Optimizing the yield of Sunyaev–Zel'dovich cluster surveys

We consider the optimum depth of a cluster survey selected using the Sunyaev–Zel'dovich effect. By using simple models for the evolution of the cluster mass function and detailed modelling for a variety of observational techniques, we show that the optimum survey yield is achieved when the average size of the clusters selected is close to the size of the telescope beam. For a total power measurement, we compute the optimum noise threshold per beam as a function of the beam size and then discuss how our results can be used in more general situations. As a by-product we gain some insight into what is the most advantageous instrumental set-up. In the case of beam switching observations one is not severely limited if one manages to set the noise threshold close to the point which corresponds to the optimum yield. Considering a variety of alternative scenarios, we discuss how robust our conclusions are to modifications in the cluster model and cosmological parameters. The precise optimum is particularly sensitive to the amplitude of fluctuations and the profile of the gas in the cluster.     

The study of topology of the Universe using multipole vectors

We study a multipole vector-based decomposition of cosmic microwave background data in order to search for signatures of a multiconnected topology of the universe. Using 10⁶ simulated maps, we analyse the multipole vector distribution on the sky for the lowest order multipoles together with the probability distribution function of statistics based on the sum of the dot products of the multipole vectors for both the simply connected flat universe and universes with the topology of a 3 torus. The estimated probabilities of obtaining lower values for these statistics as compared to the 5-yr Wilkinson Microwave Anisotropy Probe data indicate that the observed alignment of the quadrupole and octopole is statistically favoured in a 3-torus topology where at least one dimension of the fundamental domain is significantly shorter than the diameter of the observable Universe, as compared to the usual standard simply connected universe. However, none of the obtained results is able to clearly rule out the latter (at more than 97 per cent confidence level). Multipole vector statistics do not appear to be very sensitive to the signatures of a 3-torus topology if the shorter dimension of the domain becomes comparable to the diameter of the observable Universe. Unfortunately, the signatures are also significantly diluted by the integrated Sachs–Wolfe effect.     

Power spectra of CMB polarization by scattering in clusters

Mapping cosmic microwave background (CMB) polarization is an essential ingredient of current cosmological research. Particularly challenging is the measurement of an extremely weak B-mode polarization that can potentially yield unique insight on inflation. Achieving this objective requires very precise measurements of the secondary polarization components on both large and small angular scales. Scattering of the CMB in galaxy clusters induces several polarization effects whose measurements can probe cluster properties. Perhaps more important are levels of the statistical polarization signals from the population of clusters. Power spectra of five of these polarization components are calculated and compared with the primary polarization spectra. These spectra peak at multipoles  ℓ≥ 3000  , and attain levels that are unlikely to appreciably contaminate the primordial polarization signals.     

21-cm fluctuations from inhomogeneous X-ray heating before reionization

Many models of early structure formation predict a period of heating immediately preceding reionization, when X-rays raise the gas temperature above that of the cosmic microwave background. These X-rays are often assumed to heat the intergalactic medium (IGM) uniformly, but in reality will heat the gas more strongly closer to the sources. We develop a framework for calculating fluctuations in the 21-cm brightness temperature that originate from this spatial variation in the heating rate. High-redshift sources are highly clustered, leading to significant gas temperature fluctuations (with fractional variations ∼40 per cent, peaking on   k ∼ 0.1 Mpc⁻¹  scales). This induces a distinctive peak-trough structure in the angle-averaged 21-cm power spectrum, which may be accessible to the proposed Square Kilometre Array. This signal reaches the ∼10 mK level, and is stronger than that induced by Lyα flux fluctuations. As well as probing the thermal evolution of the IGM before reionization, this 21-cm signal contains information about the spectra of the first X-ray sources. Finally, we consider disentangling temperature, density and Lyα flux fluctuations as functions of redshift.     

Hard X-ray emission of the Earth's atmosphere: Monte Carlo simulations

We perform Monte Carlo simulations of cosmic ray-induced hard X-ray radiation from the Earth's atmosphere. We find that the shape of the spectrum emergent from the atmosphere in the energy range 25–300 keV is mainly determined by Compton scatterings and photoabsorption, and is almost insensitive to the incident cosmic ray spectrum. We provide a fitting formula for the hard X-ray surface brightness of the atmosphere as would be measured by a satellite-borne instrument, as a function of energy, solar modulation level, geomagnetic cut-off rigidity and zenith angle. A recent measurement by the INTEGRAL observatory of the atmospheric hard X-ray flux during the occultation of the cosmic X-ray background by the Earth agrees with our prediction within 10 per cent. This suggests that Earth observations could be used for in-orbit calibration of future hard X-ray telescopes. We also demonstrate that the hard X-ray spectra generated by cosmic rays in the crusts of the Moon, Mars and Mercury should be significantly different from that emitted by the Earth's atmosphere.     

时间相依模型与泊松模型计算结果的对比分析——以道孚及炉霍潜源为例

本文分析了华北平原第四纪主要构造格局和强震活动特点,划分了主要强震构造带,并对其发震能力作了评价。认为坝县-束鹿-邯郸断裂带、唐山-河间-磁县断裂带和黄骅-德州-东明断裂带3条北东向右旋走滑断裂带为华北平原裂谷系从早第三纪伸展拉张作用进入晚第三纪-第四纪走滑剪切拉张作用的产物,这3条断裂带分别位于3个北东向坳陷带中部,并构成了第四纪沉降中心,与营口-潍坊断裂带一起构成华北平原内的主要强震构造。本文最后提出了华北平原区划分潜在震源区应注意的几点问题,进而针对第四代区划图中华北平原区潜在震源区划分综合方案提出了补充修改意见。     

白山市三岔子区大安屯ML4.7级地震发震构造背景及地倾斜异常特征

给出了１９９４年１月２５日在吉林省白山市三岔子区大安屯地震的基本参数，烈度分布与震害，分析发震的地质构造背景，总结发震前的地倾斜异常特征。     

张强凹陷及邻区的构造应力分析

通过对张强凹陷及邻区露头构造形迹和岩心裂缝测量的应力分析，把该地区的地质历史划分出自太古代以来的８个构造期，确定了各期构造应力场状态及构造组合形式，认为晚侏罗世及白垩纪古构造应力场是断陷盆地形成、发展的主要应力场，晚侏罗世为近东西向拉张的构造应力状态；阜新组沉积期末至泉头组沉积前，由东西向拉张转为近东西向挤压，导致断陷阶段结束和上侏罗统变形；白垩纪为东西向挤压，早期区域整体沉降，晚期大面积隆升遭受剥蚀。早第三纪期为北西－南东向挤压，晚第三纪以来北东东－南西西向挤压。新生代的两期应力场仅使一些断裂继续活动，变形强度小于前两期     

基于片法对地震低活动水平区域的构造分布特征研究

文中应用片法研究了首都圈地区在39.8°～40.4°N和114.0°～115.0°E范围内的地震活动分布。 片法主要是针对地震活动分布比较稀疏、断层无法直观识别的地区,用空间扫描的方法,并结合相应的统计检验方法,来评价地震震中分布的线性特征是否显著,从而进一步识别地震断层。 该文选定的研究区域,在过去30多年的时间里共发生了1.0～5.0级地震906次,地震的活动不活跃比较符合片法的应用研究。 将该方法用于所选定区域地震数据的研究表明,其识别能力还是较好的,可以整体上刻画比较真实的地质构造特征。 对由于种种原因无法进行实测,且地震活动较低的构造区域,片法是分析其构造分布的有效补充。