天鹅座环Ar-K线发射的首次探测
First Detection of Ar-K Line Emission from the Cygnus Loop
摘要：
我们在2002年至2008年期间用XMM-牛顿（9个点）和朱雀（32个点）观测了天鹅座圈。总有效曝光时间为670.2ks。通过使用所有可用的数据，我们打算提高频谱的信噪比。相应地，由XIS和EPIC获得的累积谱显示出一些在3 keV附近的线特征，这些线特征分别归因于S He $β$和Ar He $α$线。由于天鹅座环是一个演化的超新星遗迹（$\sim$ 10，000年），与其他年轻的遗迹相比，它的温度相对较低（$<$ 1 keV），它的光谱通常在3.0 keV以上是微弱的，没有发射线，如Ar-K线曾经被检测到。Ar-K线的检测是第一次，我们发现它的丰度显着高于太阳值; 9.0 $^{+4.0}_{-3.8}$和8.4 $^{+2.5}_{-2.7}$（太阳单位），估计从XIS和EPIC光谱，分别。我们的结论是，Ar-K线起源于天鹅座环的喷出物。后续的X射线观测，以严格限制丰富的Ar喷出物的丰度将是有用的，以准确地估计祖的质量。
英文摘要：
We observed the Cygnus Loop with XMM-Newton (9 pointings) and Suzaku (32 pointings) between 2002 and 2008. The total effective exposure time is 670.2 ks. By using all of the available data, we intended to improve a signal-to-noise ratio of the spectrum. Accordingly, the accumulated spectra obtained by the XIS and the EPIC show some line features around 3 keV that are attributed to the S He$β$ and Ar He$α$ lines, respectively. Since the Cygnus Loop is an evolved ($\sim$10,000 yr) supernova remnant whose temperature is relatively low ($<$1 keV) compared with other young remnants, its spectrum is generally faint above 3.0 keV, no emission lines, such as the Ar-K line have ever been detected. The detection of the Ar-K line is the first time and we found that its abundance is significantly higher than that of the solar value; 9.0$^{+4.0}_{-3.8}$ and 8.4$^{+2.5}_{-2.7}$ (in units of solar), estimated from the XIS and the EPIC spectra, respectively. We conclude that the Ar-K line originated from the ejecta of the Cygnus Loop. Follow-up X-ray observations to tightly constrain the abundances of Ar-rich ejecta will be useful to accurately estimate the progenitor's mass.
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