Witt双曲线被预测且观测到在四重类星体中经过透镜星系附近
Witt's hyperbola is both predicted and observed to pass close to the lensing galaxies in quadruple quasars
AI总结：
该研究验证了Witt双曲线经过透镜星系附近的结论，测得39个孤立透镜系统的偏移中值为0.033角秒（约1%爱因斯坦环半径），提出将最亮像素作为中心的改进方法，可降低透镜模型拟合的维度。
摘要：
当按照Witt (1996)提出的方法，从四重引力透镜类星体的像位置构建一条矩形双曲线时，该双曲线会经过透镜星系非常近的位置。对于39个由相对孤立的星系产生透镜效应的系统样本，测得的透镜观测光心与Witt双曲线之间的垂直偏移中值为0.033角秒。Witt采用的透镜模型族预测透镜位于双曲线上，但构建双曲线时并未使用透镜的位置。该中值偏移约对应爱因斯坦环半径的1%，表明透镜势的中心与透镜的光心非常接近。通过对到Witt双曲线的垂直距离（或星系与势之间的距离）施加严格先验，在拟合数据时可将模型空间的维度减少一维。将透镜星系的最亮像素作为其中心，避免了使用平均光心作为约束的一个缺陷。
英文摘要：
When a rectangular hyperbola is constructed from the image positions of a quadruply lensed quasar, as proposed by Witt (1996), it passes very close to the the lensing galaxy. The median measured perpendicular offset between the observed light center of the lens and Witt's hyperbola is 0.013" for a sample for 39 systems lensed by a relatively isolated galaxy. The family of lens models adopted by Witt predicts that the lens lies on the hyperbola, but its position in not used for its construction. The median offset corresponds to roughly 1% of the Einstein ring radius, and suggests that the centers of the lensing potential are close to the light centers of the lens. By putting a restrictive prior on the perpendicular distance to Witt's hyperbola (or on the distance between the galaxy and the potential), one reduces by one the dimensionality of a model space when fitting data. Taking the brightest pixel of a lensing galaxy as its center avoids a shortcoming of using the average light center for a constraint.
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