Origin of [Siii] 35 mum and [Cii] 158 mum emission in the Carina nebula

Details Origin of [Siii] 35 mum and [Cii] 158 mum emission in the Carina nebula Origin of [Siii] 35 mum and [Cii] 158 mum emission in the Carina nebula

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000esasp.456..115m&link_type=abstract

ISO beyond the peaks: The 2nd ISO workshop on analytical spectroscopy. Eds. A. Salama, M.F.Kessler, K. Leech & B. Schulz. ESA-SP

Physics

2

Ism, Pdr, Fine-Structure Lines, Carina Nebula

Scientific paper

We present the results of mapping observations of the Carina nebula, an active star-forming region on the Galactic plane, with LWS01 and SWS02. The observed area was a region of 40'× 20' centered at l=287o.3 and b=-0o.6. The [Siii] 35 μm and [Cii] 158 μm lines are clearly detected at all the observed positions. The observed [Cii] intensity peaks at the center of the observed area, which is near the border between the bright Hii and molecular cloud regions, a typical photodissociation region (PDR). The [Siii] emission peak is also located at the border region, but it is slightly shifted toward the ionized region. The [Cii] emission shows a good correlation with the [Oi] 63 μm emission, which comes from atomic gas, while the [Siii] emission correlates with the [Nii] 122 μm emission from ionic gas. We do not see any clear correlation between [Siii] and [Oi], nor [Cii] and [Nii] lines. Simple model calculations indicate that the intensity of [Siii] 35 μm line can be explained only if Si in the ionized gas is nearly in the solar abundance. The [Siii] 35 μm emission is a dominant cooling line in the warm ionized medium (WIM). The fraction of [Cii] emission from the WIM should be ~ 10% of the observed intensity, indicating that the observed [Cii] emission comes mainly from the neutral region.

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