Astrophys. J., 778, 71 (2013/November-3)
The diagnostic potential of Fe lines applied to protostellar jets.
GIANNINI T., NISINI B., ANTONIUCCI S., ALCALA J.M., BACCIOTTI F., BONITO R., PODIO L., STELZER B. and WHELAN E.T.
Abstract (from CDS):
We investigate the diagnostic capabilities of iron lines for tracing the physical conditions of shock-excited gas in jets driven by pre-main sequence stars. We have analyzed the 3000-25000 Å, X-shooter spectra of two jets driven by the pre-main sequence stars ESO-Hα 574 and Par-Lup 3-4. Both spectra are very rich in [Fe II] lines over the whole spectral range; in addition, lines from [Fe III] are detected in the ESO-Hα 574 spectrum. Non-local thermal equilibrium codes solving the equations of the statistical equilibrium along with codes for the ionization equilibrium are used to derive the gas excitation conditions of electron temperature and density and fractional ionization. An estimate of the iron gas-phase abundance is provided by comparing the iron lines emissivity with that of neutral oxygen at 6300 Å. The [Fe II] line analysis indicates that the jet driven by ESO-Hα 574 is, on average, colder (Te∼ 9000 K), less dense (ne∼ 2x104/cm3), and more ionized (xe∼ 0.7) than the Par-Lup 3-4 jet (Te∼ 13,000 K, ne∼ 6x104/cm3, xe< 0.4), even if the existence of a higher density component (ne∼ 2x105/cm3) is probed by the [Fe III] and [Fe II] ultra-violet lines. The physical conditions derived from the iron lines are compared with shock models suggesting that the shock at work in ESO-Hα 574 is faster and likely more energetic than the Par-Lup 3-4 shock. This latter feature is confirmed by the high percentage of gas-phase iron measured in ESO-Hα 574 (50%-60% of its solar abundance in comparison with less than 30% in Par-Lup 3-4), which testifies that the ESO-Hα 574 shock is powerful enough to partially destroy the dust present inside the jet. This work demonstrates that a multiline Fe analysis can be effectively used to probe the excitation and ionization conditions of the gas in a jet without any assumption on ionic abundances. The main limitation on the diagnostics resides in the large uncertainties of the atomic data, which, however, can be overcome through a statistical approach involving many lines.
ISM: individual (ESO-Hα 574, Par-Lup 3-4) - ISM: jets and outflows - ISM: lines and bands - stars: pre-main sequence
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