CCD图像图像处理外文翻译@中英文翻译@外文文献翻译

附录 附录 1 翻译部分 Raw CCD images are exceptional but not perfect. Due to the digital nature of the data many of the imperfections can be compensated for or calibrated out of the final image through digital image processing. Composition of a Raw CCD Image. A raw CCD image consists of the following signal components: IMAGE SIGNAL - The signal from the source.Electrons are generated from the actual source photons. BIAS SIGNAL - Initial signal already on the CCD before the exposure is taken. This signal is due to biasing the CCD offset slightly above zero A/D counts (ADU). THERMAL SIGNAL - Signal (Dark Current thermal electrons) due to the thermal activity of the semiconductor. Thermal signal is reduced by cooling of the CCD to low temperature. Sources of Noise CCD images are susceptible to the following sources of noise: PHOTON NOISE - Random fluctuations in the photon signal of the source. The rate at which photons are received is not constant. THERMAL NOISE - Statistical fluctuations in the generation of Thermal signal. The rate at which electrons are produced in the semiconductor substrate due to thermal effects is not constant. READOUT NOISE - Errors in reading the signal； generally dominated by the on-chip amplifier. QUANTIZATION NOISE - Errors introduced in the A/D conversion process. SENSITIVITY VARIATION - Sensitivity variations from photosite to photosite on the CCD detector or across the detector. Modern CCDs are uniform to better than 1% between neighboring photosites and uniform to better than 10% across the entire surface. Noise Corrections REDUCING NOISE - Readout Noise and Quantization Noise are limited by the construction of the CCD camera and can not be improved upon by the user. Thermal Noise, however, can be reduced by cooling of the CCD (temperature regulation). The Sensitivity Variations can be removed by proper flat fielding. CORRECTING FOR THE BIAS AND THERMAL SIGNALS - The Bias and Thermal signals can be subtracted out from the Raw Image by taking what is called a Dark Exposure. The dark exposure is a measure of the Bias Signal and Thermal Signal and may simply be subtracted from the Raw Image. FLAT FIELDING -A record of the photosite to photosite sensitivity variations can be obtained by taking an exposure of a uniformly lit flat field. These variations can then be divided out of the Raw Image to produce an image essentially free from this source of error. Any length exposure will do, but ideally one which saturates the pixels to the 50% or 75% level is best. The Final Processed Image The final Processed Image which removes unwanted signals and reduces noise as best we can is computed as follows: Final Processed Image = (Raw - Dark)/Flat All of the digital image processing functions described above can be accomplished by using CCDOPS software furnished with each SBIG imaging camera. The steps to accomplish them are described in the Operating Manual furnished with each SBIG imaging camera. At SBIG we offer our technical support to help you with questions on how to improve your images. HOW TO SELECT THE CORRECT CCD IMAGING CAMERA FOR YOUR TELESCOPE When new customers contact SBIG we discuss their imaging camera application. We try to get an idea of their interests. We have found this method is an effective way of insuring that our customers get the right imaging camera for their purposes. Some of the questions we ask are as follows: What type of telescope do you presently own? Having this information allows us to match the CCD imaging Cameras parameters, pixel size and field of view to your telescope. We can also help you interface the CCD imaging cameras automatic guiding functions to your telescope. Are you a MAC or PC user? Since our software supports both of these platforms we can insure that you receive the correct software. We can also answer questions about any unique functions in one or the other. We can send you a demonstration copy of the appropriate software for your review. Do you have a telescope drive base with an autoguider port? Do you want to operate from a remote computer? Companies like Software Bisque fully support our products with telescope control and imaging camera software. Do you want to take photographic quality images of deep space objects, image planets, or perform wide field searches for near earth asteroids or supernovas? In learning about your interests we can better guide you to the optimum CCD pixel size and imaging area for the application. Do you want to make photometric measurements of variable stars or determine precise asteroid positions? From this information we can recommend a CCD imaging camera model and explain how to use the specific analysis functions to perform these tasks. We can help you characterize your imaging camera by furnishing additional technical data. Do you want to automatically guide long uninterrupted astrophotographs? As the company with the most experience in CCD autoguiding we can help you install and operate a CCD autoguider on your telescope. The Model STV has a worldwide reputation for accurate guiding on dim guide stars. No matter what type of telescope you own we can help you correctly interface it and get it working properly. SBIG CCD IMAGING CAMERAS The SBIG product line consists of a series of thermoelectrically cooled CCD imaging cameras designed for a wide range of applications ranging from astronomy, tricolor imaging, color photometry, spectroscopy, medical imaging, densitometry, to chemiluminescence and epifluorescence imaging, etc. This catalog includes information on astronomical imaging cameras, scientific imaging cameras, autoguiding, and accessories. We have tried to arrange the catalog so that it is easy to compare products by specifications and performance. The tables in the product section compare some of the basic characteristics on each CCD imaging camera in our product line. You will find a more detailed set of specifications with each individual imaging camera description. HOW TO GET STARTED USING YOUR CCD IMAGING CAMERA It all starts with the software. If theres any company well known for its outstanding imaging camera software its SBIG. Our CCDOPS Operating Software is well known for its user oriented camera control features and stability. CCDOPS is available for free download from our web site along with sample images that you can display and analyze using the image processing and analysis functions of the CCDOPS software. You can become thoroughly familiar with how our imaging cameras work and the capabilities of the software before you purchase an imaging camera. We also include CCDSoftV5 and TheSky from Software Bisque with most of our cameras at no additional charge. Macintosh users receive a free copy of EquinoX planetarium and camera control software for the MacOS-X operating system. No other manufacturer offers better software than you get with SBIG cameras. New customers receiving their CCD imaging camera should first read the installation section in their CCDOPS Operating Manual. Once you have read that section you should have no difficulty installing CCDOPS software on your hard drive, connecting the USB cable from the imaging camera to your computer, initiating the imaging camera and within minutes start taking your first CCD images. Many of our customers are amazed at how easy it is to start taking images. Additional information can be found by reading the image processing sections of the CCDOPS and CCDSoftV5 Manuals. This information allows you to progress to more advanced features such as automatic dark frame subtraction of images, focusing the imaging camera, viewing, analyzing and processing the images on the monitor, co-adding images, taking automatic sequences of images, photometric and astrometric measurements, etc. A PERSONAL TOUCH FROM SBIG At SBIG we have had much success with a program in which we continually review customers images sent to us on disk or via e-mail. We can often determine the cause of a problem from actual images sent in by a user. We review the images and contact each customer personally. Images displaying poor telescope tracking, improper imaging camera focus, oversaturated images, etc., are typical initial problems. We will help you quickly learn how to improve your images. You can be assured of personal technical support when you need it. The customer support program has furnished SBIG with a large collection of remarkable images. Many customers have had their images published in SBIG catalogs, ads, and various astronomy magazines. We welcome the chance to review your images and hope you will take advantage of our trained staff to help you improve your images. TRACK AND ACCUMULATE (U.S. Patent # 5,365,269) Using an innovative engineering approach SBIG developed an imaging camera function called Track & Accumulate (TRACCUM) in which multiple images are automatically registered to create a single long exposure. Since the long exposure consists of short images the total combined exposure significantly improves resolution by reducing the cumulative telescope periodic error. In the TRACCUM mode each image is shifted to correct guiding errors and added to the image buffer. In this mode the telescope does not need to be adjusted. The great sensitivity of the CCD virtually guarantees that there will be a usable guide star within the field of view. This feature provides dramatic improvement in resolution by reducing the effect of periodic error and allowing unattended hour long exposures. SBIG has been granted U.S. Patent # 5,365,269 for Track & Accumulate. DUAL CCD SELF-GUIDING (U.S. Patent # 5,525,793) In 1994 with the introduction of Models ST-7 and ST-8 CCD Imaging Cameras which incorporate two separate CCD detectors, SBIG was able to accomplish the goal of introducing a truly self-guided CCD imaging camera. The ability to select guide stars with a separate CCD through the full telescope aperture is equivalent to having a thermoelectrically cooled CCD autoguider in your imaging camera. This feature has been expanded to all dual sensor ST series cameras (ST-7/8/9/10/2000) and all STL series cameras (STL-1001/1301/4020/6303/11000). One CCD is used for guiding and the other for collecting the image. They are mounted in close proximity, both focused at the same plane, allowing the imaging CCD to integrate while the PC uses the guiding CCD to correct the telescope. Using a separate CCD for guiding allows 100% of the primary CCDs active area to be used to collect the image. The telescope correction rate and limiting guide star magnitude can be independently selected. Tests at SBIG indicated that 95% of the time a star bright enough for guiding will be found on a TC237 tracking CCD without moving the telescope, using an f/6.3 telescope. The self-guiding function quickly established itself as the easiest and most accurate method for guiding CCD images. Placing both detectors in close proximity at the same focal plane insures the best possible guiding. Many of the long integrated exposures now being published are taken with this self-guiding method, producing very high resolution images of deep space objects. SBIG has been granted U.S. Patent # 5,525,793 for the dual CCD Self-Guiding function. COMPUTER PLATFORMS SBIG has been unique in its support of both PC and Macintosh platforms for our cameras. The imaging cameras in this catalog communicate with the host computer through standard serial or USB ports depending on the specific models. Since there are no external plug-in boards required with our imaging camera systems we encourage users to operate with the new family of high resolution graphics laptop computers. We furnish Operating Software for you to install on your host computer. Once the software is installed and communication with the imaging camera is set up complete control of all of the imaging camera functions is through the host computer keyboard. The recommended minimum requirements for memory and video graphics are as shown below. GENERAL CONCLUSION (1) of this item from the theoretical analysis of the use of CCD technology for real-time non-contact measuring the diameter of the feasibility of measuring it is fast, efficient, accurate, high degree of automation, off-production time and so on. (2) projects to test the use of CCD technology to achieve real-time, online non-contact measurement, developed by the CCD-line non-contact diameter measurement system has a significant technology advanced and practical application of significance. (3) from the theoretical and experimental project on the summary of the utilization of CCD technology developed by SCM PV systems improve the measurement accuracy of several ways: improving crystal, a multi-pixel CCD devices and take full advantage of CCD-like device Face width. 译文 原料 CCD 图像是例外，但并非十全十美。由于数字数据的性质有很多不完善，可以得到补偿或校准出最后的形象，通过数字图像处理。 组成原料 CCD 图像。 原料 CCD 图像组成，以下信号组成部分： 图像信号 -信号从 s ource.electrons产生实际的光子源。 偏置信号 -初步信号已经在防治荒漠化公约前曝光是所采取的。这个信号是由于偏置防治荒漠化公约抵销略高于零的 A / D 计数（ adu ） 。 热信号 -信号（暗电流的热电子）由于热活性半导体。热信号是减少冷却防治荒漠化公约低温。来源噪音 CCD 图像很容易受到以下来源的噪音： 光子噪声 -随机波动，在光子的信号源。率在哪个光子收到的是不是常数。 热噪声 -统计的波动产生的热信号。率，其中电子产品在半导体基板由于热效应是不是常数。 读出噪声 -在读的错误信号 ；普遍占主导地位由芯片内建的放大器。 量化噪声 -错误介绍了在 A / D 转换过程。 敏感性的变化 -敏感性的变化，从 p hotosite，以 p hotosite 对 C CD 探测器或整个探测器。现代的 CCD 是统一，以更好地超过 1 的邻国间 photosites和统一，以更好地超过 10 ，横跨整个表面。 噪音更正减少噪音 -读出噪声和量化噪声是有限的，由建设的 C CD 相机，并不能改善后，由用户。热噪声，但是，可以减少冷却防治荒漠化公约（温度调节） 。敏感性的变化可以删除适当的平场。 纠正偏见和热的信号 -偏见和热信号可以减去从 R AW 图像，采取什么是所谓的一个黑暗的暴露。黑暗曝光，是衡量偏差信号和热信号和可能只是减去 RAW图像。 平场 -的纪录，该 photosite ，以 photosite 敏感性的 变化可以得到以一曝光，均匀点燃了 平场“ 。这些变化便可以划分出 RAW 图像，以产生一个形象，基本上是免费的从这个误差来源。任何长度的接触将尽，但理想的其中饱和像素到50 或 75 的水平是最好的。 最后处理的图像最后处理的形象，删除无用信号，并降低噪音，最好的，我们可以计算如下： 最后处理的图像 = （原料 -黑暗） /单位所有的数字图像处理功能上文所述，可以通过使用 ccdops 软件家具与每个 sbig 成像相机。步骤来完成他们所描述的操作手册家具与每个 sbig 成像相机。在 sbig 我们提供我们的技术支持，以帮助 您的问题，就如何改善你的图像。 如何选择正确的 CCD 成像相机为您的望远镜 当新客户的联系 sbig 我们讨论他们的成像相机应用。我们争取的构想他们的利益。我们发现，这种方法是一种有效方式，投保我们的客户得到正确的影像相机为他们的目的。的一些问题，我们要求分列如下： 什么类型的望远镜，你目前自己的呢？有这方面的资料，让我们以配合 CCD成像相机的参数，像素大小和领域，以便您的望远镜。我们还可以帮助您界面CCD 成像照相机的自动导向功能到您的望远镜。 你是 Mac 或 PC 使用者？由于我们的软件支持这两种平 台，我们可以保证您收到正确的软件。我们也可以回答有关任何独特功能，在一个或另一个。我们可以寄给您一个示范的副本，适当的软件，供您检阅。 你是否有望远镜的驱动器基地，你想不想经营从远程计算机呢？公司一样，软件 bisque 全力支持我们的产品与望远镜控制和成像相机软件。 你想不想采取摄影图像质量的深空物体，行星的图像，或执行广泛的领域搜寻近地小行星或 supernovas ？在学习关于您的利益，我们可以更好地引导您以最佳的 CCD 像素大小和成像等领域的应用。 你想不想使光度测量变星或确定精确的 小行星的职位？从这个信息我们可以向您推荐 CCD 成像相机型号，并解释如何使用具体分析的职能，以执行这些任务。我们可以帮助你的特点你的影像相机通过提供额外的技术数据。 你想不想自动引导长期不间断的作为该公司最的经验，防治荒漠化公约autoguiding 我们可以帮助你安装和运行了 CCD autoguider 对您的望远镜。该模型基金会已享誉全球，为正确的指导就黯淡引导星。不管什么类型的望远镜，你自己的，我们可以帮助您正确的接口，它并获得它工作正常。 sbig CCD 成像相机 该 sbig 产品线构成了一系 列的 thermoelectrically 冷却 CCD 成像相机设计的范围广泛的应用，包括从天文，三色成像，彩色测光，光谱学，医学成像，密度，化学发光和 epifluorescence 影像等，这包括信息目录对天文的影像照相机，科学成像相机， autoguiding ，及配件。我们曾尝试安排目录，使我们很容易比较产品的技术规格和性能。表中，在产品第比较的一些基本特征，在每个 CCD成像相机在我们的产品线。您会看到一个更详细的设置规格与每一个人影像相机描述。 如何开始使用您的 CCD 成像相机 这一切开始与该软件。如果有任 何公司，以及闻名，其优秀的成像相机软件，它的 sbig 。我们 ccdops 操作软件，是人所共知的，为它的用户导向的相机控制功能和稳定性。 ccdops 是提供免费下载从我们的网站，随着样本图像，您可以显示和分析，利用图像处理和分析的职能，该 ccdops 软件。你就可以成为彻底熟悉如何，我们的影像照相机的工作和能力的软件之前，请先购买一成像相机。我们还包括 ccdsoftv5和 thesky从软件 bisque与我们大部分的摄影机不得收取任何附加费用。 Maci