Modelling the X-ray cluster dipole and cluster contribution to the soft X-ray background     

V.Kolokotronis  M.Plionis  P.Coles  S.Borgani 《Monthly notices of the Royal Astronomical Society》1998,295(1):19-32

We investigate the sampling and dipole convergence properties of flux-limited samples of mock X-ray clusters in relation to their underlying 'parent' cluster distribution. To this purpose, we resort to numerical simulations of the cluster distribution and extract samples resembling the main observational features of X-ray selected cluster samples. The flux-limited samples, being quite sparse, underestimate the amplitude of the 'parent' cluster dipole by ≈ 15 per cent on average for Local Group-like observers. However, the general shapes of their dipole amplitude profiles are in relatively good agreement. We also calculate the expected contribution of clusters, selected according to the relevant criteria, to the soft (i.e. 0.1–2.4 keV) extragalactic X-ray background (XRB), using the ESO Key Project X-ray luminosity function, assuming a flat universe with vanishing cosmological constant. We obtain a value of about 10 per cent of the observed XRB flux.  相似文献   

Constraints on Ω₀ and cluster evolution using the ROSAT log N–log S relation     

B. Mathiesen  & A. E. Evrard 《Monthly notices of the Royal Astronomical Society》1998,295(4):769-780

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On the physical connections between galaxies of different types     

Shude Mao  & Mo 《Monthly notices of the Royal Astronomical Society》1998,296(4):847-855

Galaxies can be classified in two broad sequences which are likely to reflect their formation mechanism. The 'main sequence', consisting of spirals, irregulars and all dwarf galaxies, is probably produced by gas settling within dark matter haloes. We show that the sizes and surface densities along this sequence are primarily determined by the distributions of the angular momentum and formation time of dark haloes. They are well reproduced by current cosmogonies provided that galaxies form late, at z  ≲ 2. In this scenario, dwarf ellipticals were small 'discs' at z  ∼ 1 and become 'ellipticals' after they fall into cluster environments. The strong clustering of dwarf ellipticals is then a natural by-product of the merging and transformation process. The number of dwarf galaxies predicted in a cluster such as Virgo is in good agreement with the observed number. On the other hand, the 'giant branch', consisting of giant ellipticals and bulges, is probably produced by the merging of disc galaxies. Based on the observed phase-space densities of galaxies, we show that the main bodies of all giant ellipticals can be produced by dissipationless mergers of high-redshift discs. However, high-redshift discs, although denser than present-day ones, are still not compact enough to produce the high central phase-space density of some low-luminosity ellipticals. Dissipation must have occurred in the central parts of these galaxies during the merger which formed them.  相似文献   

Comparison of the SFI peculiar velocities with the IRAS 1.2-Jy gravity field     

Luiz N. da Costa  Adi Nusser  Wolfram Freudling  Riccardo Giovanelli  Martha P. Haynes  John J. Salzer  & Gary Wegner 《Monthly notices of the Royal Astronomical Society》1998,299(2):425-432

We present a comparison between the peculiar velocity fields measured from a recently completed l -band Tully–Fisher survey of field spirals (SFI) and that derived from the IRAS 1.2-Jy redshift survey galaxy distribution. The analysis is based on the expansion of these data in redshift space using smooth orthonormal functions, and is performed using low- and high-resolution expansions, with an effective smoothing scale which increases almost linearly with redshift. The effective smoothing scales at 3000 km s⁻¹ are 1500 and 1000 km s⁻¹ for the low- and high-resolution filters. The agreement between the high- and low-resolution SFI velocity maps is excellent. The general features in the filtered SFI and IRAS velocity fields agree remarkably well within 6000 km s⁻¹. This good agreement between the fields allows us to determine the parameter β = Ω^0.6 / b , where Ω is the cosmological density parameter, and b is the linear biasing factor. From a likelihood analysis on the SFI and IRAS modes we find that β = 0.6 ± 0.1, independently of the resolution of the modal expansion. For this value of β, the residual fields for the two filters show no systematic variations within 6000 km s⁻¹. Most remarkable is the lack of any coherent, redshift-dependent dipole flow in the residual field.  相似文献   

长江三峡地区枯水期强降水过程的水汽图象   总被引：5，自引：3，他引：2  

熊廷南 《气象》1998,24(6):44-47

通过对１９９６年１１月４￣６日长江三峡地区强降水过程的水汽图象、红外及可见光云图和常规气象资料的诊断分析,证灾了在水汽图象上可以看到红外云图和可见光云图上看不到的信息,而这信息对强降水预报是重要的。  相似文献   

春晓气田泥岩垮塌测井数据校正及应用     

谢月芳  陈敏 《海洋地质译丛》2009,(4):73-76

由于存在部分泥岩井眼垮塌，东海春晓气田测井曲线砂泥岩阻抗部分叠置。针对这一现象，采用未垮塌段泥岩伽马与密度拟合关系校正垮塌段泥岩密度，声波时差经本区伽德那公式拟合后求取。通过泥岩垮塌测井数据校正前后对比、直方交会、岩石物理、正演及反演效果分析，认为校正后的测井数据比较真实地反映垮塌段扩径泥岩地层特征，储层与围岩波阻抗差异明显，为储层反演、砂体空间展布分析提供了有力依据。  相似文献   

Reconstructing the history of dark energy using maximum entropy     

Caroline Zunckel  Roberto Trotta 《Monthly notices of the Royal Astronomical Society》2007,380(3):865-876

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The halo mass function from the dark ages through the present day     

Darren S. Reed  Richard Bower  Carlos S. Frenk  Adrian Jenkins  Tom Theuns 《Monthly notices of the Royal Astronomical Society》2007,374(1):2-15

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A potentially pure test of cosmic geometry: galaxy clusters and the real space Alcock–Paczyński test     

Young-Rae Kim  Rupert A. C. Croft 《Monthly notices of the Royal Astronomical Society》2007,374(2):535-546

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The shape of the gravitational potential in cold dark matter haloes     

Eric Hayashi  Julio F. Navarro †  Volker Springel 《Monthly notices of the Royal Astronomical Society》2007,377(1):50-62

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