Anomalies in physical cosmology

Peebles, P. J. E.

doi:10.1016/j.aop.2022.169159

Cited by 49 publications

(27 citation statements)

References 143 publications

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“…This appears to be the case at present. See discussions in the literature (e.g., Famaey & McGaugh 2012;Kroupa 2012;Bull et al 2016;Bullock & Boylan-Kolchin 2017;Di Valentino et al 2021;Abdalla et al 2022;Banik & Zhao 2022;Kroupa et al 2022;Peebles 2022;Perivolaropoulos & Skara 2022), although not all authors have similar views.…”

Section: Theoretical Implications Of the Gravitational Anomalymentioning

confidence: 99%

“…The observed deviation of the internal kinematics of galaxies and galaxy clusters from the Newtonian prediction is usually attributed to unidentified dark matter (DM). This has been the most popular interpretation of the astronomical data backed by the "right" amount of DM in the universe inferred from the standard cosmology based on general relativity (Peebles 2022).…”

Section: Introductionmentioning

confidence: 99%

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Breakdown of the Newton–Einstein Standard Gravity at Low Acceleration in Internal Dynamics of Wide Binary Stars

Chae¹

2023

ApJ

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A gravitational anomaly is found at weak gravitational acceleration g N ≲ 10−9 m s−2 from analyses of the dynamics of wide binary stars selected from the Gaia DR3 database that have accurate distances, proper motions, and reliably inferred stellar masses. Implicit high-order multiplicities are required and the multiplicity fraction is calibrated so that binary internal motions agree statistically with Newtonian dynamics at a high enough acceleration of ≈10−8 m s−2. The observed sky-projected motions and separation are deprojected to the 3D relative velocity v and separation r through a Monte Carlo method, and a statistical relation between the Newtonian acceleration g N ≡ GM/r 2 (where M is the total mass of the binary system) and a kinematic acceleration g ≡ v 2/r is compared with the corresponding relation predicted by Newtonian dynamics. The empirical acceleration relation at ≲10−9 m s−2 systematically deviates from the Newtonian expectation. A gravitational anomaly parameter δ obs−newt between the observed acceleration at g N and the Newtonian prediction is measured to be: δ obs−newt = 0.034 ± 0.007 and 0.109 ± 0.013 at g N ≈ 10−8.91 and 10−10.15 m s−2, from the main sample of 26,615 wide binaries within 200 pc. These two deviations in the same direction represent a 10σ significance. The deviation represents a direct evidence for the breakdown of standard gravity at weak acceleration. At g N = 10−10.15 m s−2, the observed to Newton-predicted acceleration ratio is g obs / g pred = 10 2 δ obs − newt = 1.43 ± 0.06 . This systematic deviation agrees with the boost factor that the AQUAL theory predicts for kinematic accelerations in circular orbits under the Galactic external field.

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Section: Theoretical Implications Of the Gravitational Anomalymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Breakdown of the Newton–Einstein Standard Gravity at Low Acceleration in Internal Dynamics of Wide Binary Stars

Chae¹

2023

ApJ

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“…Some of these challenges pointing to preferred directions on large cosmological scales include the quasar dipole [2][3][4][5][6], the radio galaxy dipole [7][8][9], the bulk velocity flow [10][11][12][13], the dark velocity flow [14], the CMB anomalies [15,16], the galaxy spin alignment [17][18][19], the galaxy cluster anisotropies [20], and a possible SnIa dipole [21,22]. These observational challenges of the CP may be indirectly connected with other tensions of the standard ΛCDM model including the Hubble [23][24][25] and growth ten- * leandros@uoi.gr sions [26][27][28][29] where the best fit parameter values of the model H 0 and σ 8 appear to be inconsistent when probed by different observational data. These tensions may indicate that a new degree of freedom [30][31][32][33][34][35][36] is required to be introduced in the ΛCDM model.…”

Section: Introductionmentioning

confidence: 99%

On the homogeneity of SnIa absolute magnitude in the Pantheon+ sample

Perivolaropoulos

Skara

2023

Monthly Notices of the Royal Astronomical Society

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We have analysed the Pantheon+ sample using a new likelihood model that replaces the single SnIa absolute magnitude parameter M used in the standard likelihood model of Brout et. al. (2022) with two absolute magnitude parameters M<, M> and a transition distance dcrit that determines the distance at which M changes from M< to M>. The use of this likelihood dramatically changes the quality of fit to the Pantheon+ sample for a ΛCDM background by Δχ2 = −19.6. The tension between the M< and M> best fit values is at a level more than 3σ with a best fit dcrit very close to 20 Mpc. The origin of this improvement of fit and M< − M> tension is that the new likelihood model, successfully models two signals hidden in the data: 1. The volumetric redshift scatter bias systematic and 2. A mild signal for a change of intrinsic SnIa luminosity at about 20 Mpc. This interpretation of the results is confirmed by truncating the z < 0.01 Hubble diagram data from the Pantheon+ data where the above systematic is dominant and showing that the M< − M> tension decreases from above 3σ to a little less than 2σ. It is also confirmed by performing a Monte Carlo simulation which shows that the maximum significance of the SnIa luminosity transition ($\Sigma \equiv \frac{|M_>-M_<|}{\sqrt{\sigma _{M_>}^2+\sigma _{M_<}^2}}$) in the real data, is larger than the corresponding maximum significance of $94{{\%}}$ of the corresponding homogeneous simulated samples.

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“…On the other hand, given the large scatter of the H I scaling relations found in previous studies, typically 0.2-0.3 dex in log 10 (M H I /M * ), one can expect that some galaxies will deviate significantly from the average relations. Studies of galaxies with H I anomalies should in principle provide insights into the physical processes that drive gas-related star formation and quenching, and probably also cosmological models (e.g., Peebles 2022). In this regard, there has been a rich history of studies on the H I content of early-type galaxies (ETGs; e.g., Knapp et al 1985;Wardle & Knapp 1986;Bregman et al 1992;Morganti et al 2006;di Serego Alighieri et al 2007;Grossi et al 2009;Serra et al 2012;Young et al 2014).…”

Section: Introductionmentioning

confidence: 99%

On the Existence, Rareness, and Uniqueness of Quenched H i-rich Galaxies in the Local Universe

Li,

et al. 2024

ApJ

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Using data from ALFALFA, xGASS, H i-MaNGA, and the Sloan Digital Sky Survey (SDSS), we identify a sample of 47 “red but H i-rich” (RR) galaxies with near-UV (NUV) − r > 5 and unusually high H i-to-stellar mass ratios. We compare the optical properties and local environments between the RR galaxies and a control sample of “red and H i-normal” (RN) galaxies that are matched in stellar mass and color. The two samples are similar in the optical properties typical of massive red (quenched) galaxies in the local Universe. The RR sample tends to be associated with slightly lower-density environments and has lower clustering amplitudes and smaller neighbor counts at scales from several hundred kiloparsecs to a few megaparsecs. The results are consistent with the RR galaxies being preferentially located at the center of low-mass halos, with a median halo mass ∼1012 h −1 M ⊙ compared to ∼1012.5 h −1 M ⊙ for the RN sample. This result is confirmed by the SDSS group catalog, which reveals a central fraction of 89% for the RR sample, compared to ∼60% for the RN sample. If assumed to follow the H i size–mass relation of normal galaxies, the RR galaxies have an average H i-to-optical radius ratio of R HI/R 90 ∼ 4, four times the average ratio for the RN sample. We compare our RR sample with similar samples in previous studies, and quantify the population of RR galaxies using the SDSS complete sample. We conclude that the RR galaxies form a unique but rare population, accounting for only a small fraction of the massive quiescent galaxy population. We discuss the formation scenarios of the RR galaxies.

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Anomalies in physical cosmology

Cited by 49 publications

References 143 publications

Breakdown of the Newton–Einstein Standard Gravity at Low Acceleration in Internal Dynamics of Wide Binary Stars

Breakdown of the Newton–Einstein Standard Gravity at Low Acceleration in Internal Dynamics of Wide Binary Stars

On the homogeneity of SnIa absolute magnitude in the Pantheon+ sample

On the Existence, Rareness, and Uniqueness of Quenched H i-rich Galaxies in the Local Universe

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