Two strong radio bursts at high and medium Galactic latitude

The Nasu Observatory, which is composed of eight 20 m elements, was constructed for observing radio transients over a wide field at 1400 MHz. We report on two radio transients detected in consecutive drift scanning observations at declination 32° over a period of about two months. One of the two transients, WJN J1039+3200, appeared at =10^h39^m40^s±10^s, δ=32°±0.4° on March 4, 2005, and the other one, WJN J0645+3200, appeared at =06^h45^m25^s±10^s, δ=32°±0.4° on March 24, 2005. Both exhibited flux densities in excess of 1 Jy, and the burst durations were up to two days. Since there are few examples of radio transients outside the Galactic plane, these are very important observations. We have previously reported on four radio transients with features that look like the two transients detected this time. Of these six WJN transients in total, five had a duration of up to two days, and one up to three days. Four of the transients were detected at high Galactic latitude of b > 30°. Counterparts of the six WJN transients included X-ray sources in four events and had a consistency of 66%. The consistency of γ-ray, PGC Galaxy, NVSS, and FIRST sources was concentrated at about 50%. We were not able to find any special features in the counterparts. The distribution was verified by making a log N–log S plot using data for the four previously detected transients and the new ones. As a result, the distribution of the radio transients that we observed might have an isotropic distribution not dependent on Galactic longitude and Galactic latitude. The detection probability was calculated based on the assumption of an isotropic distribution. The 2σ upper probability limit for detection of transients of 1000 mJy or more is 0.0049 [deg⁻² yr⁻¹]. We cannot yet identify these two radio transients, because their features are different from any radio bursts observed in the past.     

基于L1范数的波阻抗反演

提出了一种新的波阻抗反演方法,首先根据地下反射系数序列是一个稀疏脉冲序列这一假设,将地震波阻抗反演中的目标函数表示为L1范数约束下的L1范数优化问题,并将L1范数用一个平滑函数来近似,从而使得目标函数函数可微。然后将L1范数约束下的基追踪问题转化为无约束最优化问题,并利用基于导数的局部优化方法求解无约束优化问题,求得反射系数,进而计算得到波阻抗。模型和实际资料计算结果均表明该方法可行。     

Cotton canopy reflectance under variable solar zenith angles: Implications of use in evapotranspiration models

Evapotranspiration (ET) is an important parameter in hydrologic processes and modelling. In agricultural watersheds with competing uses of fresh water including irrigated agriculture, estimating crop evapotranspiration (ET_c) accurately is critical for improving irrigation system and basin water management. The use of remote sensing-based basal crop coefficients is becoming a common method for estimating crop evapotranspiration for multiple crops over large areas. The Normalized Difference Vegetation Index (NDVI) and the Soil Adjusted Vegetation Index (SAVI), based on reflectance in the red and near-infrared bands, are commonly used for this purpose. In this paper, we examine the effects of row crop orientation and soil background darkening due to shading and soil surface wetness on these two vegetation indices through modelling, coupled with a field experiment where canopy reflectance of a cotton crop at different solar zenith angles, was measured with a portable radiometer. The results show that the NDVI is significantly more affected than the SAVI by background shading and soil surface wetness, especially in north–south oriented rows at higher latitudes and could lead to a potential overestimation of crop evapotranspiration and irrigation water demand if used for basal crop coefficient estimation. Relationships between the analysed vegetation indices and canopy biophysical parameters such as crop height, fraction of cover and leaf area index also were developed for both indices.     

空中目标探测系统信号处理增益分析

针对利用全球导航卫星反射信号(GNSS-R)进行空中目标探测时,信号微弱无法可靠接收的问题,该文提出了一种计算信号处理增益的方法。通过合理设置信号处理算法参数,保证了对微弱信号的后续处理。首先对GNSS-R信号接收链路进行了分析,计算得到了当目标的雷达散射截面(RCS)变化时对应的目标回波功率范围;然后对空中目标上升、平飞和下降三种飞行状态双基地雷达系统几何模型进行了研究,给出了3种飞行状态下对应的有效探测时间,为接收机后续相干/非相干累加算法的处理时间提供阈值限制;最后在阈值范围内,选定合适相关时间,分析了经过相干/非相干累加处理后的反射信号输出信噪比范围。结果表明:在有效探测时间的限制下,相关处理时间取0.6s时,处理后的信噪比在10dB左右,满足一般码跟踪环所需的门限要求,可以保证接收机后续数据处理的顺利进行。     

使用ERS-1/2干涉测量SAR数据生成DEM

干涉合成孔径雷达（ＩＮＳＡＲ）数据已被证明能生产精确的数据高程模型（ＤＥＭ），我们已开发了从单视ＳＡＲ复影像数据自动生成数字高程模型的新软件，基于ＳＡＲ多视强度影像的最小二乘曩像匹配被用于复影像对的配准，达到很高的配准精度（０．０１～０．０５像元精度）。一种新的计算目标点３维坐标（Ｘ，Ｙ，Ｚ）的方程还被提出，卫星轨道，姿态和基线参数以及相位常数被纳入在方程中并被表示了时间的线性函数，利用至少６个地面控制点能够同时估算这些参数，本文还给出了意大利埃特地区ＥＲＳ－１／２ＳＡＲ数据处理结果。     

面向下一代灵活光网络的数字相干光传输技术

为了适应不同颗粒度的业务需求,最大化波分复用传输系统的频谱效率,光网络正逐渐朝着更灵活、高效、节能的趋势发展.基于带宽可变收发机（BVT）的灵活光网络传输技术因而得到了广泛的关注与研究.本文概述了国内外支持灵活光网络的数字相干光传输技术的最新研究进展,包括发射端支持传输速率可变的自适应编码、调制技术以及接收端相应的调制码型识别技术,最后对灵活光网络传输的未来研究方向进行了展望.     

VSOP and ground-based VLBI observations of Markarian 421

We have produced 22 VLBI images of the TeV blazar Markarian 421 at 11 epochs, including a Space VLBI observation with the HALCA satellite. We measure the speeds of the three innermost jet components to be 0.64±0.33, 0.48±0.09, and 0.06±0.09c (H₀=65 km s⁻¹ Mpc⁻¹). Interpretation of these subluminal speeds in terms of the high Doppler factor demanded by the TeV observations is discussed.     

Differential astrometry over 15°

We observed the pair of radio sources 1150+812 and 1803+784 in November 1993 with a VLBI array, simultaneously recording at 8.4 and 2.3 GHz. We determined the angular separation between the two sources with submilliarcsecond accuracy by using differential techniques. This result demonstrates the feasibility of high precision differential astrometry for radio sources separated in the sky by almost 15°, and opens the avenue to its application to larger samples of radio sources.     

Wide-field VLBI imaging

We discuss the technique of Wide-field imaging as it applies to Very Long Baseline Interferometry (VLBI). In the past VLBI data sets were usually averaged so severely that the field-of-view was typically restricted to regions extending a few hundred milliarcseconds from the phase centre of the field. Recent advances in data analysis techniques, together with increasing data storage capabilities, and enhanced computer processing power, now permit VLBI images to be made whose angular size represents a significant fraction of an individual antenna's primary beam. This technique has recently been successfully applied to several large separation gravitational lens systems, compact Supernova Remnants in the starburst galaxy M82, and two faint radio sources located within the same VLA FIRST field. It seems likely that other VLBI observing programmes might benefit from this wide-field approach to VLBI data analysis. With the raw sensitivity of global VLBI set to improve by a factor 4–5 over the coming few years, the number of sources that can be detected in a given field will rise considerably. In addition, a continued progression in VLBI's ability to image relatively faint and extended low brightness temperature features (such as hot-spots in large-scale astrophysical jets) is also to be expected. As VLBI sensitivity approaches the μJy level, a wide-field approach to data analysis becomes inevitable.