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.

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.

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.

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.

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.

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 Origin, Properties and Detection of Dark Matter and Dark Energy

The pictures from the James Webb Space Telescope (JWST) suggest that massive galaxies were already at the beginning of the expansion of the Universe because there was too short time to create them. It is consistent with the new cosmology presented within the Scale-Symmetric Theory (SST). The phase transitions of the initial inflation field described in SST lead to the Protoworld—its core was built of dark matter (DM). We show that the DAMA/LIBRA annual-modulation amplitude forced by the change of the Earth’s velocity (i.e. baryonic-matter (BM) velocity) in relation to the spinning DM field in our Galaxy’s halo should be very low. We calculated that in the DM-BM weak interactions are created single and entangled spacetime condensates with a lowest mass/energy of 0.807 keV—as the Higgs boson they can decay to two photons, so we can indirectly detect DM. Our results are consistent with the averaged DAMA/LIBRA/COSINE-100 curve describing the dependence of the event rate on the photon energy in single-hit events. We calculated the mean dark-matter-halo (DMH) mass around quasars, we also described the origin of the plateaux in the rotation curves for the massive spiral galaxies, the role of DM-loops in magnetars, the origin of CMB, the AGN-jet and galactic-halo production, and properties of dark energy (DE).

一种消除halo效应的去雾算法

雾天条件下获取的图像会有低对比度和低场景可见度的问题,一些去雾算法会出现halo效应现象。基于暗原色先验理论的去雾算法,花费了大量的时间在透射率的优化问题上。为此,提出一种结合暗通道去雾算法的景深优化的图像复原方法,在图像景深边缘和非景深边缘分别采用不同的模板处理得到暗图像,进而得到粗略透射率,双边滤波器进行修复粗略透射率。该算法能够有效地去除图像中的雾气,和软件抠图法相比较,不仅有效降低了halo效应,并且大大地减少了透射率处理时间,提高了处理效率。实验表明该算法的时间复杂度与图像尺寸成线性关系,相比于传统算法在计算速度上有一定提高,保障了图像处理的实时性。

一种基于Sigmoid函数的抑制Halo效应的有效算法

人们通常利用暗通道先验理论进行图像去雾,其副作用之一就是光晕现象,即Halo效应。在深入分析光晕效应特点的基础上,提出了一种基于Sigmoid函数的抑制Halo效应的有效算法。首先对带有光晕的图像进行大量观察,总结了光晕产生的位置规律及结构特性,构造了一个具有方向性的Sigmoid模板;然后对由暗通道先验理论得到的粗略透射率图进行边缘检测,获得景深突变处像素点的坐标和方向角;其次,再利用已构造的模板判断该处出现光晕的准确位置,并将非光晕区域的像素值赋给光晕区域,得到优化后的透射率图;最后引入一种容差机制还原出清晰无光晕的图像。本算法的特色在于所构造的模板仅仅处理出现光晕的区域,而不是处理整个图像区域,因此避免了传统方法中非光晕区域的颜色失真问题。实验结果表明,本算法简单易行,运行速度快,复原效果好。

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.

星系自转曲线之观测研究进展

星系自转曲线测定对星系天文学研究有着重要的意义。现已发现,除旋涡星系外,其他类别的河外星系也有自转运动,但自转曲线的特征有所不同。自转曲线研究的内容颇为丰富,如是否存在普适自转曲线,星系团环境对成员星系运动特征的可能影响,星系物质转动速度的垂向梯度问题,以及星系中暗物质的分布等,对上述内容做了相关评述。

景深边缘优化的暗通道去雾算法

雾天条件下拍摄的图像存在低对比度和低场景可见度的问题,传统的去雾算法容易产生Halo效应。为此,提出了景深边缘优化的暗通道去雾算法。该算法是基于暗原色先验理论,需要考虑消除景深边缘处的白色晕块,方法是对图像景深边缘和非景深边缘分别采用不同的模板处理得到透射图。引导滤波修复透射图,在去除多余的纹理信息的同时增强了雾天图像的边缘信息。并采用新增可见边之比、梯度化均值对去雾图像进行客观评价。实验表明该算法不仅能够有效地去除图像中的雾气,而且有效地降低了Halo效应,从整体上改善了去雾复原图像的视觉效果。

基于通道暗元素信息的快速单幅图像去雾方法

针对因大气颗粒吸收及散射因素带来视频图像质量下降的问题,分析并结合传统的基于暗通道先验的规律图像去雾算法的基础上,提出一种基于通道暗元素信息的快速单幅图像去雾方法。该方法通过计算出单像素最小分量矩阵,然后复用该单像素最小分量矩阵计算出其余滑窗模板下图像对应的最小分量矩阵,最后结合图像的边缘信息选择不同滑窗模板对应的场景透射系数完成对图像的去雾。实验与传统图像去雾算法作比较表明,该方法恢复出的图像质量较高,解决了图像去雾处理时物体边缘附近易产生光晕的问题;避免了原始算法的软抠图处理,计算量小,能够达到实时处理的目的,便于实际应用。

河外星系动力学质量的多途径测定

利用伴天体(含伴星系、球状星团、晕族天体等)的运动学观测资料,可通过多种方法估测主星系的质量(动力学质量),如自转质量、位力质量、轨道质量、投影质量、示踪质量以及星流法质量等。在诸多已测得动力学质量的河外星系中,以仙女星系(M31)的相关工作为最多,对此做了简要的介绍和讨论。

银河系恒星潮汐流的探测进展

银晕外区存在众多星流,它们或源自银河系的矮伴星系,或源自晕族球状星团,常分别称为矮星系星流和球状星团潮汐尾。星流可以利用各类示踪星,并通过不同的途径加以探测,对若干代表性矮星系星流和球状星团潮汐尾的探测进展做了简要的介绍。