一种聚焦型X射线探测器在轨性能标定方法

X射线探测器是X射线天文观测及脉冲星导航的核心器件,受发射振动、高能粒子辐射损伤及元器件老化等影响,X射线探测器空间观测性能会逐渐变化,X射线探测器在轨标定有利于观测天体X射线辐射信息的准确获取及精确建模.研究利用了脉冲星辐射能谱标定X射线探测器性能的方法,能较好地消除探测器本底及空间环境噪声的影响,通过处理脉冲星导航试验卫星(XPNAV-1卫星)的Crab脉冲星观测数据,评估了我国首款聚焦型X射线探测器的在轨性能.计算结果表明,XPNAV-1卫星上聚焦型X射线探测器的有效面积在0.6-1.9 keV能段内优于2 cm~2,其中在0.7 keV能量处取得最大值3.06 cm~2,探测效率约10%;有效面积随着探测能量增大而减小,在2—3.5 keV能段内有效面积约为1 cm~2,而大于5 keV能段的有效面积约为0.1 cm~2,且此能段估计精度明显受光子统计误差影响.同时研究了考虑能量响应矩阵的探测器有效面积标定新方法,利用地面性能测试中五个特征能谱处的能量分辨率重构其能量响应矩阵,重新标定了聚焦型X射线探测器有效面积,发现该能量响应矩阵对结果影响较小.最后建议观测某些超新星遗迹监测能量分辨率及能量线性等指标的变化.     

标定脉冲星导航探测器的荧光X射线光源

为标定X射线脉冲星导航用探测器, 设计了一种荧光X射线源, 该射线源的工作原理是 用X射线管的出射线轰击特定荧光靶材, 从而获得能量一定的荧光X射线, 并以此作为标定探测器的荧光X射线光源. 采用硅漂移半导体探测器在大气环境下测试了按上述原理搭建的荧光X射线光源的能谱分布和光子流量, 从光子流量入手推算了该荧光X射线光源用于真空系统中对探测器进行标定的可行性. 研制出了荧光X射线光源样机, 并在真空系统中对荧光X射线光源样机光子流量做了测试. 在探测距离D_x=300 cm, X射线管管流I_a=200 μA时, 所测得的荧光X射线光源光子流量可达19.57 ph/s@4.51 keV, 25.22 ph/s@5.41 keV, 33.27 ph/s@8.05 keV, 确认了所提方法的可行性, 获得了标定探测器的荧光X射线光源.     

X射线光谱数据处理平台的优化设计

在低计数率背景下X射线谱的高精度测量受X射线流的统计涨落影响,统计涨落决定了给定探测器能量分辨率的理论极限,而其他因素的影响则可以通过适当的噪声滤除和电子技术来降低.以往关于能量分辨率的研究大多利用谱反卷积对获取到的能谱进行后处理,从而降低特征峰的半高宽(FW H M).这些后处理方法是基于将获取到的能谱建模为输入能谱...     

HXMT探测器能量响应矩阵的计算

介绍硬X射线调制望远镜(HXMT)探测器能量响应矩阵的计算方法，根据实验室测量数据计算了该条件下的能量响应矩阵；利用该能量响应矩阵由直接解调法解实验室所测放射源能谱，能很好地重现放射源能量.     

聚龙一号丝阵负载Z箍缩硬X射线能谱测量

为获取聚龙一号实验装置负载放电产生硬X射线的能谱分布,设计了一套7通道硬X射线能谱仪。介绍了这套多通道硬X射线能谱仪的测谱原理、主要参数及根据测量结果回推光源辐射能谱的解谱算法。在聚龙一号装置丝阵负载物理实验中对测量系统进行考核,获得了信噪比较高的测量波形。利用最大熵方法进行解谱,获得了丝阵负载产生的硬X射线能谱分布,辐射能段主要集中在200~500 keV附近,且1 MeV以上光子份额较低。     

15～600 keV脉冲硬X射线能谱测量

介绍了基于吸收法的脉冲硬X射线能谱测量的基本原理及设计思路,完成了探测器及吸收片的选型,设计了射线准直系统,研究了散射对测量的影响,以12路PIN探测器阵列及铜、铝吸收片为测量核心部件研制了脉冲硬X射线能谱测量系统。实验测量了真空环境下"闪光二号"加速器串级二极管产生的脉冲硬X射线强度,获得了不同衰减程度的实验波形,通过解谱获得了脉冲硬X射线的能谱,光子最高能量约600 keV,平均能量约89.1 keV,与理论计算的结果比较符合。     

Si-PIN与CdTe探测器应用于X射线荧光能谱测量的研究

半导体探测器具有优异的性能因而被广泛应用于能量色散X射线荧光测量,以传统型Si-PIN半导体探测器与复合型CdTe半导体探测器为研究对象,分别从材料属性、探测效率、能量分辨率等方面对两种探测器进行对比,重点分析探测器灵敏区厚度、入射X射线能量、后级电路成型时间等因素对其性能的影响,并对由逃逸峰、空穴拖尾效应所导致的X射线荧光能谱的差异进行分析;同时,针对探测器空穴收集不完全的问题,基于FPGA设计了带有上升时间甄别功能的数字多道脉冲幅度分析器,能够有效消除空穴拖尾的影响,提高能量分辨率。从实验结果可知:对能量低于15keV的射线,Si-PIN与CdTe探测器的探测效率基本相当;对能量大于15keV的射线,CdTe探测器的的探测效率明显占优;Si-PIN探测器的最佳成形时间约为10μs,CdTe探测器的最佳成形时间约为2.6μs,因而CdTe探测器更适用于高计数率条件;对于不同能量的X射线,Si-PIN探测器的能量分辨率优于CdTe探测器;CdTe探测器具有明显的空穴拖尾效应,将CdTe探测器与带上升时间甄别功能的数字多道脉冲幅度分析器配合使用,其能量分辨率显著提高。     

激光等离子实验中的低能X射线时间谱解谱方法

利用快速Fourier变换(FFT)算法和反卷积原理对Dante谱议测量波形进行了回推获得了激光等离子体源区低能X射线辐射时间波形。解谱方法采用了W.N.Mcelroy等人提出的SANDⅡ解谱方法并与文献[6]中介绍的限幅迭代和周期性光滑技术相配合计算出了能谱时间关系的16分区结果,给出了1989年6月LF-12强激光装置实验的双束靶、漏靶诊断口,入射口的X射线时间谱以及辐射温度时间关系T_R(i)。     

MC模拟分析透射式微型X射线管目标靶厚度对输出谱的影响

透射式微型X射线管是能量色散X射线荧光分析中的主要激发源,在能量色散X射线荧光分析中希望得到谱分布较为单一的X射线管输出谱。采用MC方法,研究了透射式微型X射线管在不同目标靶厚度的情况下输出谱的特征,通过低谱段(<5 keV)和高能谱段(5~50 keV)的分析比较,高能谱段计数随厚度加大先增加而后减小,低能谱段计数则随厚度增加减小,增加目标靶厚度可以有效抑制低能谱段。在入射电子能量为50 keV和目标靶为4 Ag的条件下,X射线管输出能谱具有较高的高能谱段注量,同时有效压制低能谱段注量,适合能量色散X射线荧光分析中使用。     

硬X射线调制望远镜低能探测器量子效率标定

低能X射线望远镜是硬X射线调制望远镜卫星的主要载荷之一,探测器采用CCD236.探测器的量子效率会影响能谱拟合和绝对流量,有必要对其进行标定.利用~(55)Fe放射源,以硅漂移探测器为标准探测器,标定了CCD236在Mn-K_α(5.899 keV)和Mn-K_β(6.497 keV)能量点处的量子效率,此能段在Fe线附近,对X射线天文观测有重要价值.考虑探测器的分裂事例后,Mn-K_α和Mn-K_β处的量子效率分别为71%和62%.在-95—-30?C工作温度范围内,CCD量子效率与温度无关.利用CCD236的结构及实测的量子效率,不考虑沟阻影响,得到耗尽层厚度为38μm.对CCD236施加不同的电压,其量子效率基本不变,表明其在两相驱动下高低电平的耗尽层厚度相等,进而说明CCD236一直工作在深耗尽状态,其耗尽层到了外延层和衬底层边界,已达最大值.     

Application of a multiscale maximum entropy image restoration algorithm to HXMT observations

This paper introduces a multiscale maximum entropy(MSME) algorithm for image restoration of the Hard X-ray Modulation Telescope(HXMT),which is a collimated scan X-ray satellite mainly devoted to a sensitive all-sky survey and pointed observations in the 1-250 keV range.The novelty of the MSME method is to use wavelet decomposition and multiresolution support to control noise amplification at different scales.Our work is focused on the application and modification of this method to restore diffuse sources detected by HXMT scanning observations.An improved method,the ensemble multiscale maximum entropy(EMSME) algorithm,is proposed to alleviate the problem of mode mixing exiting in MSME.Simulations have been performed on the detection of the diffuse source Cen A by HXMT in all-sky survey mode.The results show that the MSME method is adapted to the deconvolution task of HXMT for diffuse source detection and the improved method could suppress noise and improve the correlation and signal-to-noise ratio,thus proving itself a better algorithm for image restoration.Through one all-sky survey,HXMT could reach a capacity of detecting a diffuse source with maximum differential flux of 0.5 mCrab.     

A study of the pointed observation methods and sensitivity of HXMT

The Hard X-ray Modulation Telescope (HXMT) is an X-ray astronomy satellite consisting of three slat-collimated instruments, the High Energy X-ray Instrument (HE), the Medium Energy X-ray Instrument (ME), and the Low Energy X-ray Instrument (LE). HXMT will carry out an all sky survey and make pointed observations in the 1-250 keV energy band. In order to get the source and background fluxes simultaneously in the pointed observations, two methods, i.e., the combined field of view (FOV) method and the off-axis pointing method are proposed in this paper. Comprehensive analyses of the sensitivities of the three instruments by using these two methods are presented, respectively. It is found that the off-axis pointing method has a higher sensitivity for HE and ME but a lower sensitivity for LE. Since the axes of the three instruments are aligned along the same direction, the off-axis pointing method is recommended as the main method in the pointed observation for HXMT; the combined FOV method can be used when LE is the most relevant instrument in order to satisfy the scientific objective of the observation.     

Thermal analysis and expected performance of the low energy instrument on board the HXMT satellite

The Low Energy X-ray Instrument (LE) of the Hard X-ray Modulation Telescope (HXMT) uses the Swept Charge Device (SCD) to detect the X-rays in 1-15 keV. The performance of SCD is vulnerable to temperature. We analyzed the thermal condition of LE at different satellite working attitudes with the Finite Element Method (FEM). It is shown that the angle between the sunlight and the normal line of the barrier should be less them 26°, to keep the SCD detectors working in the required temperature range, i.e. -40 ℃ to -80 ℃. We find that the performance of LE is very stable in this temperature range, with a typical energy resolution of 160 eV at 5.9 keV.     

大气压尖板电极结构重复频率纳秒脉冲放电中X射线辐射特性研究

文章通过碘化钠晶体和光电倍增管构成的X射线探测系统,研究了上升沿15ns,脉宽30-40ns量级,电压90kV的大气压重频纳秒脉冲气体放电中X射线的辐射特性,X射线有效探测能量范围为10-130keV.结果表明放电产生的X射线主要集中在20-90keV能量范围,而能量在十几keV的软X射线和超过90keV的高能X射线数量很少.X射线辐射计数随脉冲重复频率的增加而增加,随着气隙距离的改变存在峰值,且峰值出现在弥散放电模式.     

Measurements of charge transfer efficiency in a proton-irradiated swept charge device

Charged Coupled Devices (CCDs) have been successfully used in several low energy X-ray astronomical satellites over the past two decades. Their high energy resolution and high spatial resolution make them a perfect tool for low energy astronomy, such as observing the formation of galaxy clusters and the environment around black holes. The Low Energy X-ray Telescope (LE) group is developing a Swept Charge Device (SCD) for the Hard X-ray Modulation Telescope (HXMT) satellite. A SCD is a special low energy X-ray CCD, which can be read out a thousand times faster than traditional CCDs, simultaneously keeping excellent energy resolution. A test method for measuring the charge transfer efficiency (CTE) of a prototype SCD has been set up. Studies of the charge transfer inefficiency (CTI) with a proton-irradiated SCD have been performed at a range of operating temperatures. The SCD is irradiated by 3×10⁸cm^-2 10 MeV protons.     

ZnO:Ga晶体对硬X射线的时间及能量响应

 介绍了ZnO:Ga晶体对重复频率快脉冲硬X 射线的时间响应,利用X射线荧光分析仪测量了ZnO:Ga晶体对10～100 keV硬X射线的能量响应。结果表明:ZnO:Ga晶体对硬X射线响应的上升时间为316 ps,半高宽为440 ps;对40 keV以上的X射线的能量响应很平坦。该晶体可以作为一种新颖的硬X射线探测元件。     

Simulation of the in-flight calibration of the collimator alignment and PSF for HXMT

The Hard X-ray Modulation Telescope (HXMT) is an X-ray astronomical satellite in 1–250 keV, consisting of three collimated instruments. We present the in-flight calibration approach of the collimator alignment and Point Spread Function (PSF) for HXMT, using both the direct fitting method and the imaging method. According to observational simulations of the Crab Nebula, we find that these two methods produce almost the same calibration accuracy of the alignment, and with a one-day scanning observation, the alignment can be calibrated to better than 0.45′ and 0.1′ along the wide and narrow directions of the Field of View (FOV) for a detector module, which corresponds to a localization accuracy of better than 0.1′ and meets the scientific requirement.     

“阳”加速器钛丝X箍缩光源辐射特性实验研究

为了利用X箍缩产生的点光源作为背光光源对丝阵Z箍缩内爆早期的负 载内部结构进行背光照相, 在"阳"加速器(电流峰值为500-800 kA, 上升时间约80 ns)上开展了钛丝(丝交叉角度为60°) X箍缩光源辐射特性的初步实验研究. 通过X射线二极管探测器、透射光栅谱仪、晶体谱仪和狭缝相机等诊断设备获取了箍缩点光源的辐射功率达到1.5 GW左右, 辐射能量约为1 J, 光子能量为keV量级的辐射能谱范围主要集中在1-4 keV能段, 点光源尺寸小于15 μm, 其时间尺度(辐射脉冲半高宽)达到了200 ps. 对光源特征信息进行了初步分析, 同时掌握了有效获取钛丝X箍缩单脉冲点光源的方法.