Volume 397, Number 2, January II 2003
|Page(s)||693 - 710|
|Section||Interstellar and circumstellar matter|
|Published online||17 December 2002|
Near-IR echelle spectroscopy of Class I protostars: Mapping Forbidden Emission-Line (FEL) regions in [FeII]
Joint Astronomy Centre, 660 North A'ohōkū Place, University Park, Hilo, Hawaii 96720, USA
2 Dublin Institute for Advanced Studies, School of Cosmic Physics, 5 Merrion Square, Dublin 2, Ireland
3 Department of Physical Sciences, University of Hertfordshire, Hatfield, Herts AL10 9AB, UK
Corresponding author: C. J. Davis, email@example.com
Accepted: 22 October 2002
Near-IR echelle spectra in [FeII] 1.644 μm emission trace Forbidden Emission Line (FEL) regions towards seven Class I HH energy sources (SVS 13, B5-IRS1, IRAS 04239+2436, L1551-IRS5, HH 34-IRS, HH 72-IRS and HH 379-IRS) and three classical T Tauri stars (AS 353A, DG Tau and RW Aur). The parameters of these FEL regions are compared to the characteristics of the Molecular Hydrogen Emission Line (MHEL) regions recently discovered towards the same outflow sources (Davis et al. [CITE] – Paper I). The [FeII] and H2 lines both trace emission from the base of a large-scale collimated outflow, although they clearly trace different flow components. We find that the [FeII] is associated with higher-velocity gas than the H2, and that the [FeII] emission peaks further away from the embedded source in each system. This is probably because the [FeII] is more closely associated with HH-type shocks in the inner, on-axis jet regions, while the H2 may be excited along the boundary between the jet and the near-stationary, dense ambient medium that envelopes the protostar. Indeed, there is spatial and kinematic evidence that [FeII] and the more typically-used optical emission lines, the red [SII] doublet, do trace almost the same shock-excited regions in HH jets and FEL regions alike.
Key words: ISM: jets and outflows / stars: pre-main-sequence / ISM: Herbig-Haro objects
© ESO, 2003
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