade, O</au><au>Doumayrou, E</au><au>Dubreuil, D</au><au>Gallais, P</au><au>Lortholary, M</au><au>Martignac, J</au><au>Talvard, M</au><au>De Breuck, C</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Resolving the Vela C ridge with P-ArTeMiS and Herschel</atitle><jtitle>arXiv.org</jtitle><date>2012-11-01</date><risdate>2012</risdate><eissn>2331-8422</eissn><abstract>We present APEX/P-ArTéMiS 450\mu m continuum observations of RCW 36 and the adjacent ridge, a high-mass high-column density filamentary structure at the centre of the Vela C molecular cloud. These observations, at higher resolution than Herschel's SPIRE camera, reveal clear fragmentation of the central star-forming ridge. Combined with PACS far-infrared and SPIRE sub-millimetre observations from the Herschel HOBYS project we build a high resolution column density map of the region mapped with P-ArTéMiS. We extract the radial density profile of the Vela C ridge which with a ~ 0.1pc central width is consistent with that measured for low-mass star-forming filaments in the Herschel Gould Belt survey. Direct comparison with Serpens South, of the Gould Belt Aquila complex, reveals many similarities between the two regions. Despite likely different formation mechanisms and histories, the Vela C ridge and Serpens South filament share common characteristics, including their filament central widths.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1211.0275</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Columnar structure Density Filaments Low mass stars Molecular clouds Physics - Astrophysics of Galaxies Physics - Solar and Stellar Astrophysics Space telescopes Star formation |
| title | Resolving the Vela C ridge with P-ArTeMiS and Herschel |
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