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LoCuSS: Subaru weak lensing study of 30 galaxy clusters

机译：LoCuSS：斯巴鲁对30个星系团的弱透镜研究

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We use high-quality Subaru/Suprime-Cam imaging data to conduct a detailed weak lensing study of the distribution of dark matter in a sample of 30 X-ray luminous galaxy clusters at 0.15 ≤ z ≤ 0.3. A weak lensing signal is detected at high statistical significance in each cluster, the total signal-to-noise ratio of the detections ranging from 5 to 13. Comparing spherical models to the tangential distortion profiles of the clusters individually, we are unable to discriminate statistically between a singular isothermal sphere (SIS) and Navarro, Frenk, and White (NFW) models. However, when the tangential distortion profiles are combined and then models are fitted to the stacked profile, the SIS model is rejected at 6σ and 11 σ, respectively, for low (M_(vir) < 6 × 10~(14) h ~(-1) M_?) and high (M_(vir) > 6 × 10~(14) h~(-1) M_?) mass bins. We also used individual cluster NFW model fits to investigate the relationship between the cluster mass and the concentration, finding that the concentration (c _(vir)) decreases with increasing cluster mass (M_(vir)). The best-fit c_(vir)-M_(vir) relation is: c_(vir)(M _(vir)) = 8.75_(-2.89)~(+4.13) × (M _(vir)/10~(14)h~(-1) M_?) ~(-α) with α ≈ 0.40±0.19: i.e., a non-zero slope is detected at 2σ significance. This relation gives a concentration of c_(vir) = 3.48_(-1.15)~(+1.65) for clusters with M _(vir) = 10~(15) h~(-1)M~?, which is inconsistent at 4 σ significance with the values of c_(vir) ～ 10 reported for strong-lensing-selected clusters. We have found that the measurement error on the cluster mass is smaller at higher over-densities, Δ ? 500-2000, than at the virial over-density, A_(vir) ? 110; typical fractional errors at Δ ? 500-2000 are improved to σ(M_Δ)/M_Δ ? 0.1-0.2 compared with 0.2-0.3 at Δ_(vir). Furthermore, comparing the 3D spherical mass with the 2D cylinder mass, obtained from the aperture mass method at a given aperture radius, θΔ, reveals M_(2D)(< θ_Δ)/M_(3d)(< r_Δ = D1θ_Δ) ? 1-46 and 1.32 for Δ = 500 and Δ_(vir), respectively. The amplitude of this offset agrees well with that predicted by integrating an NFW model of cluster-scale halos along the line-of-sight.
机译：我们使用高质量的Subaru / Suprime-Cam影像数据对0.15≤z≤0.3的30个X射线发光星系团样本中的暗物质分布进行了详细的弱透镜研究。在每个聚类中以较高的统计显着性检测到微弱的透镜信号，检测的总信噪比范围为5到13。将球形模型与聚类的切向畸变轮廓进行比较，我们无法在统计学上进行区分在单个等温球（SIS）和Navarro，Frenk和White（NFW）模型之间。但是，当组合切向畸变轮廓并将模型拟合到堆叠轮廓时，对于低（M_（vir）<6×10〜（14）h〜（），SIS模型分别在6σ和11σ时被拒绝。 -1）M_？）和高（M_（vir）> 6×10〜（14）h〜（-1）M_？）质量块。我们还使用了个体簇NFW模型拟合来研究簇质量与浓度之间的关系，发现浓度（c_（vir））随着簇质量（M_（vir））的增加而降低。最佳拟合c_（vir）-M_（vir）关系为：c_（vir）（M _（vir））= 8.75 _（-2.89）〜（+4.13）×（M _（vir）/ 10〜（ 14）h〜（-1）M_？）〜（-α），α≈0.40±0.19：即，在2σ显着性下检测到非零斜率。对于M _（vir）= 10〜（15）h〜（-1）M〜？的簇，该关系给出了c_（vir）= 3.48 _（-1.15）〜（+1.65）的浓度，在以下位置不一致对于强镜头选择的聚类，报道的c_（vir）〜10值为4σ显着。我们发现，在较高的过密度下，簇质量的测量误差较小。 500-2000，比病毒密度高时的A_（vir）？ 110; ΔΔ处的典型分数误差将500-2000提高到σ（M_Δ）/M_Δ？ 0.1-0.2，而Δ_（vir）为0.2-0.3。此外，将在给定孔径半径θΔ下从孔径质量方法获得的3D球形质量与2D圆柱质量进行比较，得出M_（2D）（<θ_Δ）/ M_（3d）（

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