Adaptive Optics Point Spread Functions: A Comparison of Natural Guide-Star and Laser Guide-Star Adaptive Optics Point Spread Functions and Their Impact On Data Reductions

用自适应光学系统进行天文观测需要对光学系统和定标系统误差有详细的了解。点扩展函数(PSF)会影响信噪比和在拥挤场地中工作的能力。为了获得合理的(5%)测光精度，要么必须选择光圈的大小来包围PSF内的所有能量，从而抵消AO系统的影响，要么必须使用PSF的模型。此外，反卷积和其他图像增强技术的成功在很大程度上取决于对PSF的了解，该程序将使用自适应光学系统与具有不同校正阶数的自然参考源和瑞利后向散射激光信标对五个恒星场的观测进行比较。选择的五个区域是多星系统，其间隔从不到1角秒到大约1角分不等。PSF将从每一次观测的恒星图像中获得。此外，在几个波段的观测将说明PSF的波长依赖性。将根据测光标准星的观测结果进行测光定标。***

ABSTRACT Kibblewhite, Edward AST-9421406 Astronomical observations with adaptive optics systems require a detailed understanding of the optical systems and the calibration systematic errors. The Point Spread Function (PSF) affects the signal-to noise ratio and the ability to work in crowded fields. To obtain reasonable (5%) photometric accuracy, either the size of the aperture must be chosen to encircle all the energy within the PSF, negating the effect of the AO system, or a model of the PSF must be used. In addition, the success of deconvolution and the other image enhancing techniques depends greatly on knowledge of the PSF, The program will compare observations of five star fields using the adaptive optics system with a natural reference source with different orders of correction and with a Rayleigh backscattering laser beacon. The five fields of choice are multiple-star systems with separations varying from less than one arcsecond to roughly one arcminute. The PSF will be obtained from the star images in each of the observations. In addition, observations in several bands will illustrate the wavelength dependence of the PSF. Photometric calibration will be made with observations o photometric standard stars. * * *