1. Astronomical photometry at wavelengths of 8.5, 10.5, and 11.6 µm. 2. Infrared emission from asteroids at wavelengths of 8.5, 10.5, and 11.6 µm

The purpose of this thesis is to present new observations of thermal-infrared radiation from asteroids. Stellar photometry was performed to provide standards for comparison with the asteroid data. The details of the photometry and the data reduction are discussed in Part 1. A system of standard stars is derived for wavelengths of 8.5, 10.5 and 11.6 µm and a new calibration is adopted. Sources of error are evaluated and comparisons are made with the data of other observers.

The observations and analysis of the thermal-emission observations of asteroids are presented in Part 2. Thermal-emission lightcurve and phase effect data are considered. Special color diagrams are introduced to display the observational data. These diagrams are free of any model-dependent assumptions and show that asteroids differ in their surface properties.

On the basis of photometric models, (4) Vesta is thought to have a bolometric Bond albedo of about 0.1, an emissivity greater than 0.7 and a true radius that is close to the model value of 300^(+50)_(-30)km. Model albedos and model radii are given for asteroids 1, 2, 4, 5, 6, 7, 15, 19, 20, 27, 39, 44, 68, 80, 324 and 674. The asteroid (324) Bamberga is extremely dark with a model (~bolometric Bond) albedo in the 0.01 - 0.02 range, which is thought to be the lowest albedo yet measured for any solar-system body. The crucial question about such low-albedo asteroids is their number and the distribution of their orbits.

Understanding planet formation through high precision photometry and spectroscopy

From studies of protoplanetary disks to extrasolar planets and planetary debris, we aim to understand the full evolution of a planetary system. Observational constraints from ground- and space-based instrumentation allows us to measure the properties of objects near and far and are central to developing this understanding. We present here three observational campaigns that, when combined with theoretical models, reveal characteristics of different stages and remnants of planet formation. The Kuiper Belt provides evidence of chemical and dynamical activity that reveals clues to its primordial environment and subsequent evolution. Large samples of this population can only be assembled at optical wavelengths, with thermal measurements at infrared and sub-mm wavelengths currently available for only the largest and closest bodies. We measure the size and shape of one particular object precisely here, in hopes of better understanding its unique dynamical history and layered composition.

Molecular organic chemistry is one of the most fundamental and widespread facets of the universe, and plays a key role in planet formation. A host of carbon-containing molecules vibrationally emit in the near-infrared when excited by warm gas, T~1000 K. The NIRSPEC instrument at the W.M. Keck Observatory is uniquely configured to study large ranges of this wavelength region at high spectral resolution. Using this facility we present studies of warm CO gas in protoplanetary disks, with a new code for precise excitation modeling. A parameterized suite of models demonstrates the abilities of the code and matches observational constraints such as line strength and shape. We use the models to probe various disk parameters as well, which are easily extensible to others with known disk emission spectra such as water, carbon dioxide, acetylene, and hydrogen cyanide.

Lastly, the existence of molecules in extrasolar planets can also be studied with NIRSPEC and reveals a great deal about the evolution of the protoplanetary gas. The species we observe in protoplanetary disks are also often present in exoplanet atmospheres, and are abundant in Earth's atmosphere as well. Thus, a sophisticated telluric removal code is necessary to analyze these high dynamic range, high-resolution spectra. We present observations of a hot Jupiter, revealing water in its atmosphere and demonstrating a new technique for exoplanet mass determination and atmospheric characterization. We will also be applying this atmospheric removal code to the aforementioned disk observations, to improve our data analysis and probe less abundant species. Guiding models using observations is the only way to develop an accurate understanding of the timescales and processes involved. The futures of the modeling and of the observations are bright, and the end goal of realizing a unified model of planet formation will require both theory and data, from a diverse collection of sources.

CCD扫描检测光束准直度

提出一种检测光束准直度的新方法。在对波面矢高进行定义的基础上，提出CCD轴向扫描检测激光束准直度的方法。利用采样光波在会聚透镜后形成的衍射图样，测量两个相同基准衍射图样之间的距离，即可确定入射光波的波面矢高，进而确定入射光波的准直度。在给出测量原理及模拟基准衍射图样的基础上．进行了实验验证。CCD轴向扫描方法具有结构简单、加工便利、操作方便的特点，是检测光束准直度的有效方法。

基于低速面阵CCD的正弦相位调制干涉测量

正弦相位调制(SPM)干涉测量技术用于表面形貌测量时, 需要帧速高于300 frame/s的图像传感器, 同时要求调制信号频率与图像传感器帧速成确定的整数倍关系。提出一种基于低速CCD(30 frame/s)的帧速可调的高速图像传感技术, 通过控制每帧像素总数提高CCD帧速, 研制出一种高帧速图像传感器, 帧速可达300～1600 frame/s, 且每帧大小连续可调。将该CCD传感器用于正弦相位调制干涉泰曼-格林干涉仪, 测量镀膜玻璃板表面形貌, 当CCD图像传感器的帧速与调制信号频率呈16, 8, 4

A high-speed image sensing technique with adjustable frame rate based on an ordinary CCD

In the sinusoidal phase modulating interferometer technique, the high-speed CCD is necessary to detect the interference signals. The reason of ordinary CCD's low frame rate was analyzed, and a novel high-speed image sensing technique with adjustable frame rate based on ail ordinary CCD was proposed. And the principle of the image sensor was analyzed. When the maximum frequency and channel bandwidth were constant, a custom high-speed sensor was designed by using the ordinary CCD under the control of the special driving circuit. The frame rate of the ordinary CCD has been enhanced by controlling the number of pixels of every frame; therefore, the ordinary of CCD can be used as the high frame rate image sensor with small amount of pixels. The multi-output high-speed image sensor has the deficiencies of low accuracy, and high cost, while the high-speed image senor with small number of pixels by using this technique can overcome theses faults. The light intensity varying with time was measured by using the image sensor. The frame rate was LIP to 1600 frame per second (f/s), and the size of every frame and the frame rate were adjustable. The correlation coefficient between the measurement result and the standard values were higher than 0.98026, and the relative error was lower than 0.53%. The experimental results show that this sensor is fit to the measurements of sinusoidal phase modulating interferometer technique. (c) 2007 Elsevier GmbH. All rights reserved.

空间CCD凝视成像跟踪系统的作用距离分析

在充分考虑了空间背景光辐射特性以及漫反射目标对相干光和自然光的不同反射特性的基础上,利用信号检测的统计学方法,导出了空间电荷耦合器件(CCD)凝视成像跟踪系统分别在激光照明主动跟踪模式和太阳光照明被动跟踪模式下的作用距离表达式。结果表明,空间CCD凝视成像跟踪系统在脉冲能量为1mJ的激光照明主动跟踪模式下可对1m2空间漫反射目标实现10km量级范围内的跟踪;而利用太阳光照明的被动跟踪模式下的跟踪距离可达几百千米。

基于一维CCD的免疫层析试纸条检测系统

本文报道的基于一维CCD的免疫层析试纸条检测系统是一种以上转换磷光材料（UCP）作为标记物的生物传感器。该系统通过检测生物反应后试纸条上UCP颗粒的含量，计算出被测样品中特定生物分子的浓度，可以实现对多种病原体的快速定性与定量检测。本检测系统对0—60ns／ml系列标准样品的检测结果具有很好的线性响应特性，且与扫描型检测系统的检测结果十分接近。

带AGC的CCD成像系统研究

Submitted by zhangdi (zhangdi@red.semi.ac.cn) on 2009-04-13T11:45:31Z