CLASH-VLT: constraints on f(R) gravity models with galaxy clusters using lensing and kinematic analyses
CLASH-VLT: constraints on f(R) gravity models with galaxy clusters using lensing and kinematic analyses
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DOI：
10.1088/1475-7516/2017/07/023
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发表时间：
2017-07-01
影响因子：
6.4
通讯作者：
Nonino, M.
中科院分区：
文献类型：
--
作者：
Pizzuti, L.;Sartoris, B.;Nonino, M.
我们进行了最大似然运动学分析的两个动态松弛星系团MACS J1206.2-0847在z = 0.44和RXC J2248.7-4431在z = 0.35，以确定总质量分布在修改后的重力模型，使用修改版本的MAMPOSSt代码的Mamon，Biviano和Boue。我们的工作是基于运动学和透镜质量分布，使用来自哈勃望远镜的星团透镜和超新星巡天（以下简称CLASH）和甚大望远镜的光谱跟踪（以下简称CLASH-VLT）的数据。我们假设一个球形Navarro-Frenk-白色（以下简称NFW）轮廓，以便获得对模型的第五力相互作用范围λ的约束，其中该参数对环境的依赖性在所考虑的尺度上是可以忽略的（即λ = const），并将第五力强度固定为f（R）引力中预测的值。然后，我们使用的信息，从透镜分析，把其他NFW自由参数的先验。在MACSJ 1206的情况下，联合运动学+透镜分析导致在Δ χ（2）= 2.71处有效相互作用范围λ = 0.14 Mpc的上限。这是透镜效应和运动学数据之间的微小差异的结果，出现在该集群的GR中，原则上可以用重力的修改来解释。我们讨论了系统学的影响和我们的分析的局限性，以及未来的改进所获得的结果。这项工作具有有趣的影响，鉴于即将到来的和未来的大型成像和光谱调查，这将提供大量的星系团的透镜和运动质量重建。
We perform a maximum likelihood kinematic analysis of the two dynamically relaxed galaxy clusters MACS J1206.2-0847 at z = 0.44 and RXC J2248.7-4431 at z = 0.35 to determine the total mass profile in modified gravity models, using a modified version of the MAMPOSSt code of Mamon, Biviano and Boue. Our work is based on the kinematic and lensing mass profiles derived using the data from the Cluster Lensing And Supernova survey with Hubble (hereafter CLASH) and the spectroscopic follow-up with the Very Large Telescope (hereafter CLASH-VLT). We assume a spherical Navarro-Frenk-White (NFW hereafter) profile in order to obtain a constraint on the fifth force interaction range lambda for models in which the dependence of this parameter on the environment is negligible at the scale considered (i.e. lambda = const) and fixing the fifth force strength to the value predicted in f(R) gravity. We then use information from lensing analysis to put a prior on the other NFW free parameters. In the case of MACSJ 1206 the joint kinematic+lensing analysis leads to an upper limit on the effective interaction range lambda = 0.14 Mpc at Delta chi(2) = 2.71. This is consequence of the slight difference between the lensing and kinematic data, appearing in GR for this cluster, that could in principle be explained in terms of modifications of gravity. We discuss the impact of systematics and the limits of our analysis as well as future improvements of the results obtained. This work has interesting implications in view of upcoming and future large imaging and spectroscopic surveys, that will deliver lensing and kinematic mass reconstruction for a large number of galaxy clusters.