Spherical collapse in quintessence models with zero speed of sound

By P. Creminelli, Guido D'Amico, J. Noreña, L. Senatore, F. Vernizzi. 2009

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We study the spherical collapse model in the presence of quintessence with negligible speed of sound. This case is particularly motivated for w < −1 as it is required by stability. As pressure gradients are negligible, quintessence follows dark matter during the collapse. The spherical overdensity behaves as a separate closed FLRW universe, so that its evolution can be studied exactly. We derive the critical overdensity for collapse and we use the extended Press-Schechter theory to study how the clustering of quintessence affects the dark matter mass function. The effect is dominated by the modification of the linear dark matter growth function. A larger effect occurs on the total mass function, which includes the quintessence overdensities. Indeed, here quintessence constitutes a third component of virialized objects, together with baryons and dark matter, and contributes to the total halo mass by a fraction ~ (1+w)ΩQ/Ωm. This gives a distinctive modification of the total mass function at low redshift.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1260e4f473e26ced349c380f3fd26b207ec0bab3

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Citations in the corpus

Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “Encouragingly, preliminary work in this area suggests that the influence of dark energy on the mass function might be readily measurable, resulting in additional constraining power from clusters (e.g. Creminelli et al. 2010).”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, background): “…that the effect of dark energy perturbations on the mass function might be readily measurable (Abramo, Batista & Rosenfeld 2009; Park et al. 2009; Alimi et al. 2010; Creminelli et al. 2010), in which case our approach likely underestimates the ability of the data to discriminate among these models.”
Formation of Galaxy Clusters (2012, background): “…growth is affected not only because DE influences linear growth, but also because it participates non-trivially in the collapse of matter and may slow down or accelerate the formation of clusters of a given mass depending on DE equation of state (Abramo et al. 2007, Creminelli et al. 2010).”
Massive Cosmologies (2011, methodology): “We prove this by assuming the (3)For momentum conservation one should use the full covariant expression ∇Tμi that leads to the acceleration equation; in this case however, it is obtained at the linear order in ~x and requires correcting the stress-tensor by O(H2x2) quantities [23].”
Essential Building Blocks of Dark Energy (2013, methodology): “[10]) or on scales longer than the sound horizon, a consistent treatment which takes into account the time derivatives should be undertaken.”
Dust of dark energy (2010, methodology): “Nonetheless, some models exist in the literature: [1–13].”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “For instance, [347] have shown that the presence in the inflationary theory of an approximate Galilean symmetry (proposed by [904] in the context of modified gravity) generates third-order operators with two derivatives on each field.”
Galaxy Bias and non-Linear Structure Formation in General Relativity (2011, background): “This includes a Universe filled with dark matter and a cosmological constant, or with dark matter and quintessence with a very small speed of sound as the models studied in [17], while it does not apply to models with quintessence with non-vanishingly small speed of sound.”