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http://hdl.handle.net/20.500.12386/24168
Title: | [O I] 63 μm Jets in Class 0 Sources Detected By Herschel | Authors: | NISINI, Brunella Santangelo, G. Giannini, T. ANTONIUCCI, Simone Cabrit, S. CODELLA, CLAUDIO Davis, C. J. Eislöffel, J. Kristensen, L. Herczeg, G. Neufeld, D. van Dishoeck, E. F. |
Issue Date: | 2015 | Journal: | THE ASTROPHYSICAL JOURNAL | Number: | 801 | Issue: | 2 | First Page: | 121 | Abstract: | We present Herschel PACS mapping observations of the [O i] 63 μm line toward protostellar outflows in the L1448, NGC 1333-IRAS4, HH 46, BHR 71, and VLA 1623 star-forming regions. We detect emission spatially resolved along the outflow direction, which can be associated with a low-excitation atomic jet. In the L1448-C, HH 46 IRS, and BHR 71 IRS1 outflows this emission is kinematically resolved into blue- and redshifted jet lobes, having radial velocities up to 200 km s<SUP>-1</SUP>. In the L1448-C atomic jet the velocity increases with the distance from the protostar, similarly to what is observed in the SiO jet associated with this source. This suggests that [O i] and molecular gas are kinematically connected and that the latter could represent the colder cocoon of a jet at higher excitation. Mass flux rates ({{\dot{M}}<SUB>jet</SUB>}(O i)) have been measured from the [O i] 63 μm luminosity adopting two independent methods. We find values in the range (1-4) × 10<SUP>-7</SUP> {{M}<SUB>☉ </SUB>} yr<SUP>-1</SUP> for all sources except HH 46, for which an order of magnitude higher value is estimated. {{\dot{M}}<SUB>jet</SUB>}(O i) are compared with mass accretion rates (\dot{M}<SUB>acc</SUB>) onto the protostar and with {{\dot{M}}<SUB>jet</SUB>} derived from ground-based CO observations. {{\dot{M}}<SUB>jet</SUB>}(O i)/\dot{M}<SUB>acc</SUB> ratios are in the range 0.05-0.5, similar to the values for more evolved sources. {{\dot{M}}<SUB>jet</SUB>}(O i) in HH 46 IRS and IRAS4A are comparable to {{\dot{M}}<SUB>jet</SUB>}(CO), while those of the remaining sources are significantly lower than the corresponding {{\dot{M}}<SUB>jet</SUB>}(CO). We speculate that for these three sources most of the mass flux is carried out by a molecular jet, while the warm atomic gas does not significantly contribute to the dynamics of the system. | Acknowledgments: | Financial support from INAF, under PRIN2013 program “Disks, jets and the dawn of planets” is acknowledged. | URI: | http://hdl.handle.net/20.500.12386/24168 | URL: | https://iopscience.iop.org/article/10.1088/0004-637X/801/2/121 | ISSN: | 0004-637X | DOI: | 10.1088/0004-637X/801/2/121 | Bibcode ADS: | 2015ApJ...801..121N | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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Nisini_2015_ApJ_801_121.pdf | 1.36 MB | Adobe PDF | View/Open |
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