宇宙再电离时期的相关性研究，星系团中的暗物质，及修改引力理论
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摘要
宇宙再电离时期历史以及暗物质和暗能量的本质是宇宙学目前存在有待解决的重大问题。本文分三大部分,第一部分是有关宇宙再电离时期的探测,第二部分是对星系团中暗物质的研究,第三部分是对修改引力理论的研究,在这个理论下,我们不需要引入冷暗物质。
第一部分是对宇宙再电离时期的研究,这属于国家天文台重点项目21CMA的理论研究部分。大约从红移z～20第一代恒星开始大量形成到z～6宇宙被完全电离这一段时期对应宇宙的再电离时期。探测这一时期的最理想的工具是宇宙21厘米线背景辐射。另外,宇宙红外背景与软X射线背景辐射中存在未知来源的部分,有理由怀疑它们来自早期宇宙。第一代恒星所发出的紫外波段辐射和类星体所发出的硬X射线分别被红移到今天的红外和软X射线波段。它们也可以用来研究和探测早期宇宙。但是由于这些背景辐射的前景污染都过于严重,在这里我们采用互相关的方法,它可以放大有关联的信号而去掉不相关的前景。本文将分别研究来自第一代恒星的红外背景和来自类星体的X射线背景,同现有观测进行比较。我们用一个壳层模型来描述第一代恒星和类星体的21厘米辐射,并指出相对于类星体,第一代恒星对21厘米背景的贡献更大。最后给出这些信号的互相关功率谱的理论预言,并结合观测(21CMA/LOFAR,ROSAT和AKARI)讨论互相关信号的可测量性。我们看到,虽然这些互相关信号有着明显的特征,但是依然很难被观测到,这是由于现有X射线观测ROSAT和红外观测AKARI对软X射线和红外背景引入的很强的噪声。
第二部分是对星系团中暗物质的研究。标准宇宙学模型下,暗物质是星系团中的主要物质成分,它决定星系团的形成和演化。在这里,我们的研究集中在两个方面:一个是星系团CL0024+17的暗物质环(Jee et al.2007)。我们尝试在与暗物质同为无碰撞粒子的星系中寻找这样的现象。我们的研究表明,在3σ的置信级上,我们在二维投影的星系分布中无法看到类似暗物质分布的环状结构。另一个是bullet星系团所指出的暗物质中心与重子物质中心分离的现象,这一现象给出了暗物质在星系团中存在的直接证据。我们从一组星系团出发指出这样的分离在星系团中是普遍现象,并用此解释了长期存在的星系团中强引力透镜和X射线的质量差异问题。
第三部分是对修改引力理论(MOND)及其协变形式(TeVeS)的研究。我们主要研究这个理论的引力透镜效应,我们给出一个非球对称引力透镜模型,并结合CASTLES引力透镜寻天对这一模型进行研究,我们指出这个模型在MOND下可以很好的拟和多数的双像系统,但是由于MOND下测量精度和非线性效应对引力透镜影响极大,它不能拟和某些双像系统。而由于其自身的限定,无法拟和绝大多数四像系统,这是因为我们的模型无法同时产生大的剪切和大的爱因斯坦环,未来需要更为精确的三维模型。
There are three parts in this thesis. Part one is on the detection of the reionization epoch, part two focuses on dark matter in galaxy clusters, and part three presents our study of the modified gravity theory as an alternative of dark matter and dark energy.
Part one of the thesis is a contribution to the theoretical studies of the 21CMA project, one of NAOC's key project which aims at probing the epoch of reionization. The reionization epoch proceeds a period from the formation of a large amount of the first stars at z～20 to z～6 when the universe was totally ionized. This is a crucial stage of structure formation which is related to the galaxy formation and the heating, kinetic and chemical processes of the IGM. Meanwhile, the Cosmic Infrared Background (CIRB) and the Soft X-ray Background (SXRB) contain unclear components, they may come from the early universe. The UV band photons from PopIII stars and the hard X-ray photons from QSOs can be redshilted to the present infrared and soft X-ray band, respectively. These signals provide us an additional probe of the epoch of reionization. Because of the strong foregrounds of all these signals, we present a cross-correlation study. The reason is that cross-correlations can highlight the correlated signals and eliminate irrelevant foregrounds. In this thesis, we study the CIRB from PopIII stars and SXRB from QSOs. We develop a shell model to describe the 21cm signals and find that PopIII stars can provide higher 21cm signals than QSOs. At last, we predict various cross power spectra analytically, and study their detectability combined with observations (21CMA/LOFAR, ROSAT and AKARI). We find that although these cross-correlation signals have distinct features, they are difficult to be detected so far, due to the high noise of the soft X-ray and infrared backgrounds given by ROSAT and AKARI.
The second part is the study of dark matter in galaxy clusters. Our research focuses on: (1) Dark matter ring in the CL0024+17 (Jee et al. 2007). Because of the same spatial distributions of dark matter and cluster galaxies, we study the galaxy distribution to probe the ringlike structure in the dark matter distribution. We find that, at about 3σlevel, the ringlike structure seen in the dark matter measurement is not observed in the projected 2D galaxy distribution. (2) Offset between dark matter and baryonic matter center in clusters. The X-ray and lensing study of the bullet cluster show a clear offset between dark matter and baryonic matter center. This observation gave us the direct evidence that dark matter exist on cluster scales. We point out such an offset is common in the universe from a sample of clusters, and explain the long-standing mass discrepancy between strong gravitational lensing and X-ray problem in galaxy clusters.
The third part is the research about the modified gravity theory (MOND) and its covariant formalism (TeVeS). We study the gravitational lensing of covariant MOND, we develop an analytic model for non-spherical lenses in covariant MOND, and study such a model with CASTLES survey. We use this model to obtain a reasonable MOND fit to most of the double-imaged systems. However, we also find those non-isolated double-imaged systems can not be fitted well. And most quadruple-imaged systems for which no reasonable MOND fit can be obtained with our models. We argue that, this is mostly due to the intrinsic limitation of the analytic models, we indeed showed that our models were unable to produce a large Einstein ring and a large shear at the same time.
第一部分是对宇宙再电离时期的研究,这属于国家天文台重点项目21CMA的理论研究部分。大约从红移z～20第一代恒星开始大量形成到z～6宇宙被完全电离这一段时期对应宇宙的再电离时期。探测这一时期的最理想的工具是宇宙21厘米线背景辐射。另外,宇宙红外背景与软X射线背景辐射中存在未知来源的部分,有理由怀疑它们来自早期宇宙。第一代恒星所发出的紫外波段辐射和类星体所发出的硬X射线分别被红移到今天的红外和软X射线波段。它们也可以用来研究和探测早期宇宙。但是由于这些背景辐射的前景污染都过于严重,在这里我们采用互相关的方法,它可以放大有关联的信号而去掉不相关的前景。本文将分别研究来自第一代恒星的红外背景和来自类星体的X射线背景,同现有观测进行比较。我们用一个壳层模型来描述第一代恒星和类星体的21厘米辐射,并指出相对于类星体,第一代恒星对21厘米背景的贡献更大。最后给出这些信号的互相关功率谱的理论预言,并结合观测(21CMA/LOFAR,ROSAT和AKARI)讨论互相关信号的可测量性。我们看到,虽然这些互相关信号有着明显的特征,但是依然很难被观测到,这是由于现有X射线观测ROSAT和红外观测AKARI对软X射线和红外背景引入的很强的噪声。
第二部分是对星系团中暗物质的研究。标准宇宙学模型下,暗物质是星系团中的主要物质成分,它决定星系团的形成和演化。在这里,我们的研究集中在两个方面:一个是星系团CL0024+17的暗物质环(Jee et al.2007)。我们尝试在与暗物质同为无碰撞粒子的星系中寻找这样的现象。我们的研究表明,在3σ的置信级上,我们在二维投影的星系分布中无法看到类似暗物质分布的环状结构。另一个是bullet星系团所指出的暗物质中心与重子物质中心分离的现象,这一现象给出了暗物质在星系团中存在的直接证据。我们从一组星系团出发指出这样的分离在星系团中是普遍现象,并用此解释了长期存在的星系团中强引力透镜和X射线的质量差异问题。
第三部分是对修改引力理论(MOND)及其协变形式(TeVeS)的研究。我们主要研究这个理论的引力透镜效应,我们给出一个非球对称引力透镜模型,并结合CASTLES引力透镜寻天对这一模型进行研究,我们指出这个模型在MOND下可以很好的拟和多数的双像系统,但是由于MOND下测量精度和非线性效应对引力透镜影响极大,它不能拟和某些双像系统。而由于其自身的限定,无法拟和绝大多数四像系统,这是因为我们的模型无法同时产生大的剪切和大的爱因斯坦环,未来需要更为精确的三维模型。
There are three parts in this thesis. Part one is on the detection of the reionization epoch, part two focuses on dark matter in galaxy clusters, and part three presents our study of the modified gravity theory as an alternative of dark matter and dark energy.
Part one of the thesis is a contribution to the theoretical studies of the 21CMA project, one of NAOC's key project which aims at probing the epoch of reionization. The reionization epoch proceeds a period from the formation of a large amount of the first stars at z～20 to z～6 when the universe was totally ionized. This is a crucial stage of structure formation which is related to the galaxy formation and the heating, kinetic and chemical processes of the IGM. Meanwhile, the Cosmic Infrared Background (CIRB) and the Soft X-ray Background (SXRB) contain unclear components, they may come from the early universe. The UV band photons from PopIII stars and the hard X-ray photons from QSOs can be redshilted to the present infrared and soft X-ray band, respectively. These signals provide us an additional probe of the epoch of reionization. Because of the strong foregrounds of all these signals, we present a cross-correlation study. The reason is that cross-correlations can highlight the correlated signals and eliminate irrelevant foregrounds. In this thesis, we study the CIRB from PopIII stars and SXRB from QSOs. We develop a shell model to describe the 21cm signals and find that PopIII stars can provide higher 21cm signals than QSOs. At last, we predict various cross power spectra analytically, and study their detectability combined with observations (21CMA/LOFAR, ROSAT and AKARI). We find that although these cross-correlation signals have distinct features, they are difficult to be detected so far, due to the high noise of the soft X-ray and infrared backgrounds given by ROSAT and AKARI.
The second part is the study of dark matter in galaxy clusters. Our research focuses on: (1) Dark matter ring in the CL0024+17 (Jee et al. 2007). Because of the same spatial distributions of dark matter and cluster galaxies, we study the galaxy distribution to probe the ringlike structure in the dark matter distribution. We find that, at about 3σlevel, the ringlike structure seen in the dark matter measurement is not observed in the projected 2D galaxy distribution. (2) Offset between dark matter and baryonic matter center in clusters. The X-ray and lensing study of the bullet cluster show a clear offset between dark matter and baryonic matter center. This observation gave us the direct evidence that dark matter exist on cluster scales. We point out such an offset is common in the universe from a sample of clusters, and explain the long-standing mass discrepancy between strong gravitational lensing and X-ray problem in galaxy clusters.
The third part is the research about the modified gravity theory (MOND) and its covariant formalism (TeVeS). We study the gravitational lensing of covariant MOND, we develop an analytic model for non-spherical lenses in covariant MOND, and study such a model with CASTLES survey. We use this model to obtain a reasonable MOND fit to most of the double-imaged systems. However, we also find those non-isolated double-imaged systems can not be fitted well. And most quadruple-imaged systems for which no reasonable MOND fit can be obtained with our models. We argue that, this is mostly due to the intrinsic limitation of the analytic models, we indeed showed that our models were unable to produce a large Einstein ring and a large shear at the same time.
引文
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