A Roadmap to Gamma-Ray Bursts: New Developments and Applications to Cosmology

Luongo, Orlando; Muccino, M.

doi:10.3390/galaxies9040077

Cited by 36 publications

(10 citation statements)

References 260 publications

(379 reference statements)

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“…Amati et al [6] showed that the ΛCDM model is statistically favoured over the wCDM scenario. Moreover, Khadka and Ratra [7] found that the cosmological parameters obtained from GRBs were consistent with baryon acoustic oscillation and Hubble parameter measurements and the GRBs could be used as complementary and outstanding probes to trace dark energy's evolution in support of other indicators [8,9].…”

Section: Introductionmentioning

confidence: 73%

Does the GRB Duration Depend on Redshift?

et al. 2022

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Several hundred gamma-ray burst (GRB) redshifts have been determined to date. One of the other important properties—besides the distance—of the GRBs is the duration of the burst. In this paper, we analyse these two important quantities of the phenomena. In this paper, we map the two-dimensional distribution and explore some suspicious areas. As it is well known that the short GRBs are closer than the others, we search for parts in the Universe where the GRB duration is different from the others. We also analyse whether there are any ranges in the duration where the redshifts differ. We find some suspicious areas, however, no other significant region was found than the short GRB region.

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Section: Introductionmentioning

confidence: 73%

Does the GRB Duration Depend on Redshift?

et al. 2022

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“…Several empirical correlations using parameters of the light curves and spectra have been proposed to standardize the GRBs' luminosity. They include correlations between: (i) the GRB spectrum lag time τ lag and isotropic peak luminosity L (τ lag -L relation) [66]; (ii) the peak energy E p of the νF ν spectrum and the isotropic equivalent energy E iso (E p -E iso relation) [67]; (iii) the time variability V and isotropic peak luminosity (V-L relation) [68]; (iv) the peak energy of the νF ν spectrum and the isotropic peak luminosity (E p -L relation) [69]; (v) the minimum rise time τ RT of the light curve and isotropic peak luminosity (τ RT -L relation) [70]; (vi) the peak energy and collimation-corrected energy E γ (E p -E γ relation) [71,72]; (vii) the peak luminosity, the time at the end of the plateau emission phase τ a , and the luminosity at the end of the plateau phase L a (L-τ a -L a relation-Dainotti 3D fundamental plane) [73][74][75]; and others, e.g., [76][77][78][79][80][81][82][83].…”

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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“…Cosmological models have been compared and cosmological parameter constraints have been determined using various observations, including cosmic microwave background (CMB) anisotropy data, [7], that probe the highredshift Universe, and lower-redshift expansion-rate observations like those we use here. These lower-redshift data sets include better-established probes such as Hubble parameter [H(z)] data that reach to redshift z ∼ 2, and baryon acoustic oscillation (BAO) and type Ia supernova (SN Ia) measurements that reach to z ∼ 2.3, [8][9][10], as well as emerging probes such as H ii starburst galaxy (H iiG) apparent magnitude data that reach to z ∼ 2.5, [11][12][13][14][15][16], quasar angular size (QSO-AS) measurements that reach to z ∼ 2.7, [17][18][19][20][21], reverberationmeasured (RM) Mg ii and C iv quasar (QSO) measurements that reach to z ∼ 3.4, [22][23][24][25][26][27][28], and gamma-ray burst (GRB) data that reach to z ∼ 8.2, [29][30][31][32][33][34][35][36][37][38][39], of which only 118 Amati-correlated (A118) GRBs, with lower intrinsic dispersion, are suitable for cosmological purposes, [37,[40][41][42][43].…”

Section: Introductionmentioning

confidence: 99%

$H_0=69.8\pm1.3$ $\rm{km \ s^{-1} \ Mpc^{-1}}$, $Ω_{m0}=0.288\pm0.017$, and other constraints from lower-redshift, non-CMB and non-distance-ladder, expansion-rate data

Cao¹,

Ratra²

2023

Preprint

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We use updated Type Ia Pantheon+ supernova, baryon acoustic oscillation, and Hubble parameter (now also accounting for correlations) data, as well as new reverberation-measured C iv quasar data, and quasar angular size, H ii starburst galaxy, reverberation-measured Mg ii quasar, and Amaticorrelated gamma-ray burst data to constrain cosmological parameters. We show that these data sets result in mutually consistent constraints and jointly use them to constrain cosmological parameters in six different spatially-flat and non-flat cosmological models. Our analysis provides summary modelindependent determinations of two key cosmological parameters: the Hubble constant, H0 = 69.8 ± 1.3 km s −1 Mpc −1 , and the current non-relativistic matter density parameter, Ωm0 = 0.288 ± 0.017. Our summary error bars are 2.4 and 2.3 times those obtained using the flat ΛCDM model and Planck TT,TE,EE+lowE+lensing cosmic microwave background (CMB) anisotropy data. Our H0 value is very consistent with that from the local expansion rate based on the Tip of the Red Giant Branch data, is 2σ lower than that from the local expansion rate based on Type Ia supernova and Cepheid data, and is 2σ higher than that in the flat ΛCDM model based on Planck TT,TE,EE+lowE+lensing CMB data. Our data compilation shows at most mild evidence for non-flat spatial hypersurfaces, but more significant evidence for dark energy dynamics, 2σ or larger in the spatially-flat dynamical dark energy models we study.

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A Roadmap to Gamma-Ray Bursts: New Developments and Applications to Cosmology

Cited by 36 publications

References 260 publications

Does the GRB Duration Depend on Redshift?

Does the GRB Duration Depend on Redshift?

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

$H_0=69.8\pm1.3$ $\rm{km \ s^{-1} \ Mpc^{-1}}$, $Ω_{m0}=0.288\pm0.017$, and other constraints from lower-redshift, non-CMB and non-distance-ladder, expansion-rate data

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