Temporal Gain Correction for X-ray Calorimeter Spectrometers
Temporal Gain Correction for X-ray Calorimeter Spectrometers
复制标题
X 射线热量计光谱仪的时间增益校正
DOI：
10.1007/s10909-016-1503-2
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发表时间：
2016
影响因子：
2
通讯作者：
S.
中科院分区：
文献类型：
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作者：
Porter;F. S.; Chiao;M. P.; Eckart;M. E.; Fujimoto;R.; Ishisaki;Y.; Kelley;R. L.; Kilbourne;C. A.; Leutenegger;M. A.; McCammon;D.; Mitsuda;K.; Sawada;M.; Szymkowiak;A. E.; Takei;Y.; Tashiro;M.; Tsujimoto;M.; Watanabe;T.; Yamada;S.
量热X射线探测器对环境非常敏感。边界条件可以对增益具有深远的影响，包括热沉温度、局部辐射温度、偏置和读出电子器件的温度。边界条件的任何变化都可能导致探测器增益的时间变化，并损害光谱仪的能量标度和分辨率。大多数生产X射线量热光谱仪，无论是在地面上还是在太空中，都有一些跟踪增益随时间变化的方法，通常使用校准谱线。对于小的增益变化，线性拉伸校正通常就足够了。然而，检测器本质上是非线性的，并且通常事件分析，即整形、最佳滤波器等，添加额外的非线性。因此，对于大的增益变化或当需要最佳可能的精度时，线性拉伸校正是不够的。在这里，我们讨论了一种新的校正技术的基础上的非线性插值的能量尺度函数。使用Astro-H/SXS校准数据，我们证明，即使在大尺度增益变化的情况下，校正也可以在整个谱带上将X射线能量恢复到12 keV以上，优于1/10。该方法将用于使用Astro-H天文台SXS仪器的星上校准源校正在轨每像素增益的任何时间漂移。
Calorimetric X-ray detectors are very sensitive to their environment. The boundary conditions can have a profound effect on the gain including heat sink temperature, the local radiation temperature, bias, and the temperature of the readout electronics. Any variation in the boundary conditions can cause temporal variations in the gain of the detector and compromise both the energy scale and the resolving power of the spectrometer. Most production X-ray calorimeter spectrometers, both on the ground and in space, have some means of tracking the gain as a function of time, often using a calibration spectral line. For small gain changes, a linear stretch correction is often sufficient. However, the detectors are intrinsically non-linear and often the event analysis, i.e., shaping, optimal filters etc., add additional non-linearity. Thus for large gain variations or when the best possible precision is required, a linear stretch correction is not sufficient. Here, we discuss a new correction technique based on non-linear interpolation of the energy-scale functions. Using Astro-H/SXS calibration data, we demonstrate that the correction can recover the X-ray energy to better than 1 part in 10over the entire spectral band to above 12 keV even for large-scale gain variations. This method will be used to correct any temporal drift of the on-orbit per-pixel gain using on-board calibration sources for the SXS instrument on the Astro-H observatory.