The XMM Cluster Survey: testing chameleon gravity using the profiles of clusters
Hilton, Matt; Zhao, Gong-Bo; Stott, John P.; Mehrtens, Nicola; Bacon, David; Romer, A. Kathy; Viana, Pedro T. P.; Collins, Chris A.; Liddle, Andrew R.; Mann, Robert G.; Miller, Christopher J.; Nichol, Robert C.; Koyama, Kazuya; Manolopoulou, Maria; Terukina, Ayumu; Sahlén, Martin; Mayers, Julian A.; Wilcox, Harry; Rooney, Philip J.; Hood, Ross
United Kingdom, Japan, China, South Africa, United States, Portugal
Abstract
The chameleon gravity model postulates the existence of a scalar field that couples with matter to mediate a fifth force. If it exists, this fifth force would influence the hot X-ray emitting gas filling the potential wells of galaxy clusters. However, it would not influence the clusters weak lensing signal. Therefore, by comparing X-ray and weak lensing profiles, one can place upper limits on the strength of a fifth force. This technique has been attempted before using a single, nearby cluster (Coma, z = 0.02). Here we apply the technique to the stacked profiles of 58 clusters at higher redshifts (0.1 < z < 1.2), including 12 new to the literature, using X-ray data from the XMM Cluster Survey and weak lensing data from the Canada-France-Hawaii-Telescope Lensing Survey. Using a multiparameter Markov chain Monte Carlo analysis, we constrain the two chameleon gravity parameters (β and φ∞). Our fits are consistent with general relativity, not requiring a fifth force. In the special case of f(R) gravity (where β = √{1/6}), we set an upper limit on the background field amplitude today of |fR0| < 6 × 10-5 (95 per cent CL). This is one of the strongest constraints to date on |fR0| on cosmological scales. We hope to improve this constraint in future by extending the study to hundreds of clusters using data from the Dark Energy Survey.