GPU支持的高分辨率宇宙学微透镜参数测量
A GPU-Enabled, High-Resolution Cosmological Microlensing Parameter Survey
摘要：
在天气测量的时代，已知的引力透镜类星体的数量将增加一个数量级以上。这些新发现将使单类星体研究转向统计样本的调查，为测试类星体吸积盘和宽发射线区域（BELR）结构的理论模型提供了新的机会。作为为新透镜系统的涌入做准备的一个关键步骤，需要对微透镜会聚-剪切参数空间进行大规模探索，这需要计算O（10^5）高分辨率放大率图。基于已知的透镜类星体的属性，并从吸积盘/BELR建模的期望，我们确定的收敛剪切参数空间，地图大小，光滑的物质分数，和像素分辨率，应该覆盖的区域。我们描述了如何计算耗时的任务，生产~290000放大率的地图，具有足够的分辨率（10000^2像素/地图）探测尺度从吸积盘的内边缘的BELR可以实现在~400天的100 teraflop/s的高性能计算设施，其中的处理性能是实现与图形处理单元。我们通过研究透镜类星体Q2237+0305中透镜宏观模型对吸积盘约束的影响来说明参数调查的用例。我们发现，虽然所有的限制是一致的，在其目前的误差条，更密集的微透镜模型往往预测较浅的吸积盘径向温度分布。通过像这里描述的这样的大参数调查，可以充分探索微透镜测量的系统性。
英文摘要：
In the era of synoptic surveys, the number of known gravitationally lensed quasars is set to increase by over an order of magnitude. These new discoveries will enable a move from single-quasar studies to investigations of statistical samples, presenting new opportunities to test theoretical models for the structure of quasar accretion discs and broad emission line regions (BELRs). As one crucial step in preparing for this influx of new lensed systems, a large-scale exploration of microlensing convergence-shear parameter space is warranted, requiring the computation of O(10^5) high resolution magnification maps. Based on properties of known lensed quasars, and expectations from accretion disc/BELR modelling, we identify regions of convergence-shear parameter space, map sizes, smooth matter fractions, and pixel resolutions that should be covered. We describe how the computationally time-consuming task of producing ~290000 magnification maps with sufficient resolution (10000^2 pixel/map) to probe scales from the inner edge of the accretion disc to the BELR can be achieved in ~400 days on a 100 teraflop/s high performance computing facility, where the processing performance is achieved with graphics processing units. We illustrate a use-case for the parameter survey by investigating the effects of varying the lens macro-model on accretion disc constraints in the lensed quasar Q2237+0305. We find that although all constraints are consistent within their current error bars, models with more densely packed microlenses tend to predict shallower accretion disc radial temperature profiles. With a large parameter survey such as the one described here, such systematics on microlensing measurements could be fully explored.
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