一种改进的车头SURF特征提取和匹配

通过对加速鲁棒性算法特征关键点提取和匹配的研究,提出一种改进的车头加速鲁棒性特征点提取方法,该方法在车头图像像素梯度变化较大的范围内提取关键点,然后采用最近邻比例算法进行特征点匹配。实验结果表明,提出的改进方法不仅能够筛选出鲁棒性较强的关键点,同时提高了特征的提取速度和匹配效率,在总时间上比尺度不变特征变换算法提高了3~6倍;比加速鲁棒性算法提高了近1/4。     

Detection and extraction of signals from the epoch of reionization using higher-order one-point statistics

Detecting redshifted 21-cm emission from neutral hydrogen in the early Universe promises to give direct constraints on the epoch of reionization (EoR). It will, though, be very challenging to extract the cosmological signal (CS) from foregrounds and noise which are orders of magnitude larger. Fortunately, the signal has some characteristics which differentiate it from the foregrounds and noise, and we suggest that using the correct statistics may tease out signatures of reionization. We generate mock data cubes simulating the output of the Low Frequency Array (LOFAR) EoR experiment. These cubes combine realistic models for Galactic and extragalactic foregrounds and the noise with three different simulations of the CS. We fit out the foregrounds, which are smooth in the frequency direction, to produce residual images in each frequency band. We denoise these images and study the skewness of the one-point distribution in the images as a function of frequency. We find that, under sufficiently optimistic assumptions, we can recover the main features of the redshift evolution of the skewness in the 21-cm signal. We argue that some of these features – such as a dip at the onset of reionization, followed by a rise towards its later stages – may be generic, and give us a promising route to a statistical detection of reionization.     

A search for the 53-MHz OH line near G48.4−1.4 using the National MST Radar Facility

We present the results of a search for the ground-state hyperfine transition of the OH radical near 53 MHz using the National Mesosphere–Stratosphere–Troposphere (MST) Radar Facility at Gadanki, India. The observed position was G48.4−1.4 near the Galactic plane. The OH line is not detected. We place a 3σ upper limit for the line flux density at 39 Jy from our observations. We also did not detect recombination lines (RLs) of carbon, which were within the frequency range of our observations. The 3σ upper limit of 20 Jy obtained for the flux density of carbon RLs, along with observations at 34.5 and 327 MHz, are used to constrain the physical properties of the line-forming region. Our upper limit is consistent with the line emission expected from a partially ionized region with electron temperature, density and path lengths in the range 20–300 K, 0.03–0.3 cm⁻³ and 0.1–170 pc, respectively.     

A source of high-velocity white dwarfs

We investigate whether the recently observed population of high-velocity white dwarfs can be derived from a population of binaries residing initially within the thin disc of the Galaxy. In particular, we consider binaries where the primary is sufficiently massive to explode as a Type II supernova. A large fraction of such binaries are broken up when the primary then explodes as a supernova, owing to the combined effects of the mass loss from the primary and the kick received by the neutron star on its formation. For binaries where the primary evolves to fill its Roche lobe, mass transfer from the primary leads to the onset of a common envelope phase during which the secondary and the core of the primary spiral together as the envelope is ejected. Such binaries are the progenitors of X-ray binaries if they are not broken up when the primary explodes. For those systems that are broken up, a large number of the secondaries receive kick velocities ∼100–200 km s⁻¹ and subsequently evolve into white dwarfs. We compute trajectories within the Galactic potential for this population of stars and relate the birth rate of these stars over the entire Galaxy to those seen locally with high velocities relative to the local standard of rest (LSR) . We show that for a reasonable set of assumptions concerning the Galactic supernova rate and the binary population, our model produces a local number density of high-velocity white dwarfs compatible with that inferred from observations. We therefore propose that a population of white dwarfs originating in the thin disc may make a significant contribution to the observed population of high-velocity white dwarfs.     

Red companions to a z=2.15 radio-loud quasar

We have conducted observations of the environment around the z =2.15 radio-loud quasar 1550–269 in search of distant galaxies associated either with it or the z =2.09 C  iv absorber along its line of sight. Such objects will be distinguished by their red colours, R − K >4.5. We find five such objects in a 1.5 arcmin² field around the quasar, with typical K ' magnitudes of ∼20.4 and no detected R -band emission. We also find a sixth object with K =19.6±0.3, and undetected at R , just two arcsec from the quasar. The nature of all these objects is currently unclear, and will remain so until we have determined their redshifts. We suggest that it is likely that they are associated with either the quasar or the C  iv absorber, in which case their properties might be similar to those of the z =2.38 red Ly α emitting galaxies discovered by Francis et al. The small separation between the quasar and the brightest of our objects suggests that it may be the galaxy responsible for the C  iv metal line absorption system. The closeness to the quasar and the red colour might have precluded similar objects from being uncovered in previous searches for emission from C  iv and damped absorbers.     

A Solution of Einstein's Field Equations fora Tachyonic Gas: Possible Astrophysical Applications

In this paper we show that a change in the signs of some of the metric components of the solution of the field equations for the classical cosmic string results in a solution which we interpret as a time-dependent wall composed of tachyons. We show that the walls have the property of focusing the paths of particles which pass through them. As an illustration of this focusing, we demonstrate the results of a simple simulation of the interaction between one such tachyon wall and a rotating disk of point masses. This interaction leads to the temporary formation of spiral structures. These spiral structures exist for a time on the order of one galactic rotation. This revised version was published online in July 2006 with corrections to the Cover Date.     

The evolution of the z distribution of normal neutron stars in the Galaxy

Under the two initial 1‐D one parameter velocity distribution forms (one is normal, the other is exponential), the z direction scale height evolution of normal neutron stars in the Galaxy is studied by numerical simulation. We do statistics for the cases at different time segments, also do statistics for the cumulative cases made of each time segment. The results show in the cumulative cases the evolution curves of the scale heights are smoother than in the each time segment, i.e., the cumulation improve the signal‐to‐noise ratio. Certainly the evolution cases are different at different Galactic disk locations, which also have very large difference from the average cases in the whole disk. In the initial stages of z evolution of normal neutron stars, after the beginning transient states, the cumulative scale heights increase linearly with time, and the cumulative scale height increasing rates have linear relationship with the initial velocity distribution parameters, which have larger fluctuation in the vicinity of the Sun than in the whole disk. We utilize the linear relationship of the cumulative scale height increasing rates vs. the initial velocity distribution parameters in the vicinity of the Sun to make comparison with the observation near the Sun. The results show if there is no magnetic decay, then the deserved initial velocity parameters are obvious lower than the present well known results from some authors; whereas if introducing magnetic decay, for the 1‐D normal case we can make consistence among concerning results using magnetic decay time values which are supported by some authors, while for the 1‐D exponential case the results show the lackness of young pulsar samples in the larger z in the vicinity of the Sun (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

一种面向遥感影像内容认证的多级权限管理方法

完整性认证是遥感影像获得有效利用的前提,完整性无法确定的遥感影像,其使用价值将大打折扣。传统认证技术没有顾及遥感影像认证过程中的特殊性,并不是所有用户都有权甄别遥感影像是否经过扰动。而且,传统认证技术对数据进行二进制级别的认证,已不能满足遥感影像的内容认证需求。本文从内容认证的角度研究遥感影像的多级权限管理,提出一种基于感知哈希技术与单向函数的遥感影像多级认证权限的管理方法。感知哈希技术能用很少的信息表征遥感影像的有效内容,并对不改变影像内容的操作保持鲁棒性,与密码学Hash函数有着显著的区别。多级权限的管理则通过建立与权限矢量对应的密钥矢量来实现,权限较高的用户可以通过自己的密钥计算出低权限用户的密钥,反之则不行。本方法首先以单向函数生成不同等级的权限密钥,然后,根据不同区域的地物影像进行敏感等级的划分,最后,计算不同区域影像的感知哈希序列,并通过不同级别的密钥加密生成的感知哈希序列。用户认证影像内容完整性时,根据权限的不同认证不同敏感度的影像。实验与分析表明,该算法能有效实现遥感影像的认证权限管理,并具有较高的实现效率和安全性。     

ETM+全色波段及其多光谱波段图像的融合应用

Landsat-7ETM+的全色波段与多光谱波段有相同的太阳高度角和其他环境条件,影像获取时间一致,两种不同分辨率的数据可以不经配准而实现高精度融合。目前常用的图像融合方法很多,究竟哪种方法更适合于ETM+图像,本次试验采用HIS变换、Brovey变换、SFIM变换、加权融合4种方法,分别实现ETM+Pan与ETM+的多光谱波段的融合,并从空间纹理信息、光谱真实性2个方面进行定量和定性地评价。研究表明,从综合角度出发,基于SFIM变换的融合方法产生的光谱扭曲和失真较小,同时很大程度地保持了高分辨率的全色波段的空间纹理细节信息,是一种适合于ETM+图像融合的较佳方法。