Testing dark energy after pre-recombination early dark energy

Wang, Hao; Piao, Yun-Song

doi:10.48550/arxiv.2201.07079

Cited by 2 publications

(2 citation statements)

References 81 publications

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“…See Fig. 6 in [58] for an attempt to modify late dark energy. However, it is important to note that the lensing anomaly is only a naive reflection of the oscillation pattern on this Planck TT spectrum.…”

Section: Why Does the High-part Of Planck Tt Not Favor The Ede Model?mentioning

confidence: 99%

Towards early dark energy and $n_s$=1 with Planck, ACT and SPT

Jiang,

Piao

2022

Preprint

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We investigate the constraints on early dark energy (EDE) by combining the most recent CMB observations available, ACT DR4, SPT-3G, and Planck2018 ( TT,max = 1000) data. This combined CMB dataset favors non-zero EDE fractions and large Hubble constants, i.e. H 0 = 72.3(73.4) +2.2 −1.7 and 73.32(72.98) +0.68 −0.95 km/s/Mpc for axion-like EDE and AdS-EDE, respectively. The inclusion of BAO+Pantheon data has little efffect on the results. The axion-like EDE can fit the data significantly better (∆χ 2 −10) than ΛCDM, which is mainly driven by the ACT data. It is found again that if the current H 0 measured locally is correct, complete resolution of the Hubble tension seems to be pointing towards a scale invariant Harrison-Zeldovich spectrum of primordial scalar perturbation, i.e. n s = 1 for H 0 ∼ 73 km/s/Mpc.

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Section: Why Does the High-part Of Planck Tt Not Favor The Ede Model?mentioning

confidence: 99%

Towards early dark energy and $n_s$=1 with Planck, ACT and SPT

Jiang,

Piao

2022

Preprint

Self Cite

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“…One can allow for late-time evolving DE with EDE, but late universe observations are largely consistent with Λ[90]. Interestingly, EDE may also be consistent with a scale invariant spectral index, n s ≈ 1[91].…”

mentioning

confidence: 94%

Is Local $H_0$ At Odds With Dark Energy EFT?

Lee,

Colgáin

et al. 2022

Preprint

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Local H 0 determinations currently fall in a window between H 0 ∼ 70 km/s/Mpc (TRGB) and H 0 ∼ 76 km/s/Mpc (Tully-Fisher). In contrast, BAO data calibrated in an early ΛCDM universe are largely consistent with Planck-ΛCDM, H 0 ∼ 67.5 km/s/Mpc. Employing a generic two parameter family of evolving equations of state (EoS) for dark energy (DE) w DE (z) and mock BAO data, we demonstrate that if i) w DE (z = 0) < −1 and ii) integrated DE density less than ΛCDM, then H 0 increases. EoS that violate these conditions at best lead to modest H 0 increases within 1σ. Tellingly, Quintessence and K-essence satisfy neither condition, whereas coupled Quintessence can only satisfy ii). Beyond these seminal DE Effective Field Theories (EFTs), we turn to explicit examples. Working model agnostically in an expansion in powers of redshift z, we show that Brans-Dicke/ f (R) and Kinetic Gravity Braiding models within the Horndeski class can lead to marginal and modest increases in H 0 , respectively. We confirm that as far as increasing H 0 is concerned, no DE EFT model can outperform the phenomenological two parameter family of the DE models. Evidently, the late universe may no longer be large enough to accommodate H 0 , BAO and DE described by EFT.

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Testing dark energy after pre-recombination early dark energy

Cited by 2 publications

References 81 publications

Towards early dark energy and $n_s$=1 with Planck, ACT and SPT

Towards early dark energy and $n_s$=1 with Planck, ACT and SPT

Is Local $H_0$ At Odds With Dark Energy EFT?

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