Zeitschriftenartikel: „Hubble tension“

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Netchitailo, Vladimir S. „Hubble Tension“. Journal of High Energy Physics, Gravitation and Cosmology 08, Nr. 02 (2022): 392–401. http://dx.doi.org/10.4236/jhepgc.2022.82030.

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Molchanov, A. B. „The Hubble Law: Its Relational Justification and the Hubble Tension“. Gravitation and Cosmology 28, Nr. 2 (Juni 2022): 133–38. http://dx.doi.org/10.1134/s0202289322020104.

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Molchanov, A. B. „The Hubble Law: Its Relational Justification and the Hubble Tension“. Gravitation and Cosmology 28, Nr. 2 (Juni 2022): 133–38. http://dx.doi.org/10.1134/s0202289322020104.

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Beltrán Jiménez, Jose, Dario Bettoni und Philippe Brax. „Screening away the H0 tension“. International Journal of Modern Physics D 29, Nr. 14 (05.09.2020): 2043010. http://dx.doi.org/10.1142/s0218271820430105.

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This Essay explores consequences of a dark nonlinear electromagnetic sector in a universe with a net dark charge for matter. The cosmological dynamics can be described by a Lemaître model and can be understood, thanks to a screening mechanism driven by the electromagnetic nonlinearities that suppress the dark force on small scales. Only at low redshift, when the screening scale enters the Hubble horizon, do cosmological structures commence to feel the dark repulsion. This repulsive force enhances the local value of the Hubble constant, thus providing a promising scenario for solving the Hubble tension. Remarkably, the dark electromagnetic interaction can have a crucial impact on peculiar velocities, i.e. introducing a bias in their reconstruction methods, and having the potential to explain the presence of a dark flow.

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Bag, Satadru, Varun Sahni, Arman Shafieloo und Yuri Shtanov. „Phantom Braneworld and the Hubble Tension“. Astrophysical Journal 923, Nr. 2 (01.12.2021): 212. http://dx.doi.org/10.3847/1538-4357/ac307e.

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Abstract Braneworld models with induced gravity exhibit phantom-like behavior of the effective equation of state of dark energy. They can, therefore, naturally accommodate higher values of H 0, preferred by recent local measurements while satisfying the cosmic microwave background constraints. We test the background evolution in such phantom braneworld scenarios with the current observational data sets. We find that the phantom braneworld prefers a higher value of H 0 even without the R19 prior, thereby providing a much better fit to the local measurements. Although this braneworld model cannot fully satisfy all combinations of cosmological observables, among existing dark energy candidates the phantom brane provides one of the most compelling explanations of cosmic evolution.

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Rameez, Mohamed, und Subir Sarkar. „Is there really a Hubble tension?“ Classical and Quantum Gravity 38, Nr. 15 (15.07.2021): 154005. http://dx.doi.org/10.1088/1361-6382/ac0f39.

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Alestas, George, und Leandros Perivolaropoulos. „Late-time approaches to the Hubble tension deforming H(z), worsen the growth tension“. Monthly Notices of the Royal Astronomical Society 504, Nr. 3 (20.04.2021): 3956–62. http://dx.doi.org/10.1093/mnras/stab1070.

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ABSTRACT Many late-time approaches for the solution of the Hubble tension use late time smooth deformations of the Hubble expansion rate H(z) of the Planck18/ΛCDM best fit to match the locally measured value of H0 while effectively keeping the comoving distance to the last scattering surface and Ω0mh2 fixed to maintain consistency with Planck CMB measurements. A well-known problem of these approaches is that they worsen the fit to low z distance probes. Here, we show that another problem of these approaches is that they worsen the level of the Ω0m − σ8 growth tension. We use the generic class of CPL parametrizations corresponding to evolving dark energy equation of state parameter $w(z)=w_0+w_1\frac{z}{1+z}$ with local measurements H0 prior and identify the pairs (w0, w1) that satisfy this condition. This is a generic class of smooth deformations of H(z) that are designed to address the Hubble tension. We show that for these models the growth tension between dynamical probe data and CMB constraints is worse than the corresponding tension of the standard Planck18/ΛCDM model. We justify this feature using a full numerical solution of the growth equation and fit to the data, as well as by using an approximate analytic approach. The problem does not affect recent proposed solutions of the Hubble crisis involving a SnIa intrinsic luminosity transition at zt ≃ 0.01.

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Berechya, Dror, und Ulf Leonhardt. „Lifshitz cosmology: quantum vacuum and Hubble tension“. Monthly Notices of the Royal Astronomical Society 507, Nr. 3 (06.08.2021): 3473–85. http://dx.doi.org/10.1093/mnras/stab2345.

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ABSTRACT Dark energy is one of the greatest scientific mysteries of today. The idea that dark energy originates from quantum vacuum fluctuations has circulated since the late ’60s, but theoretical estimations of vacuum energy have disagreed with the measured value by many orders of magnitude, until recently. Lifshitz theory applied to cosmology has produced the correct order of magnitude for dark energy. Furthermore, the theory is based on well-established and experimentally well-tested grounds in atomic, molecular and optical physics. In this paper, we confront Lifshitz cosmology with astronomical data. We find that the dark–energy dynamics predicted by the theory is able to resolve the Hubble tension, the discrepancy between the observed and predicted Hubble constant within the standard cosmological model. The theory is consistent with supernovae data, Baryon Acoustic Oscillations and the Cosmic Microwave Background. Our findings indicate that Lifshitz cosmology is a serious candidate for explaining dark energy.

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Gonzalez, Mark, Mark P. Hertzberg und Fabrizio Rompineve. „Ultralight scalar decay and the Hubble tension“. Journal of Cosmology and Astroparticle Physics 2020, Nr. 10 (09.10.2020): 028. http://dx.doi.org/10.1088/1475-7516/2020/10/028.

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Vishwakarma, Ram Gopal. „Resolving Hubble tension with the Milne model“. International Journal of Modern Physics D 29, Nr. 14 (Oktober 2020): 2043025. http://dx.doi.org/10.1142/s0218271820430257.

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The recent measurements of the Hubble constant based on the standard [Formula: see text]CDM cosmology reveal an underlying disagreement between the early-Universe estimates and the late-time measurements. Moreover, as these measurements improve, the discrepancy not only persists but becomes even more significant and harder to ignore. The present situation places the standard cosmology in jeopardy and provides a tantalizing hint that the problem results from some new physics beyond the [Formula: see text]CDM model. It is shown that a nonconventional theory — the Milne model — which introduces a different evolution dynamics for the Universe, alleviates the Hubble tension significantly. Moreover, the model also averts some long-standing problems of the standard cosmology, for instance, the problems related with the cosmological constant, the horizon, the flatness, the Big Bang singularity, the age of the Universe and the nonconservation of energy.

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Alexander, Stephon, und Evan McDonough. „Axion-dilaton destabilization and the Hubble tension“. Physics Letters B 797 (Oktober 2019): 134830. http://dx.doi.org/10.1016/j.physletb.2019.134830.

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Adhikari, Saroj, und Dragan Huterer. „Super-CMB fluctuations and the Hubble tension“. Physics of the Dark Universe 28 (Mai 2020): 100539. http://dx.doi.org/10.1016/j.dark.2020.100539.

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Hu, Jian-Ping, und Fa-Yin Wang. „Hubble Tension: The Evidence of New Physics“. Universe 9, Nr. 2 (10.02.2023): 94. http://dx.doi.org/10.3390/universe9020094.

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The ΛCDM model provides a good fit to most astronomical observations but harbors large areas of phenomenology and ignorance. With the improvements in the precision and number of observations, discrepancies between key cosmological parameters of this model have emerged. Among them, the most notable tension is the 4σ to 6σ deviation between the Hubble constant (H0) estimations measured by the local distance ladder and the cosmic microwave background (CMB) measurement. In this review, we revisit the H0 tension based on the latest research and sort out evidence from solutions to this tension that might imply new physics beyond the ΛCDM model. The evidence leans more towards modifying the late-time universe.

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Suyu, Sherry H. „Progress toward an accurate Hubble Constant“. Proceedings of the International Astronomical Union 13, S336 (September 2017): 80–85. http://dx.doi.org/10.1017/s1743921318000133.

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AbstractThe Hubble constant is a key cosmological parameter that sets the present-day expansion rate as well as the age, size, and critical density of the Universe. Intriguingly, there is currently a tension in the measurements of its value in the standard flat ΛCDM model – observations of the Cosmic Microwave Background with the Planck satellite lead to a value of the Hubble constant that is lower than the measurements from the local Cepheids-supernovae distance ladder and strong gravitational lensing. Precise and accurate Hubble constant measurements from independent probes, including water masers, are necessary to assess the significance of this tension and the possible need of new physics beyond the current standard cosmological model. We present the progress toward an accurate Hubble constant determination.

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McGaugh, Stacy S. „Early Galaxy Formation and the Hubble Constant Tension“. Research Notes of the AAS 7, Nr. 2 (14.02.2023): 20. http://dx.doi.org/10.3847/2515-5172/acba9a.

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Abstract Tension between local determinations of the Hubble constant and the value found in fits to the cosmic microwave background (CMB) acoustic power spectrum have emerged as finer angular scales (higher multipoles ℓ) have been measured in the latter. Independent observations indicate that massive galaxies emerged at higher redshift than anticipated in the standard ΛCDM structure formation paradigm. If genuine, these early galaxies would cause excess gravitational lensing of the CMB, adding an anomalous source of power at high ℓ. I suggest that accommodating this anomalous source of power in multiparameter fits might be the root cause of the Hubble tension rather than systematics in local measurements.

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Choudhury, Shouvik Roy, Steen Hannestad und Thomas Tram. „Massive neutrino self-interactions and the Hubble tension“. Journal of Physics: Conference Series 2156, Nr. 1 (01.12.2021): 012016. http://dx.doi.org/10.1088/1742-6596/2156/1/012016.

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Abstract We consider flavour independent neutrino self-interactions among massive neutrinos mediated by a heavy scalar against cosmological data. Such a model had previously shown to have potential in completely resolving the Hubble tension for the very strong interaction case with coupling strength ∼ 109 times the Fermi constant, by delaying the onset of neutrino free-streaming until matter-radiation equality. Our cosmological model consists of a total nine parameters which includes the six ACDM parameters and three parameters related to neutrinos: sum of neutrino masses (Σmν ), neutrino energy density (Neff ), and the effective coupling strength, log10 [GeffMeV2]. With the latest CMB data from the Planck 2018 data release as well as auxiliary data, we find that the region in parameter space with such strong interactions is still present in the posterior distribution. However, high-l polarisation data from the Planck 2018 release disfavours this strongly interacting mode even though it cannot yet be excluded. Our resuts show that the neutrino mass bounds obtained from cosmological data remain robust against when considering neutrino self-interactions. We also find that the high-l polarisation data also does not allow for high values of H 0 that can solve the current Hubble discrepancy, i.e. this model is not a viable solution to the same.

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Schöneberg, Nils, Julien Lesgourgues und Deanna C. Hooper. „The BAO+BBN take on the Hubble tension“. Journal of Cosmology and Astroparticle Physics 2019, Nr. 10 (09.10.2019): 029. http://dx.doi.org/10.1088/1475-7516/2019/10/029.

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Blinov, Nikita, Celeste Keith und Dan Hooper. „Warm decaying dark matter and the hubble tension“. Journal of Cosmology and Astroparticle Physics 2020, Nr. 06 (03.06.2020): 005. http://dx.doi.org/10.1088/1475-7516/2020/06/005.

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Borhanian, Ssohrab, Arnab Dhani, Anuradha Gupta, K. G. Arun und B. S. Sathyaprakash. „Dark Sirens to Resolve the Hubble–Lemaître Tension“. Astrophysical Journal 905, Nr. 2 (21.12.2020): L28. http://dx.doi.org/10.3847/2041-8213/abcaf5.

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Benedetto, E., A. Feoli und A. L. Iannella. „A determination of the Ω0mh2 cosmological parameter without tension“. Modern Physics Letters A 36, Nr. 22 (15.07.2021): 2150157. http://dx.doi.org/10.1142/s0217732321501571.

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Measurements for the expansion rate of the universe disagree. Indeed, local measurements suggest a higher value of the Hubble constant than those performed through the cosmic microwave background. This fact led to a very interesting debate within the scientific community. The paper is not devoted to give solutions to the problem of “Hubble tension”. The aim of this paper is, on the contrary, to deduce the [Formula: see text] cosmological parameter from a theoretical point of view, using only two experimental data: the temperature of CMB today and the temperature of photons near the decoupling time.

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Romano, Antonio Enea. „Hubble trouble or Hubble bubble?“ International Journal of Modern Physics D 27, Nr. 09 (Juli 2018): 1850102. http://dx.doi.org/10.1142/s021827181850102x.

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The recent analysis of low-redshift supernovae (SN) has increased the apparent tension between the value of [Formula: see text] estimated from low and high redshift observations such as the cosmic microwave background (CMB) radiation. At the same time other observations have provided evidence of the existence of local radial inhomogeneities extending in different directions up to a redshift of about [Formula: see text]. About [Formula: see text] of the Cepheids used for SN calibration are directly affected because they are located along the directions of these inhomogeneities. We compute with different methods the effects of these inhomogeneities on the low-redshift luminosity and angular diameter distance using an exact solution of the Einstein’s equations, linear perturbation theory and a low-redshift expansion. We confirm that at low redshift the dominant effect is the nonrelativistic Doppler redshift correction, which is proportional to the volume averaged density contrast and to the comoving distance from the center. We derive a new simple formula relating directly the luminosity distance to the monopole of the density contrast, which does not involve any metric perturbation. We then use it to develop a new inversion method to reconstruct the monopole of the density field from the deviations of the redshift uncorrected observed luminosity distance respect to the [Formula: see text]CDM prediction based on cosmological parameters obtained from large scale observations. The inversion method confirms the existence of inhomogeneities whose effects were not previously taken into account because the [Formula: see text] [G. Lavaux and M. J. Hudson, Mon. Not. R. Astron. Soc. 416 (2011) 2840] density field maps used to obtain the peculiar velocity [J. Carrick et al., Mon. Not. R. Astron. Soc. 450 (2015) 317] for redshift correction were for [Formula: see text], which is not a sufficiently large scale to detect the presence of inhomogeneities extending up to [Formula: see text]. The inhomogeneity does not affect the high redshift luminosity distance because the volume averaged density contrast tends to zero asymptotically, making the value of [Formula: see text] obtained from CMB observations insensitive to any local structure. The inversion method can provide a unique tool to reconstruct the density field at high redshift where only SN data is available, and in particular to normalize correctly the density field respect to the average large scale density of the Universe.

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Kenworthy, W. D’Arcy, Adam G. Riess, Daniel Scolnic, Wenlong Yuan, José Luis Bernal, Dillon Brout, Stefano Casertano, David O. Jones, Lucas Macri und Erik R. Peterson. „Measurements of the Hubble Constant with a Two-rung Distance Ladder: Two Out of Three Ain’t Bad“. Astrophysical Journal 935, Nr. 2 (01.08.2022): 83. http://dx.doi.org/10.3847/1538-4357/ac80bd.

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Abstract The three-rung distance ladder, which calibrates Type Ia supernovae (SNe Ia) through stellar distances linked to geometric measurements, provides the highest precision direct measurement of the Hubble constant. In light of the Hubble tension, it is important to test the individual components of the distance ladder. For this purpose, we report a measurement of the Hubble constant from 35 extragalactic Cepheid hosts measured by the SH0ES team, using their distances and redshifts at cz ≤ 3300 km s−1, instead of any more distant SNe Ia, to measure the Hubble flow. The Cepheid distances are calibrated geometrically in the Milky Way, NGC 4258, and the Large Magellanic Cloud. Peculiar velocities are a significant source of systematic uncertainty at z ∼ 0.01, and we present a formalism for both mitigating and quantifying their effects, making use of external reconstructions of the density and velocity fields in the nearby universe. We identify a significant source of uncertainty originating from different assumptions about the selection criteria of this sample, whether distance or redshift limited, as it was assembled over three decades. Modeling these assumptions yields central values ranging from H 0 = 71.7 to 76.4 km s−1 Mpc−1. Combining the four best-fitting selection models yields H 0 = 72.9 − 2.2 + 2.4 as a fiducial result, at 2.4σ tension with Planck. While SNe Ia are essential for a precise measurement of H 0, unknown systematics in these supernovae are unlikely to be the source of the Hubble tension.

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Wang, Jiaxin, und Xinhe Meng. „Finding possibility of dynamical dark energy with Hubble parameters“. Modern Physics Letters A 29, Nr. 32 (20.10.2014): 1450155. http://dx.doi.org/10.1142/s0217732314501557.

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The Hubble parameter is a critical measurement in cosmology, which contains the most direct information of the cosmic expansion history. Since discrepancy is found between low redshift and high redshift estimations of Hubble constant, we are interested in whether that tension indicates dynamical dark energy. In this paper, we emphasize that the observed Hubble parameters at various redshifts, along with observed Hubble constant, can help us in probing the evolutional behavior of the mysterious dark energy. Null hypothesis tests are carried out with two diagnostic approaches. We find out that, according to the present measurements of Hubble parameters, rejection of constant dark energy is captured at 1σ level from null tests with and without the observed value of Hubble constant.

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Haslbauer, Moritz, Indranil Banik und Pavel Kroupa. „The KBC void and Hubble tension contradict ΛCDM on a Gpc scale − Milgromian dynamics as a possible solution“. Monthly Notices of the Royal Astronomical Society 499, Nr. 2 (23.10.2020): 2845–83. http://dx.doi.org/10.1093/mnras/staa2348.

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ABSTRACT The KBC void is a local underdensity with the observed relative density contrast δ ≡ 1 − ρ/ρ0 = 0.46 ± 0.06 between 40 and 300 Mpc around the Local Group. If mass is conserved in the Universe, such a void could explain the 5.3σ Hubble tension. However, the MXXL simulation shows that the KBC void causes 6.04σ tension with standard cosmology (ΛCDM). Combined with the Hubble tension, ΛCDM is ruled out at 7.09σ confidence. Consequently, the density and velocity distribution on Gpc scales suggest a long-range modification to gravity. In this context, we consider a cosmological MOND model supplemented with $11 \, \rm {eV}/c^{2}$ sterile neutrinos. We explain why this νHDM model has a nearly standard expansion history, primordial abundances of light elements, and cosmic microwave background (CMB) anisotropies. In MOND, structure growth is self-regulated by external fields from surrounding structures. We constrain our model parameters with the KBC void density profile, the local Hubble and deceleration parameters derived jointly from supernovae at redshifts 0.023−0.15, time delays in strong lensing systems, and the Local Group velocity relative to the CMB. Our best-fitting model simultaneously explains these observables at the $1.14{{\ \rm per\ cent}}$ confidence level (2.53σ tension) if the void is embedded in a time-independent external field of ${0.055 \, a_{_0}}$. Thus, we show for the first time that the KBC void can naturally resolve the Hubble tension in Milgromian dynamics. Given the many successful a priori MOND predictions on galaxy scales that are difficult to reconcile with ΛCDM, Milgromian dynamics supplemented by $11 \, \rm {eV}/c^{2}$ sterile neutrinos may provide a more holistic explanation for astronomical observations across all scales.

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Schöneberg, Nils, und Guillermo Franco Abellán. „A step in the right direction? Analyzing the Wess Zumino Dark Radiation solution to the Hubble tension“. Journal of Cosmology and Astroparticle Physics 2022, Nr. 12 (01.12.2022): 001. http://dx.doi.org/10.1088/1475-7516/2022/12/001.

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Abstract The Wess Zumino Dark Radiation (WZDR) model first proposed in [1] shows great promise as a well-motivated simple explanation of the Hubble tension between local and CMB-based measurements, reducing the tension from 4.8σ to around 2.7σ. In this work we investigate the assumptions made in the original proposal and confront the model with additional independent data sets. We show that the original assumptions can have an impact on the overall results but are usually well motivated. If one assumes that the abundance of the WZDR is already produced during times relevant for big bang nucleosynthesis, the ability of the model to ease the Hubble tension is restricted. We further demonstrate that the preference for negative Ω k observed in Planck data remains at a similar level as for the ΛCDM model, while the AL tension is slightly increased. Furthermore, the tension between Planck data for ℓ < 800 and ℓ ≥ 800 is significantly reduced for the WZDR model. The Planck-independent data sets show slightly more permissive bounds on the Hubble parameter, allowing the tension to be further reduced from 2.7σ to 2.1σ (CMB-independent) or 1.9σ (ACT+WMAP). However, no combination shows a large preference for the presence of WZDR. We also investigate whether additional dark radiation-dark matter interactions can help in easing the S 8 tension as well. Assuming all of the dark matter to be interacting and a temperature-independent scattering rate, we find that the CMB data are too restrictive on this additional component as to allow a significant decrease in the clustering.

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Sharov, G. S., und E. S. Sinyakov. „Cosmological models, observational data and tension in Hubble constant“. Mathematical Modelling and Geometry, Nr. 1 (02.03.2020): 1–20. http://dx.doi.org/10.26456/mmg/2020-811.

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We analyze how predictions of cosmological models depend on a choice of described observational data, restrictions on ﬂatness, and how this choice can alleviate the H tension. These eﬀects are demonstrated in the wCDM model in comparison with the standard ΛCDM model. We describe the Pantheon sample observations of Type Ia supernovae, 31 Hubble parameter data points H(z) from cosmic chronometers, the extended sample with 57 H(z) data points and observational manifestations of cosmic microwave background radiation (CMB). For the wCDM and ΛCDM models in the ﬂat case and with spatial curvature, we calculate χfunctions for all observed data in diﬀerent combinations, estimate optimal values of model parameters and their expected intervals. For both considered models the results essentially depend on a choice of data sets. In particular, for the wCDM model with H(z) data, supernovae and CMB the 1σ estimations may vary from H = 67.52km /(s·Mpc) (for all N = 57 Hubble parameter data points) up to H = 70.87 /(s·Mpc) for the ﬂat case (k = 0) and N = 31. These results might be a hint how to alleviate the problem of H tension: diﬀerent estimates of the Hubble constant may be connected with ﬁlters and a choice of observational data.

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Yang, Weiqiang, Supriya Pan, Eleonora Di Valentino, Olga Mena und Alessandro Melchiorri. „2021-H₀ odyssey: closed, phantom and interacting dark energy cosmologies“. Journal of Cosmology and Astroparticle Physics 2021, Nr. 10 (01.10.2021): 008. http://dx.doi.org/10.1088/1475-7516/2021/10/008.

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Abstract Up-to-date cosmological data analyses have shown that (a) a closed universe is preferred by the Planck data at more than 99% CL, and (b) interacting scenarios offer a very compelling solution to the Hubble constant tension. In light of these two recent appealing scenarios, we consider here an interacting dark matter-dark energy model with a non-zero spatial curvature component and a freely varying dark energy equation of state in both the quintessential and phantom regimes. When considering Cosmic Microwave Background data only, a phantom and closed universe can perfectly alleviate the Hubble tension, without the necessity of a coupling among the dark sectors. Accounting for other possible cosmological observations compromises the viability of this very attractive scenario as a global solution to current cosmological tensions, either by spoiling its effectiveness concerning the H0 problem, as in the case of Supernovae Ia data, or by introducing a strong disagreement in the preferred value of the spatial curvature, as in the case of Baryon Acoustic Oscillations.

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Park, Youngsoo, und Eduardo Rozo. „Concordance cosmology?“ Monthly Notices of the Royal Astronomical Society 499, Nr. 4 (01.09.2020): 4638–45. http://dx.doi.org/10.1093/mnras/staa2647.

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ABSTRACT We propose a new intuitive metric for evaluating the tension between two experiments, and apply it to several data sets. While our metric is non-optimal, if evidence of tension is detected, this evidence is robust and easy to interpret. Assuming a flat Lambda cold dark matter (ΛCDM) cosmological model, we find that there is a modest 2.2σ tension between the Dark Energy Survey (DES) Year 1 results and the Planck measurements of the cosmic microwave background. This tension is driven by the difference between the amount of structure observed in the late-time Universe and that predicted from fitting the Planck data, and appears to be unrelated to the tension between Planck and local estimates of the Hubble rate. In particular, combining DES, baryon acoustic oscillations, big bang nucleosynthesis, and supernovae measurements recover a Hubble constant and sound horizon consistent with Planck, and in tension with local distance–ladder measurements. If the tension between these various data sets persists, it is likely that reconciling all current data will require breaking the flat ΛCDM model in at least two different ways: one involving new physics in the early Universe, and one involving new late-time Universe physics.

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Chantavat, T. „The Hubble tension problem with variation of the speed of light from Pantheon supernova dataset“. Journal of Physics: Conference Series 2431, Nr. 1 (01.01.2023): 012082. http://dx.doi.org/10.1088/1742-6596/2431/1/012082.

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Abstract We investigate how the tension with the Hubble parameter between early-time and late-time observations could be alleviated with the deviation in the speed of light model. In order to test the model, the data of 1,048 spectroscopically confirmed type Ia supernova with redshift range 0.01 < z < 2.3 from Pantheon Supernova is analysed. We found that the deviation in the local speed of light Δc/c = (-0.115 ± 5.087) × 10−5 and the temporal deviation in the speed of light (1/c)(dc/dt) = (7.20 ± 23.34) × 10−18 yr−1 when combining the Pantheon supernova dataset with other constraints. Our result shows that the data prefers sightly higher value of the speed of light in the past albeit with a large uncertainty. The model alleviates the Hubble tension problem by reducing the Hubble parameter to 71.72 ± 1.40 km s−1 Mpc−1 closer to the early-time value.

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Castello, Sveva, Marcus Högås und Edvard Mörtsell. „A cosmological underdensity does not solve the Hubble tension“. Journal of Cosmology and Astroparticle Physics 2022, Nr. 07 (01.07.2022): 003. http://dx.doi.org/10.1088/1475-7516/2022/07/003.

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Abstract A potential solution to the Hubble tension is the hypothesis that the Milky Way is located near the center of a matter underdensity. We model this scenario through the Lemaître-Tolman-Bondi formalism with the inclusion of a cosmological constant (ΛLTB) and consider a generalized Gaussian parametrization for the matter density profile. We constrain the underdensity and the background cosmology with a combination of data sets: the Pantheon Sample of type Ia supernovae (both the full catalogue and a redshift-binned version of it), a collection of baryon acoustic oscillations data points and the distance priors extracted from the latest Planck data release. The analysis with the binned supernovae suggests a preference for a -13 % density drop with a size of approximately 300 Mpc, interestingly matching the prediction for the so-called KBC void already identified on the basis of independent analyses using galaxy distributions. The constraints obtained with the full Pantheon Sample are instead compatible with a homogeneous cosmology and we interpret this radically different result as a cautionary tale about the potential bias introduced by employing a binned supernova data set. We quantify the level of improvement on the Hubble tension by analyzing the constraints on the B-band absolute magnitude of the supernovae, which provides the calibration for the local measurements of H 0. Since no significant difference is observed with respect to an analogous fit performed with a standard ΛCDM cosmology, we conclude that the potential presence of a local underdensity does not resolve the tension and does not significantly degrade current supernova constraints on H 0.

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Mörtsell, Edvard, Ariel Goobar, Joel Johansson und Suhail Dhawan. „The Hubble Tension Revisited: Additional Local Distance Ladder Uncertainties“. Astrophysical Journal 935, Nr. 1 (01.08.2022): 58. http://dx.doi.org/10.3847/1538-4357/ac7c19.

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Abstract In a recent paper, we investigated possible systematic uncertainties related to the Cepheid color–luminosity calibration method and their influence on the tension between the Hubble constant as inferred from distances to Type Ia supernovae and the cosmic microwave background as measured with the Planck satellite. Here, we study the impact of other sources of uncertainty in the supernova distance ladder, including Cepheid temperature and metallicity variations, supernova magnitudes, and GAIA parallax distances. Using Cepheid data in 19 Type Ia supernova host galaxies from Riess et al., anchor data from Riess et al., and a set of recalibrated Milky Way Cepheid distances, we obtain H 0 = 71.9 ± 2.2 km s−1 Mpc−1, 2.0σ from the Planck value. Excluding Cepheids with estimated color excesses E ˆ ( V − I ) = 0.15 mag to mitigate the impact of the Cepheid color–luminosity calibration, the inferred Hubble constant is H 0 = 68.1 ± 2.6 km s−1 Mpc−1, removing the tension with the Planck value.

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32

Krishnan, C., R. Mohayaee, E. Ó. Colgáin, M. M. Sheikh-Jabbari und L. Yin. „Does Hubble tension signal a breakdown in FLRW cosmology?“ Classical and Quantum Gravity 38, Nr. 18 (23.08.2021): 184001. http://dx.doi.org/10.1088/1361-6382/ac1a81.

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33

Normann, Ben David, und Iver Håkon Brevik. „Can the Hubble tension be resolved by bulk viscosity?“ Modern Physics Letters A 36, Nr. 27 (07.09.2021): 2150198. http://dx.doi.org/10.1142/s0217732321501984.

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We show that the cosmic bulk viscosity estimated in our previous works is sufficient to bridge the [Formula: see text] value inferred from observations of the early universe with the value inferred from the local (late) universe.

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34

van Putten, Maurice H. P. M. „Accelerated cosmological expansion without tension in the Hubble parameter“. EPJ Web of Conferences 168 (2018): 08005. http://dx.doi.org/10.1051/epjconf/201816808005.

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The H0-tension problem poses a confrontation of dark energy driving latetime cosmological expansion measured by the Hubble parameter H(z) over an extended range of redshifts z. Distinct values H0 ≃ 73 km s–1 Mpcs–1 and H0 ≃ 68 km s–1 Mpcs–1 obtain from surveys of the Local Universe and, respectively, ΛCBM analysis of the CMB. These are representative of accelerated expansion with H′(0) ≃ 0 by [see formula in PDF] and, respectively, H′(0) > 0 in ΛCDM, where [see formula in PDF] is a fundamental frequency of the cosmological horizon in a Friedmann-Robertson-Walker universe with deceleration parameter q(z) = -1 + (1+z)H–1 H′(z). Explicit solution H(z) = H0 [see formula in PDF] and, respectively, H(z) = H0[see formula in PDF] are here compared with recent data on H(z) over 0 ≲ z ≲ 2.The first is found to be free of tension with H0 from local surveys, while the latter is disfavored at 2:7σ A further confrontation obtains in galaxy dynamics by a finite sensitivity of inertia to background cosmology in weak gravity, putting an upper bound of m ≲ 10–30 eV on the mass of dark matter. A C0 onset to weak gravity at the de Sitter scale of acceleration adS = cH(z), where c denotes the velocity of light, can be seen in galaxy rotation curves covering 0 ≲ z ≲ 2 Weak gravity in galaxy dynamics hereby provides a proxy for cosmological evolution.

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35

Mörtsell, Edvard, und Suhail Dhawan. „Does the Hubble constant tension call for new physics?“ Journal of Cosmology and Astroparticle Physics 2018, Nr. 09 (17.09.2018): 025. http://dx.doi.org/10.1088/1475-7516/2018/09/025.

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36

Bengaly, Carlos A. P., Chris Clarkson und Roy Maartens. „The Hubble constant tension with next-generation galaxy surveys“. Journal of Cosmology and Astroparticle Physics 2020, Nr. 05 (29.05.2020): 053. http://dx.doi.org/10.1088/1475-7516/2020/05/053.

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37

Zhdanov, V., und O. Stashko. „Hubble parameter in f(R)-gravity“. Bulletin of Taras Shevchenko National University of Kyiv. Astronomy, Nr. 61 (2020): 22–25. http://dx.doi.org/10.17721/btsnua.2020.61.22-25.

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In view of the famous problem with the “Hubble constant tension” there is a number of approaches to modify the cosmological equations and correspondingly modify Hubble parameter H(z) in order to to relieve the tension between the “early” and “late” Hubble constants. f(R)– gravity is one of such possible modifications. We discuss how to choose the Lagrangian in the f(R)– gravity on account of observational data within the homogeneous isotropic cosmology. The equation is obtained that enable us to derive f(R) for given Hubble parameter H(z). This yields a second order differential equation with corresponding degrees of freedom. If H(z) corresponds to that obtained from usual Friedmann equations, this equation yields a condition for f(R) to mimic the observable quantities of the standard ΛCDM with the above-mentioned freedom. To reduce this freedom on needs additional considerations, which involve the other observable quantities, such as those which appear in considerations of cosmological perturbations on the isotropic and homogeneous background. Also, we consider the reverse problem to find for given f(R). This is fulfilled within an approximation in case of small deviation of f(R) from the General Relativity value.

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38

Greene, Kylar L., und Francis-Yan Cyr-Racine. „Hubble distancing: focusing on distance measurements in cosmology“. Journal of Cosmology and Astroparticle Physics 2022, Nr. 06 (01.06.2022): 002. http://dx.doi.org/10.1088/1475-7516/2022/06/002.

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Abstract The Hubble-Lemaître tension is currently one of the most important questions in cosmology. Most of the focus so far has been on reconciling the Hubble constant value inferred from detailed cosmic microwave background measurement with that from the local distance ladder. This emphasis on one number — namely H 0 — misses the fact that the tension fundamentally arises from disagreements of distance measurements. To be successful, a proposed cosmological model must accurately fit these distances rather than simply infer a given value of H 0. Using the newly developed likelihood package `distanceladder', which integrates the local distance ladder into MontePython, we show that focusing on H 0 at the expense of distances can lead to the spurious detection of new physics in models which change late-time cosmology. As such, we encourage the observational cosmology community to make their actual distance measurements broadly available to model builders instead of simply quoting their derived Hubble constant values.

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39

Stávek, Jiří. „How to Relieve the Hubble Constant Tension? (Earth´s Gravitational Redshift + Earth´s Diurnal Aberration)“. European Journal of Applied Physics 4, Nr. 2 (11.04.2022): 35–39. http://dx.doi.org/10.24018/ejphysics.2022.4.2.164.

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There were published very precise experimental values of the Hubble constant H0 in the range 66 -74 km/s/Mpc during the last decade. There is a very active discussion in the H0 community how to relieve this Hubble constant tension. In our model we have described the cosmological redshift as the expansion of old photons in the Earth´s gravitational field: the joint effect of the Earth´s gravitational redshift and the Earth´s diurnal aberration. This model predicts the value of the Hubble constant on the surface of the Earth EARTHH0 = 66.71 km/s/Mpc and on the board of the Hubble Space Telescope (HST) HSTH0 = 72.34 km/s/Mpc. The value H0 determines the expansion of old photons in the Earth´s gravitational field and not the age of the Universe or the age of that old photon. In order to falsify this model in the spirit of Karl Popper we predict the value of H0 for the surface of the Moon as MOONH0 = 6.62 km/s/Mpc. This experiment for the determination of the value H0 on the Moon´s surface is technically possible with the existing technology during this decade while several advanced countries have plans to realize experiments on the surface of the Moon. This proposed experiment on the surface of the Moon might open a new epoch in the description of our cosmological models.

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Mörtsell, Edvard, Ariel Goobar, Joel Johansson und Suhail Dhawan. „Sensitivity of the Hubble Constant Determination to Cepheid Calibration“. Astrophysical Journal 933, Nr. 2 (01.07.2022): 212. http://dx.doi.org/10.3847/1538-4357/ac756e.

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Abstract Motivated by the large observed diversity in the properties of extragalactic extinction by dust, we reanalyze the Cepheid calibration used to infer the Hubble constant, H 0, from Type Ia supernovae, using Cepheid data in 19 Type Ia supernova host galaxies from Riess et al. and anchor data from Riess et al. Unlike the SH0ES team, we do not enforce a fixed universal color–luminosity relation to correct the Cepheid magnitudes. Instead, we focus on a data-driven method, where the optical colors and near-infrared magnitudes of the Cepheids are used to derive individual color–luminosity relations for each Type Ia supernova host and anchor galaxy. We present two different analyses, one based on Wesenheit magnitudes, resulting in H 0 = 73.2 ± 1.3 km s−1 Mpc−1, a 4.2σ tension with the value inferred from the cosmic microwave background. In the second approach, we calibrate an individual extinction law for each galaxy, with noninformative priors using color excesses, yielding H 0 = 73.9 ± 1.8 km s−1 Mpc−1, in 3.4σ tension with the Planck value. Although the two methods yield similar results, in the latter approach, the Hubble constants inferred from the individual Cepheid absolute distance calibrator galaxies range from H 0 = 68.1 ± 3.5 km s−1 Mpc−1 to H 0 = 76.7 ± 2.0 km s−1 Mpc−1. Taking the correlated nature of H 0 inferred from individual anchors into account, and allowing for individual extinction laws, the Milky Way anchor is in 2.1–3.1 σ tension with the NGC 4258 and Large Magellanic Cloud anchors, depending on prior assumptions regarding the color–luminosity relations and the method used for quantifying the tension.

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41

Gough, Michael Paul. „Information Dark Energy Can Resolve the Hubble Tension and Is Falsifiable by Experiment“. Entropy 24, Nr. 3 (09.03.2022): 385. http://dx.doi.org/10.3390/e24030385.

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We consider the role information energy can play as a source of dark energy. Firstly, we note that if stars and structure had not formed in the universe, elemental bits of information describing the attributes of particles would have exhibited properties similar to the cosmological constant. The Landauer equivalent energy of such elemental bits would be defined in form and value identical to the characteristic energy of the cosmological constant. However, with the formation of stars and structure, stellar heated gas and dust now provide the dominant contribution to information energy with the characteristics of a dynamic, transitional, dark energy. At low redshift, z < ~1.35, this dark energy emulates the cosmological constant with a near-constant energy density, w = −1.03 ± 0.05, and an energy total similar to the mc2 of the universe’s ∼1053 kg of baryons. At earlier times, z > ~1.35, information energy was phantom, differing from the cosmological constant, Λ, with a CPL parameter difference of ∆wo = −0.03 ± 0.05 and ∆wa = −0.79 ± 0.08, values sufficient to account for the H0 tension. Information dark energy agrees with most phenomena as well as Λ, while exhibiting characteristics that resolve many tensions and problems of ΛCDM: the cosmological constant problem; the cosmological coincidence problem; the H0 tension, and the σ8 tension. As this proposed dark energy source is not usually considered, we identify the expected signature in H(a) that will enable the role of information dark energy to be falsified by experimental observation.

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Di Valentino, Eleonora, und Alessandro Melchiorri. „Neutrino Mass Bounds in the Era of Tension Cosmology“. Astrophysical Journal Letters 931, Nr. 2 (26.05.2022): L18. http://dx.doi.org/10.3847/2041-8213/ac6ef5.

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Abstract The measurements of cosmic microwave background (CMB) anisotropies made by the Planck satellite provide extremely tight upper bounds on the total neutrino mass scale (Σm ν < 0.26 eV at 95% C.L.). However, as recently discussed in the literature, the Planck data show anomalies that could affect this result. Here we provide new constraints on neutrino masses using the recent and complementary CMB measurements from the Atacama Cosmology Telescope DR4 and the South Pole Telescope SPT-3G experiments. We found that both the ACT-DR4 and SPT-3G data, when combined with WMAP, mildly suggest a neutrino mass with Σm ν = 0.68 ± 0.31 and 0.46 − 0.36 + 0.14 eV at 68% C.L., respectively. Moreover, when CMB lensing from the Planck experiment is included, the ACT-DR4 data now indicate a neutrino mass above the two standard deviations, with Σ m ν = 0.60 − 0.50 + 0.44 eV at 95% C.L., while WMAP+SPT-3G provides a weak upper limit of Σm ν < 0.37 eV at 68% C.L. Interestingly, these results are consistent with the Planck CMB+lensing constraint of Σ m ν = 0.41 − 0.25 + 0.17 eV at 68% C.L. when variations in the A lens parameter are considered. We also show that these indications are still present after the inclusion of BAO or Type Ia supernova data in extended cosmologies that are usually considered to solve the so-called Hubble tension. In this respect, we note that in these models, CMB+BAO constraints prefer a higher neutrino mass for higher values of the Hubble constant. A combination of ACT-DR4, WMAP, BAO, and constraints on the Hubble constant from the SH0ES collaboration gives Σ m ν = 0.39 − 0.25 + 0.13 eV at 68% C.L. in extended cosmologies.

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Di Valentino, Eleonora, Ankan Mukherjee und Anjan A. Sen. „Dark Energy with Phantom Crossing and the H0 Tension“. Entropy 23, Nr. 4 (29.03.2021): 404. http://dx.doi.org/10.3390/e23040404.

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We investigate the possibility of phantom crossing in the dark energy sector and the solution for the Hubble tension between early and late universe observations. We use robust combinations of different cosmological observations, namely the Cosmic Microwave Background (CMB), local measurement of Hubble constant (H0), Baryon Acoustic Oscillation (BAO) and SnIa for this purpose. For a combination of CMB+BAO data that is related to early universe physics, phantom crossing in the dark energy sector was confirmed at a 95% confidence level and we obtained the constraint H0=71.0−3.8+2.9 km/s/Mpc at a 68% confidence level, which is in perfect agreement with the local measurement by Riess et al. We show that constraints from different combinations of data are consistent with each other and all of them are consistent with phantom crossing in the dark energy sector. For the combination of all data considered, we obtained the constraint H0=70.25±0.78 km/s/Mpc at a 68% confidence level and the phantom crossing happening at the scale factor am=0.851−0.031+0.048 at a 68% confidence level.

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Hall, Alex. „Cosmology from weak lensing alone and implications for the Hubble tension“. Monthly Notices of the Royal Astronomical Society 505, Nr. 4 (31.05.2021): 4935–55. http://dx.doi.org/10.1093/mnras/stab1563.

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ABSTRACT We investigate the origin of Lambda cold dark matter parameter constraints in weak lensing, with a focus on the Hubble constant. We explain why current cosmic shear data are sensitive to the parameter combination $S_8 \propto \sigma _8 \Omega _{\rm m}^{0.5}$, improving upon previous studies through use of the halo model. Motivated by the ongoing discrepancy in measurements of the Hubble constant from high and low redshifts, we explain why cosmic shear provides almost no constraint on H0 by showing how the lensing angular power spectrum depends on physical length-scales in the dark matter distribution. We derive parameter constraints from galaxy lensing in KiDS and cosmic microwave background weak lensing from Planck and SPTpol, separately and jointly, showing how degeneracies between σ8 and Ωm can be broken. Using lensing and big bang nucleosynthesis to calibrate the sound horizon measured in projection by baryon acoustic oscillations gives $H_0 = 67.4 \pm 0.9 \,\, \mathrm{km} \, \mathrm{s}^{-1} \, \mathrm{Mpc}^{-1}$, consistent with previous results from Planck and the Dark Energy Survey. We find that a toy Euclid-like lensing survey provides only weak constraints on the Hubble constant due to degeneracies with other parameters that affect the shape of the lensing correlation functions. If external priors on ns, the baryon density, and the amplitude of baryon feedback are available, then sub-per cent H0 constraints are achievable with forthcoming lensing surveys.

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Tiwari, Prabhakar, Rahul Kothari und Pankaj Jain. „Superhorizon Perturbations: A Possible Explanation of the Hubble–Lemaître Tension and the Large-scale Anisotropy of the Universe“. Astrophysical Journal Letters 924, Nr. 2 (01.01.2022): L36. http://dx.doi.org/10.3847/2041-8213/ac447a.

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Abstract Current cosmological observations point to a serious discrepancy between the observed Hubble parameter obtained using direct versus cosmic microwave background radiation measurements. Besides this so-called Hubble–Lemaître tension, we also find considerable evidence in diverse cosmological observables that indicate violation of the cosmological principle. In this paper, we suggest that both these discrepancies are related and can be explained by invoking superhorizon perturbations in the universe. We implement this by considering a single superhorizon mode and showing that it leads to both a dipole in large-scale structures and a shift in the Hubble–Lemaître parameter. Furthermore, the shift is found to be independent of redshift up to a certain distance. This is nicely consistent with the data.

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Kameli, Hamed, und Shant Baghram. „Mass assembly history of dark matter haloes in the light of H0 tension“. Monthly Notices of the Royal Astronomical Society 511, Nr. 2 (18.01.2022): 1601–8. http://dx.doi.org/10.1093/mnras/stac129.

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ABSTRACT The Hubble tension may introduce a new course of action to revise the standard Lambda cold dark matter (ΛCDM) model to unravel dark energy and dark matter physics. The Hubble parameter can be reconstructed by late-time observations of the background evolution model independently. We relate the reconstructed Hubble parameter to the structure formation and large-scale structure observables in this work. We use excursion set theory to calculate the number density of dark matter haloes and the mass function of progenitors. We obtain results for both the Markov and non-Markov extensions of excursion set theory in the context of spherical and ellipsoidal collapse. We show that the number density of dark matter haloes in the reconstructed model has ∼2σ difference in comparison with the Planck 2018 ΛCDM in the mass range M ≳ 1012 M⊙. We also compare the dark matter halo progenitor mass function with the pair-galaxy statistics and their mass assembly history from observational data of the Hubble Space Telescope Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. Due to complications in distinguishing the ratio of accretion and merger in mass assembly, our result on the pair fraction is for illustration only. However, the ∼5 times more accurate observations will be promising for distinguishing the reconstructed model and the Planck 2018 ΛCDM.

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Shimon, Meir. „Possible resolution of the Hubble tension with Weyl invariant gravity“. Journal of Cosmology and Astroparticle Physics 2022, Nr. 04 (01.04.2022): 048. http://dx.doi.org/10.1088/1475-7516/2022/04/048.

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Abstract We explore cosmological implications of a genuinely Weyl invariant (WI) gravitational interaction. The latter reduces to general relativity in a particular conformal frame for which the gravitational coupling and active gravitational masses are fixed. Specifically, we consider a cosmological model in this framework that is dynamically identical to the standard model (SM) of cosmology. However, kinematics of test particles traveling in the new background metric is modified thanks to a new (cosmological) fundamental mass scale, γ, of the model that emerges as an integration constant of the classical field equations. Since the lapse-function of the new metric is radially-dependent any incoming photon experiences (gravitational) red/blueshift in the comoving frame, unlike in the SM. Distance scales are modified as well due to the scale γ. The claimed 4.4σ tension level between the locally measured Hubble constant, H 0, with SH0ES and the corresponding value inferred from the cosmic microwave background (CMB) could then be significantly alleviated by an earlier-than-thought recombination. Assuming vanishing spatial curvature, either one of the Planck 2018 (P18) or dark energy survey (DES) yr1 data sets subject to the SH0ES prior imply that γ -1 is O(100) times larger than the Hubble scale, H 0 -1. Considering P18+SH0ES or P18+DES+SH0ES data set combinations, the odds against vanishing γ are over 1000:1 and 2000:1, respectively, and the model is strongly favored over the SM with a deviance information criterion (DIC) gain ≳ 10 and ≳ 12, respectively. The H 0 tension is reduced in this model to ∼ 1.5 and 1.3 σ, respectively. Allowing for a non-vanishing spatial curvature, γ -1 halves to O(50) times H 0 -1. The capacity of two other major cosmological probes, baryonic oscillations and type Ia supernovae, SNIa, to distinguish between the models is also discussed. We conclude that the H 0 tension may simply result from a yet unrecognized fundamental symmetry of the gravitational interaction — Weyl invariance.

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Shimon, Meir. „Possible resolution of the Hubble tension with Weyl invariant gravity“. Journal of Cosmology and Astroparticle Physics 2022, Nr. 04 (01.04.2022): 048. http://dx.doi.org/10.1088/1475-7516/2022/04/048.

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Abstract We explore cosmological implications of a genuinely Weyl invariant (WI) gravitational interaction. The latter reduces to general relativity in a particular conformal frame for which the gravitational coupling and active gravitational masses are fixed. Specifically, we consider a cosmological model in this framework that is dynamically identical to the standard model (SM) of cosmology. However, kinematics of test particles traveling in the new background metric is modified thanks to a new (cosmological) fundamental mass scale, γ, of the model that emerges as an integration constant of the classical field equations. Since the lapse-function of the new metric is radially-dependent any incoming photon experiences (gravitational) red/blueshift in the comoving frame, unlike in the SM. Distance scales are modified as well due to the scale γ. The claimed 4.4σ tension level between the locally measured Hubble constant, H 0, with SH0ES and the corresponding value inferred from the cosmic microwave background (CMB) could then be significantly alleviated by an earlier-than-thought recombination. Assuming vanishing spatial curvature, either one of the Planck 2018 (P18) or dark energy survey (DES) yr1 data sets subject to the SH0ES prior imply that γ -1 is O(100) times larger than the Hubble scale, H 0 -1. Considering P18+SH0ES or P18+DES+SH0ES data set combinations, the odds against vanishing γ are over 1000:1 and 2000:1, respectively, and the model is strongly favored over the SM with a deviance information criterion (DIC) gain ≳ 10 and ≳ 12, respectively. The H 0 tension is reduced in this model to ∼ 1.5 and 1.3 σ, respectively. Allowing for a non-vanishing spatial curvature, γ -1 halves to O(50) times H 0 -1. The capacity of two other major cosmological probes, baryonic oscillations and type Ia supernovae, SNIa, to distinguish between the models is also discussed. We conclude that the H 0 tension may simply result from a yet unrecognized fundamental symmetry of the gravitational interaction — Weyl invariance.

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49

Adhikari, Saroj. „The Hubble tension in the non-flat Super−ΛCDM model“. Physics of the Dark Universe 36 (Juni 2022): 101005. http://dx.doi.org/10.1016/j.dark.2022.101005.

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50

Castello, Sveva, Marcus Högås und Edvard Mörtsell. „Erratum: A cosmological underdensity does not solve the Hubble tension“. Journal of Cosmology and Astroparticle Physics 2022, Nr. 09 (01.09.2022): E01. http://dx.doi.org/10.1088/1475-7516/2022/09/e01.

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