Relieving the Hubble Tension with Primordial Magnetic Fields

Jedamzik, Karsten; Pogosian, Levon

doi:10.1103/physrevlett.125.181302

Cited by 179 publications

(110 citation statements)

References 129 publications

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“…Figure 3 shows the best fit values of r d h, H 0 , and S 8 in models from Refs. 13,14,18,23,24,[28][29][30]32 . Note that there are other proposed early-time solutions to the Hubble tension.…”

Section: Resultsmentioning

confidence: 99%

“…Proposals in class (i) include the presence of early dark energy [12][13][14][15][16][17] , extra radiation in either neutrinos [18][19][20][21] or some other dark sector [22][23][24][25][26][27] , and dark energy-dark matter interactions 28 . Proposals in class (ii) include primordial magnetic fields 29 , non-standard recombination 30 , or varying fundamental constants 31,32 . In this work we show that any early-time solution which only changes r ⋆ can never fully resolve the Hubble tension without being in significant tension with either the weak lensing (WL) surveys 33,34 or BAO 35 observations.…”

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confidence: 99%

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

2021

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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 achieve a higher Hubble constant with lower values of matter density Ωmh2 run into tension with the observations of baryon acoustic oscillations, while models with larger Ωmh2 develop tension with galaxy weak lensing data.

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Section: Resultsmentioning

confidence: 99%

mentioning

confidence: 99%

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

2021

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“…Figure 1: Known constraints on IGMF [5,6] and hints of existence of cosmological magnetic field from CMB [7], 21 cm line [12] and baryogenesis [13], compared to the sensitivity of different detection techniques. Black upper bound is from the analysis of CMB signal by [14].…”

Section: Akorochkinmentioning

confidence: 99%

“…However, primordial nature of these fields is yet to be established. [7] have shown that account of the magnetic field driven turbulence on plasma at the epoch of recombination can relax the 4.4 tension between estimates of the Hubble parameter from the Cosmic Microwave Background (CMB) measurement [8] and present-day universe measurements using supernovae type Ia [9] and based on gravitationally lensed systems [10]. The resulting magnetic field strength ∝ 10 −11 G.…”

Section: Introductionmentioning

confidence: 99%

Sensitivity of the gamma-ray method for strong primordial magnetic fields

Korochkin¹,

Kalashev²,

Neronov³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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Primordial magnetic field with the strength in 1-10 pG range can resolve the tension between different measurements of the Hubble constant and provide explanation for the excess opacity in 21 cm line at redshift 15 < < 20, if it is present during recombination and reionisation epochs. This field can also survive in the voids of the Large Scale Structure in the present day universe. We study the sensitivity reach of gamma-ray technique for measurement of such relatively strong cosmological magnetic field using deep exposure(s) of the nearest hard spectrum blazar(s) with CTA telescopes. We show that the gamma-ray measurement method can sense the primordial magnetic field with the strength up to 10 −11 G. Combination of the Cosmic Microwave Background and gamma-ray constraints can thus sense the full range of possible cosmological magnetic fields to confirm or rule out their relevance to the problem of the origin of cosmic magnetic fields, as well as their influence on recombination and reionisation epochs.

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“…Recently in the Ref. [18], authors show that PMFs can be used as a remedy to resolve the Hubble tension between different observations. The present-day amplitude of these MFs is constrained from the big bang nucleosynthesis, formation of structures and cosmic microwave background anisotropies and polarization [17,19,20].…”

Section: Introductionmentioning

confidence: 99%

Constraint on primordial magnetic fields in the light of ARCADE 2 and EDGES observations

Natwariya

2021

Eur. Phys. J. C

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We study the constraints on primordial magnetic fields (PMFs) in the light of the Experiment to Detect the Global Epoch of Reionization Signature (EDGES) low-band observation and Absolute Radiometer for Cosmology, Astrophysics and Diffuse Emission (ARCADE 2). ARCADE 2 observation detected extra-galactic excess radio radiation in the frequency range 3–90 GHz. The enhancement in the radio radiation is also supported by the first station of the Long Wavelength Array (LWA1) in the frequency range 40–80 MHz. The presence of early radiation excess over the cosmic microwave background can not be completely ruled out, and it may explain the EDGES anomaly. In the presence of decaying PMFs, 21 cm differential brightness temperature can modify due to the heating of the gas by decaying magnetic fields, and we can constraint the magnetic fields. For excess radiation fraction ($$A_r$$ A r ) to be LWA1 limit, we show that the upper bound on the present-day magnetic field strength, $$B_0$$ B 0 , on the scale of 1 Mpc is $$\lesssim 3.7$$ ≲ 3.7 nG for spectral index $$n_B=-2.99$$ n B = - 2.99 . While for $$n_B=-1$$ n B = - 1 , we get $$B_0\lesssim 1.1\times 10^{-3}$$ B 0 ≲ 1.1 × 10 - 3 nG. We also discuss the effects of first stars on IGM gas evolution and the allowed value of $$B_0$$ B 0 . For $$A_r$$ A r to be LWA1 limit, we get the upper constraint on magnetic field to be $$B_0(n_B=-2.99)\lesssim 4.9\times 10^{-1}$$ B 0 ( n B = - 2.99 ) ≲ 4.9 × 10 - 1 nG and $$B_0(n_B=-1)\lesssim 3.7\times 10^{-5}$$ B 0 ( n B = - 1 ) ≲ 3.7 × 10 - 5 nG. By decreasing excess radiation fraction below the LWA1 limit, we get a more stringent bound on $$B_0$$ B 0 .

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Relieving the Hubble Tension with Primordial Magnetic Fields

Cited by 179 publications

References 129 publications

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

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

Sensitivity of the gamma-ray method for strong primordial magnetic fields

Constraint on primordial magnetic fields in the light of ARCADE 2 and EDGES observations

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