Early Dark Energy from Massive Neutrinos as a Natural Resolution of the Hubble Tension

Sakstein, Jeremy; Trodden, Mark

doi:10.1103/physrevlett.124.161301

Cited by 246 publications

(167 citation statements)

References 70 publications

(78 reference statements)

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“…[24]; a prototypical model realization goes by the name "early dark energy" (EDE) [25]. Many EDE-like models have been proposed, both in the context of the H 0 tension [25][26][27][28][29][30][31][32][33] and other areas of cosmological phenomenology (e.g., Refs. [34][35][36]).…”

Section: Introductionmentioning

confidence: 99%

Constraining early dark energy with large-scale structure

et al. 2020

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An axion-like field comprising ∼10% of the energy density of the Universe near matter-radiation equality is a candidate to resolve the Hubble tension; this is the "early dark energy" (EDE) model. However, as shown in Hill et al., the model fails to simultaneously resolve the Hubble tension and maintain a good fit to both cosmic microwave background (CMB) and large-scale structure (LSS) data. Here, we use redshift-space galaxy clustering data to sharpen constraints on the EDE model. We perform the first EDE analysis using the full-shape power spectrum likelihood from the Baryon Oscillation Spectroscopic Survey (BOSS), based on the effective field theory (EFT) of LSS. The inclusion of this likelihood in the EDE analysis yields a 25% tighter error bar on H 0 compared to primary CMB data alone, yielding H 0 ¼ 68.54 þ0.52 −0.95 km=s=Mpc (68% C.L.). In addition, we constrain the maximum fractional energy density contribution of the EDE to f EDE < 0.072 (95% C.L.). We explicitly demonstrate that the EFT BOSS likelihood yields much stronger constraints on EDE than the standard BOSS likelihood. Including further information from photometric LSS surveys,the constraints narrow by an additional 20%, yielding H 0 ¼ 68.73 þ0.42 −0.69 km=s=Mpc (68% C.L.) and f EDE < 0.053 (95% C.L.). These bounds are obtained without including local-Universe H 0 data, which is in strong tension with the CMB and LSS, even in the EDE model. We also refute claims that Markov-chain Monte Carlo analyses of EDE that omit SH0ES from the combined dataset yield misleading posteriors. Finally, we show that upcoming Euclid/DESI-like spectroscopic galaxy surveys will greatly improve the EDE constraints. We conclude that current data preclude the EDE model as a resolution of the Hubble tension, and that future LSS surveys can close the remaining parameter space of this model.

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Section: Introductionmentioning

confidence: 99%

Constraining early dark energy with large-scale structure

et al. 2020

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“…Early-time solutions aim to reduce r with essentially two possibilities: (i) a coincidental increase of the Hubble expansion around recombination or (ii) new physics that alters the rate of recombination. Proposals in class (i) include the presence of early dark energy [13][14][15][16][17][18] , extra radiation in either neutrinos [19][20][21][22] or some other dark sector [23][24][25][26][27][28] , and dark energy-dark matter interactions 29 . Proposals in class (ii) include primordial magnetic fields 30 , non-standard recombination 31 , or varying fundamental constants 32,33 .…”

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confidence: 99%

Why reducing the cosmic sound horizon can not fully resolve the Hubble tension

Jedamzik

Pogosian

Zhao

2020

Preprint

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The mismatch between the locally measured expansion rate of the universe and the one inferred from the cosmic microwave background measurements by Planck in the context of the standard ΛCDM, known as the Hubble tension, has become one of the most pressing problems in cosmology. A large number of amendments to the ΛCDM model have been proposed in order to solve this tension. Many of them introduce new physics, such as early dark energy, modifications of the standard model neutrino sector, extra radiation, primordial magnetic fields or varying fundamental constants, with the aim of reducing the sound horizon at recombination r*. We demonstrate here that any model which only reduces r* can never fully resolve the Hubble tension while remaining consistent with other cosmological datasets. We show explicitly that models which operate at lower matter density Ωmh2 run into tension with the observations of baryon acoustic oscillations, while models operating at higher Ωmh2 develop tension with galaxy weak lensing data.

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“…One interesting type of models in this category deals with the scalar field playing the role of early dark energy, viz. the field could behave like a cosmological constant at early times (redshifts z 3000) and then dilute away like radiation or faster at later times [45][46][47][48]. If this were the case, the sound horizon at decoupling would be reduced resulting in a larger H 0 value inferred from BAO and CMB data.…”

Section: Introductionmentioning

confidence: 99%

H0 tension and the string swampland

et al. 2020

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We realize the Agrawal-Obied-Vafa swampland proposal of fading dark matter for solving the H 0 tension by the model of Salam-Sezgin and its string realization of Cvetič-Gibbons-Pope. The model describes a compactification of six-dimensional supergravity with a monopole background on a 2sphere. In four dimensions, there are two scalar fields, X and Y , and the effective potential in the Einstein frame is an exponential with respect to Y times a quadratic polynomial in the field e −X . When making the volume of the 2-sphere large, namely for large values of Y , there appears a tower of states, which according to the infinite distance swampland conjecture becomes exponentially massless. We confront the model with recent cosmological observations. We show that this set up is well equipped to explain the overall data even when considering local measurements of H 0 , and that it can potentially ameliorate the tension between low-redshift observations and measurements of the cosmic microwave background. Indeed, the tower of string states that emerges from the rolling of Y constitutes a portion of the dark matter, and the way in which the X particle and its KK excitations evolve over time (refer to as fading dark matter) is responsible for reducing the H 0 tension.

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Early Dark Energy from Massive Neutrinos as a Natural Resolution of the Hubble Tension

Cited by 246 publications

References 70 publications

Constraining early dark energy with large-scale structure

Constraining early dark energy with large-scale structure

Why reducing the cosmic sound horizon can not fully resolve the Hubble tension

H0 tension and the string swampland

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