Photometric Analysis for Asteroid(81)Terpsichore using Convex Inversion and Phase Function Fitting Methods

The shapes and rotation states(periods and pole orientations)of main-belt asteroids are important for understanding their formation and evolution.In order to obtain sufficient photometric data covering different apparitions for asteroid(81)Terpsichore,ground-based photometric observations in 2020 and 2021 were carried out.By combining published and newly obtained photometric data,we calculated the shape and spin parameters for(81)Terpsichore using the convex inversion method.With this method,we have derived a best fitted pole orientation—(22.2±_(3.1)^(3.3°),17.5±_(5.5)^(10.8°))with a spin period of 10.94±_(0.01)^(0.01)h.Based on the derived convex shape of(81)Terpsichore,we have fitted the H,G+1,G_(2)phase function using the calibrated TESS data and Gaia data after accounting for the lightcurve amplitude correction.As a result,we have derived its absolute magnitude H=8.68±_(0.19)^(0.22)mag with corresponding phase function parameters G_(1)=0.82±_(0.10)^(0.09)and G_(2)=0.02±_(0.02)^(0.03).

Photometric Calibration of the Lunar-based Ultraviolet Telescope for Its First Six Months of Operation on the Lunar Surface

We describe the photometric calibration of the Lunar-based Ultraviolet Telescope（LUT）, the first robotic astronomical telescope working on the lunar surface, for its first six months of operation on the lunar surface. Two spectral datasets（set A and B） from near-ultraviolet（NUV） to the optical band were constructed with 44 International Ultraviolet Explorer（IUE） standards, because of the LUT＇s relatively wide wavelength coverage. Set A was obtained by extrapolating the IUE NUV spectra（λ 〈 3200 ） to the optical band based upon the theoretical spectra of stellar atmosphere models. Set B was composed of theoretical spectra from 2000 to 8000 extracted from the same model grid. In total, seven standards have been observed in15 observational runs until May 2014. The calibration results show that the photometric performance of LUT is highly stable in its first six months of operation. The magnitude zero points obtained from the two spectral datasets are also consistent with each other, i.e., zp = 17.54 ± 0.09 mag（set A） and zp = 17.52 ± 0.07 mag（set B）.

Photometric and Spectroscopic Study of Two Low Mass Ratio Contact Binary Systems:CRTS J225828.7-121122 and CRTSJ030053.5+230139

The study reports photometric and spectroscopic observations of two recently recognized contact binary systems.Both systems show total eclipses and analysis of the light curves indicates both have very low mass ratios of less than 0.3.We derive absolute parameters from color and distance based calibrations and show that,although both have low mass ratios,they are likely to be in a stable orbit and unlikely to merge.In other respects,both systems have characteristics similar to other contact binaries with the secondary larger and brighter than their main sequence counterparts and we also find that the secondary is considerably denser than the primary in both systems.

PC-VINS-Mono: A Robust Mono Visual-Inertial Odometry with Photometric Calibration

Feature detection and Tracking, which heavily rely on the gray value information of images, is a very importance procedure for Visual-Inertial Odometry (VIO) and the tracking results significantly affect the accuracy of the estimation results and the robustness of VIO. In high contrast lighting condition environment, images captured by auto exposure camera shows frequently change with its exposure time. As a result, the gray value of the same feature in the image show vary from frame to frame, which poses large challenge to the feature detection and tracking procedure. Moreover, this problem further been aggravated by the nonlinear camera response function and lens attenuation. However, very few VIO methods take full advantage of photometric camera calibration and discuss the influence of photometric calibration to the VIO. In this paper, we proposed a robust monocular visual-inertial odometry, PC-VINS-Mono, which can be understood as an extension of the opens-source VIO pipeline, VINS-Mono, with the capability of photometric calibration. We evaluate the proposed algorithm with the public dataset. Experimental results show that, with photometric calibration, our algorithm achieves better performance comparing to the VINS-Mono.

太阳系外行星探测技术概述

自20世纪90年代首次发现太阳系外行星(以下简称系外行星)以来,系外行星探测技术取得了飞速发展。目前已探测到超过5500颗系外行星,其中包括类地行星、超级地球、气态巨行星及冰巨行星等多种类型。这些发现极大地拓展了人类对自身周围环境和宇宙的认知,为理解行星形成和演化提供了宝贵的观测依据,也为寻找宜居行星和地外生命提供了重要线索。通过介绍系外行星探测的多种核心技术,包括原理和应用特点,旨在对比和分析不同探测方法的技术特征。通过分析多种探测技术的优势和局限性,为行星探测研究提供了实践参考和发展趋势展望。

高精度电压电流转换电路中电流镜校准技术

电流镜输出误差主要由3个不同失配源造成:漏源电压(V_(DS)),阈值电压(V_(th)),跨导系数(β)。其中,第一项V_(DS)失配通常是由有限输出阻抗引起的确定性误差,该误差可以通过使用级联结构以及增益提升技术避免,后两项V_(th)和β失配是由工艺引起的随机性误差。为解决电流镜因工艺失配现象导致的电压电流(Voltage to Current)转换电路精度、线性度较差的问题,提出了一种动态元件匹配(Dynamic Element Match,DEM)以及修调技术(TRIM)相结合的电流镜校准方法,该方法使用TRIM技术将待校准输出电流镜支路和基准电流镜支路之间的误差电流,通过电容与MOS管转换成校准电流后反馈流入待校准输出电流镜支路完成校准,并通过DEM技术切换多条待校准输出电流镜支路完成校准的同时使输出误差平均化。本文采用SMIC 0.18μm BCD工艺对所提出的V-I转换电路进行了电路设计,仿真结果表明,V-I转换电路的输出电流的失配误差从0.12%下降到了0.03%,有效位数ENOB达到了11.2 bit,总谐波失真THD为−72.6 dB。

基于曲面拟合的光学偏折系统显示屏标定方法

针对透射式光学偏折系统中最关键的标定环节,提出使用曲面拟合方式拟合显示屏幕面形分布。建立基于透射式光学偏折术的波前检测仿真模型,分析两种不同的显示屏面形拟合方法对波前测量的影响。仿真结果显示:平面屏幕模型波前像差均方根误差(RMS)值为0.8375μm,而曲面屏幕模型仿真波前像差RMS值仅为0.0596μm。采用透射式光学偏折系统对球面透镜进行波前测量,曲面屏幕模型中波前像差RMS值为0.1371μm,平面屏幕模型中波前像差RMS值为1.4326μm。实验结果表明:使用曲面拟合效果明显优于平面拟合效果,证明了曲面拟合屏幕模型的可行性。

On the Identification of N-rich Metal-poor Field Stars with Future Chinese Space Station Telescope

During the long term evolution of globular clusters(GCs), some member stars are lost to the field. The recently found nitrogen-rich(N-rich) metal-poor field stars are promising candidates of these GC escapees, since N enhancement is the fingerprint of chemically enhanced populations in GCs. In this work, we discuss the possibility of identifying N-rich metal-poor field stars with the upcoming Chinese Space Station Telescope(CSST). We focus on the main survey camera with NUV, u, g, r, i, z, y filters and slitless spectrograph with a resolution about 200.The combination of UV sensitive equipment and prominent N-related molecular lines in the UV band bodes well for the identification: the color–color diagram of(u-g) versus(g-r) is capable of separating N-rich field stars from normal halo stars, if metallicity can be estimated without using the information on u-band photometry.Besides, the synthetic spectra show that a signal-to-noise ratio of 10 is sufficient to identify N-rich field stars. In the near future, a large sample of N-rich field stars found by CSST, combined with state-of-the-art N-body simulations will be crucial to deciphering GC-Galaxy co-evolution.

The First Ground-based White Light Lunar Polarization Imaging:A New Kind of FeO Observation on the Near Side of the Moon

Lunar optical polarization is a fascinating phenomenon that occurs when sunlight reflects off the surface of the Moon and becomes polarized.This study employs a novel split-focus plane polarimetric camera to conduct the initial white light polarimetric observations on the near side of the Moon.We obtained the linear degree of polarization(DOP)parameters of white light by observation from the eastern and western hemispheres of the Moon.The findings indicate that the white light polarization is lower in the lunar highland than in the lunar maria overall.Combining the analysis of lunar soil samples,we noticed and determined that the DOP parameters of white light demonstrate high consistency with iron oxide on the Moon.This study may serve as a new diagnostic tool for the Moon.

Accelerating Asteroidal Period and Pole Inversion from Multiple Lightcurves Using Parallel Differential Evolution and Cellinoid Shape Model

Determining asteroid properties provides valuable physical insights but inverting them from photometric lightcurves remains computationally intensive.This paper presents a new approach that combines a simplified Cellinoid shape model with the Parallel Differential Evolution(PDE)algorithm to accelerate inversion.The PDE algorithm is more efficient than the Differential Evolution algorithm,achieving an extraordinary speedup of 37.983 with 64 workers on multicore CPUs.The PDE algorithm accurately derives period and pole values from simulated data.The analysis of real asteroid lightcurves validates the method’s reliability:in comparison with results published elsewhere,the PDE algorithm accurately recovers the rotational periods and,given adequate viewing geometries,closely matches the pole orientations.The PDE approach converges to solutions within 20,000 iterations and under one hour,demonstrating its potential for large-scale data analysis.This work provides a promising new tool for unveiling asteroid physical properties by overcoming key computational bottlenecks.

基于超声的标准发动机动态燃速测试技术

以标准发动机的动态燃速测试技术为研究对象,应用超声测厚原理获取固定声速点火条件下的发动机动态燃速、压强数据;分析提出一种基于特征点的动态燃烧信号辨识方法,获取发动机点火过程中推进剂退移厚度与时间变化数据;通过试验的方法建立常温状态不同压强下的声速校准模型,结合测试过程压强数据计算得到发动机点火过程中超声的实时声速,代入前期在固定声速条件下获取的推进剂退移厚度与时间数据中,通过求导获取点火过程中发动机的实时燃速。计算结果表明:基于超声的动态燃速测试方法能够实现整机的动态燃速测试,具有较高的时间分辨精度,其中基于超声的动态燃速测试燃烧时间与传统压强-时间曲线计算得到的燃烧时间误差为0.235%。此外,对比发动机点火后压强-时间与动态燃速-时间曲线发现,发动机建压完成后的动态燃速与压强曲线变化趋势呈一定相似性。

A Study of the Comets with Large Perihelion Distances C/2019 L3(ATLAS)and C/2019 O3(Palomar)

This work analyzes the photometric data of the Oort spike comets C/2019 L3(ATLAS)and C/2019 O3(Palomar)obtained between 2016 and 2023 by the ATLAS network and the Belgian Olmen Observatory.The comets Palomar and ATLAS have a typical and unusually high activity level,respectively,based on the Afρparameter corrected to phase angle zero at perihelion.The absolute magnitude of comets ATLAS and Palomar in the o-band is 4.71±0.05 and 4.16±0.02 respectively.The cometary activity of comets ATLAS and Palomar probably began at r>13 au before perihelion and will end at r>14 au after perihelion,which means that they could remain active until the second half of 2026.The nucleus of comet ATLAS has a minimum radius of 7.9 km,and the nucleus of comet Palomar could be a little larger.The c-o colors of the comets ATLAS and Palomar are redder and bluer,respectively,at perihelion than the solar twin YBP 1194.These comets showed a bluish trend in the coma color with decreasing heliocentric distance.Comet Palomar probably had two outbursts after its perihelion,each releasing about 10^(8)kg of dust.The slopes of the photometric profile of the comae of these comets were between 1and 1.5,indicating a steady state during the observation campaign.

微小液体流量校准技术

微小液体被广泛应用于微反应器中,具有传热传质效率高、高通量、集成化、方便控制等优势,微小液体流量计可以实现对样品的精确控制,但在极低流量下(μL/min乃至nL/min),微小液体流量计存在计量基标准不完善、校准难度大等问题。本文综述了目前在微小液体流量计量领域所采用的几种校准技术,主要包括质量法和体积法,并根据现有的研究给出了这些技术目前所能达到的校准范围和不确定度。分析表明,现有的质量法微小液体流量校准技术在应用于微小液体时仍具有不足,需要进一步研究多种作用机制的影响;体积法微小液体流量校准技术有多种实现方式,虽然目前仍处于探索阶段,但在未来有望成为更具有研究前景的一种方法。最后,结合微小液体流量计量技术的发展和先进测量体系的建设,展望了微小液体流量计量的发展前景。

联合光度立体视觉和图像校正的磨粒三维形貌重建

分析铁谱技术在机械装备磨损状态检测中发挥了重要作用,但其仅能提供磨粒二维图像,导致磨粒形貌信息不足。为实现磨粒三维形貌的精确重建,联合光度立体视觉和图像校正,为精确重建磨粒的三维形貌,联合光度立体视觉和图像。该方法首先采用大津阈值法由全光源图像识别磨粒与背景区域;然后为消除LED发光强度差异对磨粒形貌重建的影响,结合平面形状和朗伯反射模型确定背景区域的理想成像亮度,并校正各光度图像序列的亮度;最后根据光度立体视觉方法,由校正后光度图像序列重建磨粒的三维形貌。以不同类型的磨粒为测试样本,将所提出的方法的重建结果与激光共聚焦显微镜的测量结果进行对比。结果表明:重建磨粒的形貌参数误差小于15%,表明提出的方法能够精确重建磨粒的三维形貌。

便携式非甲烷总烃检测仪校准方法

建立了一种便携式非甲烷总烃检测仪的校准方法。根据便携式非甲烷总烃检测仪的工作原理,提出了示值误差、重复性、漂移等校准项目,示值误差不大于±5%,定量重复性不大于2%,零点漂移不大于±2%,量程漂移不大于±3%。使用标准气体稀释装置将摩尔分数为3.0%的甲烷标准气体稀释至仪器满量程浓度的10%、40%、60%通入仪器,经过数据验证,该校准方法较为可行,可以用于便携式非甲烷总烃检测仪的校准。

机器人参数及标定试验研究

随着智能制造进程的推进,工业机器人因其活动范围大、成本较低和适用于柔性生产等优点开始被应用于加工制造领域中,执行如磨抛、钻孔等任务。在轮毂磨抛加工中,一般需要离线编程技术生成复杂的轮毂磨抛加工路径,这需要机器人拥有较高的绝对定位精度,而现有机器人的绝对定位精度达不到使用需求。为了提高机器人的绝对定位精度,机器人标定是一种常用的手段。文章阐述了标定误差模型的建立,并进行了机器人运动学参数标定试验,验证了标定误差模型的准确性。

基于AB755系列变频器转炉倾动主从控制改造

转炉倾动装置是冶炼过程中的关键设备,冶炼过程中,炉体倾动系统需要进行±360°旋转,旋转过程中由于液态钢水重心随着转炉倾角的变化而变化,同时炉体具有势能负载特性,因此对传动系统有更高的要求。文章基于AB755系列变频器在120t转炉倾动系统上的成功应用,从传动主从控制逻辑、抱闸控制逻辑、三用一备冗余控制方案、调试重点难点进行详细介绍。

Method for array gain and phase uncertainties calibration based on ISM and ESPRIT

A new method for array calibration of array gain and phase uncertainties, which severely degrade the performance of spatial spectrum estimation, is presented. The method is based on the idea of the instrumental sensors method （ISM）, two well-calibrated sensors are added into the original array. By applying the principle of estimation of signal parameters via rotational invariance techniques （ESPRIT）, the direction-of-arrivals （DOAs） and uncertainties can be estimated simultaneously through eigen-decomposition. Compared with the conventional ones, this new method has less computational complexity while has higher estimation precision, what＇s more, it can overcome the problem of ambiguity. Both theoretical analysis and computer simulations show the effectiveness of the proposed method.

Flux Calibration of the BATC Survey and Its Application for Checking the Consistency of the Oke-Gunn Standards

Four Oke-Gunn (OG) standards, HD 19445, HD 84937, BD+26 2606 and BD+17 4708 are used as standard stars for flux calibration in the BATC project. They are also widely used in the visual wavelength region in many other photometric projects. Over the years we have observed on 58 good photometric nights, and the data obtained are used for flux calibration. Normally two or three OG standards are observed in every photometric night. The data are used for getting the atmospheric extinction coefficients and instrumental magnitude zero point. We also use these data to make inter-comparisons among the magnitudes of these standard stars. As a result, we found the magnitudes of HD 19445, HD 84937 and BD+17 4708 to agree well with those estimated in previous work to within 0.03 magnitude. However, BD+26 2606 shows a larger deviation especially at short wavebands. Possible reasons are analyzed and the revised magnitudes are obtained for these standards. It is shown that the quality of flux calibration of the BATC fields is significantly approved by applying the new magnitudes.

Photometric investigation on the W-subtype contact binary V1197 Her

Multi-color light curves of V1197 Her were obtained with the 2.4 meter optical telescope at the Thai National Observatory and the Wilson-Devinney(W-D)program was used to model the observational light curves.The photometric solutions reveal that V1197 Her is a W-subtype shallow contact binary system with a mass ratio of q=2.61 and a fill-out factor of f=15.7%.The temperature difference between the primary star and secondary star is only 140 K in spite of the low degree of contact,which means that V1197 Her is not only in geometrical contact configuration but is also already under thermal contact status.The orbital inclination of V1197 Her is as high as i=82.7?,and the primary star is completely eclipsed at the primary minimum.The totally eclipsing characteristic implies that the determined physical parameters are highly reliable.The masses,radii and luminosities of the primary star(star 1)and secondary star(star2)are estimated to be M1=0.30(1)M⊙,M2=0.77(2)M⊙,R1=0.54(1)R⊙,R2=0.83(1)R⊙,L1=0.18(1)L⊙and L2=0.38(1)L⊙.The evolutionary statuses of the two component stars are drawn in the Hertzsprung-Russell diagram,showing that the less massive but hotter primary star is more evolved than the secondary star.The period of V1197 Her is decreasing continuously at a rate of d P/dt=-2.58×10^-7 day·year^-1,which can be explained by mass transfer from the more massive star to the less massive one at a rate of dM2/dt=-1.61×10^-7 M⊙year^-1.The light curves of V1197 Her are reported to show the O’Connell effect.Thus,a cool spot is added to the more massive star to model the asymmetry in the light curves.