Suzaku Observation Of The Cygnus Loop

Details Suzaku Observation Of The Cygnus Loop Suzaku Observation Of The Cygnus Loop

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.3507t&link_type=abstract

American Astronomical Society Meeting 208, #35.07; Bulletin of the American Astronomical Society, Vol. 38, p.111

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In November, 2006, we observed the north-east limb of the Cygnus Loop with Suzaku. The FOV of the XIS (CCD camera) is only 18’ square. Therefore, we only covered a very small portion of the Loop although we selected the brightest region. The XIS has two types of CCDs: FI and BI. The BI-CCD is quite a new type of device and has high QE at low energy while the FI-CCD is conventional one. There is no clear difference in QE above 1 keV whereas there is a big difference below 1 keV. The BI-CCD clearly detects emission lines below 0.5 keV. Since the CCDs on Suzaku have been improved their performance, we can see some emission line structures below 0.5 keV even in the FI-CCD spectrum. The strongest peak comes from He-like O (0.57 keV). Three clear peaks are seen below 0.5 keV. They mainly come from emission lines of N (0.43keV), C (0.37 keV) and, so-called C-band (around 0.27 keV). The C-band comes from C (neutral) in the optical blocking filter.In general, we usually assumed the abundances for C, N and O to be equal to each other, only because we could see no emission from C and N. In the Suzaku CCD camera, we can separately determine the abundances for these elements. The quick analysis shows that C is more abundant that N and O than those in solar values. Since C, N and O play an important role in the nuclear reaction inside stars, we can investigate the evolution of the matter in detail.

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