HXMT卫星地面样机成像实验

硬X射线调制望远镜(HXMT)致力于实现硬X射线能段的高灵敏度巡天.HXMT地面样机已在中国科学院高能物理研究所粒子天体物理重点实验室建成.它包括18个栅条准直的NaI(Tl)/CsI(Na)复合晶体探测器,总有效探测面积为5000cm². 探测器工作在20—250keV,视场范围5.7°×5.7°通过近距离放射源成像实验和直接解调成像方法的使用,地面样机能够达到2'点源定位精度和5'角分辨率(FWHM).     

空间硬X射线调制望远镜

用宇宙作为物理实验室,探索在地球上无法企及的条件下,例如极早期宇宙或黑洞视界附近强引力场中的物理规律,已成为新世纪物理学和天文学共同的前沿课题;空间天文观测是其中一个最重要的研究途径.自主研制和发放空间硬X射线调制望远镜(HXMT),实现中国空间天文卫星零的突破,是中国<"十一·五"空间科学发展规划>的目标之一.HXMT将实现宽波段X射线(1-250 keV)巡天,其中在硬X射线波段具有世界最高灵敏度和空间分辨率,发现大批被尘埃遮挡的超大质量黑洞和未知类型天体,探测宇宙硬X射线背景辐射;HXMT还将通过对黑洞和其他高能天体宽波段X射线时变和能谱的观测,研究致密天体极端物理条件下的动力学和辐射过程.基于成像技术创新提出HXMT项目迄今已有15年,能不能抓住技术创新所提供的科学机遇仍然是一个严重的挑战.     

封面照片说明

 中科院高能所研究人员正在研制的硬X射线调制望远镜HXMT,是目前世界上具有高灵敏度和较好空间分辨本领的空间硬X射线望远镜。该探测系统由18个单体组成,每个单体包括一个板条式准直器和一个探测面积为280平方厘米的NaI/CsI复合晶体探测器。     

基于单片有源像素传感器的探测模块测试研究

硅像素探测器因具有优异的空间分辨率、极高的耐计数能力和较低的功耗等优点,近年来已被广泛应用于高能对撞机实验的顶点探测器和内径迹探测器.基于MIMOSA28芯片的硅像素探测器研究是北京谱仪Ⅲ漂移室内室的升级预研方案之一,该方案计划建造一个漂移室内室1/10规模的模型.探测模块是该模型的基本探测单元.为了对探测模块的性能进行研究,搭建了实验室测试系统.该系统主要由五层探测模块、读出电子学系统以及数据获取系统组成.本文围绕带有触发标记的连续数据读出方法的实现、探测模块的噪声水平和放射源响应测试以及击中位置重建算法研究展开.测试结果验证了探测模块工作性能良好,触发读出逻辑正确,而且重建算法准确有效,为后续探测模块性能的进一步研究奠定了基础.     

高时间分辨MRPC的位置灵敏读出方法

根据MRPC工作机制和高时间分辨的特性, 研制一种位置灵敏MRPC原型及读出方法. 该探测器具有10个220μm气隙, 有效探测面积为20cm×20cm. 前端电子学采用专用ASIC芯片, 具有快时间响应和输入电荷-输出信号宽度的转换功能. 采取同时读取信号传输时间差和感应信号分布的方法实现两维读出. 对该探测器性能的束流测试结果显示: 沿着读出条方向及其垂直方向的位置分辨分别为4.5mm和1.6mm, 其时间分辨达到63ps, 探测效率>95%.     

HXMT卫星的观测规划与数据处理

正HXMT卫星在轨运行期间,需要开展一系列的空间观测,以便对天文现象进行研究。空间探测涉及到多个过程,需要考虑多种因素的约束,本文将详细给出从观测任务的提出,到任务安排、数据处理及科学分析的全过程。一、引言硬X射线调制望远镜(HXMT)是我国首颗X射线天文卫星,卫星发射升空后,预期在轨工作四年。在此期间,为实现预期的科学目标,将开展一系列的空间X射线探测,通过对这些观测数据的处理分析,     

写在前面的话

正我国第一颗X射线天文望远镜——硬X射线调制望远镜(HXMT)——预计于2016年年底发射升空。HXMT的成功研制表明我国在空间X射线天文探测器设计、制造以及配套的性能测试(标定)以及地面科学应用系统等方面取得了全面突破,跻身国际上少数能够自主研制一颗X射线天文卫星的全部科学仪器的国家。为介绍X射线天文科学研究和HXMT的基本情     

基于Rydberg原子天线的太赫兹测量

Rydberg原子在微波和太赫兹频段具有极大的电偶极矩,利用量子干涉效应可实现对该频段电磁波场强的高灵敏探测,理论上灵敏度可达到远高于现有探测技术的水平.基于Rydberg原子量子效应的电磁场探测及精密测量技术在太赫兹的场强和功率计量、太赫兹通信和太赫兹成像等方面有着巨大的应用前景.本文回顾了基于Rydberg原子量子干涉效应实现电磁波电场自校准和可溯源测量的基本理论和实验技术,详细介绍了基于Rydberg原子的高灵敏太赫兹场强测量、太赫兹近场高速成像和太赫兹数字通信的基本原理和技术方案.最后简单介绍了本研究团队正在开展的基于Rydberg原子的太赫兹探测工作.     

直接解调方法在嫦娥一号卫星X射线谱仪地面验证实验数据分析中的应用

"嫦娥一号"卫星是我国的第一颗月球探测卫星,运行轨道高度为200 km,预计工作寿命为一年,其上配备的X射线成像谱仪具备了对月表进行X射线探测、成像和对太阳X射线进行监测的功能.该X射线谱仪由两个全同的探测器阵列组成,其中,为了实现对月表主要化学元素分布及其含量进行探测的科学目标,在每个探测器阵列还配备了2个低能探测器单元.这4路低能探测器单元的面积为25 mm2,采用的都是厚度为500 μm,具有优良探测性能的Si-PIN探测器,其探测能区为1～10 keV,能量分辨率为～5%@5.9 kev.文章主要介绍了嫦娥一号卫星X射线谱仪的地面验证实验,并且根据X射线谱仪的能量响应矩阵,利用直接解调方法和基本参数法对X射线谱仪地面验证实验中的探测数据,特别是对盲测样品中的Mg,Al,Si等元素进行了定性和定量分析.     

三环型波导微环谐振器无热化生物传感器

针对温度波动对生物传感器探测性能的影响,本文提出了一种三环型波导微环谐振器无热化生物传感器。传感器芯片以3个微环谐振器为一个传感单元,3个微环谐振器并联排列,且分别工作在1 500、1 550和1 580 nm波长,以其中两个为基本探测微环,另外一个作为备用微环。由于3个微环工作波长不同,可通过运算消去温度对探测谱线变化值的影响项,从而实现传感器的无热化探测。相对于传统的无热化方案,本方案制备材料不受限,且无需参考微环,不存在浪费面积,集成度更高。另外备用微环的设计可以防止部分微环工作失常时传感器无法工作情况的发生,提高了系统的稳定性及可靠性。     

HXMT主探测器磁屏蔽设计与实验结果

硬X射线调制望远镜(HXMT)致力于实现硬X射线的高灵敏度巡天观测, 描绘硬X射线天图, 并对特殊天体作高灵敏度连续观测, 得到其辐射的能谱和时间变化等. 为了减少空间磁场对观测的影响, 确保本底计数的稳定性和能谱测量的精度, 我们用坡莫合金制成的磁屏蔽罩对HXMT主探测器的光电倍增管(PMT)进行了磁屏蔽处理. 实测表明, 在地面地磁场环境下PMT的最大增益变化幅度为6%; 它与自动增益控制系统配合能使在轨PMT增益变化幅度小于1%, 探测器本底计数变化小于0.1%.     

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.     

Development of a prototype of the ME readout electronics onboard the HXMT satellite

A prototype of the ME readout electronics onboard the Hard X-ray Modulate Telescope (HXMT) satellite is developed. Application Specific Integrated Chip (ASIC) is used to construct the front end electronics due to a large number of detectors. Field Programmable Gate Array (FPGA) is connected to the ASIC as a state machine controller and data FIFO in the DAQ system. A USB board is designed to communicate between the DAQ system and the computer. The design goals and features, the operation of the system and the preliminary performance of the prototype are described. The testing results show that the design goals of the prototype system have been achieved.     

Calibrating the HXMT collimators using diffuse illumination

We propose a new method to calibrate the HXMT collimators by measuring the optical point spread function (PSF) of the hard X-ray modulation telescope (HXMT). The light transmission of the collimator at different viewing angles with a camera and a diffuse backlight placed behind the collimator is measured. This method is much easier to accomplish than measuring the PSF with a parallel optical beam. The experimental results are very consistent with the simulations. The PSF of the collimator of the high energy X-ray telescope on HXMT is found to be in good agreement with the design, with accuracy better than 1 arcmin.     

Development of a prototype of the ME readout electronics onboard the HXMT satellite

A prototype of the ME readout electronics onboard the Hard X-ray Modulate Telescope （HXMT） satellite is developed. Application Specific Integrated Chip （ASIC） is used to construct the front end electronics due to a large number of detectors. Field Programmable Gate Array （FPGA） is connected to the ASIC as a state machine controller and data FIFO in the DAQ system. A USB board is designed to communicate between the DAQ system and the computer. The design goals and features, the operation of the system and the preliminary performance of the prototype are described. The testing results show that the design goals of the prototype system have been achieved.     

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.     

Silicon detector technology development in India for the participation in international experiments

A specific research and development program has been carried out by BARC in India to develop the technology for large area silicon strip detectors for application in nuclear and high energy physics experiments. These strip detectors will be used as pre-shower detector in the CMS experiment at LHC, CERN for π ⁰/λ rejection. The fabrication technology to produce silicon strip detectors with very good uniformity over a large area of ∼40 cm², low leakage currents of the order of 10 nA/cm² per strip and high breakdown voltage of >500 V has been developed by BARC. The production of detectors is already under way to deliver 1000 detector modules for the CMS and 90% production is completed. In this paper, research and development work carried out to develop the detector fabrication technology is briefly described. The performance of the silicon strip detectors produced in India is presented. The present status of the detector technology is discussed.      

100 mK bolometers for the submillimetre common-user bolometer array (scuba) I. Design and construction

We describe the design and construction of bolometric detectors for SCUBA - the Submillimetre Common-User Bolometer Array for the James Clerk Maxwell Telescope in Hawaii. The instrument contains 131 individual detectors, in two arrays, optimized for the submillimetre atmospheric transmission windows. The detectors are cooled by dilution refrigeration to a temperature of 100 mK, so that the receiver performance will be limited by photon noise from the sky and telescope background in all wavebands. A future paper will describe the performance of the detectors with reference to typical data obtained during the laboratory commissioning period.     

Observation constraints of the hard X-ray modulation telescope HXMT

The hard X-ray modulation telescope HXMT is a low orbit X-ray space telescope whose main science goals are to accomplish a hard X-ray all sky survey and to study timing and spectral characteristics of X-ray sources. HXMT has three kinds of science instruments: the high energy X-ray detector (HE), the medium energy X-ray detector (ME) and the low energy X-ray detector (LE). The observation schedule of HXMT is a key to achieving the science goal of HXMT, and the analysis of the observation constraints is one of the first tasks in making the observation schedule. This paper analyzes how the observation constraints influence the sky visibility and the visible time distribution of X-ray sources and discusses the schedule strategy with regard to the observation constraints.