Predicting the clustering of X-ray selected galaxy clusters in flux-limited surveys     

L. Moscardini  S. Matarrese  F. Lucchin  P. Rosati 《Monthly notices of the Royal Astronomical Society》2000,316(2):283-298

We present a model to predict the clustering properties of X-ray selected clusters in flux-limited surveys. Our technique correctly accounts for past light-cone effects on the observed clustering and follows the non-linear evolution in redshift of the underlying dark matter correlation function and cluster bias factor. The conversion of the limiting flux of a survey into the corresponding minimum mass of the hosting dark matter haloes is obtained by using theoretical and empirical relations between mass, temperature and X-ray luminosity of galaxy clusters. Finally, our model is calibrated to reproduce the observed cluster counts adopting a temperature–luminosity relation moderately evolving with redshift. We apply our technique to three existing catalogues: the ROSAT Brightest Cluster Sample (BCS); the X-ray Brightest Abell-type Cluster sample (XBACs); and the ROSAT –ESO Flux-Limited X-ray sample (REFLEX). Moreover, we consider an example of possible future space missions with fainter limiting flux. In general, we find that the amplitude of the spatial correlation function is a decreasing function of the limiting flux and that the Einstein–de Sitter models always give smaller correlation amplitudes than open or flat models with low matter density parameter Ω_0m. In the case of the XBACs catalogue, the comparison with previous estimates of the observational spatial correlation shows that only the predictions of models with Ω_0m=0.3 are in good agreement with the data, while the Einstein–de Sitter models have too low a correlation strength. Finally, we use our technique to discuss the best strategy for future surveys. Our results show that, to study the clustering properties of X-ray selected clusters, the choice of a wide area catalogue, even with a brighter limiting flux, is preferable to a deeper, but smaller area, survey.  相似文献   

Gravitational lensing effects on high-redshift Type II supernova studies with the Next Generation Space Telescope     

Simone Marri  rea Ferrara  Lucia Pozzetti 《Monthly notices of the Royal Astronomical Society》2000,317(2):265-272

We derive the expected Type II supernova (SN) differential number counts, N ( m ), and Hubble diagram for SCDM and LCDM cosmological models, taking into account the effects of gravitational lensing (GL) produced by the intervening cosmological mass. The mass distribution of dark matter haloes (i.e. the lenses) is obtained by means of a Monte Carlo method applied to the PressSchechter mass function. The haloes are assumed to have a Navarro, Frenk & White (NFW) density profile, in agreement with recent simulations of hierarchical cosmological models. Up to z =15, the (SCDM, LCDM) models predict a total number of (857, 3656) SNII yr¹ in 100 surveyed 44 arcmin² fields of the Next Generation Space Telescope ( NGST ). NGST will be able to reach the peak of the N ( m ) curve, located at AB 30(31) for SCDM (LCDM) in J and K wavelength bands, and detect (75 per cent, 51 per cent) of the above SN events. This will allow a detailed study of the early cosmic star formation history, as traced by SNIIe. N ( m ) is only very mildly affected by the inclusion of lensing effects. In addition, GL introduces a moderate uncertainty in the determination of cosmological parameters from Hubble diagrams, when these are pushed to higher z . For example, for a 'true' LCDM with (_M=0.4, =0.6), without proper account of GL, one would instead derive We briefly compare our results with previous similar work and discuss the limitations of the model.  相似文献   

Triaxial haloes and particle dark matter detection     

N. W. Evans  C. M. Carollo  P. T. de Zeeuw 《Monthly notices of the Royal Astronomical Society》2000,318(4):1131-1143

This paper presents the properties of a family of scale-free triaxial haloes. We adduce arguments to suggest that the velocity ellipsoids of such models are aligned in conical coordinates. We provide an algorithm to find the set of conically aligned velocity second moments that support a given density against the gravity field of the halo. The case of the logarithmic ellipsoidal model – the simplest triaxial generalization of the familiar isothermal sphere – is examined in detail. The velocity dispersions required to hold up the self-consistent model are analytic. The velocity distribution of the dark matter can be approximated as a triaxial Gaussian with semiaxes equal to the velocity dispersions.
There are roughly 20 experiments worldwide that are searching for evidence of scarce interactions between weakly interacting massive-particle dark matter (WIMP) and detector nuclei. The annual modulation signal, caused by the Earth's rotation around the Sun, is a crucial discriminant between WIMP events and the background. The greatest rate is in June, the least in December. We compute the differential detection rate for energy deposited by the rare WIMP–nucleus interactions in our logarithmic ellipsoidal halo models. Triaxiality and velocity anisotropy change the total rate by up to ∼40 per cent, and have a substantial effect on the amplitude of the annual modulation signal. The overall rate is greatest, but the amplitude of the modulation is weakest, in our radially anisotropic halo models. Even the sign of the signal can be changed. Restricting attention to low energy events, the models predict that the maximum rate occurs in December, and not in June.  相似文献   

Deep galaxy counts, extragalactic background light and the stellar baryon budget   总被引：1，自引：0，他引：1  

Piero Madau  Lucia Pozzetti 《Monthly notices of the Royal Astronomical Society》2000,312(2):L9-L15

We assess the constraints imposed by the observed extragalactic background light (EBL) on the cosmic history of star formation and the stellar-mass density today. The logarithmic slope of the galaxy number–magnitude relation from the Southern Hubble Deep Field imaging survey is flatter than 0.4 in all seven UBVIJHK optical bandpasses, i.e. the light from resolved galaxies has converged from the UV to the near-IR. We find a lower limit to the surface brightness of the optical extragalactic sky of about 15 nW m⁻² sr⁻¹, comparable to the intensity of the far-IR background from COBE data. Assuming a Salpeter initial mass function with a lower cut-off consistent with observations of M subdwarf disc stars, we set a lower limit of Ω_g+s h ²>0.0013  I ₅₀ to the visible (processed gas + stars) mass density required to generate an EBL at a level of 50  I ₅₀ nW m⁻² sr⁻¹; our 'best-guess' value is Ω_g+s h ²≈0.0031  I ₅₀. Motivated by the recent microlensing results of the MACHO collaboration, we consider the possibility that massive dark haloes around spiral galaxies are composed of faint white dwarfs, and show that only a small fraction (≲5 per cent) of the nucleosynthetic baryons can be locked in the remnants of intermediate-mass stars forming at z _F≲5, as the bright early phases of such haloes would otherwise overproduce the observed EBL.  相似文献   

The baryonic and dark matter properties of high-redshift gravitationally lensed disc galaxies     

P. Salucci  A. M. Swinbank  A. Lapi  I. Yegorova  R. G. Bower  Ian Smail  G. P. Smith 《Monthly notices of the Royal Astronomical Society》2007,382(2):652-656

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基于显著性分析的SAR溢油图像中暗斑区域检测方法研究     

吕新荣  李云  温春苗  任鹏 《海洋科学》2021,45(4):90-96

为了提高合成孔径雷达(syntheticapertureradar,SAR)图像中海上溢油的检测精度,设计了一种图像显著性和均值偏移分割相结合的暗斑检测方法,验证了该方法在SAR溢油图像暗斑识别中的有效性,为溢油区域的准确检测奠定了基础。针对SAR溢油图像中暗斑区域在人类视觉中属于感兴趣区域的特性,利用图像显著性检测方法对整幅SAR图像进行处理生成显著性图像,然后利用均值偏移方法在SAR图像的Lab空间将图像分割成不同区域,最后在显著性图像上利用每个区域的平均显著性值与动态阈值之间的关系确定溢油图像中的暗斑区域。实验结果表明,该方法不需要人工交互,且能够有效地提取出SAR图像溢油中的暗斑区域。  相似文献   

重子物质对暗物质晕形状和角动量的影响          下载免费PDF全文

张瑶瑶  戴才萍 《天文学报》2021,62(6):65

利用高精度大样本的冷暗物质($\Lambda$ cold dark matter, $\Lambda$CDM)宇宙学数值模拟的数据, 对重子物质如何影响暗物质晕的形状和角动量进行了研究.使用了3种数值模拟数据, 纯暗物质模拟、含辐射冷却、恒星形成和动力学超新星反馈的模拟, 包含活动星系核反馈效应的恒星形成模拟. 对这3种模拟, 还进行了不同红移处的比较. 主要结果如下.重子物理过程会改变暗物质晕的质量分布, 特别是有活动星系核反馈机制的情况下.比如, 活动星系核反馈会减少大质量暗物质晕的形成.随着宇宙的演化, 暗物质晕的空间形态逐渐由扁变圆. 重子物质的存在会加速暗物质晕形状的变化过程, 而且会使暗物质晕形状变得更圆. 但是活动星系核的反馈会对这一加速效应产生抑制.重子物质对暗物质晕的影响与暗物质晕的质量和半径都存在一定的依赖性.暗物质晕的质量越大, 它会呈现更扁的形态. 同时, 重子物质对任意质量的暗物质晕或暗物质晕在任意半径处的变圆均有一定的促进作用,尽管活动星系核反馈会抑制这一促进作用.特别是对于暗物质晕在0.2--0.6倍维里半径处的形状, 重子物质的影响尤为明显.此外, 重子物质的存在会对暗物质晕的角动量产生显著影响, 它会增大暗物质的角动量. 暗物质晕的自旋参数与质量无相关性, 但是与暗物质晕的半径存在一定的相关性.  相似文献   

泥岩成岩作用研究进展与展望     

赵建华  金之钧 《沉积学报》2021,39(1):58-72

泥岩成岩作用研究在页岩油气革命的推动下取得了一系列重要进展,已成为沉积学和石油地质学研究的一个前缘领域.泥岩成岩作用不仅控制着油气的生成和运移,同时对物质组成、微观结构、储层物性和力学性质都具有重要影响.本文围绕这一领域,阐述了国内外相关研究现状,展望了未来的发展趋势.当前泥岩成岩作用研究进展主要体现在4个方面:1)矿...  相似文献   

荷载-干湿循环共同作用下泥岩的压缩特性     

谈云志  胡莫珍  周玮韬  左清军  汪洪星  喻波 《岩土力学》2016,37(8):2165-2171

泥岩遇水易崩解泥化,特别是耦合荷载作用后,其力学性能衰减更加明显。为掌握泥岩在环境因素和外部荷载作用下的性能演化规律,开展了干湿循环与上覆荷载共同作用下的压缩特性试验。发现初次浸水后压实泥岩发生膨胀,但随着干湿循环作用的进行,泥岩试样发生压缩变形。然后,对压实泥岩试样进行孔隙分析,结果表明,泥岩孔隙分布呈现双峰特征,峰值大约位于0.3 ?m和10.0 ?m孔径处,干湿循环和荷载的作用引起孔隙体积减小,特别是对大孔径孔隙的影响最显著。最后,依据泥岩的膨胀、压缩和孔隙分布特征,提出了压实泥岩的孔隙-荷载-水分相互作用模型,将压实泥岩的孔隙体积分为团粒内孔隙和团粒间孔隙两类;分析了荷载-干湿循环引起泥岩团粒崩解破碎和充填团粒之间孔隙的演变过程。揭示了泥岩孔隙-水分-荷载的相互作用机制,为泥岩路基的填筑提供了理论参考。  相似文献   

含软弱夹层厚煤层巷帮外错滑移机制与支护研究     

黄庆享  赵萌烨  张强峰  邵水才  马矿生 《岩土力学》2016,37(8):2353-2358

含泥岩软夹层大采高工作面回采巷道外错式变形破坏是巷道支护的新课题。通过对三道沟煤矿含软夹矸层5-2厚煤层回采巷道变形实测和围岩钻孔窥视,发现了巷道顶板存在垂直裂隙,巷道两帮破坏区集中于夹矸层附近,且具有副帮大于正帮的特征,巷道变形主要来自于相邻采空区的影响。通过数值计算和物理模拟,揭示了相邻工作面侧方支承压力导致顶板产生垂直向裂隙,引起顶板与巷道夹矸层以上煤体沿软夹层向相邻采空区外错滑移的机制。建立了含软夹矸层巷道自稳平衡拱支护模型,提出了加强巷道上帮支护,控制外错滑移破坏的控制原则,给出了顶板锚索与煤帮长锚杆加强支护方案,工程实践取得了成功。  相似文献