dc.contributor |
Universitat de Barcelona |
dc.contributor.author |
Hoyle, Ben |
dc.contributor.author |
Jiménez, Raúl (Jiménez Tellado) |
dc.contributor.author |
Verde, Licia |
dc.date |
2019-04-08T11:06:02Z |
dc.date |
2019-04-08T11:06:02Z |
dc.date |
2011-05-04 |
dc.date |
2019-04-08T11:06:03Z |
dc.identifier.citation |
1550-7998 |
dc.identifier.citation |
603936 |
dc.identifier.uri |
http://hdl.handle.net/2445/131763 |
dc.format |
11 p. |
dc.format |
application/pdf |
dc.language.iso |
eng |
dc.publisher |
American Physical Society |
dc.relation |
Reproducció del document publicat a: https://doi.org/10.1103/PhysRevD.83.103502 |
dc.relation |
Physical Review D, 2011, vol. 83, num. 10, p. 103502 |
dc.relation |
https://doi.org/10.1103/PhysRevD.83.103502 |
dc.rights |
(c) American Physical Society, 2011 |
dc.rights |
info:eu-repo/semantics/openAccess |
dc.subject |
Física de partícules |
dc.subject |
Experiments |
dc.subject |
Cúmuls de galàxies |
dc.subject |
Particle physics |
dc.subject |
Experiments |
dc.subject |
Clusters of galaxies |
dc.title |
Too big, too early? Multiple high-redshift galaxy clusters: implications |
dc.type |
info:eu-repo/semantics/article |
dc.type |
info:eu-repo/semantics/publishedVersion |
dc.description.abstract |
To date, 14 high-redshift ( z > 1.0 ) galaxy clusters with mass measurements have been observed, spectroscopically confirmed, and are reported in the literature. These objects should be exceedingly rare in the standard Λ cold dark matter ( Λ CDM ) model. We conservatively approximate the selection functions of these clusters' parent surveys and quantify the tension between the abundances of massive clusters as predicted by the standard Λ CDM model and the observed ones. We alleviate the tension, considering non-Gaussian primordial perturbations of the local type, characterized by the parameter f NL , and derive constraints on f NL arising from the mere existence of these clusters. At the 95 % confidence level, f NL > 467 , with cosmological parameters fixed to their most likely WMAP5 values, or f NL ≳ 123 (at 95 % confidence) if we marginalize over prior WMAP5 parameters. In combination with f NL constraints from cosmic microwave background and halo bias, this determination implies a scale dependence of f NL at ≃ 3 σ . Given the assumptions made in the analysis, we expect any future improvements to the modeling of the non-Gaussian mass function, survey volumes, or selection functions to increase the significance of f NL > 0 found here. In order to reconcile these massive, high- z clusters with f NL = 0 , their masses would need to be systematically lowered by 1.5 σ , or the σ 8 parameter should be ∼ 3 σ higher than cosmic microwave background (and large-scale structure) constraints. The existence of these objects is a puzzle: it either represents a challenge to the Λ CDM paradigm or it is an indication that the mass estimates of clusters are dramatically more uncertain than we think. |