Speckle-interferometric Study of Close Visual Binary System HIP 11253(HD 14874)using Gaia(DR2 and EDR3)

We present a comprehensive set of physical and geometrical parameters for each of the components of the close visual binary system HIP 11253(HD 14874).We present an analysis for the binary and multiple stellar systems with the aim to obtain a match between the overall observational spectral energy distribution of the system and the spectral synthesis created from model atmospheres using Al-Wardat's method for analyzing binary and multiple stellar systems.The epoch positions are used to determine the orbital parameters and the total mass.The parameters of both components are derived as:T_(eff)^(a)=6025,T_(eff)^(b)=4710,logg_(a)=4.55,logg_(b)=4.60,R_(a)=1.125 R_(⊙),R_(b)=0.88R_(⊙),L_(a)=1.849 L_(⊙),L_(b)=0.342 L_(⊙).Our analysis shows that the spectral types of the components are F9 and K3.By combining the orbital solution with the parallax measurements of Gaia DR2 and EDR3,we estimate the individual masses using the H-R diagram as M_(a)=1.09 M_(⊙)and M_(b)=0.59 M_(⊙)for using Gaia DR2 parallax and M_(a)=1.10 M_(⊙)and M_(b)=0.61 M_(⊙)for using Gaia EDR3 parallax.Finally,the location of both system's components on the stellar evolutionary tracks is presented.

Estimating statistics of sky brightness using radio interferometric observations

Radio interferometers are used to construct high resolution images of the sky at radio frequencies and are the key instruments for accessing the statistical properties of the evolution of neutral hydrogen over cosmic time. Here we use simulated observations of the model sky to assess the efficacy of different estimators of the large-scale structure and power spectrum of the sky brightness distribution. We find that while the large-scale distribution can be reasonably estimated using the reconstructed image from interferometric data, estimates of the power spectrum of the intensity fluctuations calculated from the image are generally biased. This bias is found to be more pronounced for diffuse emission. The visibility based power spectrum estimator, however, gives an unbiased estimate of the true power spectrum. This work demonstrates that for an observation with diffuse emission the reconstructed image can be used to estimate the large-scale distribution of the intensity, while to estimate the power spectrum, visibility based methods should be preferred.With the upcoming experiments aimed at measuring the evolution of the power spectrum of the neutral hydrogen distribution, this is a very important result.

Fine-grained distributed averaging for large-scale radio interferometric measurement sets

The Square Kilometre Array(SKA)would be the world’s largest radio telescope with eventually over a square kilometre of collecting area.However,there are enormous challenges in its data processing.The use of modern distributed computing techniques to solve the problem of massive data processing in the SKA is one of the most important challenges.In this study,basing on the Dask distribution computational framework,and taking the visibility function integral processing as an example,we adopt a multi-level parallelism method to implement distributed averaging over time and channel.Dask Array was used to implement super large matrix or arrays with supported parallelism.To maximize the usage of memory,we further exploit the data parallelism provided by Dask that intelligently distributes the computational load across a network of computer agents and has a built-in fault tolerance mechanism.The validity of the proposed pattern was also verified by using the Common Astronomy Software Application(CASA),wherein we analyze the smearing effects on images reconstructed from different resolution visibilities.

A Novel Two-dimensional Low-redundancy Array Design for Solar Radio Imaging

The radioheliograph is an extensive array of antennas operating on the principle of aperture synthesis to produce images of the Sun.The image acquired by the telescope results from convoluting the Sun’s true brightness distribution with the antenna array’s directional pattern.The imaging quality of the radioheliograph is affected by a multitude of factors,with the performance of the“dirty beam”being simply one component.Other factors such as imaging methods,calibration techniques,clean algorithms,and more also play a significant influence on the resulting image quality.As the layout of the antenna array directly affects the performance of the dirty beam,the design of an appropriate antenna configuration is critical to improving the imaging quality of the radioheliograph.Based on the actual needs of observing the Sun,this work optimized the antenna array design and proposed a twodimensional low-redundancy array.The proposed array was compared with common T-shaped arrays,Y-shaped arrays,uniformly spaced circular arrays,and three-arm spiral arrays.Through simulations and experiments,their performance in terms of sampling point numbers,UV coverage area,beam-half width,sidelobe level,and performance in the absence of antennas are compared and analyzed.It was found that each of these arrays has its advantages,but the two-dimensional low-redundancy array proposed in this paper performs best in overall evaluation.It has the shortest imaging calculation time among the array types and is highly robust when antennas are missing,making it the most suitable choice.

Possible Habitats for NH_(3),NH_(2)D,H^(13)CN,HC^(15)N,SO,and C^(18)O in the Initial Conditions of High-mass Star Formation

The initial condition of high-mass star formation is a complex area of study because of the high densities(n_(H_(2))>106cm^(-3))and low temperatures(T_(dust)<18 K)involved.Under such conditions,many molecules become depleted from the gas phase by freezing out onto dust grains.However,the N-bearing and deuterated species could remain gaseous under these extreme conditions,suggesting that they may serve as ideal tracers.In this paper,using the Plateau de Bure Interferometer and Very Large Array observations at 1.3 mm,3.5 mm,and 1.3 cm,we investigate the possible habitats for NH_(3),NH_(2)D,H^(13)CN,HC^(15)N,SO,and C^(18)O in eight massive precluster and protocluster clumps G18.17,G18.21,G23.97N,G23.98,G23.44,G23.97S,G25.38,and G25.71.We found that the NH3cores are in good agreement with the 3.5 mm peak emission,but the NH_(3)is much more extended than the 3.5 mm emission structure.The SO distributions agree well with the 3.5 mm peaks for the evolved star formation stage,but we did not detect any SO emission in the four earliest star formation sources.C^(18)O is a poor tracer in conditions of the cold(■18 K)and dense(■10^(4)cm^(-3))cores,e.g.,the prestellar cores.We also found that the NH_(2)D cores are mainly located in the temperature range of 13.0-20.0 K,and the NH_(2)D lines may be strongly depleted above 20 K.

The RFI Fast Mitigation Algorithm Based on Block LMS Filter

The radio telescope possesses high sensitivity and strong signal collection capabilities.While receiving celestial radiation signals,it also captures Radio Frequency Interferences(RFIs)introduced by human activities.RFI,as signals originating from sources other than the astronomical targets,significantly impacts the quality of astronomical data.This paper presents an RFI fast mitigation algorithm based on block Least Mean Square(LMS)algorithm.It enhances the traditional adaptive LMS filter by grouping L adjacent time-sampled points into one block and applying the same filter coefficients for filtering within each block.This transformation reduces multiplication calculations and enhances algorithm efficiency by leveraging the time-domain convolution theorem.The algorithm is tested using baseband data from the Parkes 64 m radio telescope's pulsar observations and simulated data.The results confirm the algorithm's effectiveness,as the pulsar profile after RFI mitigation closely matches the original pulsar profile.

Numerical simulation of time delay interferometry for TAIJI and new LISA

The success of LISA Pathfinder in demonstrating the LISA drag-free requirement paved the way for using space interferometers to detect low-frequency and middle-frequency gravitational waves(GWs). The TAIJI GW mission and the new LISA GW mission propose using an arm length of 3 Gm(1 Gm = 10~6 km) and an arm length of 2.5 Gm respectively. For a space laser-interferometric GW antenna,due to astrodynamical orbit variation, time delay interferometry(TDI) is needed to achieve nearly equivalent equal-arms for suppressing the laser frequency noise below the level of optical path noise, acceleration noise, etc in order to attain the requisite sensitivity. In this paper, we simulate TDI numerically for the TAIJI mission and the new LISA mission. To do this, we work out a set of 2200-day(6-year) optimized science orbits for each mission starting on 2028 March 22 using the CGC 2.7.1 ephemeris framework. Then we use the numerical method to calculate the residual optical path differences of the first-generation TDI configurations and the selected second-generation TDI configurations. The resulting optical path differences of the second-generation TDI configurations calculated for TAIJI, new LISA and eLISA are well below their respective requirements for laser frequency noise cancelation. However, for the first-generation TDI configurations, the original requirements need to be relaxed by 3 to 30 fold to be satisfied. For TAIJI and the new LISA, about one order of magnitude relaxation would be good and recommended; this could be borne on the laser stability requirement in view of recent progress in laser stability, or the GW detection sensitivities of the second-generation TDIs have to be used in the diagnosis of the observed data instead of the commonly used X, Y and Z TDIs.

A new demodulation technique for optical fiber interferometric sensors with[3×3]directional couplers

Optical fiber interferometric sensors based on [3×3] couplers have been used in many fields. A new technique is proposed to demodulate output signals of this kind of sensors. The technique recovers the signal of interest by fitting coefficients of elliptic （Lissajous） curves between each fiber pair. Different from other approaches, this technique eliminates the dependence on the idealization of [3×3] coupler, provides enhanced tolerance to the variance of photoelectric converters, and is anti-polarization in a certain extent. The main algorithm has been successfully demonstrated both by numerical simulation and experimental result.

Research on fiber-optic interferometric hydrophone array using frequency division multiplying technique

From the point of view of system design, a configuration of fiber-optic interferomet- ric hydrophone array and its modulation and demodulation approach using frequncy division multiplexing technique based on Phase Generated Carrier (PGC) is introduced. And the em- phasis on demonstrating the relationship among the number of units N, the detectable signal amplitude D and the detectable frequency ws through analyzing the frequency spectrum of the output signal of the J × K array and the key factor which restricts N, D, Ws for increasing are presented. The maximum phare shift and the law of its variation according to frequency are specially analyzed. The results induced from some relative theory were verified by experiments.

干涉星敏感器测角精度影响因素的研究

为了提高传统星敏感器的姿态测量精度,可将干涉测角技术与传统星敏感器相结合,即在传统星敏感器质心定位技术的基础上,利用星像点的光强信息进一步进行细分,从而突破了质心定位的精度限制,形成具有大视场高精度的干涉星敏感器。本文对制约干涉星敏感器测角精度的因素进行深入研究,重点研究干涉条纹的分割误差对测角精度的影响机理。通过研究分析,得出以下结论:光锲阵列不等分误差不是影响干涉星敏感器测角精度的主要因素;莫尔条纹周期与光楔阵列整体通光尺寸不匹配误差小于1%时,可保证单因素测角误差小于0.01";对于莫尔条纹取向与光楔阵列排布方向不正交误差,条纹旋转角度应当小于0.1°,可保证单因素测角误差小于0.01"。所以,应在实际加工与装调过程中抑制上述两个主要误差,从而使干涉星敏感器的实际测角精度接近高精度理论值。

The Edge Sensor of Segmented Mirror Based on Fringes of Equal Thickness

Co-phase and co-focus detection is one of the key technologies for large-aperture segmented mirror telescopes.In this paper,a new edge sensor based on fringes of equal thickness is developed,which can detect each segment's relative piston,tilt,and tip errors from the interferograms.Based on the co-focus demand for many ground-based seeing limited segmented mirror telescopes,an edge sensor prototype based on such a principle is built and applied in the indoor segmented mirror experiment system in the lab.According to the co-focus requirement of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope,many simulations and experiments are carried out for cofocus error detection of the segmented mirror system.Experiment results show that the co-focus accuracy is better than 002 rms,which can meet the co-focus requirements of most large or extremely large segmented mirror astronomical telescopes.

A Simulation of Calibration and Map-making Errors of the Tianlai Cylinder Pathfinder Array

The Tianlai cylinder array is a pathfinder for developing and testing 21 cm intensity mapping techniques.In this paper,we use numerical simulation to assess how its measurement is affected by thermal noise and the errors in calibration and map-making process,and the error in the sky map reconstructed from a drift scan survey.Here we consider only the single frequency,unpolarized case.The beam is modeled by fitting to the electromagnetic simulation of the antenna,and the variations of the complex gains of the array elements are modeled by Gaussian processes.Mock visibility data are generated and run through our data processing pipeline.We find that the accuracy of the current calibration is limited primarily by the absolute calibration,where the error comes mainly from the approximation of a single dominating point source.We then studied the m-mode map-making with the help of Moore-Penrose inverse.We find that discarding modes with singular values smaller than a threshold could generate visible artifacts in the map.The impacts of the residue variation of the complex gain and thermal noise are also investigated.The thermal noise in the map varies with latitude,being minimum at the latitude passing through the zenith of the telescope.The angular power spectrum of the reconstructed map show that the current Tianlai cylinder pathfinder,which has a shorter maximum baseline length in the North-South direction,can measure modes up to l■2πb_(NS)/λ~200 very well,but would lose a significant fraction of higher angular modes when noise is present.These results help us to identify the main limiting factors in our current array configuration and data analysis procedure,and suggest that the performance can be improved by reconfiguration of the array feed positions.

太阳系人造天体VLBI观测

简单介绍了VLBI技术用于太阳系人造天体观测的进展状况，并对这一研究方向的天文研究课题作了展望。

光纤Bragg光栅在动态应变测量中的研究

为了将光纤光栅的传感特性应用于结构健康监测和高频应力作用下的材料力学性能测试中,对光纤光栅动态应变传感的测量进行了研究.设计了基于相位载波(PGC)零差法的非平衡Mach-Zender干涉解调系统,并对相位载波解调技术进行了分析.通过对比冲击实验和频谱分析,实验结果证明该检测方法有效可行,可以得到稳定的测量信号,系统在10kHz的频率范围内有良好的频率响应.

基于白光干涉的MEMS三维表面形貌测量

利用白光干涉垂直扫描原理,设计了测量微机电系统(MEMS)表面形貌特征的垂直扫描白光干涉系统.该系统由垂直扫描位移工作台驱动被测件,通过检测被测件表面的干涉条纹变化得到表面形貌.垂直扫描位移工作台利用压电陶瓷驱动柔性铰链结构进行纳米驱动,光栅传感器监控整个垂直扫描过程,对压电陶瓷的非线性误差进行实时补偿.垂直扫描位移工作台的性能分析表明:分辨率达到1 nm,定位精度小于10 nm.同时采用图像分析技术对光学仪器测量台阶出现的噪声进行了消噪处理,试验结果表明垂直扫描白光干涉系统能够实现MEMS三维表面形貌的高精度测量.

结合InSAR的幂指数Knothe模型参数拟合与评估

针对目前我国矿山开采沉陷监测方法与预计模型中存在的不足,提出一种采用水准与InSAR(合成孔径雷达干涉测量)技术相结合的幂指数Knothe模型参数估算方法,并分析该模型的拟合预测精度。首先选取某矿区工作面作为实验区,收集该工作面的8次水准测量数据与5景雷达影像提取水准点的时序沉降信息,其次分析实验区随开采活动引起的岩层移动变形结果,然后利用两者结合得到的时序沉降信息与单独水准测量数据分别估算幂指数Knothe模型的未知参数,得到2组地表下沉拟合曲线。最后利用该2组曲线估算水准点处的拟合值和预测值,并与实测值进行对比,分析InSAR结果对模型拟合预测精度的影响。结果表明,InSAR测量精度满足实际矿山开采要求,与岩层移动变形结果相符;InSAR测量结果可优化水准点的拟合下沉曲线,显著提高幂指数Knothe模型的拟合预测精度。

悬浮扩散共聚法制备聚合物GRIN小球及对折射率梯度分布的控制

选用 MMA为单体 M1、 3 FEA为单体 M2 ,通过悬浮扩散共聚法制备了可见光透过率为 90 %的聚合物GRIN小球 .采用剪切干涉法测得小球内的折射率基本上呈抛物线型球对称梯度分布 ,折射率差Δn达到0 .0 1 9.

VLBI相位连接以及相时延解算的新方法研究

甚长基线干涉测量(VLBI,Very Long Baseline Interferometry)能够提高深空探测器测定轨的精度,目前应用于深空探测中的多为差分VLBI技术(?VLBI).差分VLBI相关相位中存在时间间隔,把不同时间段的相位无整周模糊度地连接起来能清晰地反映卫星运动轨迹,有助于提高卫星的测定轨精度和开展行星无线电科学研究.同时,VLBI相时延因其超高的精度有广泛应用,但解算条件苛刻.基于此,首先利用两个频点的差分相位与单频点相位变化趋势一致的思想,研究了一种新方法连接差分VLBI单频点的相位;然后提出一种利用窄带宽(1 MHz)中的两个频点相位解算相时延的方法,并用嫦娥三号(CE3)着陆器的数据做了实际解算和验证;最后给出了仅利用数天VLBI相时延对着陆器进行定位的方法,得到的结果为(44.1239°N,19.5106°W),和事后基于美国月球侦察轨道器(LRO)窄角相机(NAC)影像数据的定位结果(44.12189°N,19.51129°W)相比,差异为百米左右,验证了仅利用VLBI相时延也能进行着陆器定位的有效性.

数字散斑干涉技术在形貌测量中的应用及进展

介绍了数字散斑干涉技术用于形貌测量的基本原理及其发展，对几种主要的测量方法进行了分类与对比，分析了各种方法的特点。

以密度为导向的条纹正则优化方法

在光学干涉测量技术中,准确地实现条纹正则化是提取条纹图中的相位信息的前提.文中基于双重正交带通滤波器的正则优化法,提出了以条纹密度信息为质量评估标准来引导条纹正则化的优化方法,包含条纹图局部优化与整体优化两部分,是对双重正交带通滤波器的正则化方法的改进.首先以条纹背景强度和振幅具有的局部线性与连续性特征设计能量函数,并通过最小化能量函数获取背景强度和条纹振幅的值;然后根据高低密度区域条纹的分析,提出密度对正则化过程的导向作用以及局部优化的可行性.实验结果表明,以密度为导向的条纹正则优化法具有均方误差低、抗噪性高等优点;提出的条纹正则优化方法在操作上不需要对噪声严重的条纹图进行除噪预处理,对背景强度与振幅的线性与非线性变化可同时处理,具有较高的条纹处理效率和准确性,可应用于复杂的条纹图正则化处理.