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Browsing by Author "Antoniucci, S."

Browsing by Author "Antoniucci, S."

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  • H2O line mapping at high spatial and spectral resolution. Herschel observations of the VLA 1623 outflow 
    Bjerkeli, P.; Liseau, R.; Larsson, B.; Rydbeck, G.; Nisini, B.; Tafalla, M.; Antoniucci, S.; Benedettini, M.; Bergman, P.; Cabrit, S.; Giannini, T.; Melnick, G.; Neufeld, D.; Santangelo, G.; van Dishoeck, E. F. (2012)
    Context. Apart from being an important coolant, water is known to be a tracer of high-velocity molecular gas. Recent models predict relatively high abundances behind interstellar shockwaves. The dynamical and physical ...
  • Mapping water in protostellar outflows with Herschel. PACS and HIFI observations of L1448-C 
    Nisini, B.; Santangelo, G.; Antoniucci, S.; Benedettini, M.; Codella, C.; Giannini, T.; Lorenzani, A.; Liseau, R.; Tafalla, M.; Bjerkeli, P.; Cabrit, S.; Caselli, P.; Kristensen, L.; Neufeld, D.; Melnick, G.; van Dishoeck, E. F. (2013)
    Context. Water is a key probe of shocks and outflows from young stars because it is extremely sensitive to both the physical conditions associated with the interaction of supersonic outflows with the ambient medium and the ...
  • [O I] 63 µm Jets in Class 0 Sources Detected By Herschel 
    Nisini, B.; Santangelo, G.; Giannini, T.; Antoniucci, S.; Cabrit, S.; Codella, C.; Davis, C. J.; Eislöffel, J.; Kristensen, L.; Herczeg, G.; Neufeld, D.; van Dishoeck, E. F. (2015)
    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 ...
  • Water distribution in shocked regions of the NGC 1333-IRAS 4A protostellar outflow 
    Santangelo, G.; Nisini, B.; Codella, C.; Lorenzani, A.; Yildiz, U. A.; Antoniucci, S.; Bjerkeli, P.; Cabrit, S.; Giannini, T.; Kristensen, L. E.; Liseau, R.; Mottram, J. C.; Tafalla, M.; van Dishoeck, E. F. (2014)
    Context. Water is a key molecule in protostellar environments because its line emission is very sensitive to both the chemistry and the physical conditions of the gas. Observations of H<SUB>2</SUB>O line emission from ...

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