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

Abstract

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.

Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies

“…As quintessence models generally lead to w DE > −1 and exacerbate the Hubble constant tension [641,870], these are generally not viable DE models. More generally, DE models with w DE > −1 can be shown to be at odds with H 0 and S 8 tension [871][872][873].…”

“…To solve (or at least relax) the H 0 tension in the context of MG models, instead of modifying the matter content, the gravitational sector is modified in a manner that current cosmic dynamics is derived. In particular, it is easy to argue that Newton's constant needs to decrease as the Universe evolves in order to stand a chance of resolving cosmological tensions [871][872][873]. There has been several proposals in GR that follows this line of thought [19,928].…”

“…However, see Refs. [870,873], where it is argued that DE models in a general class of scalar-tensor theories, including quintessence and a good class of Horndeski theories, perform worse than ΛCDM model as far as the H 0 increasing is concerned. Moreover, a similar result is discussed in Refs.…”

“…• They are purely phenomenological, usually motivated by fine tuned effective scalar field potentials, and a number of these scalar models can be shown to exacerbate tensions [870][871][872][873].…”

Gaussian processes and effective field theory of $f(T)$ gravity under the $H_0$ tension

“…This tension suggests possible deviation from the standard ΛCDM cosmological model, inspiring people to explore the physical reasons behind this phenomenon. In particular, since the new data show greater tension, this issue has again aroused a lot of attention and research [10][11][12][13][14][15][16][17][18][19][20][21][22][23].…”