Cosmic structure and dark energy

By Eric Linder, Adrian Jenkins. 2003

190 citations recorded by the source corpus.

Dark energy has a dramatic effect on the dynamics of the Universe, causing the recently discovered acceleration of the expansion. The dynamics are also central to the behaviour of the growth of large-scale structure, offering the possibility that observations of structure formation provide a sensitive probe of the cosmology and dark energy characteristics. In particular, dark energy with a time-varying equation of state can have an influence on structure formation stretching back well into the matter-dominated epoch. We analyse this impact, first calculating the linear perturbation results, including those for weak gravitational lensing. These dynamical models possess definite observable differences from constant equation of state models. Then we present a large-scale numerical simulation of structure formation, including the largest volume to date involving a time-varying equation of state. We find the halo mass function is well described by the Jenkins et al. mass function formula. We also show how to interpret modifications of the Friedmann equation in terms of a time-variable equation of state. The results presented here provide steps toward realistic computation of the effect of dark energy in cosmological probes involving large-scale structure, such as cluster counts, the Sunyaev–Zel'dovich effect or weak gravitational lensing.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b6ee5e8ba384ce32ccdb655552f4be8274d905bf

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Citations in the corpus

Cosmological parameters from lensing power spectrum and bispectrum tomography (2003, methodology): “For example,g(a) for dark energy cosmologies are shown in Figure 2 of Linder & Jenkins (2003).”
The dynamics of quintessence, the quintessence of dynamics (2007, background): “Early work with dynamical quintessence included that of Klypin et al. (2003); Linder & Jenkins (2003), with many following investigations.”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, background): “…provided by Jenkins is approximately accurate (within ∼20 per cent) among models with constant w = −1 and some evolving w models (Klypin et al. 2003; Linder & Jenkins 2003; Łokas et al. 2004; Kuhlen et al. 2005).4 Other authors have studied the dependence of f (σ ) on redshift beyond that…”
The growth of structure in interacting dark energy models (2009, methodology): “Following the typical approach in non-interacting dark energy models, we use the parametrization of the equation of state for the dark energy [31, 32],”
The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z=0.9 (2011, background): “The growth rate of this structure with time is a key discriminant between cosmological models (e.g., Linder & Jenkins 2003, Linder & Cahn 2007, Nesseris & Perivolaropoulos 2008).”
The Cosmological simulation code GADGET-2 (2005, background): “Linder & Jenkins (2003) and Dolag et al. (2004a) independently studied dark energy cosmologies.”
Confronting Lemaitre–Tolman–Bondi models with observational cosmology (2008, background): “ observables, that will help decide between the diﬀerent scenarios in the future, is the Hubble parameter H(z). Under the assumption that the correct background is a ﬂat FRW cosmology we can write it [22] H2 T,L(z) H2 in = (1+z)3Ω in +(1− Ωin)exp 3 Z1+z 1 dlog(1+z′)(1+wT,L eﬀ (z ′)) , (49) where H”
Cosmological parameters from supernova observations: A critical comparison of three data sets (2003, background): “…2002; Kujat et al. 2002; Minty, Heavens, & Hawkins 2002; Maor et al. 2002; Weller & Albrecht 2002; Gerke & Efstathiou 2002; Rowan-Robinson 2002; Linder & Jenkins 2003; Padmanabhan & Choudhury 2003; Visser 2004; Caresia, Matarrese, & Moscardini 2004; Alcaniz 2004; Wang & Mukherjee 2004;…”
Bayesian physical reconstruction of initial conditions from large-scale structure surveys (2012, methodology): “For a general cosmology the growth factor D+(a) can be obtained by numerical solution of the linear growth equation (see e.g. Turner & White 1997; Wang & Steinhardt 1998; Linder & Jenkins 2003): d2D+(a) da2 + 1 a ( 3 + d lnH d lna ) dD+(a) da − 3 2 Ωm(a)D+(a) a2 = 0 (A1)”
WMAP constraints on low redshift evolution of dark energy (2004, background): “…the observations of galaxy clustering, temperature anisotropies in the CMBR and the high-redshift supernovae (Perlmutter et al. 1999; Lee & Ng 2003; Linder & Jenkins 2003; Pogosyan et al. 2003; Tegmark et al. 2003; Huterer & Cooray 2004; Lee, Lee & Ng 2004; Maccio et al. 2004; Multamaki et al.…”
New constraints on dark energy from the observed growth of the most X-ray luminous galaxy clusters (2007, background): “It has since been verified that this fitting function is approximately universal (within ∼ 20 per cent) among models with constant w 6= −1 and some evolving-w models (Klypin et al. 2003; Linder & Jenkins 2003; Lokas et al. 2004; Kuhlen et al. 2005).”