Suzaku Observation of the Carina Nebula

Details Suzaku Observation of the Carina Nebula Suzaku Observation of the Carina Nebula

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.3505h&link_type=abstract

American Astronomical Society Meeting 208, #35.05; Bulletin of the American Astronomical Society, Vol. 38, p.111

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Scientific paper

The massive star forming region, Carina nebula, contains many massive main-sequence and post-main-sequence stars such as Eta Carina, WR25 and Trumper 14. ROSAT and Chandra have observed 10-100 times stronger diffuse X-ray emission from this nebula than any other HII regions in our Galaxy. Such diffuse X-ray emission from star forming regions is supposed to originate from shock heating of massive stellar winds or super nova remnants (SNR), but diffuse emission from the Carina nebula do not necessarily accompany massive star clusters nor known SNRs.The X-ray CCD detector XIS onboard the Suzaku observatory has good spectral resolution and efficiency in the soft band below 1 keV. A Suzaku observation of Eta Carina in August 2005 covered northern and southern parts of the diffuse X-ray emission and clearly resolved emission lines from those regions for the first time. The northern region emits stong lines from highly ionized Ne and O ions, while the southern region emits strong lines from highly ionized Fe and O ions and weak line from hydrogen-like C. This result may suggest that the northern emission is originated in the Wolf-Rayet (WC) winds and/or combined emission from low mass young stars, while the southern emission is produced by Type II SNRs.

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