Are Type Ia Supernovae Reliable Distance Indicators？

Recent applications of type Ia supernovae(SNe Ia)in cosmology have successfully revealed the accelerating expansion of the universe.However,as distance indicators used in measuring the expansion history of the universe and probing the nature of dark energy,these objects must pass more strict tests.We propose a K-S test to investigate if there exists any systematic bias when deriving the luminosity distances under the standard candle assumption. Two samples,one comprising 71 high-redshift SNe Ia and the other,44 nearby ones,are used in our investigation.We find that it is likely there exists a bias in the adopted samples,which is probably caused by a systematic error,e.g.in the color parameter used in the luminosity calibration and a bias may be caused by the SN evolution or by varying properties of the dust surrounding the SNe Ia.     

云南地区现今地壳水平运动与变形特征

利用云南地区 1999、2 0 0 0、2 0 0 1年共 10 0余个测站的GPS资料 ,获得了该区现今水平运动与形变的特征图像。研究结果认为 :①根据变形与运动特征 ,云南地区可划分为 4个运动单元 ,即滇西地区、滇东地区、滇中东北地区和滇中西南地区 ;剔除整体运动后 ,它们的优势水平运动分别为 :滇西地区以 5 .2± 0 .6mm/a向W 31°N运动 ,滇东地区以 4 .8± 1.8mm/a向E2 6°N运动 ,滇中东北地区以 5 .2± 0 .6mm/a向S4 4°E运动 ,滇中西南地区则基本不动。②相邻单元的平均差异运动分别为 :滇西地区相对滇中东北地区的运动为 10 .9± 1.1mm/a ,方向为W 39°N(张性右旋 ) ,相对滇中西南地区的运动为 5 .3± 1.3mm/a ,方向为W 4 1°N(右旋 ) ;滇中东北地区相对滇中西南地区的运动为 5 .6± 1.6mm/a ,方向为E36°S(左旋 ) ;滇东地区相对滇中东北地区的运动为 6 .2± 1.6mm/a ,方向为N3°E(左旋 )。③从断裂走滑活动看 ,红河断裂两侧的差异运动并不是由红河断裂的活动所形成的 ,而是在很广阔的空间上自西向东渐变而成的 ,跨距达数百km ;小江断裂两侧的差异运动也非完全是小江断裂本身的活动 ,差异运动的渐变空间至少在 6 0km以上。④云南地区的地壳运动方式可能是“断块活动”和“连续变形”的组合 ,或许“连续变形”     

On the deprojection of clusters of galaxies combining X-ray, Sunyaev–Zeldovich temperature decrement and gravitational lensing maps

Knowledge of the intrinsic shape of galaxy clusters is very important in investigating cosmic structure formation and astrophysical processes. The reconstruction of the 3D structure usually relies on deprojecting 2D X-ray, Sunyaev–Zeldovich (SZ) and/or gravitational lensing observations. As known, a joint analysis of these data sets can provide the elongation of the cluster along the line of sight together with its length and width in the plane of the sky. An unbiased measurement of the Hubble constant can be also inferred. Due to some intrinsic degeneracies, the observational constraints obtained from such projected data sets are not enough to allow an unique inversion. In general, the projected maps can be at the same time compatible with prolate, oblate and with many triaxial configurations. Even a prolate cluster might be interpreted as an oblate system and vice versa. Assuming that the cluster is axially symmetric is likely to overestimate the intrinsic ellipticity, whereas the system always looks rounder performing the inversion under the hypothesis of a triaxial cluster aligned with the line of sight. In general, analysing triaxial clusters under the prolate or oblate assumption may introduce strong biases even when the clusters are actually near to axial symmetry whereas the systematics introduced assuming the cluster to be aligned with the line of sight are more under control.     

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A robust method for measuring the Hubble parameter

We obtain a robust, non-parametric, estimate of the Hubble constant from the linear diameters and rotation velocities of galaxies in the recent KLUN sample, calibrated using Cepheid distances to Hubble Space Telescope Key Project galaxies. There are two key features that make our analysis considerably more robust than previous work. First, the method is independent of the spatial distribution of galaxies and is insensitive to Malmquist bias. It may, therefore, be applied to more distant samples than so-called 'plateau' methods – making it much less vulnerable to the impact of peculiar motions in the Local Supercluster. Secondly, we include information on the galaxy rotation velocities in a fully non-parametric manner: unlike the conventional Tully–Fisher relation we reconstruct a robust estimate of the cumulative distribution function of galaxy diameter at given rotation velocity, without requiring the assumption of, for example, a linear Tully–Fisher relation with symmetric Gaussian residuals.
Using this robust method we find H ₀=65±6 km s⁻¹ Mpc⁻¹ from our analysis – in excellent agreement with many recent determinations of the Hubble parameter, although somewhat larger than previous results using galaxy diameters.     

Calculating horizontal stress orientations with full or partial knowledge of the tectonic stress tensor

Earthquakes potentially serve as abundant and cost-effective gauges of tectonic stress provided that reliable means exist of extracting robust stress parameters. Several algorithms have been developed for this task, each of which typically provides information on the orientations of the three principal stresses and a single stress magnitude parameter. A convenient way of displaying tectonic stress results is to map the azimuth of maximum horizontal compressive stress, which is usually approximated using the azimuth of the larger subhorizontal principal stress. This approximation introduces avoidable errors that depend not only on the principal stress axes' plunges but also on the value of the stress magnitude parameter. Here we outline a method of computing the true direction of maximum horizontal compressive stress ( S _H) and show that this computation can be performed using only the four stress parameters obtained in routine focal mechanism stress estimation. Using theoretical examples and new stress inversion results obtained with focal mechanism data from the central Grímsey lineament, northern Iceland, we show that the S _H axis may differ by tens of degrees from its commonly adopted proxy. In order to most appropriately compare tectonic stress estimates with other geophysical parameters, such as seismic fast directions or geodetically measured strain rate tensors, or to investigate spatiotemporal variations in stress, we recommend that full use be made of the routinely estimated stress parameters and that a formal axis of maximum horizontal compression be calculated.     

Mapping Paleo‐Fire Boundaries from Binary Point Data: Comparing Interpolation Methods

Fire history studies have traditionally emphasized temporal rather than spatial properties of paleo‐fire regimes. In this study we compare four methods of mapping paleo‐fires in central Washington from binary point data: indicator kriging, inverse distance weighting, Thiessen polygons, and an expert approach. We evaluate the results of each mapping method using a test (validation) dataset and receiver operating characteristic plots. Interpolation methods perform well, but results vary with fire size and spatial pattern of points. Though all methods involve some subjectivity, automated interpolation methods perform well, are replicable, and can be applied across varying landscapes.     

单层褶皱变形过程中最大主应力与水平应变的变化及其影响因素

对地质构造进行定量半定量研究是地质工作者近几十年来一直努力的方向,构造数值模拟是有效的定量研究方法之一。褶皱是一种典型的构造类型,对褶皱构造进行定量半定量研究也一直是构造地质学家们所致力解决的研究课题。本文结合近年来单层褶皱构造数值模拟研究进展,以及笔者近几年来对单层褶皱所进行的数值模拟实验研究,主要论述了单层褶皱变形的影响因素,单层褶皱变形过程中的最大主应力与水平应变的变化及其影响因素等。数值模拟技术为褶皱变形提供了一种新的研究方法,该方法在构造地质领域将有很好的发展前景。     

模糊理论在遥感图像分类中的应用

利用2000年假彩色遥感图像,采用模糊C-均值法中的欧氏距离和马氏距离法对崇明东滩的遥感图像进行了处理。通过对白色覆盖物、未耕种土地、一号水稻田、水体和二号水稻田的分类结果表明,欧氏距离的聚类结果优于马氏距离。