用羊八井二期/加密阵列数据寻找3～10TeV能区的宇宙伽玛暴
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摘要
宇宙γ射线暴发现象(Garoma-Ray Bursts，简称γ暴或GRB)是上个世纪的一个重要天文发现，同时也是保留至今的最大天文之谜。γ暴问题与宇宙暗物质、恒星级(巨型)黑洞天体的观测认证以及活动星系核的物理解释一起，合称为“伴随人类进入二十一世纪的四大天文难题”。
γ暴是一种强烈的瞬态(transient)暴发过程，最早是由前苏联的核爆炸监测卫星维拉(Vela)在1967年偶然发现的．自γ暴现象被发现至今的三十多年时间里，人们对该现象进行了大量的实验观测，证实了它的真实存在并取得了较丰富的观测资料，与此同时，围绕γ暴的起源、初始能源和辐射过程等问题，人们建立了数百个理论模型，试图对之进行解释，但这些模型都只能部分地解释γ暴的某些特征，同时这些模型之间还存在较多分歧。从费米(1fm=10~(-15)m)尺度的宇宙原生黑洞，到数十公里尺度的中子星，都被作为γ暴的候选天体进行了考察。在美国天文卫星CGRO上的BASTE实验之前，γ暴现象集中联系于银河内磁中子星上的局部物理过程；BASTE实验把γ暴推向了宇宙学距离，这使γ暴与宇宙暗物质，原生黑洞，引力波以及强相互作用等现代物理问题联系了起来。目前关于γ暴的理论模型可以说是“众说纷纭，各执一词”，其数目之多甚至有让人“目不暇接，无所适从”的感觉。因此，目前的观测数据还不足以对γ暴现象作出圆满的解释。
观测表明，γ暴的发生时间和空间位置是完全随机的，至今未发现γ暴有重复暴发现象，这使人们很难对之进行有预先准备的观测；γ暴的持续时间往往很短，这造成难于对之进行细致的观测。γ暴的上述特征是造成其观测困难的主要原因，同时也是难以对之作出全面而圆满的理论解释的原因。
γ暴的起源问题，也即γ暴的发生距离问题，在γ暴的研究中起着至关重要的作用。目前γ暴的起源之争，集中于该现象是发生在银河系内的过程，还是普遍发生在宇宙学距离上的过程。因为按观测数据推算，暴的不同起源对应着不同的爆发能量，其量值甚至可相差二十几个数量级。不同量级的释放能量自然对应不同的物理过程。所以，没有γ暴源的距离的知识，就不能准确地判断暴的产生机制，也就不能对该现象作出正确的解释。虽然目前关于γ暴的卫星实验已观测到了数千个γ暴，并对γ暴的时间结构、能谱形状以及空间分布等方面作了集中研究，但卫星实验由于受其探测器接收面积的限制，对γ暴到达方向的定位精度较低，故不能很好的确定γ暴的对应天体。因此目前只能通过间接的方法来判断这些暴的起源。早期的观测资料和BASTE实验都表明γ暴的空间分布呈高度各向同性，其频率一大小谱(logN(〉S)—logS)表明随距离增加弱暴数目有增多的趋势，这显示了γ暴的宇宙学起源。γ暴在其它波段的
【
g
一
伴随物…ounerprt）可以提供其距离的有关信息，但目前关于Y暴伴随物的观
测信息还相当缺乏，还不能给确定其距离提供太多帮助．意大利一荷兰天文卫
星BePPOSAX在1997年观测到数个丁暴的光学、射电、X射线等多波段“余辉
恒fterglow厂，但这也仅给丫暴起源的研究带来一丝“曙光＼＿，
是否存在超高能p1TeV＊暴，或丫暴的超高能伴随物，是一个有意义的
问题．因为1－100DV的初级宇宙丁光子在穿过宇宙学距离时，将遭到宇宙
红外背景光子和微波背景光子的强烈吸收而不能达到地球大气顶部．固此，如
果找到了1一100TeV能区的丁暴，或观测到了）暴的1－10（）Te伴随丫光
子，就可判定丫暴为银河系内起源；否则，若没有观测到上述过程，也可给出
7暴发生距离的上限情息．同样由于受其探测器接受面积的限制，卫星实验一
般工作于GeV能区，它对超高能7暴的观测是无能为力的．目前卫星实验所
观测到的丫暴的光子能量主要集中于10KeV—10MeV，只有少量丫暴的光子
能量达GeV量级．天文观测的地面实验和空间实验历来有着互相衔接、互相补
充、互相验证的关系，二者的作用不可互相替代，因此，用地面设施寻找超高
能区的Y暴，自然有十分重要的意义．
西藏羊八井二期／加密阵列目前在世界同类装置中，具有最高的簇射触发
率和最低的观测阈能，其角分辨率好于1＼ 因此很适合于进行超高能，暴的4
观测寻找．本文第七章使用羊八井二期／加密阵列1997年2月至1998年6月
期间的重建数据，进行了3－10Dv能区丁暴的全天区独立寻找，同时也进行
了3DV能区＊＊8＊即暴的符合寻找．在丁暴的独立寻找工作中采用分＊n方
法，取时间间隔凸t—IS、105、1005三种情况，对 EAS事例进行了统计分
析．在上述分析中，使用的羊八井二期阵列Kibet 11）和加密阵列叮ibet HD）所
得到的＊＊s事例分别约为2石Xlo帅5亿）个和4．SXlo…8亿）个．统计结果
表明，有较多事例团显示了对背景的超出，其中有部分事例团的统计显著性明
显超过了3。 同时，有少数事例团的统计显著性达到了4a水平，显示了存在
3－10
The phenomenon of Gamma-Ray Bursts(GRB) is an important discovery in astronomy, which obtained in the 70s of the last century. Upto now, the nature and the origin of GRBs remains a long-stand mystery. Gamma-Ray Bursts, Dark Matters, Black Holes and Active Galactic Nuclei(AGN) are commonly recognized to be "the four major unsolved problems in astronomy".
Gamma-Ray Bursts is a strong and transientive course of explosive energy relase. The first dection of GRBs was made occasionally by the former Soviet nuclear monitoring satellites of Vela in 1967. During the past more than 30 years, the subject of GRBs has received consider-able attention, both theoretically and experimentally. More than several hundreds of theoretical modela for GRBs has been proposed to explain GRBs' origin, primary energy source and radia-tion mechanism. Candidate objects for GRBs ranged fronti Fermi-sized cosmic primordial black holes to lOkm-sized accreting neutron stars. The widely differing scenarios of energy relase and 7-ray production mechanism of a GRB was examined in these modela. There is, however, much disagreement on the explanation for GRBs. The consensus beforce the BASTE experiment which aboard on the satellite of CGRO appears to be that the GRBs originate somehow on or near neutron stars. These neutron stars are known to exist in the Galaxy and to be with intense magnetic field. The BASTE experiment imply that GRBs are very common events which being occur frequently in the cosmic space. Many of the models are favored that GRBs should be associated with some advanced subjects of physics, such as dark matter, primordial black hole, gravitational wave and strong interaction. Although a wealth of information about GRBs has been obtained, these informations has proven insufficient to constrain GRB models to reach an acceptable explanation to the phenomenon of GRBs.
Because of the brief, transient nature of GRBs, and due to the obvious difficulty in not knowing a priori when and where a GRB will occur, it is diffcult to achieve a pre-waiting and detailed observation. This brings the great diffculty to GRBs' observation and theoretical study.
One of the major observation goal is to determine the arrivial direction of a GRB, or the host object of a GRB. This is a key question to the models of GRBs. The amount of relased energy of a GRB can not be estimated accurately without the GRB's distance, and as a consequent, the actual radiation mechanism of GRBs would not be established correctly.
The satellite experiments of GRBs are usually to be done with large error in direction measurment because of its small area of the detector. Although the satellite experiment has detected several thousands of GRBs and get rich information about the time structure, energy spectrum and spatial distribution of GRBs, but they can not give clear conclusion for the origin of GRBs. The early observation of GRBs and the latter BASTE experiment both confirmed that the spatial distribution of GRBs is highly isotropy and the curve of logN(>S)-logS shows that the number of weak GRBs rise with their distances. So the cosmological model of GRBs was commonly considered. The information of a counterpart, a GRB-related radiation at other energy band, can provide a part of knowledge about the distance of a GRB. The satellite
experiment of BeppoSAX has detected the afterglow of some GRBs in energy band of light, radio wave and X-rays. But the lack of observed counterparts at present can provide less help to determine the origin of GRBs.
Searches for the UHE(ultra-high energy, >!TeV) GRBs can help determine whether or not the GRBs are distributed cosmologicallv. Because the UHE 7-rays are strongly attenuated by the extragalactic background radiation field of the infrared and 2.7K microwave photons. The UHE detectors of ground-based experiment should be insensitive to the cosmological GRBs. Ground-based experiment and satellite experiment work at different energy region, their data should be examined and supported by each other. The energy of 7-rays in GRBs
γ暴是一种强烈的瞬态(transient)暴发过程，最早是由前苏联的核爆炸监测卫星维拉(Vela)在1967年偶然发现的．自γ暴现象被发现至今的三十多年时间里，人们对该现象进行了大量的实验观测，证实了它的真实存在并取得了较丰富的观测资料，与此同时，围绕γ暴的起源、初始能源和辐射过程等问题，人们建立了数百个理论模型，试图对之进行解释，但这些模型都只能部分地解释γ暴的某些特征，同时这些模型之间还存在较多分歧。从费米(1fm=10~(-15)m)尺度的宇宙原生黑洞，到数十公里尺度的中子星，都被作为γ暴的候选天体进行了考察。在美国天文卫星CGRO上的BASTE实验之前，γ暴现象集中联系于银河内磁中子星上的局部物理过程；BASTE实验把γ暴推向了宇宙学距离，这使γ暴与宇宙暗物质，原生黑洞，引力波以及强相互作用等现代物理问题联系了起来。目前关于γ暴的理论模型可以说是“众说纷纭，各执一词”，其数目之多甚至有让人“目不暇接，无所适从”的感觉。因此，目前的观测数据还不足以对γ暴现象作出圆满的解释。
观测表明，γ暴的发生时间和空间位置是完全随机的，至今未发现γ暴有重复暴发现象，这使人们很难对之进行有预先准备的观测；γ暴的持续时间往往很短，这造成难于对之进行细致的观测。γ暴的上述特征是造成其观测困难的主要原因，同时也是难以对之作出全面而圆满的理论解释的原因。
γ暴的起源问题，也即γ暴的发生距离问题，在γ暴的研究中起着至关重要的作用。目前γ暴的起源之争，集中于该现象是发生在银河系内的过程，还是普遍发生在宇宙学距离上的过程。因为按观测数据推算，暴的不同起源对应着不同的爆发能量，其量值甚至可相差二十几个数量级。不同量级的释放能量自然对应不同的物理过程。所以，没有γ暴源的距离的知识，就不能准确地判断暴的产生机制，也就不能对该现象作出正确的解释。虽然目前关于γ暴的卫星实验已观测到了数千个γ暴，并对γ暴的时间结构、能谱形状以及空间分布等方面作了集中研究，但卫星实验由于受其探测器接收面积的限制，对γ暴到达方向的定位精度较低，故不能很好的确定γ暴的对应天体。因此目前只能通过间接的方法来判断这些暴的起源。早期的观测资料和BASTE实验都表明γ暴的空间分布呈高度各向同性，其频率一大小谱(logN(〉S)—logS)表明随距离增加弱暴数目有增多的趋势，这显示了γ暴的宇宙学起源。γ暴在其它波段的
【
g
一
伴随物…ounerprt）可以提供其距离的有关信息，但目前关于Y暴伴随物的观
测信息还相当缺乏，还不能给确定其距离提供太多帮助．意大利一荷兰天文卫
星BePPOSAX在1997年观测到数个丁暴的光学、射电、X射线等多波段“余辉
恒fterglow厂，但这也仅给丫暴起源的研究带来一丝“曙光＼＿，
是否存在超高能p1TeV＊暴，或丫暴的超高能伴随物，是一个有意义的
问题．因为1－100DV的初级宇宙丁光子在穿过宇宙学距离时，将遭到宇宙
红外背景光子和微波背景光子的强烈吸收而不能达到地球大气顶部．固此，如
果找到了1一100TeV能区的丁暴，或观测到了）暴的1－10（）Te伴随丫光
子，就可判定丫暴为银河系内起源；否则，若没有观测到上述过程，也可给出
7暴发生距离的上限情息．同样由于受其探测器接受面积的限制，卫星实验一
般工作于GeV能区，它对超高能7暴的观测是无能为力的．目前卫星实验所
观测到的丫暴的光子能量主要集中于10KeV—10MeV，只有少量丫暴的光子
能量达GeV量级．天文观测的地面实验和空间实验历来有着互相衔接、互相补
充、互相验证的关系，二者的作用不可互相替代，因此，用地面设施寻找超高
能区的Y暴，自然有十分重要的意义．
西藏羊八井二期／加密阵列目前在世界同类装置中，具有最高的簇射触发
率和最低的观测阈能，其角分辨率好于1＼ 因此很适合于进行超高能，暴的4
观测寻找．本文第七章使用羊八井二期／加密阵列1997年2月至1998年6月
期间的重建数据，进行了3－10Dv能区丁暴的全天区独立寻找，同时也进行
了3DV能区＊＊8＊即暴的符合寻找．在丁暴的独立寻找工作中采用分＊n方
法，取时间间隔凸t—IS、105、1005三种情况，对 EAS事例进行了统计分
析．在上述分析中，使用的羊八井二期阵列Kibet 11）和加密阵列叮ibet HD）所
得到的＊＊s事例分别约为2石Xlo帅5亿）个和4．SXlo…8亿）个．统计结果
表明，有较多事例团显示了对背景的超出，其中有部分事例团的统计显著性明
显超过了3。 同时，有少数事例团的统计显著性达到了4a水平，显示了存在
3－10
The phenomenon of Gamma-Ray Bursts(GRB) is an important discovery in astronomy, which obtained in the 70s of the last century. Upto now, the nature and the origin of GRBs remains a long-stand mystery. Gamma-Ray Bursts, Dark Matters, Black Holes and Active Galactic Nuclei(AGN) are commonly recognized to be "the four major unsolved problems in astronomy".
Gamma-Ray Bursts is a strong and transientive course of explosive energy relase. The first dection of GRBs was made occasionally by the former Soviet nuclear monitoring satellites of Vela in 1967. During the past more than 30 years, the subject of GRBs has received consider-able attention, both theoretically and experimentally. More than several hundreds of theoretical modela for GRBs has been proposed to explain GRBs' origin, primary energy source and radia-tion mechanism. Candidate objects for GRBs ranged fronti Fermi-sized cosmic primordial black holes to lOkm-sized accreting neutron stars. The widely differing scenarios of energy relase and 7-ray production mechanism of a GRB was examined in these modela. There is, however, much disagreement on the explanation for GRBs. The consensus beforce the BASTE experiment which aboard on the satellite of CGRO appears to be that the GRBs originate somehow on or near neutron stars. These neutron stars are known to exist in the Galaxy and to be with intense magnetic field. The BASTE experiment imply that GRBs are very common events which being occur frequently in the cosmic space. Many of the models are favored that GRBs should be associated with some advanced subjects of physics, such as dark matter, primordial black hole, gravitational wave and strong interaction. Although a wealth of information about GRBs has been obtained, these informations has proven insufficient to constrain GRB models to reach an acceptable explanation to the phenomenon of GRBs.
Because of the brief, transient nature of GRBs, and due to the obvious difficulty in not knowing a priori when and where a GRB will occur, it is diffcult to achieve a pre-waiting and detailed observation. This brings the great diffculty to GRBs' observation and theoretical study.
One of the major observation goal is to determine the arrivial direction of a GRB, or the host object of a GRB. This is a key question to the models of GRBs. The amount of relased energy of a GRB can not be estimated accurately without the GRB's distance, and as a consequent, the actual radiation mechanism of GRBs would not be established correctly.
The satellite experiments of GRBs are usually to be done with large error in direction measurment because of its small area of the detector. Although the satellite experiment has detected several thousands of GRBs and get rich information about the time structure, energy spectrum and spatial distribution of GRBs, but they can not give clear conclusion for the origin of GRBs. The early observation of GRBs and the latter BASTE experiment both confirmed that the spatial distribution of GRBs is highly isotropy and the curve of logN(>S)-logS shows that the number of weak GRBs rise with their distances. So the cosmological model of GRBs was commonly considered. The information of a counterpart, a GRB-related radiation at other energy band, can provide a part of knowledge about the distance of a GRB. The satellite
experiment of BeppoSAX has detected the afterglow of some GRBs in energy band of light, radio wave and X-rays. But the lack of observed counterparts at present can provide less help to determine the origin of GRBs.
Searches for the UHE(ultra-high energy, >!TeV) GRBs can help determine whether or not the GRBs are distributed cosmologicallv. Because the UHE 7-rays are strongly attenuated by the extragalactic background radiation field of the infrared and 2.7K microwave photons. The UHE detectors of ground-based experiment should be insensitive to the cosmological GRBs. Ground-based experiment and satellite experiment work at different energy region, their data should be examined and supported by each other. The energy of 7-rays in GRBs
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