We calculate the strong lensing probability as a function of the image separation Δθ in TeVeS (tensor-vector-scalar) cosmology, which is a relativistic version of MOND (MOdified Newtonian Dynamics). The lens, often an elliptical galaxy, is modeled by the Hernquist profile. We assume a flat cosmology with Ω_b = 1 — Ω_A = 0.04 and the simplest interpolating function μ(x) = min (1, x). For comparison, we recalculated the probabilities for lenses by singular isothermal sphere (SIS) galaxy halos in LCDM with a Schechter fit velocity function. The amplification bias is calculated based on the magnification of the second bright image rather than on the total of the two brighter images. Our calculations show that the Hernquist model predicts insufficient but acceptable probabilities in flat TeVeS cosmology compared with the results of the well-defined combined sample of the Cosmic Lens All-Sky Survey (CLASS) and the Jodrell Bank/Very Large Array Astrometric Survey (JVAS); at the same time, it predicts higher probabilities than the SIS model in LCDM at small image separations.
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机译：我们根据TeVeS（张量-矢量-标量）宇宙学中的图像分离Δθ计算强透镜发生概率，这是MOND（修正牛顿动力学）的相对论版本。镜头通常是椭圆星系，由亨奎斯特轮廓建模。我们假设一个平坦的宇宙学，其中Ω_b= 1 —Ω_A= 0.04并且最简单的插值函数μ（x）= min（1，x）。为了进行比较，我们通过具有Schechter拟合速度函数的LCDM中的奇异等温球（SIS）星系光晕重新计算了镜片的概率。放大偏差是根据第二个亮图像的放大倍数而不是两个亮图像的总和来计算的。我们的计算结果表明，与明确定义的宇宙透镜全天候调查（CLASS）和Jodrell Bank /超大型阵列占星调查（JVAS）组合样本的结果相比，Hernquist模型预测的平面TeVeS宇宙学的概率不足但可以接受）;同时，在小图像分离情况下，它预测的概率要高于LCDM中的SIS模型。
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