论文标题
解剖强镜星系簇MS 0440.5+0204。 I.质量密度曲线
Dissecting the Strong-lensing Galaxy Cluster MS 0440.5+0204. I. The Mass Density Profile
论文作者
论文摘要
我们提供了Galaxy群集MS \，0440.5+0204的参数强镜头建模（位于$ z $ = 0.19）。我们使用三种不同的模型对群集进行了强烈的镜头重建。第一个模型使用四个多个成像系统的图像位置（提供26个约束）。第二个结合了强烈的透镜约束与集群的动态信息（速度分散）。第三个使用从弱镜头计算出的质量作为附加约束。我们的三个模型同样很好地重现了弧的图像位置，其根平方图像等于$ \ $ \ $ 0.5 $ \ arcsec $。然而，在第三个模型中，速度分散和弱透明质量的包含使我们能够在尺度半径上获得更好的约束，以及质量谱的视线速度分散。对于此模型，我们获得$ r_s $ = 132 $^{+30} _ { - 32} $ kpc，$σ_s$ = 1203 $^{+46} _ { - 47} $ s $ s $ s $^{ - 1} $ \ times10^{14} $ \，m $ _ {\ odot} $和高浓度，$ c_ {200} $ = 9.9 $^{+2.2} _ { - 1.4} $。最后，我们使用了派生的质量剖面来计算高达1.5 MPC的质量。我们将其与先前报道的X射线估计值进行了比较，这是一个很好的协议。
We present a parametric strong lensing modeling of the galaxy cluster MS\,0440.5+0204 (located at $z$ = 0.19). We have performed a strong lensing mass reconstruction of the cluster using three different models. The first model uses the image positions of four multiple imaged systems (providing 26 constraints). The second one combines strong lensing constraints with dynamical information (velocity dispersion) of the cluster. The third one uses the mass calculated from weak lensing as an additional constraint. Our three models reproduce equally well the image positions of the arcs, with a root-mean-square image equal to $\approx$0.5$\arcsec$. However, in the third model, the inclusion of the velocity dispersion and the weak-lensing mass allows us to obtain better constraints in the scale radius and the line-of-sight velocity dispersion of the mass profile. For this model, we obtain $r_s$ = 132$^{+30}_{-32}$ kpc, $σ_s$ = 1203$^{+46}_{-47}$ km s$^{-1}$, M$_{200}$ = 3.1$^{+0.6}_{-0.6}$ $\times10^{14}$\,M$_{\odot}$, and a high concentration, $c_{200}$ = 9.9$^{+2.2}_{-1.4}$. Finally, we used our derived mass profile to calculate the mass up to 1.5 Mpc. We compare it with X-ray estimates previously reported, finding a good agreement.
