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CLASH-VLT : constraints on f ( R ) gravity models with galaxy clusters using lensing and kinematic analyses

L. Pizzuti, B. Sartoris, L. Amendola, S. Borgani, A. Biviano, K. Umetsu, A. Mercurio, P. Rosati, I. Balestra, G.B. Caminha, M. Girardi, C. Grillo and M. Nonino

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 Bou'e. Ou... Full description

Main Author: Pizzuti, Lorenzo
Contributors: Amendola, Luca | Author
Published: 13 July 2017
Contained in: Journal of cosmology and astroparticle physics London : IOP, 2003 (2017,07) Artikel-Nummer 023, ? Seiten
Journal Title: Journal of cosmology and astroparticle physics
Fulltext access:
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Links: Volltext (dx.doi.org)
Volltext (stacks.iop.org)
ISSN: 1475-7516
DOI: 10.1088/1475-7516/2017/07/023
Regional Holdings: TIB – German National Library of Science and Technology
Language: English
Notes: Gesehen am 15:09.2017
ID (e.g. DOI, URN): 10.1088/1475-7516/2017/07/023
PPN (Catalogue-ID): 1563556952
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520 |a 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 Bou'e. 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 λ for models in which the dependence of this parameter on the environment is negligible at the scale considered (i.e. λ= 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 λ≤1.61 mpc at Δχ 2 =2.71 on the marginalized distribution. For RXJ 2248 instead a possible tension with the ΛCDM model appears when adding lensing information, with a lower limit λ≥0.14 mpc at Δχ 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. 
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