Si and Fe abundance study in star-forming regions

Details Si and Fe abundance study in star-forming regions Si and Fe abundance study in star-forming regions

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop20612o&link_type=abstract

Spitzer Proposal ID #20612

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Scientific paper

We propose to examine the depletion of Si and Fe in HII regions and reflection nebulae with IRS LH and SH module. We will observe the [SiII] 35 micron and [FeII] 26 micron emissions to estimate the gas-phase abundance of Si and Fe, which reflect the dust destruction in the observed region. Other lines such as [FeIII] 23 micron, [FeII] 18 micron, and [SIII] 19 and 33 micron can be used to translate safely the ratio of the line emissions to the abundance ratio. We plan to observe two groups of targets: (a) HII region/PDR complexes or reflection nebulae studied by ISO or KAO, and (b) giant HII regions located at various location in the Galactic plane. For the group (a) targets, we will derive gas-phase Si and Fe abundance relative to N or O in the HII region or PDR, respectively, giving the degree of the destruction of Si-bearing and Fe-bearing dust grains in each phase. For the group (b) targets, we will derive the relative gas phase abundance of Si/Fe. The proposed observations will be the first study of the Fe depletion in low density regions. They also provide the depletion pattern of Si/Fe in various environments such as the density and the phase (HII region or PDR) over the Galactic scale and give us significant observational constraint on the dust processing in the ISM and the dust model.

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