Observations of Molecular Hydrogen in the Carina Nebula

Details Observations of Molecular Hydrogen in the Carina Nebula Observations of Molecular Hydrogen in the Carina Nebula

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...545..885l&link_type=abstract

The Astrophysical Journal, Volume 545, Issue 2, pp. 885-891.

Astronomy and Astrophysics

Astronomy

6

Ism: H Ii Regions, Ism: Individual (Carina Nebula), Ism: Molecules, Ultraviolet: Ism

Scientific paper

We present a study of molecular-hydrogen absorption lines in the continuum spectra of three early-type stars in the Carina Nebula, HD 93129a, HD 93250, and HD 303308, made with the Berkeley Extreme and Far-Ultraviolet Spectrometer (BEFS) on the ORFEUS telescope in 1993 September. The instrument possesses an intermediate spectral resolving power (λ/Δλ=3000) over the wavelength range λλ390-1170.We derive column densities for the H2 rotational levels up to J''=6 and estimate the kinetic temperature and the UV radiation fields at the surface of the clouds in the nebula. All three stars show strong H2 absorption features, indicating that the Carina Nebula contains abundant molecular hydrogen. The UV radiation field strength seems to be correlated with the angular distance of the target star from η Car, implying that the clouds might be located close to η Car. We derive the absolute distances between the clouds and η Car, which are in good agreement with the angular positions of these stars. We also examine the morphology of the Carina Nebula based on the present result, as well as previous CO observations, and derive the conversion factor N(H2)/W(12CO) in this region.

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