English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/146325
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL
Exportar a otros formatos:

Herschel PACS far-IR spectral imaging of a jet from an intermediate mass protostar in the OMC-2 region

AuthorsGonzález-García, B.; Manoj, P.; Watson, D.M.; Vavrek, R.; Megeath, S.T.; Stutz, A.M.; Osorio, Mayra ; Wyrowski, F.; Fischer, W.; Tobin, J.J.; Sánchez-Portal, M.; Diaz Rodriguez, A.K. ; Wilson, T.L.
KeywordsStars: formation
Techniques: spectroscopic
ISM: jets and outflows
Issue Date2016
PublisherEDP Sciences
CitationAstronomy and Astrophysics 596: A26 (2016)
AbstractWe present the first detection of a jet in the far-IR [O I] lines from an intermediate mass protostar. This jet was detected in a Herschel/PACS spectral mapping study in the [O I] lines of OMC-2 FIR 3 and FIR 4, two of the most luminous protostars in Orion outside of the Orion Nebula. The spatial morphology of the fine structure line emission reveals the presence of an extended photodissociation region (PDR) and a narrow, but intense jet connecting the two protostars. The jet seen in [O I] emission is spatially aligned with the Spitzer/IRAC 4.5 μm jet and the CO (6-5) molecular outflow centered on FIR 3. The mass-loss rate derived from the total [O I] 63 μm line luminosity of the jet is 7.7 × 10Myr, more than an order of magnitude higher than that measured for typical low-mass class 0 protostars. The implied accretion luminosity is significantly higher than the observed bolometric luminosity of FIR 4, indicating that the [O I] jet is unlikely to be associated with FIR 4. We argue that the peak line emission seen toward FIR 4 originates in the terminal shock produced by the jet driven by FIR 3. The higher mass-loss rate that we find for FIR 3 is consistent with the idea that intermediate-mass protostars drive more powerful jets than their low-mass counterparts. Our results also call into question the nature of FIR 4. © ESO, 2016.
Identifiersdoi: 10.1051/0004-6361/201527186
issn: 1432-0746
Appears in Collections:(IAA) Artículos
Files in This Item:
File Description SizeFormat 
IAA_2016_aa27186-15.pdf2,03 MBAdobe PDFThumbnail
Show full item record
Review this work

Related articles:

WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.