There are currently several energy and luminosity correlations for gamma-ray bursts (GRBs). Some, like the lag-luminosity and variability relations [1] [2] , were obtained from the light curves, while others were obtained from the spectra and include the Amati relation [3] [4] [5] [6] , the Ghirlanda relation [7] , the Yonetoku relation [8] [9] , and the Liang-Zhang relation [10] . The importance of these correlations resides in their potential use as cosmological probes that might help in constraining cosmological models [10] - [16] , and also as tools that might help in probing the physics of GRBs [17] [18] .

Some studies have looked at possible inherent problems that these relations might suffer from, like the circularity problem and selection effects [19] [20] [21] [22] [23] . Other studies have investigated the possible redshift evolution of these correlations [24] - [29] since these relations are typically calibrated over a wide range in redshift (roughly 0.1 < z < 9), and thus it becomes incumbent to study their possible dependence on z, if they are to be utilized as cosmological probes.

The purpose of this paper is to provide a brief review of a well-known GRB energy and luminosity correlation―namely, the Amati relation, and to discuss its potential use as a cosmological probe.

The Amati relation is a correlation between a GRB’s equivalent isotropic energy, , and its intrinsic (i.e., rest-frame) peak energy, , in the nF_n spectrum. It was first discovered by Amati et al. in 2002 and confirmed by later studies [3] [4] [5] [6] . It is necessary to know the redshift, z, of the GRB since is calculated from the observed peak energy, , by the following relation:

The Amati relation is given by:

where K and m are constants, and is in keV. In Amati’s original study, m » 0.5 and K » 95. However, later studies [30] with expanded data samples found mean values of = 0.45 and = 141.

Alternatively, the Amati relation can be expressed logarithmically as:

where the normalization, A, and the slope, B, are constants, and where is the mean value of the intrinsic peak energy for the entire data sample. A recent study [31] involving 65 GRBs found that although the values of A and B fluctuate slightly depending on the redshift range of the sample, the approximate mean values are » 53 and » 1, assuming is measured in units of erg.

Before we can utilize the Amati relation as a cosmological probe, we need to check its robustness. One of the central issues concerning the Amati relation is whether the fitting parameters are constant. A recent study [32] used a data sample of 47 GRBs to investigate the robustness of the Amati relation and to investigate whether the fitting parameters evolve with redshift. The authors found no redshift evolution of the Amati relation. Furthermore, although they found some outliers, they concluded that the Amati relation is genuine and not due to selection effects. This conclusion was confirmed by [31] who used a sample of 65 GRBs taken from [33] to investigate any possible redshift evolution. The authors binned the data after carrying out the proper z-correction and k-correction. They obtained good fits for the binned data and confirmed that the fitting parameters do not evolve with redshift.

Another problem that arises when we try to employ the Amati relation as a cosmological probe is the circularity problem, which refers to the fact that in order to calibrate the relation, one must assume a cosmological model in the first place. Two recent studies [34] [35] looked deeply into this problem and showed that it is essential to take proper account of this issue, otherwise an error of up to 13% could be introduced into the values of the cosmological parameters.

Early attempts to constrain cosmological parameters, like the matter density parameter W_M, had limited success due to the paucity of data points [36] . Recently, however, there has been a revived interest in GRB cosmology mainly due to the increased availability of high caliber data. For instance, a recent study explored the cosmological evolution of 200 Swift GRBs and used the results to put limits on the star formation rate [37] . Other recent studies [38] [39] [40] have investigated how GRBs can be utilized to constrain dark energy, the first stars, and the pre-galactic metal enrichment. The Amati relation and other similar correlations have also taken a recent boost as cosmological probes, since the abundance of high quality data has reduced the extrinsic scatter in these correlations [36] .

Gamma-ray bursts hold great promise as cosmological probes since they can be observed to huge distances (z > 9) and their radiation is unencumbered by any intervening dust. The most effective way of using them as cosmological probes is by utilizing one of the currently available energy and luminosity correlations.

In this brief review we focused on one of these correlations―namely, the Amati relation. It is a correlation between the equivalent isotropic energy and the intrinsic peak energy. Early attempts to employ the Amati relation as a cosmological probe faced several hurdles, like the circularity problem, the extrinsic scatter, and the paucity of data points. However, as high quality data samples have become available, the scatter in the correlation has diminished and the Amati relation has become more robust. In the near future, the Amati relation will be an effective cosmological tool that will shed light on many cosmological issues, like the density parameters and the star formation rate.

The author would like to thank the anonymous referee for the useful remarks that helped improve the paper.

Azzam, W.J. (2016) A Brief Review of the Amati Relation for GRBs. International Journal of Astronomy and Astrophysics, 6, 378-383. http://dx.doi.org/10.4236/ijaa.2016.64030