Searching the Parameters of Dark Matter Halos on the Basis of Dwarf Galaxies’ Dynamics

Article devoted to searching the parameters of dark matter halos on the base of dwarf galaxies’ dynamics (Messier 32 and Leo I). For doing this, we propose the new approach founded on construction the coupled elliptical trajectory for a probe body in the gravitational fields of Newtonian potential and potential of dark matter’s halo. This allows more accuracy estimate its central density for the Navarro-Frenk-White profile and free parameter for the Einasto profile . Our result is in good correlation with results of other authors that are got by different numerical methods.

The mass of the Galactic dark matter halo from-9000 LAMOST DR5 K giants

We constrain the mass of the Milky Way＇s dark matter halo, based on the kinematics of 9627 K giants at Galactocentric distances ranging over 5 kpc 〈 r 〈 120 kpc drawn from LAMOST DR5.The substructure in this sample has been identified and removed carefully to enable construction of the underlying line-of-sight velocity dispersion at different radii from the Galactic center. We interpret the radial profile of the line-of-sight velocity dispersion using a spherical Jeans equation under the assumptions of anisotropy/isotropy and that radial velocity dispersion is approximately equal to line-ofsight velocity dispersion σ_r（r）≈σ_（los）（r）. If we assume that the dark matter halo follows an NFW profile and the stellar halo is isotropic（β = 0）, then σlos（r） can be directly used to estimate the virial mass of the Galactic dark matter halo, M_（vir） = 1.08_（-0.14）^（＋0.17） ×10^（12） M⊙, and concentration parameter c = 18.5＋-2.9.3.6 In case that the stellar halo is anisotropic, we cannot avoid differentiation of sparse velocity dispersions according to the Jeans equation, which may cause overestimation of the mass. We use an isotropic case to test and find that d ln（σ_（los）~2 （r））/d ln r overestimates the virial mass by 15% but within 1-σ error. We use d ln（σ2 los（r））/d ln r to fit the NFW profile and get M_（vir） = 1.11_（-0.20）^（＋0.24） ×10^（12） M⊙and c = 13.8-2.2＋3.0 in case of β = 0.3.

An empirical model to form and evolve galaxies in dark matter halos

Based on the star formation histories of galaxies in halos with different masses, we develop an empirical model to grow galaxies in dark matter halos. This model has very few ingredients, any of which can be associated with observational data and thus be efficiently assessed. By applying this model to a very high resolution cosmological N-body simulation, we predict a number of galaxy properties that are a very good match to relevant observational data. Namely, for both centrals and satellites, the galaxy stellar mass functions up to redshift z=4 and the conditional stellar mass functions in the local universe are in good agreement with observations. In addition, the two point correlation function is well predicted in the different stellar mass ranges explored by our model. Furthermore, after applying stellar population synthesis models to our stellar composition as a function of redshift, we find that the luminosity functions in the 0.1 u,0.19, 0.1r, 0.1i and 0.1z bands agree quite well with the SDSS observational results down to an absolute magnitude at about -17.0. The SDSS conditional luminosity function itself is predicted well. Finally, the cold gas is derived from the star formation rate to predict the HI gas mass within each mock galaxy. We find a remarkably good match to observed HI-to-stellar mass ratios. These features ensure that such galaxy/gas catalogs can be used to generate reliable mock redshift surveys.

Extinction of Light in the Galactic Halo: First Observational Evidence of the Interaction of Light and Dark Matter

We study the distribution of quasars on the celestial sphere according to ground-based SDSS and space-based WISE and Gaia observations. All distributions as a function of galactic latitude, b, exhibit a decrease in quasar frequency well outside the dust in and near the galactic plane. We prove that the observed decrease in quasar frequency at high galactic latitudes is not accompanied by reddening, meaning that it can not be caused by dust. The scattering of light by the circumgalactic gas is negligible because the Thomson scattering cross section is very small. We conclude the observed scattering of light must be caused by dark matter in the galactic halo. We determine the mass and charge of dark matter particles. If the dark matter particle is a fermion its mass, mDMand charge eDM=δe, where e is the elementary charge are: mDM=3.2×10−2eV and δ=3.856×10−5. If however the dark matter particle is spinless then: mDM=0.511eV and δ=2.132×10−4. These values for the charge of a dark matter particle are orders of magnitude higher than the upper limit of the neutrino charge according to laboratory experiments. Consequently, dark matter particles are not charged neutrinos. Since dark matter particles are charged, they must emit and absorb electromagnetic radiation. However, PDM~δ2, or: PDM~1.487×10−9Pe, where Peis the power output of a single electron.

Constraints on ultracompact minihalos using neutrino signals from gravitino dark matter decay

Ultracompact dark matter minihalos （UCMHs） would be formed during the early universe if there were large density perturbations. If dark matter can decay into particles described by the standard model, such as neutrinos, these objects would become potential astrophysical sources of emission which could be detected by in- struments such as IceCube. In this paper, we investigate neutrino signals from nearby UCMHs due to gravitino dark matter decay and compare these signals with the back- ground neutrino flux which is mainly from the atmosphere to obtain constraints on the abundance of UCMHs.

On the Dark Matter’s Halo Theoretical Description

We argued that the standard field scalar potential couldn’t be widely used for getting the adequate galaxies’ curve lines and determining the profiles of dark matter their halo. For discovering the global properties of scalar fields that can describe the observable characteristics of dark matter on the cosmological space and time scales, we propose the simplest form of central symmetric potential celestial-mechanical type, i.e. U(φ) = –μ/φ. It was shown that this potential allows get rather satisfactorily dark matter profiles and rotational curves lines for dwarf galaxies. The good agreement with some previous results, based on the N-body simulation method, was pointed out. A new possibility of dwarf galaxies’ masses estimation was given, also.

Pairwise Velocity Statistics of Dark Halos

We have accurately evaluated the halo pairwise velocity dispersion and the halo mean streaming velocity in the LCDM model (the fiat ω0 = 0.3 model) using a set of high-resolution N-body simulations. Based on the simulation results, we have developed a model for the pairwise velocity dispersion of halos. Our model agrees with the simulation results over all scales we studied. We have also tested the model of Sheth et al. for the mean streaming motion of halos derived from the pair-conservation equation. We found that their model reproduces the simulation data very well on large scale, but under-predicts the streaming motion on scales r < 10 h-1 Mpc. We have introduced an empirical relation to improve their model. These improved models are useful for predicting the redshift correlation functions and the redshift power spectrum of galaxies if the halo occupation number model, e.g. the cluster weighted model, is given for the galaxies.

Detection of a Physical Difference between the CDM Halos in Simulation and in Nature

Numerical simulation is an important tool that is helpful for us to understand the process of structure formation in the universe. However, many simulation results of cold dark matter （CDM） halos on a small scale are inconsistent with observations： the central density profile is too cuspy and there are too many substructures, Here we point out that both the problems may be connected with a hitherto unrecognized bias in the simulated halos. Although CDM halos in nature and in simulation are both virialized systems of collisionless CDM particles, gravitational encounter cannot be neglected in the simulated halos because they contain many fewer particles. We demonstrate this by two numerical experiments, showing that there is a difference on the microcosmic scale between the natural and simulated halos. The simulated halo is more akin to globular clusters where gravitational encounter is known to lead to such drastic phenomena as core collapse. Such an artificial core collapse process appears to link the two problems together in the bottom-up scenario of structure formation in the ACDM universe. The discovery of this bias also has implications on the applicability of the Jeans theorem in galactic dynamics.

Gravitational lensing properties of an isothermal universal halo profile

N-body simulations predict that dark matter halos with different mass scales are described by a universal model, the Navarro-Frenk-White （NFW） den- sity profiles. As a consequence of baryonic cooling effects, these halos will become more concentrated, and similar to an isothermal sphere over a large range in radii （～ 300 h-1 kpc）. The singular isothermal sphere （SIS） model however has to be trun- cated artificially at large radii since it extends to infinity. We model a massive galaxy halo as a combination of an isothermal sphere and an NFW density profile. We give an approximation for the mass concentration at different baryon fractions and present exact expressions for the weak lensing shear and flexion for such a halo. We compare the lensing properties with the SIS and NFW profiles. We find that the combined pro- file can generate higher order lensing signals at small radii and is more efficient in generating strong lensing events. In order to distinguish such a halo profile from the SIS or NFW profiles, one needs to combine strong and weak lensing constraints for small and large radii.

Galactic Haloes from Self-Interacting Neutrinos

The objective of this research is to provide an explanation of galactic haloes using established particles and forces using recent theoretical developments. Light fermions, with masses on the order of 1 eV/c2, are not a leading candidate for dark matter because of their large free-streaming scale length and their violation of the Tremaine-Gunn bound. With a self-interaction of fermions, the free-streaming scaling length is reduced, and the tenets of the Tremaine-Gunn bound are not applicable. Binding of neutrinos via a feeble SU(3) force is considered as a model for such interactions. The assumed sum of masses of the three neutrino flavors is 0.07 eV/c2. The resulting form of matter for such bound neutrinos is found to be a degenerate Fermi fluid. Pressure-equilibrium approaches applied to this fluid provide cuspy solutions and match observationally-inferred profiles for galactic haloes. Such approaches also match the observed total enclosed mass for galaxies similar to the Milky Way. The computed structures are found to be stable. The hypothesis is considered in view of observationally-inferred halo-halo interactions and gives results that are consistent with the observed Bullet cluster halo interaction. The theory gives agreement with observationally-inferred properties of dark matter near earth. Questions related to interaction rates, consistency with SN1987a data, the cosmic microwave background, the issue of SU(3) interactions between neutrinos and quarks, free-streaming after neutrino decoupling, and dark-matter abundance are addressed in a companion paper.

A Remark on Using Gravitational Lensing Probability as a Probe of the Central Regions of CDM Halos

We calculate the gravitational lensing probabilities by cold dark matter (CDM) halos with different density profiles, and compare them with current observations from the Cosmic Lens All-Sky Survey (CLASS) and the Jodrell-Bank VLA Astrometric Survey (JVAS). We find that the lensing probability is dramatically sensitive to the clumping of the dark matter, or quantitatively, the concentration parameter. We also find that our predicted lensing probabilities in most cases show inconsistency with the observations. It is argued that high lensing probability may not be an effective tool for probing the statistical properties of inner structures of dark matter halos.

The pairwise velocity difference of over 2000 BHB stars in the Milky Way halo

Models of hierarchical galaxy formation predict that the extended stellar halos of galaxies like our Milky Way show a great deal of sub-structure, arising from disrupted satellites. Spatial sub-structure is directly observed, and has been quantified, in the Milky Way＇s stellar halo. Phase-space conservation implies that there should be sub-structure in position-velocity space. Here, we aim to quantify such position-velocity sub-structure, using a state-of-the art data set having over 2000 blue horizontal branch （BHB） stars with photometry and spectroscopy from SDSS. For stars in dynamically cold streams （＂young＂ streams）, we expect that pairs of objects that are physically close also have similar velocities. Therefore, we apply the well-established ＂pairwise velocity difference＂ （PVD） statistic （｜ △Vlos ｜） （△r）, where we expect （｜ △Vlos ｜） to drop for small separations At. We calculate the PVD for the SDSS BHB sample and find 〈｜ △Vlos ｜〉（△r） ≈ const., i.e. no such signal. By making mock-observations of the simulations by Bullock ＆ Johnston and applying the same statistic, we show that for individual, dynamically young streams, or assemblages of such streams, （｜ △Vlos ｜） drops for small distance separations At, as qualitatively expected. However, for a realistic complete set of halo streams, the pair-wise velocity difference shows no signal, as the simulated halos are dominated by ＂dynamically old＂ phase-mixed streams. Our findings imply that the sparse sampling and the sample sizes in SDSS DR6 are still insufficient to use the position-velocity sub-structure for a stringent quantitative data-model comparison. Therefore, alternate statistics must be explored and much more densely sampled surveys, dedicated to the structure of the Milky Way, such as LAMOST, are needed.

Alignment between galaxies and large-scale structure

Based on the Sloan Digital Sky Survey DR6 （SDSS） and the ＇Millennium Simulation （MS）, we investigate the alignment between galaxies and large-scale structure. For this purpose, we develop two new statistical tools, namely the alignment correlation function and the cos（20）-statistic. The former is a two-dimensional extension of the traditional two-point correlation function and the latter is related to the ellipticity correlation function used for cosmic shear measurements. Both are based on the cross correlation between a sample of galaxies with orientations and a reference sample which represents the large-scale structure. We apply the new statistics to the SDSS galaxy catalog. The alignment correlation function reveals an overabundance of reference galaxies along the major axes of red, luminous （L 〉 ～L＊） galaxies out to projected separations of 60 h-lMpc. The signal increases with central galaxy luminosity. No alignment signal is detected for blue galaxies. The cos（2θ）-statistic yields very similar results. Starting from a MS semi-analytic galaxy catalog, we assign an orientation to each red, luminous and central galaxy, based on that of the central region of the host halo （with size similar to that of the stellar galaxy）. As an alternative, we use the orientation of the host halo itself. We find a mean projected misalignment between a halo and its central region of -25°. The misalignment decreases slightly with increasing luminosity of the central galaxy. Using the orientations and luminosities of the semi-analytic galaxies, we repeat our alignment analysis on mock surveys of the MS. Agreement with the SDSS results is good if the central orientations are used. Predictions using the halo orientations as proxies for cen- tral galaxy orientations overestimate the observed alignment by more than a factor of 2. Finally, the large volume of the MS allows us to generate a two-dimensional map of the alignment correlation function, which shows the reference galaxy distribution to be flat- tened parallel to the orientations of red luminous galaxies with axis ratios of -0.5 and ,-0.75 for halo and central orientations, respectively. These ratios are almost independent of scale out to 60 h^-1 Mpc.

暗物质晕次结构的演化研究进展

一般认为暗晕是通过等级成团方式形成的:小质量暗晕先形成,进而通过并合形成较大质量的暗晕。并合后的小质量暗晕形成所谓的次结构,目前关于次结构的演化过程和分布特点尚无明确结论。介绍了利用数值模拟、半解析模型和观测来研究次结构分布和演化的进展,并特别讨论了次结构的并合时标、质量函数和空间分布等特性。

利用微引力透镜效应搜寻银河系内的重子暗物质

该文综述了利用微引力透镜效应来搜寻银河系内重子暗物质的原理、观测方法和结果以及当前国际上几个小组的工作和主要进展。简要回顾了对重子暗物质的认识过程,其中广泛分布于星系之中的暗天体被称为晕族大质量致密天体(MACHO)。综述了一些关于引力透镜的一些基本概念和基本公式,其中简单讨论了强引力透镜、弱引力透镜和微引力透镜的区别,并列出微引力透镜的两个重要参数光深和光变时标的定义及表达式。详细阐述了对于MACHO探测的方法和一些观测效应细节。综述了目前几个小组的工作,包括MACHO小组和EROS小组等.其中MACHO小组近来的工作得出MACHO为银晕的重要组成部分,其质量比例约为20%;而EROS最近工作得出的质量比例上限为7%。

暗物质晕普适性的数值分析

N体数值模拟计算发现暗物质晕具有几乎普适的密度轮廓,比如NFW轮廓、Moore轮廓和Einasto轮廓等,而速度各向异性和密度轮廓的对数斜率近似成线性关系.同样有证据显示赝相空间密度ρ/σ3与半径r成幂律关系.本文从金斯方程的角度出发通过自洽性研究考察了这几种常用密度轮廓的鲁棒性问题.数值计算和分析比较的结果表明各向异性密度轮廓并不具有鲁棒性,进而可以推测暗物质晕的这一数值特性缺乏真正的普适性.

暗物质晕中星系的配置(英文)

基于杨小虎的博士论文《宇宙大尺度结构的统计研究》中第4部分内容整理缩写而成.讨论如何利用星系-星系的弱引力透镜观测来获得星系光度-暗物质晕质量之间的关系;并介绍建立的条件光度函数模型,在这个模型中预言了给定质量的暗物质晕中所能形成的不同光度的星系的概率.这些结果给出了讨论星系形成理论中各种物理过程的判据.基于这个模型还预言了一些宇宙中光的分布行为:如宇宙中超过一半的光是来自质量小于1012太阳质量的暗物质晕中.

类银河系卫星星系系统的平面演化统计

银河系的卫星星系倾向于分布在一个平面上,研究这种平面分布的形成原因有助于人们理解标准宇宙学模型和暗物质晕中的星系分布.使用半解析星系形成模型,通过从统计角度追踪卫星星系平面性的演化历史对类银河系卫星星系呈平面分布的现象进行研究.使用半解析星系模型产生的模拟数据,以与银河系系统质量相当为主要限制条件,按当前卫星星系分布的平面性程度选取3个子样本,分别用恒星质量最大的11颗或前20%的卫星星系的质量张量对应的短长轴比(c/a)表征平面性,计算了近~10 Gyr内3个子样本的整体演化情况.结果表明:在统计上,大部分平面性结构是过渡性的短暂现象.虽然用c/a表征的平面性会受计入卫星数目的影响,但上述结论对用质量最大的前20%卫星星系计算c/a的样本依然成立.

暗物质主晕与其子晕的自旋方向相关性研究

利用高精度大样本A冷暗物质（Acolddarkmatter，ACDM）宇宙学数值模拟的结果，对暗物质主晕与其子晕的自旋方向相关性进行了研究。本文用两者自旋方向夹角的余弦值（COSθ）作为指标，观察（COSθ）随两者之间距离以及红移的变化。若暗物质晕的自旋方向在空间随机分布，则按统计理论可得（COSθ）应为0；若（COSθ）大于0，则表示暗晕之间自旋方向正相关；若（COSθ）小于0，则表示暗晕之间自旋方向反相关。主要得到三个结果：第一，子晕自旋方向在空间的分布非随机，越靠近主晕内部，（COSθ）越大且为正值，与主晕的自旋方向相关性越强烈。当子晕与主晕质量相当时，在主晕的百分之一个维里半径（virialradiusl距离处，耦合信号非常强烈，（COS0）高达约0．8；而在主晕的维里半径距离处，相关性几乎不存在。第二，子晕与主晕的质量比越大，相关性越强烈。当子晕与主晕质量比相同时，对于不同质量主晕，如1011±0.5^M，1012±0.5^h-1^M，1013±0.5^h-1^M,10 14±0.5^h-1M（其中Me为太阳质量，九为无量纲哈勃常数），相关性曲线几乎重合。第三，该相关性不依赖于红移。但高红移处仍需更高精度模拟进一步验证。这是首次对暗物质主晕与其子晕自旋方向相关性进行的系统性研究，且相关强度较类似物理量的相关更强。末尾简要讨论了产生该相关性的可能原因和可深入进行的后续研究。

暗晕的并合

系统介绍暗晕-暗晕并合在理论方面的形成与发展,并简要介绍了其在数值模拟检验(冷暗物质模型)及拟合方面的进展。暗晕-暗晕并合率问题可与星系-星系并合率联系,正确地定义暗晕-暗晕并合率很重要,影响并合率的因素却很多,从数值模拟所得到的拟合公式往往存在较大差异,这些差异主要来自于定义:对并合的定义(并合树的建立),对暗晕质量的定义以及并合暗晕前身质量比的定义。数值模拟输出的时间步长也会对此有所影响,此外暗晕并合率也与环境强烈相关。对这些因素所导致的差异做了简单比较。此外,对于暗晕并合率的统计可分为对不同红移处的拟合和对z=0时刻对其并合历史的拟合,其中后者对不同质量的暗晕往往能给出一个较统一的拟合公式。