A four lens camera design

A camera design with only four lens elements gives good imaging performance at a working focal ratio of f/4.4.     

Laue diffraction lenses for astrophysics: Theoretical concepts

Beyond the present technologies, Laue diffraction lenses are very promising tools in the field of gamma-ray astrophysics. The theoretical concepts of this kind of instruments are based on the Laue diffraction in crystals, discovered almost 100 years ago. Though they are commonly used in crystallography, their application to γ-ray focusing in astrophysics requires some specific developments, e.g. in terms of energy and imaging responses. The present article describes the physics of X-ray diffraction in crystals. In the context of the Darwin model of mosaic crystals, some peculiar aspects, relevant to the astrophysical observation, are discussed. The evaluation and optimization of diffraction efficiency are discussed, especially with rigards to the crystal’s mosaicity and thickness, its spatial extent and deviations to the “ideally imperfect” Darwin model. PACS 95.55.Ka, 61.50.Ah, 61.10.−i, 41.50.+h     

中国铂族元素矿床类型和地质特征

根据成矿地质环境、容矿岩石类型、元素共生组合、矿床地质特征和成矿作用性质，将我国的铂族元素矿床划分为岩浆型、热液弄才外生型三大类型和九个亚类，而赋存于基性超基性岩体中的铜镍型铂族元素矿床是我国最重要的铂族元素矿床。     

球面散射屏远场散斑的若干统计特征

本文采用标量衍射理论导出球面屏衍射的瑞利-索末菲公式及其远场近似。并据此导出球面散射屏远场散斑的若干统计特征。     

On the existence of transverse relativistic aberrations in moving mirror

Relativistic aberration and Doppler effects on rotating mirrors have been claimed (Ragazzoni & Claudi, 1995) and later refuted (Hickson, Bhatia & Iovino, 1995). While an experimental confirmation of the absence of the Doppler effect has been carried out in 1974, a measurement of the absence of the aberration effect is missing. It is shown that analyzing published data on the LAGEOS pulse-return signature an experimental confirmation of the absence of the effect is obtained.     

中国大气环境光学探测研究

激光/波谱技术促进了大气立体监测技术的发展,以光学探测和光谱数据解析为核心、以紫外、可见到红外全光谱为探测波段的各种高分辨率光学监技术,在中国逐渐实现了从近地面到100 km大气气象要素和大气痕量成分实时探测的能力,以及近地面到50 km大气多要素的实验模拟能力。光学技术以高灵敏度、高分辨率、高选择性、多组分以及实时等优势,在大气环境领域日益发挥作用,为研究大气污染演变与气象过程相互作用、大气细粒子污染和光化学烟雾形成机理等基础科学问题研究提供数据支持,为揭示城市和区域尺度的大气复合污染特征、量化其环境影响,提供科技支撑。     

Palomar and Table Mountain observations of 9P/Tempel 1 during the Deep Impact encounter: First results

We present the first results of the Palomar Adaptive Optics observations taken during the Deep Impact encounter with 9P/Tempel 1 in July 2005. We have combined the Palomar near-IR imaging data with our visual wavelength images obtained simultaneously at JPL's Table Mountain Observatory to cover the total wavelength range from 0.4 to 2.3 μm in the B, V, R, I, J, H, and K filter bands, spanning the dates from 2005 July 03-07. We also include in our overall analysis images taken on the pre-encounter dates of June 1 and June 15, 2005. The broad wavelength range of our observations, along with high temporal resolution, near-IR sensitivity, and spatial resolution of our imaging, have enabled us to place constraints on the temperature of the impact flash and incandescent plume of >700 K, and to provide mean dust velocities of order approximately 1.25 h after impact derived from our 1.64 μm observations. Our ejected dust mass estimates, as derived from our near-IR observations, are an order of magnitude less than those previously reported for visual wavelength observations.     

SWIFT: An adaptive optics assisted I/z band integral field spectrograph

SWIFT is an adaptive optics assisted integral field spectrograph covering the I and z astronomical bands (0.7–1.0 μm) at a spectral resolving power R  5000. At its heart is an all-glass image slicer with high throughput based on a novel de-magnifying design allowing a compact instrument. SWIFT profits from two recent developments: (i) the improved ability of second generation adaptive optics systems to correct for atmospheric turbulence in SWIFTS’s bandpass, and (ii) the availability of CCD array detectors with high quantum efficiency at very red wavelengths. It is a dedicated integral field spectrograph, specifically built to address a range of interesting astrophysical questions.     

NAOMI/OASIS on-sky performance

NAOMI is the AO system of the 4.2-m William Herschel Telescope on La Palma. It delivers an AO-corrected image to a lenslet array at the focal plane of the optical integral-field spectrograph OASIS. The resulting 1100 spectra are imaged onto a high-QE, low-fringing MITLL3 CCD. A range of spectroscopic and spatial (0.09–0.42 arcsec/lenslet) configurations is available. At wavelength  0.7 μm, the NAOMI-corrected FWHM is typically half that of the natural seeing. Scheduled OASIS observing began in semester 2004B, with 9 programmes awarded a total of 26 nights during the first year of operation. A Rayleigh laser guide star is under development, with first light expected summer 2006. In conjunction with NAOMI/OASIS, this will provide a unique facility: AO-corrected optical integral-field spectroscopy anywhere on the northern sky.