基于微扫描镜的激光投影

利用微机械加工技术制造出一种新型微扫描镜,结合半导体激光器,可用于投影显示.激光器发出的光束被两个分别沿着X轴、Y轴扭转的镜面相继反射,扫描出二维图形.实验测得扫描镜在15 V电压,频率为扫描镜谐振频率2倍的方波信号驱动下,镜子的光学扫描角度达±12°.由于每个镜子都沿各自轴以简谐规律扭转,扫描所得投影为李萨如图形.通过分析图形的形成原理并用Matlab仿真,选出了适用用于任意图案显示的扫描镜谐振频率组合(X轴2 400 Hz, Y轴2 425 Hz).该组合可以形成194×192个像素点,刷新频率为25 Hz.在此基础上提出了一种通过调制激光开关来进行投影显示的方法.     

Search for a stochastic background of 100-MHz gravitational waves with laser interferometers

This Letter reports the results of a search for a stochastic background of gravitational waves (GW) at 100 MHz by laser interferometry. We have developed a GW detector, which is a pair of 75-cm baseline synchronous recycling (resonant recycling) interferometers. Each interferometer has a strain sensitivity of approximately 10;{-16} Hz;{-1/2} at 100 MHz. By cross-correlating the outputs of the two interferometers within 1000 seconds, we found h{100};{2}Omega_{gw}<6 x 10;{25} to be an upper limit on the energy density spectrum of the GW background in a 2-kHz bandwidth around 100 MHz, where a flat spectrum is assumed.     

Displacement-noise-free gravitational-wave detection with a single Fabry-Perot cavity: A toy model

We propose a detuned Fabry-Perot cavity, pumped through both the mirrors, as a toy model of the gravitational-wave (GW) detector partially free from displacement noise of the test masses. It is demonstrated that the noise of cavity mirrors can be eliminated, but the one of lasers and detectors cannot. The isolation of the GW signal from displacement noise of the mirrors is achieved in a proper linear combination of the cavity output signals. The construction of such a linear combination is possible due to the difference between the reflected and transmitted output signals of detuned cavity. We demonstrate that in low-frequency region the obtained displacement-noise-free response signal is much stronger than the -limited sensitivity of displacement-noise-free interferometers recently proposed by S. Kawamura and Y. Chen. However, the loss of the resonant gain in the noise cancelation procedure results is the sensitivity limitation of our toy model by displacement noise of lasers and detectors.     

The effects of heating on mechanical loss in tantala/silica optical coatings

Second-generation interferometric gravitational-wave detectors will operate at temperatures noticeably above room temperature. Study was done to determine what effect elevated temperatures would have on the Q and coating thermal noise of the detector mirrors. Results show that increased temperature increases loss angle in a manner that is more significant at higher frequencies. Trends show that the increased temperature will have a negligible effect at the low (100 Hz) frequencies important to second-generation detectors.     

Displacement-noise-free gravitational-wave detection with two Fabry-Perot cavities

We propose two detuned Fabry-Perot cavities, each pumped through both the mirrors, positioned in line as a toy model of the gravitational-wave (GW) detector free from displacement noise of the test masses. It is demonstrated that the noise of cavity mirrors can be completely excluded in a proper linear combination of the cavities output signals. This model is illustrated by a simplified round trip model (without Fabry-Perot cavities). We show that in low-frequency region the obtained displacement-noise-free response signal is stronger than the one of the interferometer recently proposed by S. Kawamura and Y. Chen.     

Upper limits on gravitational-wave emission in association with the 27 Dec 2004 giant flare of SGR1806-20

At the time when the giant flare of SGR1806-20 occurred, the AURIGA "bar" gravitational-wave (GW) detector was on the air with a noise performance close to stationary Gaussian. This allows us to set relevant upper limits, at a number of frequencies in the vicinities of 900 Hz, on the amplitude of the damped GW wave trains, which, according to current models, could have been emitted, due to the excitation of normal modes of the star associated with the peak in x-ray luminosity.     

Generation of a stable low-frequency squeezed vacuum field with periodically poled KTiOPO4 at 1064 nm

We report the generation of a stable continuous-wave low-frequency squeezed vacuum field with a squeezing level of 7.4+/-0.1 dB at 1064 nm, the wavelength at which laser-interferometric gravitational wave (GW) detectors operate, using periodically poled KTiOPO4 (PPKTP) in a subthreshold optical parametric oscillator. The squeezing was observed in a broad band of frequencies above 700 Hz where the sensitivity of the currently operational GW detectors is limited by shot noise. PPKTP has the advantages of higher nonlinearity, smaller pump-induced seed absorption, and wider temperature tuning range than alternative nonlinear materials such as MgO-doped or periodically poled LiNbO3, and is, therefore, an excellent material for generation of squeezed vacuum fields for application to laser interferometers for GW detection.     

紧凑重频PFN-Marx脉冲发生器

研制了一台紧凑重频脉冲形成网络(PFN)-Marx脉冲发生器,由PFN-Marx发生器、脉冲充电单元、重频触发单元等组成。PFN-Marx发生器模块采用全电感隔离,直径为480 mm,长度为700 mm。脉冲充电单元采用中储电容加脉冲变压器方法,单次充电可以满足10次输出。重频触发单元采用变压器和磁开关一体化设计的全固态Marx发生器技术,输出电压大于50 kV,前沿小于100 ns。脉冲发生器早期输出电参数为单次10 GW,脉冲宽度100 ns,前沿10 ns,阻抗40 。重频工作时输出功率7 GW,频率5 Hz。后期调整后电参数更改为单次10 GW,脉冲宽度70 ns,前沿10 ns,阻抗50 。重复频率工作时稳定输出功率8 GW,频率10 Hz,单串10个脉冲。初步的应用研究中,利用改进后的平台,在5 GW条件下驱动磁控管获得了S波段约1 GW的微波输出。     

Multiwall carbon nanotube absorber on a thin-film lithium niobate pyroelectric detector

Multiwall carbon nanotubes (MWNTs) were applied in a bulk layer to a pyroelectric film to increase the detector sensitivity nearly fourfold without a substantial penalty to the low-frequency response (4-100 Hz). In addition, the spectral sensitivity over the wavelength range from 600 to 1800 nm was uniformly enhanced, with variations less than 1%. The results demonstrate the suitability of MWNTs as an efficient thermal absorber having low thermal mass.     

An experimental demonstration of resonant sideband extraction for laser-interferometric gravitational wave detectors

Resonant sideband extraction is a new optical configuration for laser-interferometric gravitational wave detectors with Fabry-Perot cavities in the arms. It reduces the thermal load on the beam splitter and the coupling mirrors of the cavities and also allows one to adapt the frequency response of the detector to a variety of requirements. We report the first experimental demonstration using a table-top setup at a detuned operating point. An increase of sensitivity by 6 dB was observed for artificial signals at frequencies above the arm cavity bandwidth, and the overall transfer function agreed well with theoretical predictions.     

Optical scattering measurements and implications on thermal noise in Gravitational Wave detectors test-mass coatings

Photographs of the LIGO Gravitational Wave detector mirrors illuminated by the standing beam were analyzed with an astronomical software tool designed to identify stars within images, which extracted hundreds of thousands of point-like scatterers uniformly distributed across the mirror surface, likely distributed through the depth of the coating layers. The sheer number of the observed scatterers implies a fundamental, thermodynamic origin during deposition or processing. These scatterers are a possible source of the mirror dissipation and thermal noise foreseen by V. Braginsky and Y. Levin, which limits the sensitivity of observatories to Gravitational Waves. This study may point the way towards the production of mirrors with reduced thermal noise and an increased detection range.     

Cryogenics and Einstein Telescope

The dominant noises which limit the present sensitivity of the gravitational wave detectors are the thermal noise of the suspended mirrors and the shot noise. For the third generation of gravitational wave detectors as the Einstein Telescope (ET), the reduction of the shot noise implies to increase the power stored in the detector at 1 MW level and, at the same time, to compensate the huge optic distortion due to induced thermal lensing. At low temperature it is possible to reduce both these effects. However, lowering the temperature of the test masses without injecting vibration noise from the cooling system is a technological challenge. We review here the thermal noise impact on the ultimate ET sensitivity limit and we discuss possible cryogenic configurations to cool the mirror.     

X光反射镜的辐照损伤实验研究

叙述了利用LF-11装置的线聚焦来模拟LF-12装置的线聚焦辐照Ge靶荡实验,测得沿激光焦线的轴向上所产生的X光和散射光强度,由此获得在LF-12装置上所完成的“类Ne-GeX光激光双程放大实验”中,起反射作用的Si/Mo多层膜X光反射镜在受到113MW/cm~2X光和227MW/cm~2散射光辐照时,其有效寿命为440ps,在50MW/cm~2X光和101MW/cm~2散射光辐照时,其有效寿命为700ps。     

Challenges in thermal noise for 3rd generation of gravitational wave detectors

Various noise sources limit the sensitivity of current interferometric gravitational wave detectors, including seismic noise, thermal noise of the optical components and suspension elements and photon shot noise. Plans are in place for a suite of hardware upgrades which should increase the sensitivity of these detectors by reducing the various noise sources. With these designs for 2nd generation detectors mature, techniques for further improvement of detector sensitivity by a factor of approximately 10 are under study. A particular challenge is the reduction of the thermal noise associated with the interferometer mirrors and their suspensions. We review the current status of research on thermal noise in interferometric gravitational wave detectors. Aspects of possible techniques for use in future ‘3rd generation detectors’ such as cryogenics and diffractive optics are discussed.     

Optical ac coupling to overcome limitations in the detection of optical power fluctuations

A high-sensitivity detection method for optical power fluctuations is demonstrated based on photodetection in reflection of an optical resonator with a specific impedance matching. That resonator is used to reduce the carrier power reflected by the resonator while preserving the power fluctuation sidebands for frequencies above the resonator bandwidth. A sensitivity of 7 x 10(-10) Hz(-1/2) for relative power fluctuations was achieved with only 3 mA of detected photocurrent and 99.6% of the power remained for downstream experiments. As in the widely used ac coupling of electrical signals, this technique overcomes dynamic-range limits and reduces detector noise associated with large carrier amplitudes of the optical field.     

S波段相对论速调管放大器相位稳定性的优化设计及实验研究北大核心CSCD

为了有效提高器件输出微波相位的稳定性,对S波段强流相对论速调管放大器输出微波相位特性开展了理论研究和优化设计。理论分析结果表明,束流发射和传输均匀性、腔内杂频和强流脉冲电压波动是影响器件输出微波相位稳定性的重要原因,通过优化二极管结构,增加吸波材料以及优化腔体结构和参数等手段可以有效地减小上述因素对输出微波相位稳定性的影响,提高器件工作的稳定性。对优化后的器件开展了实验研究,得到单台单次输出功率GW量级基础上,100 ns内相位标准差约10°,单台重频5 Hz工作输出微波相位标准差约20°,两台同时工作输出微波相位差抖动约20°的结果,满足了实际应用的需求。     

Photon-number-resolving detection at a telecommunications wavelength with a charge-integration photon detector

We demonstrate multiphoton discrimination at a telecommunications wavelength with the readout frequency of 40 Hz by a charge-integration photon detector (CIPD). The CIPD consists of an InGaAs pin photodiode and a GaAs junction field effect transistor as a preamplifier in a charge-integration circuit, which is cooled to 4.2 K to reduce thermal noise. The quantum efficiency of the CIPD (the detector itself) is 80% for 1530 nm light, and the readout noise is measured as 0.26 electrons at 40 Hz. We can construct Poisson distributions of photocarrier numbers with distinct peaks at each photocarrier number, corresponding to a signal-to-noise ratio of about 3.     

基于单矢量差分能量检测器的扩频水声通信

通过获得扩频处理增益, 直接序列扩频水声通信系统具有较高的稳定性, 是高质量水声通信及远程水声通信的首选通信方式. 但复杂的海洋环境使得直扩系统在解扩时受到载波相位跳变的影响, 这将导致直扩系统的扩频处理增益下降. 为此, 本文针对直扩系统提出了差分能量检测器算法, 通过比较接收端相关器输出能量完成解码, 并与有源平均声强器算法相结合, 提出单矢量差分能量检测器算法. 该算法具有很好的抗载波相位跳变和多途扩展干扰的能力, 并可对信号方位信息实时跟踪估计, 利用估计方位进行矢量组合可获得矢量处理增益, 从而保证直扩系统可以在低信噪比、时变信道条件下稳定工作. 通过仿真分析和大连海试试验, 验证了本文提出的单矢量差分能量检测器算法的有效性和稳健性.     

Upper limit on gravitational wave backgrounds at 0.2 Hz with a torsion-bar antenna

We present the first upper limit on gravitational wave (GW) backgrounds at an unexplored frequency of 0.2 Hz using a torsion-bar antenna (TOBA). A TOBA was proposed to search for low-frequency GWs. We have developed a small-scaled TOBA and successfully found Ω(gw)(f)<4.3×10(17) at 0.2 Hz as demonstration of the TOBA's capabilities, where Ω(gw)(f) is the GW energy density per logarithmic frequency interval in units of the closure density. Our result is the first nonintegrated limit to bridge the gap between the LIGO band (around 100 Hz) and the Cassini band (10(-6)-10(-4) Hz).     

Thermal-noise limit in the frequency stabilization of lasers with rigid cavities

We evaluate thermal noise (Brownian motion) in a rigid reference cavity used for frequency stabilization of lasers, based on the mechanical loss of cavity materials and the numerical analysis of the mirror-spacer mechanics with the direct application of the fluctuation dissipation theorem. This noise sets a fundamental limit for the frequency stability achieved with a rigid frequency-reference cavity of order 1 Hz/ square root Hz (0.01 Hz/ square root Hz) at 10 mHz (100 Hz) at room temperature. This level coincides with the world-highest level stabilization results.