Weak lensing measurement of filamentary structure with the SDSS BOSS and Subaru Hyper Suprime-Cam data
Weak lensing measurement of filamentary structure with the SDSS BOSS and Subaru Hyper Suprime-Cam data
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DOI：
10.1093/mnras/staa1390
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发表时间：
2019-05
影响因子：
4.8
通讯作者：
Hiroto Kondo;H. Miyatake;M. Shirasaki;N. Sugiyama;A. Nishizawa
中科院分区：
文献类型：
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作者：
Hiroto Kondo;H. Miyatake;M. Shirasaki;N. Sugiyama;A. Nishizawa
利用斯巴鲁超超级凸轮（HSC）第一年星系形状目录，我们报道了斯隆数字巡天（SDSS）III/重子振荡光谱巡天（BOSS）CMASS星系对之间的弱透镜测量。尽管这些调查之间有140 $deg$^2 $的小重叠，我们还是检测到了3.9 $\sigma $显著性的细丝透镜信号，这是在这个红移范围内星系尺度晕之间细丝的最高信噪比透镜测量。我们推导出一个理论上的预测和协方差使用模拟星表的基础上全天空光线跟踪模拟。我们发现，暗条特性的内在散射和大尺度结构沿着视线的涨落是协方差的主要成分，源星系的内在形状噪声不再限制我们的透镜测量。这一事实证明了HSC调查的统计能力，因为它的深度观测和源星系的高数量密度。我们的结果与理论预测一致，并支持“粗”丝模型。随着HSC调查区域的增加，我们将能够研究详细的细丝性质，如暗物质分布和细丝的红移演化。
We report the weak lensing measurement of filaments between Sloan Digital Sky Survey (SDSS) III/Baryon Oscillation Spectroscopic Survey (BOSS) CMASS galaxy pairs at $z\sim0.55$, using the Subaru Hyper Suprime-Cam (HSC) first-year galaxy shape catalogue. Despite of the small overlap of $140$ deg$^2$ between these surveys we detect the filament lensing signal at 3.9$\sigma$ significance, which is the highest signal-to-noise lensing measurement of filaments between galaxy-scale halos at this redshift range. We derive a theoretical prediction and covariance using mock catalogues based on full-sky ray-tracing simulations. We find that the intrinsic scatter of filament properties and the fluctuations in large scale structure along the line-of-sight are the primary component of the covariance and the intrinsic shape noise from source galaxies no longer limits our lensing measurement. This fact demonstrates the statistical power of the HSC survey due to its deep observations and high number density of source galaxies. Our result is consistent with the theoretical prediction and supports the "thick" filament model. As the HSC survey area increases, we will be able to study detailed filament properties such as the dark matter distributions and redshift evolution of filaments.