Studying galaxy troughs and ridges using weak gravitational lensing with the Kilo-Degree Survey
Studying galaxy troughs and ridges using weak gravitational lensing with the Kilo-Degree Survey
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DOI：
10.1093/mnras/sty2589
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发表时间：
2018-05
影响因子：
4.8
通讯作者：
M. Brouwer;V. Demchenko;J. Harnois-D'eraps;Maciej Bilicki;C. Heymans;H. Hoekstra;K. Kuijken;M. Alpaslan;S. Brough;Yan-Chuan Cai;M. Costa-Duarte;A. Dvornik;T. Erben;H. Hildebrandt;B. Holwerda;P. Schneider;C. Sif'on;E. van Uitert-E.-van Uitert-2130243441
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作者：
M. Brouwer;V. Demchenko;J. Harnois-D'eraps;Maciej Bilicki;C. Heymans;H. Hoekstra;K. Kuijken;M. Alpaslan;S. Brough;Yan-Chuan Cai;M. Costa-Duarte;A. Dvornik;T. Erben;H. Hildebrandt;B. Holwerda;P. Schneider;C. Sif'on;E. van Uitert-E.-van Uitert-2130243441
我们研究宇宙星系密度场中的投影欠密度，称为“槽”，以及它们的过密度对应物，我们称之为“脊”。我们确定这些地区使用明亮的样本的前景星系的光度千度调查（KiDS），专门选择模仿光谱星系和质量大会调查。利用来自KiDS的背景星系，我们测量了槽/脊的弱引力透镜轮廓。我们量化了它们的透镜强度A的幅度作为星系密度百分位数秩P和星系过密度δ的函数，并发现星系密度分布的偏斜度反映在弱透镜测量的总质量分布中。我们解释我们的结果使用模拟星系目录从Marenostrum学院科学德l 'Espai（MICE）模拟，并找到一个很好的协议与我们的观察。使用从Scinet LightCone Simulations（SLICS）模拟目录中导出的信噪比权重，我们最佳地堆叠角半径θ（A）= {5，10，15，20} arcmin的KiDS槽的透镜信号，从而得到{16.8，14.9，10.13，7.55} sigma检测。最后，我们使用一个体积有限的星系样本来选择槽，分成两个红移在0.1 <z <0.3之间的仓。对于横向共动半径R-A = 1.9 h（70）（-1）Mpc的槽/脊，我们发现低红移和高红移样品之间的共动过量表面密度作为P和δ的函数没有显著差异。使用MICE和SLICS模拟，我们预测，槽和脊的演变可以检测到引力透镜使用更深，更广泛的透镜调查，如那些从大型综合巡天望远镜和欧几里得。
We study projected underdensities in the cosmic galaxy density field known as 'troughs', and their overdense counterparts, which we call 'ridges'. We identify these regions using a bright sample of foreground galaxies from the photometric Kilo-Degree Survey (KiDS), specifically selected to mimic the spectroscopic Galaxy And Mass Assembly survey. Using background galaxies from KiDS, we measure the weak gravitational lensing profiles of the troughs/ridges. We quantify the amplitude of their lensing strength A as a function of galaxy density percentile rank P and galaxy overdensity delta, and find that the skewness in the galaxy density distribution is reflected in the total mass distribution measured by weak lensing. We interpret our results using the mock galaxy catalogue from the Marenostrum Institut de Ciencies de l'Espai (MICE) simulation, and find a good agreement with our observations. Using signal-to-noise weights derived from the Scinet LIghtCone Simulations (SLICS) mock catalogue we optimally stack the lensing signal of KiDS troughs with an angular radius theta(A) = {5, 10, 15, 20} arcmin, resulting in {16.8, 14.9, 10.13, 7.55} sigma detections. Finally, we select troughs using a volume-limited sample of galaxies, split into two redshift bins between 0.1 <z <0.3. For troughs/ridges with transverse comoving radius R-A = 1.9 h(70)(-1) Mpc, we find no significant difference in the comoving excess surface density as a function of P and delta between the low- and high-redshift sample. Using the MICE and SLICS mocks we predict that trough and ridge evolution could be detected with gravitational lensing using deeper and wider lensing surveys, such as those from the Large Synoptic Survey Telescope and Euclid.