On the dynamics of a dark sector coupling

Yang, Weiqiang; Pan, Supriya; Mena, Olga; Di Valentino, Eleonora

doi:10.1016/j.jheap.2023.09.001

Cited by 19 publications

(10 citation statements)

References 118 publications

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“…While this paper was in the final stages of preparation ref. [64] appeared which considers interacting dark energy models including an interacting vacuum scenario (which they refer to as ξ 0 IVSA) that coincides with our model where Q = βHV . Their analysis using the same CMB plus Pantheon data matches our own constraints very closely in this case.…”

Section: Jcap01(2023)042mentioning

confidence: 69%

Observational constraints on interacting vacuum energy with linear interactions

Kaeonikhom

Assadullahi

Schewtschenko

et al. 2023

J. Cosmol. Astropart. Phys.

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We explore the bounds that can be placed on interactions between cold dark matter and vacuum energy, with equation of state w = -1, using state-of-the-art cosmological observations. We consider linear perturbations about a simple background model where the energy transfer per Hubble time, Q/H, is a general linear function of the dark matter density, ρc , and vacuum energy, V. We explain the parameter degeneracies found when fitting cosmic microwave background (CMB) anisotropies alone, and show how these are broken by the addition of supernovae data, baryon acoustic oscillations (BAO) and redshift-space distortions (RSD). In particular, care must be taken when relating redshift-space distortions to the growth of structure in the presence of non-zero energy transfer. Interactions in the dark sector can alleviate the tensions between low-redshift measurements of the Hubble parameter, H0 , or weak-lensing, S8 , and the values inferred from CMB data. However these tensions return when we include constraints from supernova and BAO-RSD datasets. In the general linear interaction model we show that, while it is possible to relax both the Hubble and weak-lensing tensions simultaneously, the reduction in these tensions is modest (reduced to less slightly than 4σ and 2σ respectively).

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Section: Jcap01(2023)042mentioning

confidence: 69%

Observational constraints on interacting vacuum energy with linear interactions

Kaeonikhom

Assadullahi

Schewtschenko

et al. 2023

J. Cosmol. Astropart. Phys.

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“…When considering only the best-fit values from the CMB, we find the welldocumented Planck preference for a phantom equation of state [208,209], with the best-fit value reading w = −2.04. Given the well-known degeneracy between the effects produced by a phantom w and increasing the present-day expansion rate of the Universe, interacting phantom models can provide a much larger value of H 0 [147] and, in fact, we obtain a best-fit value H 0 = 103.8 km/s/Mpc. This essentially indicates that, without including datasets at lower redshifts, breaking this line of degeneracy proves challenging and values JCAP05(2024)097 The color map refers to the value of χ 2 JWST so that the color pattern in the figure represents the direction towards which one needs to move in the parameter space to improve the fit to JWST data.…”

Section: Jcap05(2024)097mentioning

confidence: 75%

A double take on early and interacting dark energy from JWST

Forconi,

Giarè,

Mena

et al. 2024

J. Cosmol. Astropart. Phys.

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The very first light captured by the James Webb Space Telescope (JWST) revealed a population of galaxies at very high redshifts more massive than expected in the canonical ΛCDM model of structure formation. Barring, among others, a systematic origin of the issue, in this paper, we test alternative cosmological perturbation histories. We argue that models with a larger matter component Ω m and/or a larger scalar spectral index ns can substantially improve the fit to JWST measurements. In this regard, phenomenological extensions related to the dark energy sector of the theory are appealing alternatives, with Early Dark Energy emerging as an excellent candidate to explain (at least in part) the unexpected JWST preference for larger stellar mass densities. Conversely, Interacting Dark Energy models, despite producing higher values of matter clustering parameters such as σ 8, are generally disfavored by JWST measurements. This is due to the energy-momentum flow from the dark matter to the dark energy sector, implying a smaller matter energy density. Upcoming observations may either strengthen the evidence or falsify some of these appealing phenomenological alternatives to the simplest ΛCDM picture.

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“…Previously C2 has been studied in [17,18]. Recently one can find renewed interest in the interaction from the bulk of recent literature [20][21][22][23]. In [23] the authors use C2 in both M1 and M2.…”

Section: Model Analysismentioning

confidence: 99%

“…Recently one can find renewed interest in the interaction from the bulk of recent literature [20][21][22][23]. In [23] the authors use C2 in both M1 and M2. They constrain their results using latest CMB, BAO and Pantheon data.…”

Section: Model Analysismentioning

confidence: 99%

Some classes of interacting two-fluid model of the expanding universe

Bhattacharya

2024

Phys. Scr.

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We consider interacting dark matter-dark energy models arising out of a general interaction term $Q=f(\rho_{m},\rho_{d},\dot{\rho}_{m},\dot{\rho}_{d}).$ Here $f$ is a functional relation connecting the energy densities $\rho_{m}$ and $\rho_{d}$ and their derivatives w.r.t. time $t.$ In our model we consider two interacting barotropic fluid with constant equation of state $\omega_{m}$ and $\omega_{d}.$ By considering a dynamical interaction between them we trace out the cosmological evolution dynamics of the universe. We analytically solve the model by considering a constant ratio between the two fluids and then track the corresponding analytical results using observational data from the baryon acoustic oscillation measurements, Type Ia supernovae measurements and the local Hubble constant measurements. From this general setting we introduce three different models and nine different interaction function. Our final aim is to set up a comparative analysis of the various class of models under the different interaction function using common theoretical and numerical analysis.

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On the dynamics of a dark sector coupling

Cited by 19 publications

References 118 publications

Observational constraints on interacting vacuum energy with linear interactions

Observational constraints on interacting vacuum energy with linear interactions

A double take on early and interacting dark energy from JWST

Some classes of interacting two-fluid model of the expanding universe

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