Late-time acceleration in a slow-moving Galileon field

Adak, Debabrata; Ali, Amna; Majumdar, Debasish

doi:10.1103/physrevd.88.024007

Cited by 16 publications

(17 citation statements)

References 67 publications

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“…SNeIa are considered standard candles at peak luminosity and therefore they have been used not only to determine the Hubble constant (at relatively low redshifts) but also to trace the curvature of the Hubble relation at high redshifts (see Perlmutter et al 1998, 1999; Riess et al 1998, 2004; Tonry et al 2003; Astier et al 2006; D07; Riess 2007; Wood‐Vasey et al 2007; Kowalski et al 2008; Hicken et al 2009; Amanullah et al 2010; Adak, Bandyopadhyay & Majumdar 2011; Kim 2011; Li et al 2011; March et al 2011; Wang, Li & Li 2011). In practice one relates the distance modulus of the SNIa to its luminosity distance, d L , through which the cosmological parameters enter: and which for a flat universe (Ω k = 0) reduces to The main result of numerous studies using this procedure is that distant SNeIa’s are on average dimmer by ∼0.2 mag than expected in an Einstein–de Sitter model, which translates in them being ∼10 per cent further away than expected.…”

Section: Cosmological Parameters From the Hubble Relationmentioning

confidence: 99%

A strategy to measure the dark energy equation of state using the H ii galaxy Hubble function and X-ray active galactic nuclei clustering: preliminary results

Plionis

Terlevich

Basilakos

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We explore the possibility of setting stringent constraints to the dark energy equation of state using alternative cosmic tracers like (a) the Hubble relation using H ii galaxies, which can be observed at much higher redshifts (z≲ 3.5) than those currently traced by Type Ia supernovae (SNeIa) samples, and (b) the large‐scale structure using the clustering of X‐ray selected active galactic nuclei (AGN), which have a redshift distribution peaking at z∼ 1. In this paper we use extensive Monte Carlo simulations to define the optimal strategy for the recovery of the dark energy equation of state using the high‐redshift (z≳ 2) Hubble relation, but accounting also for the effects of gravitational lensing, which for such high redshifts can significantly affect the derived cosmological constraints. We investigate the size of the sample of high‐z H ii galaxies needed to provide useful constraints in the dark energy equation of state. Based on a ‘figure of merit’ analysis, we provide estimates for the number of 2 ≲z≲ 3.5 tracers needed to reduce the cosmological solution space, presently provided by the Constitution SNIa set, by a desired factor. The analysis is given for any level of rms distance modulus uncertainty and we find that an expected reduction (i.e. by ∼20–40 per cent) of the current level of H ii‐galaxy‐based distance modulus uncertainty does not provide a significant improvement in the derived cosmological constraints. It is much more efficient to increase the number of tracers than to reduce their individual uncertainties. Finally, we propose a framework to put constraints on the dark energy equation of state by using the joint likelihood of the X‐ray AGN clustering and of the Hubble relation cosmological analyses. A preliminary joint analysis using the X‐ray AGN clustering of the 2XMM survey and the Hubble relation of the Constitution SNIa set provide Ωm= 0.31 ± 0.01 and w=−1.06 ± 0.05. We also find that the joint SNIa–2XMM analysis provides significantly more stringent cosmological constraints, increasing the figure of merit by a factor of ∼2, with respect to that of the joint SNIa–baryonic acoustic oscillation analysis.

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Section: Cosmological Parameters From the Hubble Relationmentioning

confidence: 99%

A strategy to measure the dark energy equation of state using the H ii galaxy Hubble function and X-ray active galactic nuclei clustering: preliminary results

Plionis

Terlevich

Basilakos

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…It is observed in Refs. [43,44] that if Slotheon field model of dark energy is considered, then the slow rolling criteria will be more favoured than the standard quintessence dark energy model. This is because the former induces an extra friction which favours the slow rolling nature of the field.…”

Section: Coupled Quintessence Dark Energy Modelmentioning

confidence: 99%

“…In this work we take both the dark energy and dark matter as real scalar fields and treat the interactions in a way which is more fundamental in nature. Here, we consider two dark energy models, the standard quintessence dark energy model and the Slotheon field dark energy model [43][44][45]. The Slotheon dark energy model is a modified gravity model, inspired by extra-dimensional theories.…”

Section: Introductionmentioning

confidence: 99%

Addressing the high-f problem in pseudo-Nambu–Goldstone boson dark energy models with dark matter–dark energy interaction

2020

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We consider a dark energy scenario driven by a scalar field $$\phi $$ ϕ with a pseudo-Nambu–Goldstone boson (pNGB) type potential $$V(\phi )=\mu ^4 \left( 1+ \mathrm{cos}(\phi /f) \right) $$ V ( ϕ ) = μ 4 1 + cos ( ϕ / f ) . The pNGB originates out of breaking of spontaneous symmetry at a scale f close to Planck mass $$M_\mathrm{{pl}}$$ M pl . We consider two cases namely the quintessence dark energy model with pNGB potential and the other, where the standard pNGB action is modified by the terms related to Slotheon cosmology. We demonstrate that for this pNGB potential, high-f problem is better addressed when the interaction between dark matter and dark energy is taken into account and that Slotheon dark energy scenario works even better over quintessence in this respect. To this end, a mass limit for dark matter is also estimated.

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“…Note that this field π moves slower than the ordinary scalar in scalar field theory and hence the nomenclature. The action for the Slotheon field is given as [6]…”

Section: Background Evolution and Perturbation Of Slotheon Field Darkmentioning

confidence: 99%

Perturbations for Slotheon Field Dark Energy and its Evolution

Majumdar¹,

Mukhopadhyay²

2020

Proceedings of European Physical Society Conference on High Energy Physics — PoS(EPS-HEP2019)

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We consider in this work a Slotheon scalar field for Dark Energy. A Slotheon field is inspired by extra dimensional models of Dvali, Gabadadze and Porrati (DGP) related to brane world. In the decoupling limit of this model, the DGP theory in Minkowski space-time is described by a scalar field that obeys a shift symmetry. When extended to curved space time this scalar field is termed as Slotheon field. In this work we calculate general relativistic perturbations by deriving the Dark Energy and matter perturbation equations and solve them numerically. The results are then compared with similar quantities derived from ΛCDM model. It appears that the Slotheon field model for Dark Energy is more akin to Dark energy in ΛCDM model than that in standard Quintessence model. A comparison has also been made between the matter power spectra obtained from Slotheon model and ΛCDM model.

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Late-time acceleration in a slow-moving Galileon field

Cited by 16 publications

References 67 publications

A strategy to measure the dark energy equation of state using the H ii galaxy Hubble function and X-ray active galactic nuclei clustering: preliminary results

A strategy to measure the dark energy equation of state using the H ii galaxy Hubble function and X-ray active galactic nuclei clustering: preliminary results

Addressing the high-f problem in pseudo-Nambu–Goldstone boson dark energy models with dark matter–dark energy interaction

Perturbations for Slotheon Field Dark Energy and its Evolution

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