Cosmic microwave anisotropies from BPS semilocal strings

TL;DR

This paper calculates the CMB anisotropy spectra from semilocal cosmic strings using simulations, deriving constraints on their parameters and comparing models with and without defects.

Contribution

First-ever simulation-based calculation of CMB anisotropies from semilocal strings and analysis of their cosmological constraints.

Findings

Gmu = 5.3x10^{-6} reproduces anisotropy at l=10

Upper bound Gmu<2.0x10^{-6} from combined data

Models with defects are statistically inconclusive compared to no-defect models

Abstract

We present the first ever calculation of cosmic microwave background CMB anisotropy power spectra from semilocal cosmic strings, obtained via simulations of a classical field theory. Semilocal strings are a type of non-topological defect arising in some models of inflation motivated by fundamental physics, and are thought to relax the constraints on the symmetry breaking scale as compared to models with (topological) cosmic strings. We derive constraints on the model parameters, including the string tension parameter mu, from fits to cosmological data, and find that in this regard BPS semilocal strings resemble global textures more than topological strings. The observed microwave anisotropy at l = 10 is reproduced if Gmu = 5.3x10^{-6} (G is Newton's constant). However as with other defects the spectral shape does not match observations, and in models with inflationary perturbations plus semilocal strings the 95% confidence level upper bound is Gmu<2.0x10^{-6} when CMB data, Hubble Key Project and Big Bang Nucleosynthesis data are used (c.f. Gmu<0.9x10^{-6} for cosmic strings). We additionally carry out a Bayesian model comparison of several models with and without defects, showing models with defects are neither conclusively favoured nor disfavoured at present.