2014A&A...566A.129A -
Astronomy and Astrophysics, volume 566A, 129-129 (2014/6-1)
The HH 34 outflow as seen in [FeII] 1.64 µm by LBT-LUCI.
ANTONIUCCI S., LA CAMERA A., NISINI B., GIANNINI T., LORENZETTI D., PARIS D. and SANI E.
Abstract (from CDS):
Dense atomic jets from young stars copiously emit in [FeII] IR lines, which can, therefore, be used to trace the immediate environments of embedded protostars. We want to investigate the morphology of the bright [FeII] 1.64µm line in the jet of the source HH34 IRS and compare it with the most commonly used optical tracer [SII]. We analyse a 1.64µm narrow-band filter image obtained with the Large Binocular Telescope (LBT) LUCI instrument, which covers the HH34 jet and counterjet. A point spread function deconvolution algorithm was applied to enhance spatial resolution and make the IR image directly comparable to a [SII] HST image of the same source. The [FeII] emission is detected from both the jet, the (weak) counter-jet, and from the HH34-S and HH34-N bow shocks. The deconvolved image allows us to resolve jet knots close to about 1''from the central source. The morphology of the [FeII] emission is remarkably similar to that of the [SII] emission, and the relative positions of [FeII] and [SII] peaks are shifted according to proper motion measurements, which were previously derived from HST images. An analysis of the [FeII]/[SII] emission ratio shows that Fe gas abundance is much lower than the solar value with up to 90% of Fe depletion in the inner jet knots. This confirms previous findings on dusty jets, where shocks are not efficient enough to remove refractory species from grains.
Abstract Copyright:
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Journal keyword(s):
stars: protostars - stars: mass-loss - stars: jets - ISM: jets and outflows - ISM: abundances - techniques: image processing
Simbad objects:
12
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