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TOP > Report & Column > The Forefront of Space Science > 2014 > X-ray Precision Spectroscopic Observation of the Supernova Remnant

The Forefront of Space Science

X-ray Precision Spectroscopic Observation of the Supernova Remnant
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Summary and Expectations of ASTRO-H

We introduced the current situation that the XMM-Newton RGS is working efficiently in the research on X-ray precise spectroscopic observations of SNR and is opening up the forefront of the research. Due to limitations of space, we could only introduce the results of the Puppis A, but we have also obtained interesting results from several other SNR as the first in the world.

On the other hand, the power of the ASTRO-H SXS, which is being launched in the year of 2015, is great especially for the extended celestial bodies such as the SNR. The RGS was efficient only for the locally bright structures or the apparently small SNR, but there is no such limitation for the SXS. Therefore, the amount of observation targets will increase dramatically and we may be able to detect the feeble emission lines that have never been observed before for the first time, or do detailed studies on the spatial variation of the X-ray spectrum. In addition, we can study the ion temperature and the turbulent velocity by measuring the width of each emission line accurately. Furthermore, since the SXS is also sensitive to the high energy X-rays, precise emission line diagnosis of the iron group elements is able to be conducted for the first time. Besides these, there may be great discoveries unexpected. The ASTRO-H project team is making observation plans based on various ideas and preparing for the launch. We are all looking forward to the new developments that the ASTRO-H will show to us.

Figure 3
Figure 3. Observation Simulation of the ASTRO-H SXS [click on picture to enlarge.]
This indicates the field of view (3 arc minutes × 3 arc minutes) of the ASTRO-H SXS with a white square on the X-ray image of the SN 1006 SNR taken by the Chandra. The graph is the SXS spectrum (simulation of the emission line from silicon Kα) of ASTRO-H, which is expected in this field. According to the Doppler shift of the front and rear side of the expanding shell, we expect that each emission line can be divided into two components, blue and red. The models in dotted lines are the SXS spectrum expected when the irregular movement of plasma (thermal motion and turbulent motion) is strenuous.

(Satoru Katsuda)

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