论文标题
Z〜2-9星系由Hubble Frontier Field群集I：源选择和表面密度 - 磁化约束从> 2500星系
z~2-9 Galaxies magnified by the Hubble Frontier Field Clusters I: Source Selection and Surface Density-Magnification Constraints from >2500 galaxies
论文作者
论文摘要
我们组装了大量的全面样本，分别是2534 Z〜2、3、4、5、6、7、8和9个星系，由Hubble Frontier Fields（HFF）程序的六个群集镜头。 Making use of the availability of multiple independent magnification models for each of the HFF clusters and alternatively treating one of the models as the "truth," we show that the median magnification factors from the v4 parametric models are typically reliable to values of 30 to 50, and in one case to 100. Using the median magnification factor from the latest v4 models, we estimate the UV luminosities of the 2534 lensed z~2-9 galaxies, finding sources as faint在Z〜3和-12.9 mag处为-12.4 mag在Z〜7。我们明确说明了在HFF簇中与MU的表面密度 - 磁化关系的功能，以限制远处的星系特性和簇透镜特性。基于Sigma（Z）与MU关系，我们表明，现有公共模型的中位数倍率估计值必须是对MU的真实放大倍数的可靠预测指标，即MU <15（95％的置信度）。我们还使用观察到的Sigma（Z）与MU关系来得出对亮度功能的演变的限制，从Z〜7到Z〜2微弱的末端斜率，表明只有在选择效率没有强大的依赖性依赖放大因子Mu时，微弱的端斜率结果才能与空白视野研究保持一致。只有在非常低的光度星系很小的情况下，只有在深镜头探针中未解决的情况下才是这种情况。
We assemble a large comprehensive sample of 2534 z~2, 3, 4, 5, 6, 7, 8, and 9 galaxies lensed by the six clusters from the Hubble Frontier Fields (HFF) program. Making use of the availability of multiple independent magnification models for each of the HFF clusters and alternatively treating one of the models as the "truth," we show that the median magnification factors from the v4 parametric models are typically reliable to values of 30 to 50, and in one case to 100. Using the median magnification factor from the latest v4 models, we estimate the UV luminosities of the 2534 lensed z~2-9 galaxies, finding sources as faint as -12.4 mag at z~3 and -12.9 mag at z~7. We explicitly demonstrate the power of the surface density-magnification relations Sigma(z) vs. mu in the HFF clusters to constrain both distant galaxy properties and cluster lensing properties. Based on the Sigma(z) vs. mu relations, we show that the median magnification estimates from existing public models must be reliable predictors of the true magnification mu to mu<15 (95% confidence). We also use the observed Sigma(z) vs. mu relations to derive constraints on the evolution of the luminosity function faint-end slope from z~7 to z~2, showing that faint-end slope results can be consistent with blank-field studies if, and only if, the selection efficiency shows no strong dependence on the magnification factor mu. This can only be the case if very low luminosity galaxies are very small, being unresolved in deep lensing probes.
