Cherenkov gamma-ray telescopes: Past,present, future. The ALEGRO project

A brief overview of the history of atmospheric Cherenkov gamma-ray telescopes is given. Topical problems of modern astrophysics and fundamental physics to be solved with these instruments are listed. The ALEGRO project of a low-threshold gamma-ray observatory is characterized in detail. The aim of this project is to examine cosmic gamma-ray sources (especially the rapidly variable gamma-ray sources, gamma-ray transients) with high statistics of detected photons in the energy range of 5–50 GeV.     

基于压缩感知理论的非线性γ谱分析方法

γ谱分析是一种重要的放射性核素定量分析方法. 弱峰的检测和重叠峰的分解是γ 谱分析中的难点. 为了解决这两个问题, 基于压缩感知理论, 提出了一种新的γ 谱分析方法. 这一方法从谱仪对γ 谱调制的物理机理出发, 通过数学建模, 将γ 谱分析转化为一个以真实γ 谱为解的求逆问题, 并在压缩感知理论框架下, 运用γ 谱特征峰的稀疏性, 进行逆问题的求解, 直接获得γ 谱的估计结果. 数值模拟结果和蒙特卡洛模拟结果表明: 该方法能在降低统计涨落的同时, 有效减小谱仪调制带来的能谱展宽, 从而提高γ 谱分析精度. 关键词： γ谱分析')" href="#">γ谱分析 压缩感知 非线性 逆问题     

基于信息理论的γ能谱辨识新方法

提出了一种基于相对熵的放射源γ能谱识别方法。首先,利用主成分分析(PCA)算法压缩数据,构造γ射线能谱的特征空间。然后,采用随机化技术(RT)来使特征空间中γ射线能谱的特征值归一化,这样,γ射线能谱的特征空间可以看作是概率空间。最后,定义两个概率空间的相对熵来测量两个γ射线能谱的相对差异。大量实验表明,所提方法能够更加有效地辨识γ射线能谱, 不仅计算量小,而且对诸如统计浮动、谱峰偏移、底噪等因素具有很高的鲁棒性。     

Characteristics of the GAMMA-400 gamma-ray telescope for searching for dark matter signatures

The GAMMA-400 gamma-ray telescope currently under development is designed to measure fluxes of gamma rays and electron-positron cosmic-ray components, which could be associated with the annihilation or decay of dark matter particles, and to survey in detail the celestial sphere in order to search for and investigate discrete gamma-ray sources; to measure the energy spectra of Galactic and extragalactic dif- fuse gamma-ray emissions; and to study gamma-ray bursts and the gamma-ray emissions of active Sun. The GAMMA-400 energy range is 100 MeV to 3000 GeV. The gamma-ray telescope has an angular resolution of ～0.01°, an energy resolution of ～1%, and a proton rejection factor of ～10⁶. The GAMMA-400 will be installed on Russia’s Navigator space platform. Observations are planned to commence in 2018.     

Gamma-ray direct observations from space

Summary This paper is devoted to problems of gamma-ray astronomy in the energy range <10¹¹ eV. Measurements of spectra and fluxes in this energy range are carried out by means of direct observations from space. Most of the discussed results have been performed with the four telescopes of the Compton Gamma-Ray Observatory. The main topics of the paper are: diffuse galactic gamma-ray emission, point-like galactic gamma-ray sources, gamma-ray line emission, gamma-ray bursts and active galactic nuclei. Rapporteur talk given at the XXIV International Cosmic-Ray Conference, Rome, August 28–September, 8, 1995.     

High-resolution gamma-ray radiography produced by a laser-plasma driven electron source

An electron beam from a laser-plasma accelerator is converted into a gamma-ray source using bremsstrahlung radiation in a dense material. The gamma-ray beam has a pointlike source size because it is generated by a high quality electron beam with a small source size and a low divergence. Using this gamma-ray source, the radiography of complex and dense objects with submillimeter resolution is performed. It is the first evidence of a gamma-ray source size of a few hundreds micrometers produced with laser-driven accelerators. This size is consistent with results from Monte Carlo simulations.     

Consistent empirical physical formula construction for recoil energy distribution in HPGe detectors by using artificial neural networks

The gamma-ray tracking technique is a highly efficient detection method in experimental nuclear structure physics. On the basis of this method, two gamma-ray tracking arrays, AGATA in Europe and GRETA in the USA, are currently being tested. The interactions of neutrons in these detectors lead to an unwanted background in the gamma-ray spectra. Thus, the interaction points of neutrons in these detectors have to be determined in the gamma-ray tracking process in order to improve photo-peak efficiencies and peak-to-total ratios of the gamma-ray peaks. In this paper, the recoil energy distributions of germanium nuclei due to inelastic scatterings of 1–5 MeV neutrons were first obtained by simulation experiments. Secondly, as a novel approach, for these highly nonlinear detector responses of recoiling germanium nuclei, consistent empirical physical formulas (EPFs) were constructed by appropriate feedforward neural networks (LFNNs). The LFNN-EPFs are of explicit mathematical functional form. Therefore, the LFNN-EPFs can be used to derive further physical functions which could be potentially relevant for the determination of neutron interactions in gamma-ray tracking process.     

用于脉冲n/γ混合场γ强度测量的ICI探测器

研制成功一种基于康普顿效应, 用于脉冲裂变n/γ混合场γ强度绝对测量的新型辐射探测器—ICI(绝缘体－导体－绝缘体)探测器. 除具有现有真空康普顿和介质康普顿探测器时间响应快、线性电流大、抗辐射干扰能力强等优点外,该探测器从结构上抑制了真空康普顿在快脉冲γ测量中的前后负冲信号, 并且工作时不需要高真空, 而γ灵敏度却与同尺寸介质康普顿探测器相当. 由于其探测灵敏介质厚度小于2mm, 因而在群脉冲辐射探测中, 不会显著影响后续和周围探测器的 测量环境, 是一种探测脉冲γ射线较理想的探测器.     

Experimental research on performances of the imaging plates applied in gamma-ray imaging

Experimental studies on the basic characteristics of IPs applied in T-ray imaging are carried out by utilizing isotopic y-ray sources. The 1.25 MeV T-ray sensitivity of the BAS-MS and BAS-TR imaging plates and their enhanced sensitivity by covering appropriate Compton conversion foils are measured based on the studies of the image intensity linear calibration, time attenuation laws and the influence of scanning parameter settings. The energy-dependent T-ray sensitivity of the IPs is also obtained by the studies of the measured sensitivity and the Monte Carlo simulated energy deposition in the IPs＇ sensitive layer. Furthermore, a method of a sandwich detection structure as well as its primary experimental validations are presented in order to increase the gamma-to-neutron ratio in a y/n mixed radiation field.     

Scientific tasks and present status of the GAMMA-400 project

The GAMMA-400 telescope is designed to investigate discrete high-energy gamma-ray sources in the energy range of 0.1–3000 GeV, to measure the energy spectra of galactic and extragalactic diffuse gammaray emissions, and to study gamma-ray bursts and gamma-ray emissions from an active Sun. The gamma-ray telescope has an angular resolution of ～0.01°, an energy resolution of ～1%, and a proton rejection factor of ～10⁶. Its special assignment is to measure fluxes of gamma rays, electrons, and positrons that could be associated with the annihilation or decay of dark matter particles.     

GAMMA-RAY AND X-RAY EMISSION FROM GAMMA-RAY-LOUD BLAZARS

We present a strong correlation of the gamma-ray (above 100 MeV) mean spectral indices α_γ and X-ray (1 keV) mean spectral indices α_X for 34 gamma-ray-loud blazars (16 BL Lac objects and 18 flat spectrum radio quasars). A strong correlation is also found between the gamma-ray flux densities F_γ and X-ray flux densities F_X in the low state for 47 blazars (17 BL Lac and 30 flat spectrum radio quasars). Possible correlation on the gamma-ray emission mechanism is discussed. We suggest that the main gamma-ray radiation mechanism is probably the synchrotron process. The gamma-ray emission may be somewhat different from that of BL Lac objects and flat spectrum radio quasars.     

Relativistic Beaming in Gamma-Ray Bursts

Relativistic beaming effect is an important radiation mechanism in explaining gamma-ray bursts, according to recent observed data by Compton Gamma-ray Observatory (CGRO). Pair production optical depth and relationship between Lorentz factor and spectral index have been calculated in considering non-uniform distribution of beam photons in gamma-ray bursts in this paper. As a comparison, we also calculate the minimum Lorenta factor for 54 observed gamma-ray bursts by CGRO.     

紧凑型单能伽马射线源

基于高亮度电子束与超短强激光相互作用的逆康普顿散射X/γ射线源具有单色性好、能量可调、偏振可控等特点,在核安全及核安保领域具有广泛的应用前景。清华大学将研制国际上首套能量达MeV的紧凑准单能伽马源装置并开展包括先进辐射成像、基于核共振荧光的物质分析检测等应用工作。给出该光源设计方案,以及针对其关键性能指标进行的优化及光源最终性能指标。目前已完成光源的设计,正在进行部件的加工采购,预计将于2023年启动装置的安装调试工作,于2025年完成项目的调试和验收。     

Gamma-ray emission in the radio galaxy NGC 5128

The results of experiments on scanning discrete high-energy cosmic gamma-ray sources obtained with the GLONASS onboard equipment in 2004–2010 are presented. A synchrotron pulsating hard gamma-ray source has been detected in the radio galaxy NGC 5128. It is hypothesized that the gamma-ray fluxes from NGC 5128 are bent near the collapsing structure located in the vicinity of the Boomerang Nebula.     

Gravitational Collapse of a Spherical Star with Heat Flow as a Possible Energy Mechanism of Gamma-Ray Bursts

We investigate the gravitational collapse of a spherically symmetric, inhomogeneous star, which is described by a perfect fluid with heat flow and satisfies the equation of state p = p/3 at its center. In the process of the gravitational collapse, the energy of the whole star is emitted into space. And the remaining spacetime is a Minkowski one without a remnant at the end of the process. For a star with a solar mass and solar radius, the total energy emitted is at the order of 10^54 erg, and the time-scale of the process is about 8 s. These are in the typical values for a gamma-ray burst. Thus, we suggest the gravitational collapse of a spherical star with heat flow as a possible energy mechanism of gamma-ray bursts.     

Comparison of two position sensitive gamma-ray detectors based on continuous YAP and pixellated NaI(TI) for nuclear medical imaging applications

Dedicated position sensitive gamma-ray detectors based on position sensitive photomultiplier tubes (PSPMTs) coupled to scintillation crystals, have been used for the construction of compact gamma-ray imaging systems, suitable for nuclear medical imaging applications such as small animal imaging and single organ imaging and scintimammography. In this work, the performance of two gamma-ray detectors：a continuous YAP scintillation crystal coupled to a Hamamastu R2486 PSPMT and a pixellated NaI(TI) scintillation array crystal coupled to the same PSPMT, is compared. The results show that the gamma-ray detector based on a pixellated NaI(TI) scintillation array crystal is a promising candidate for nuclear medical imaging applications, since their performance in terms of position linearity, spatial resolution and effective field of view (FOV) is superior than that of the gamma-ray detector based on a continuous YAP scintillation crystal. However, a better photodetector (Hamamatau H8500 Flat Panel PMT, for example) coupled to the continuous crystal is also likely a good selection for nuclear medicine imaging applications.     

γ射线暴的研究概况

γ射线暴是宇宙中自从大爆炸以来最猛烈的爆发现象，它在几十秒钟的时间内所释放的能量相当于太阳一生（约一百亿年）所释放能量的几百倍！文章简要介绍了γ射线暴的新近研究进展，其中包括：简要说明了观测事实，并在此基础上建立标准火球模型，阐述了γ射线暴及其余辉的运动和演化规律，讨论了偏离标准模型的种种观测现象以及这些后标准效应所包含的重要天体物理意义。进而讨论了至今仍不清楚的能源机制问题，也指出了这个领域的研究前景。     

Comparison of two position sensitive gamma-ray detectors based on continuous YAP and pixellated NaI(TI) for nuclear medical imaging applications

Dedicated position sensitive gamma-ray detectors based on position sensitive photomultiplier tubes (PSPMTs) coupled to scintillation crystals, have been used for the construction of compact gamma-ray imaging systems, suitable for nuclear medical imaging applications such as small animal imaging and single organ imaging and scintimammography. In this work, the performance of two gamma-ray detectors: a continuous YAP scintillation crystal coupled to a Hamamastu R2486 PSPMT and a pixellated NaI(TI) scintillation array crystal coupled to the same PSPMT, is compared. The results show that the gamma-ray detector based on a pixellated NaI(TI) scintillation array crystal is a promising candidate for nuclear medical imaging applications,since their performance in terms of position linearity, spatial resolution and effective field of view (FOV) is superior than that of the gamma-ray detector based on a continuous YAP scintillation crystal. However, a better photodetector (Hamamatau H8500 Flat Panel PMT, for example) coupled to the continuous crystal is also likely a good selection for nuclear medicine imaging applications.     

The effective growth of gamma-ray background during a thunderstorm

We present here the results of gamma-ray emission intensity measurements made during thunderstorm. The gamma-ray intensity background (GRB) grows up in an order of magnitude in the active phase of a storm. This growth is shown to be directly connected with the growth of the thundercloud electric field. Besides, the fast changes of GRB (GRB-jumps) are revealed. GRB-jumps are shown to be determined by atmospheric discharges exactly, what mean the strong direct influence of the electric field in atmosphere on gamma-ray emission.     

Extragalactic electromagnetic cascades as a possible instrument for the study of background radio emission

We analyzed the diffuse gamma-ray emission generated in the interactions between cosmic rays of ultrahigh energies and the background radiation in extragalactic space. The intensity of gamma-ray emission was calculated within a simplified model for energies E ≈ 10¹⁴ eV in different assumptions concerning the cosmic ray sources with the use of different estimates of nonthermal background radiation. It was shown that the gamma-ray radiation intensity in this energy range depends on the background radio emission and that under different assumptions concerning the radio background it can differ tens of times. It was concluded that gamma-ray emission can serve as a test for the models of background radio-frequency radiation.