天体物理厚透镜引起的连续图象畸变
Continuous image distortion by astrophysical thick lenses
摘要：
由于弱引力透镜的图像失真检查使用非微扰的方法集成的测地线偏差和光学标量方程沿零测地线连接观察者到一个遥远的来源。我们开发的方法不断地改变从光源到观察者的光束的形状，而不参考天体物理学相关场景中的透镜平面。我们比较了投影面积和半长半短轴的比率所观察到的椭圆形图像形状的圆形源从连续的，厚透镜的方法与通常假设的薄透镜近似。我们发现，对于真实星系团的截断奇异等温球和NFW模型，常用的薄透镜近似在预测像面积和轴比方面的精度优于1/10 ^4。对于由两个质量较大的团簇组成的非对称厚透镜，在红移到Δz = 0.2时，我们发现，将像畸变模拟为单个透镜平面上的两个团簇，在像面积或轴比方面不会产生大于0.5%的相对误差
英文摘要：
Image distortion due to weak gravitational lensing is examined using a non-perturbative method of integrating the geodesic deviation and optical scalar equations along the null geodesics connecting the observer to a distant source. The method we develop continuously changes the shape of the pencil of rays from the source to the observer with no reference to lens planes in astrophysically relevant scenarios. We compare the projected area and the ratio of semi-major to semi-minor axes of the observed elliptical image shape for circular sources from the continuous, thick-lens method with the commonly assumed thin-lens approximation. We find that for truncated singular isothermal sphere and NFW models of realistic galaxy clusters, the commonly used thin-lens approximation is accurate to better than 1 part in 10^4 in predicting the image area and axes ratios. For asymmetric thick lenses consisting of two massive clusters separated along the line of sight in redshift up to Δz = 0.2, we find that modeling the image distortion as two clusters in a single lens plane does not produce relative errors in image area or axes ratio more than 0.5%
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