Possible discrepancies between cosmological and electroweak observables in Higgs Inflation

Abstract

In this work, we revisit the non-minimally coupled Higgs Inflation scenario and investigate its observational viability in light of the current Cosmic Microwave Background, Baryon Acoustic Oscillation and type Ia Supernovae data. We explore the effects of the Coleman-Weinberg approximation to the Higgs potential in the primordial universe, connecting the predictions for the Lagrangian parameters at inflationary scales to the electroweak observables through Renormalization Group methods at two-loop order. Initially, we find that electroweak scale measurements may be dissonant to the limits obtained from the cosmological data sets used in the analysis. Specifically, an ≈ 8σ-discrepancy between the inflationary parameters and the value of the Monte Carlo reconstructed top quark mass is found. However, considering the most recent results obtained by the CMS Collaboration from differential cross-section measurements of the top quark production a good agreement is obtained.

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

“…In this subsection, we list some specific solutions of interest to the community that cannot be classified in the previous sections, whether because they are broad enough to enclose very different scenarios, or they simply have an impact along the whole cosmic history. We refer the reader to the more complete review [48] or the original papers for a more detailed discussion of proposed solutions of the Hubble tension in: inflationary models [1058][1059][1060][1061], self-interacting dark matter [1062], Über-gravity [1063], Nonlocal gravity [1064], Modified Gravity [927,1065], unified fluid [1066], quintessential models [1067], screened fifth forces [1068], Generalized Chaplygin gas models [1069][1070][1071][1072], Viscous Generalized Chaplygin gas [1073], addition of extra SNIa systematic uncertainties with a varying DE [1074], metastable DE [1075][1076][1077], Super-ΛCDM [1078,1079], DM-photon coupling [1080], Local Inhomogeneity [1081], Interaction in the anisotropic Universe [1082], Heisenberg uncertainty [1083,1084], Enhanced Early gravity model [97,1085], CMB monopole temperature [601], Decaying Ultralight Scalar [1086], Decaying coupled fermions [1087], Early mass varying neutrino DE [1088], Neutrino-majoron interactions [1089][1090]…”

Constraining non-minimally coupled β-exponential inflation with CMB data

“…Such a mechanism has proven to be able to solve a number of fine-tuning problems of the Standard Cosmology, and also a theory for the origin of structure in the universe that explains the Cosmic Microwave Background (CMB) anisotropies and the large-scale distribution of galaxies [2][3][4][5]. Currently, cosmological observations give very strong support to the inflationary paradigm, showing a preference for plateau over monomial potentials of the inflaton field φ, but still agreeing with several classes of models (see [6][7][8][9][10][11][12][13][14][15][16] for recent analyses for different classes of models). On the other hand, the possibility of a non-minimal coupling of the inflaton to gravity has been investigated since the first models of inflation [17][18][19].…”

An empirical investigation into cosmological tensions

“…Several possibilities have been investigated, like varying the number of neutrinos species [1,3,4], considering both a closed and an open universe [5][6][7][8][9][10] or also reformulating the H 0 tension as a tension in the CMB monopole temperature T 0 [11]. More in general, a plethora of proposals to alleviate the tension have been studied and here we can roughly classify them into few categories [12] as the early dark energy [13][14][15][16] and late dark energy [17] models, interacting dark energy mechanisms [18][19][20][21][22][23][24][25], models with extra relativistic degrees of freedom [26][27][28][29][30][31][32], models with extra interactions [33][34][35], unified cosmologies [36], modified gravity [37][38][39][40][41][42][43], non-standard inflationary models [4,44], modified recombination history [45], physics of the c...…”