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Diffuse X-Ray Emission from the Carina Nebula Observed with Suzaku

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Diffuse X-Ray Emission from the Carina Nebula Observed with Suzaku Triggered Star Formation in a Turbulent ISM Proceedings IAU Symposium No. 237, 2006 c 2007 International Astronomical Union B. G. Elmegreen & J. Palouˇs, eds. doi:10.1017/S1743921307002098 Diffuse X-ray emission from the Carina Nebula observed with Suzaku K. Hamaguchi1,2,R.Petre1 and the Suzaku η Carina team 1NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA email: [email protected] 2Universities Space Research Association, 10211 Wincopin Circle, Suite 500, Columbia, MD 21044-3432, USA Abstract. The Carina Nebula possesses the brightest soft diffuse X-ray emission among the Galactic giant HII regions, but the origin has not been known yet. The XIS1 back-illuminated CCD camera onboard the Suzaku X-ray observatory has the best spectral resolution for extended soft sources so far, and is therefore capable of measuring these key emission lines in the soft diffuse plasma. Suzaku observed the Carina nebula on 2005 Aug. 29. The XIS1 spectra of the Carina nebula clearly showed spatial variations in emission line strengths. In the south, the spectrum showed strong L-shell lines of iron ions and K-shell lines of silicon ions, while in the north these lines were much weaker. Fitting the spectra with an absorbed thin-thermal 21 −2 plasma model with kT ∼ 0.2, 0.6 keV and NH ∼ 1−2 × 10 cm showed that the silicon and iron abundance is about 2−3 times higher in the south than in the north. Because of its large size (∼40 pc), the diffuse emission in the Carina nebula might have been produced by an old supernova, or a super shell produced by multiple supernovae. Keywords. ISM: abundances, supernova remnants, X-rays: ISM Fe L complex HD 93250 Tr 14 North Line profiles are black: similar grey: different Eta Car WR 25 HD 93205 South 5' Figure 1. Left: XMM-Newton image with the source regions defined. Right: Suzaku normalized spectra of the north (lower curve) and south. See details for Hamaguchi et al. (2006). Acknowledgements K. H. is financially supported by the US Chandra grant No. GO3-4008A. Reference Hamaguchi et al. 2006, PASJ submitted 421 Downloaded from https://www.cambridge.org/core. IP address: 170.106.35.93, on 24 Sep 2021 at 23:41:45, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S1743921307002098.
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