Some statistical remarks on the giant GRB ring

Balázs, L. G.; Rejtő, Lídia; Tusnády, Gábor

doi:10.1093/mnras/stx2550

Cited by 22 publications

(38 citation statements)

References 118 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Lately, with the help of multi-and uni-variate statistical analysis techniques an intermediate group was found [3,4,5,6,7,8,9,10,11,12,13]. Furthermore, recent publications have discovered large structures based on GRBs: the HerculesBorealis great wall at z ≈ 2 [14,15] and the Giant GRB ring at z ≈ 0.8 [16,17]. More GRBs with known redshift are necessary to understand the genesis of these structures.…”

Section: Introductionmentioning

confidence: 99%

New results in applying the machine learning to GRB redshift estimation

Rácz¹,

Ribli²,

Bagoly

et al. 2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

View full text Add to dashboard Cite

Section: Introductionmentioning

confidence: 99%

New results in applying the machine learning to GRB redshift estimation

Rácz¹,

Ribli²,

Bagoly

et al. 2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

View full text Add to dashboard Cite

“…Nowadays using multi-and uni-variate statistical analysis techniques an intermediate group was found [3,4,5,6,7,8,9,10,11,12]. Moreover, more huge structures have been published recently which were created by GRBs: the Hercules-Borealis great wall at z ≈ 2 [13,14] and the GRB ring at z ≈ 0.8 [15,16]. The genesis of these structures is not known yet.…”

Section: Introductionmentioning

confidence: 99%

Spectral classification and variation of Fermi GRBs

Rácz¹,

Balázs²,

Toth³

et al. 2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

View full text Add to dashboard Cite

The Fermi GBM catalog contains general physical quantities of the observed objects and also estimated parameters (peak energy, spectral indices, intensity) from four fitted spectral models (Band, smoothly broken power law, Comptonized, power law) for the peak flux and the fluence. We studied the nature of the errors of the peak flux, the fluence, and duration parameters. We have found a linear correlation between the logarithm of the measured quantities and their error bars. We interpret our results as an indication that the peak flux, fluence and duration follow a Poissonic distribution.

show abstract

“…Focusing again on the growing mode D (+) 1 (28) and using the definitions (9) and (32), as well as the Friedmann equations (2), we find…”

Section: Effective Screening Length To Rule Them Allmentioning

confidence: 92%

Duel of cosmological screening lengths

Canay

Eingorn

2020

Physics of the Dark Universe

View full text Add to dashboard Cite

Two distinct perturbative approaches have been recently formulated within General Relativity, arguing for the screening of gravity in the ΛCDM Universe. In this paper we compare them and show that the offered screening concepts, each characterized by its own interaction range, can peacefully coexist. Accordingly, we advance a united scheme, determining the gravitational potential at all scales, including regions of nonlinear density contrasts, by means of a simple Helmholtz equation with the effective cosmological screening length. In addition, we claim that cosmic structures may not grow at distances above this Yukawa range and confront its current value with dimensions of the largest known objects in the Universe.As the science rapidly progresses, higher and higher accuracy of observations is achieved. For instance, such a future space mission as Euclid [3,4,5] is designed to probe the Universe expansion with unprecedented precision and impose new restrictions on dark energy, dark matter, and various cosmological parameters. In this connection, the legitimate demand for an advanced theory soars up too. In particular, it is quite natural to expect that Newtonian gravity is modified at large distances and ultimately reconciled with the standard relativistic perturbation theory. By dint of our narration, we aim at sparking interest in two distinct approaches [6,7] relying on General Relativity, which argue that gravity is actually screened, ceasing to be longrange far enough from its every single source. Hereinafter this Yukawa-type screening is sometimes called "cosmological" or "cosmic", since it originates from the presence of the cosmological background.Both cosmic screening approaches have been formulated in the framework of the standard ΛCDM (Λ cold dark matter) model, which is consistent with the observational data [8], though it is noteworthy that currently there is tension between the direct local measurement of the Hubble constant and the value of this very constant following from the Planck data on cosmic microwave background temperature and polarization (see, e.g., [9,10,11]). Furthermore, both original papers [6,7] focus on the matter-and Λ-dominated stages of the Universe evolution, so radiation and relativistic neutrinos are disregarded (though the results of [6] have been subsequently generalized to the case of additional perfect fluids with linear and nonlinear equations of state [12,13,14], as well as to the cases of nonzero spatial curvature [15], f (R) gravity [16] and the phantom braneworld model [17]).From the mathematical point of view, the cosmological Yukawa screening inevitably comes into play when the Einstein equation for the gravitational potential (scalar perturbation) is reduced to the Helmholtz equation, which replaces its popular rival of Poisson type. Meanwhile, the underlying physical reasons and resulting screening ranges are different in [6] and [7]. The scheme of [6] (see additionally [18,19]) is rooted in the so-called discrete cosmology studying how discrete gravitating mass...

show abstract

Some statistical remarks on the giant GRB ring

Cited by 22 publications

References 118 publications

New results in applying the machine learning to GRB redshift estimation

New results in applying the machine learning to GRB redshift estimation

Spectral classification and variation of Fermi GRBs

Duel of cosmological screening lengths

Contact Info

Product

Resources

About