Gamma-Ray Burst Constraints on Cosmological Models from the Improved Amati Correlation

Liu, Yang; Liang, Nan; Xie, Xiaoyao; Yuan, Zunli; Yu, Hongwei; Wu, Puxun

doi:10.3847/1538-4357/ac7de5

Cited by 25 publications

(8 citation statements)

References 90 publications

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“…We find that the H 0 value from GRBs at high redshift and OHD (h = -+ 0.677 0.029 0.029 ) seem to favor the one from the Planck cosmic microwave background (CMB) observations, which is consistent with previous analyses (Liu et al 2022b). We also find the Ω m value of our results for the flat ΛCDM model with GRBs at high redshift and OHD (W = Finally, we also use the A219 and A118 data set to constrain the ΛCDM and wCDM models by using the method of simultaneous fitting.…”

Section: Constraints On Cosmological Modelssupporting

confidence: 91%

“…For the Amati relation, the authors compile a data set of 118 bursts (the A118 sample), including recent Fermi observations samples from the total 220 GRBs (the A220 sample) with the smallest intrinsic dispersion, which is suitable for constraining cosmological parameters. With the A220 and the A118 GRB samples, Cao et al (2022aCao et al ( , 2022b) have used the Amati relation in conjunction with the Dainotti-correlated GRB data sets 6 compiled recently by Hu et al (2021) and Wang et al (2022) to constrain cosmological model parameters; Liu et al (2022aLiu et al ( , 2022b have proposed the improved Amati relations, which contains a redshift-dependent term, via a powerful statistical tool called copula.…”

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confidence: 99%

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Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae

Liang

Xie

et al. 2022

ApJ

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In this paper, we calibrate the Amati relation (the E p–E iso correlation) of gamma-ray bursts (GRBs) in a cosmology-independent way. By using a Gaussian process to reconstruct the smoothed luminosity distance from the Pantheon type Ia supernovae sample, we utilize the reconstructed results to calibrate the E p–E iso correlation with the Markov Chain Monte Carlo method and construct a Hubble diagram with the A220 GRB data, in which there are A118 GRB data with the higher qualities appropriate for cosmological purposes. With 98 GRBs at 1.4 < z ≤ 8.2 in the A118 sample and the observed Hubble data, we obtain Ωm = 0.346 − 0.069 + 0.048 , h = 0.677 − 0.029 + 0.029 for the flat ΛCDM model, and Ωm = 0.314 − 0.055 + 0.072 , h = 0.705 − 0.069 + 0.055 , w = − 1.23 − 0.64 + 0.33 for the flat wCDM model, which are consistent with those from fitting the coefficients of the Amati relation and the cosmological parameters simultaneously.

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Section: Constraints On Cosmological Modelssupporting

confidence: 91%

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confidence: 99%

Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae

Liang

Xie

et al. 2022

ApJ

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“…Recently, copula is used successfully in GRB cosmology and gives an improved Amati correlation of GRBs (Liu et al 2022a). Utilizing this improved Amati correlation to calibrate GRBs, the GRB data can give cosmological results, which are consistent with what were obtained from other popular data (Liu et al 2022b).…”

Section: Introductionsupporting

confidence: 81%

Redshift-evolutionary X-Ray and UV Luminosity Relation of Quasars from Gaussian Copula

Wang

Liu

Yuan

et al. 2022

ApJ

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We construct a three-dimensional and redshift-evolutionary X-ray and ultraviolet (L X –L UV ) luminosity relation for quasars from the powerful statistic tool called copula, and find that the constructed L X –L UV relation from copula is more viable than the standard one and the observations favor the redshift-evolutionary relation more than 3σ. The Akaike and Bayes information criterions indicate that the quasar data support strongly the three-dimensional L X –L UV relation. Our results show that the quasars can be regarded as a reliable indicator of the cosmic distance if the L X –L UV relation from copula is used to calibrate quasar data.

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“…A cosmological model is typically used to standardize GRB correlations, which leads to the circularity problem (i.e., using a model to calibrate data and using the data to test the model). Several methods to avoid this problem were discussed by Liu et al [84]. They used the Amati correlation, which connects the spectral peak energy E P and isotropic equivalent radiated energy E iso [85], and improved it by employing the Gaussian copula statistical tool on Amati correlation.…”

Section: Gamma-ray Bursts Hubble Diagrammentioning

confidence: 99%

Constraining Coupling Constants’ Variation with Supernovae, Quasars, and GRBs

Gupta

2023

Symmetry

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Dirac, in 1937, proposed the potential variation of coupling constants derived from his large numbers hypothesis. Efforts have continued since then to constrain their variation by various methods, including astrophysical and cosmological observations. We briefly discuss several methods used for the purpose while focusing primarily on the use of supernovae type 1a, quasars, and gamma-ray bursts as cosmological probes for determining cosmological distances. Supernovae type Ia (SNeIa) are considered the best standard candles since their intrinsic luminosity can be determined precisely from their light curves. However, they have only been observed up to about redshift z = 2.3, mostly at z ≤ 1.5. Quasars are the brightest non-transient cosmic sources in the Universe. They have been observed up to z = 7.5. Certain types of quasars can be calibrated well enough for their use as standard candles but with a higher degree of uncertainty in their intrinsic luminosity than SNeIa. Gamma-ray bursts (GRBs) are even brighter than quasars, and they have been observed up to z = 9.4. They are sources of highly transient radiation lasting from tens of milliseconds to several minutes and, in rare cases, a few hours. However, they are even more challenging to calibrate as standard candles than quasars. Both quasars and GRBs use SNeIa for distance calibration. What if the standard candles’ intrinsic luminosities are affected when the coupling constants become dynamic and depend on measured distances? Assuming it to be constant at all cosmic distances leads to the wrong constraint on the data-fitted model parameters. This paper uses our earlier finding that the speed of light c, the gravitational constant G, the Planck constant h, and the Boltzmann constant k vary in such a way that their variation is interrelated as \({G \sim c^{3} \sim h^{3} \sim k^{3/2}}\) with \({\overset{.}{G}/G = 3\overset{.}{c}/c = 3\overset{.}{h}/h = 1.5\overset{.}{k}/k}\) = 3.90(±0.04) × \({10^{-10}}\) yr\({^{-1}}\) and corroborates it with SNeIa, quasars, and GRBs observational data. Additionally, we show that this covarying coupling constant model may be better than the standard \({\Lambda}\)CDM model for using quasars and GRBs as standard candles and predict that the mass of the GRBs scales with z as \({((1+z)^{1/3}-1)}\). Noether’s symmetry on the coupling constants is now transferred effectively to the constant in the function relating to their variation.

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Gamma-Ray Burst Constraints on Cosmological Models from the Improved Amati Correlation

Cited by 25 publications

References 90 publications

Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae

Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae

Redshift-evolutionary X-Ray and UV Luminosity Relation of Quasars from Gaussian Copula

Constraining Coupling Constants’ Variation with Supernovae, Quasars, and GRBs

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