Gamma Ray Burst afterglow and prompt-afterglow relations: An overview

Abstract

The mechanism responsible for the afterglow emission of Gamma Ray Bursts (GRBs) and its connection to the prompt γ-ray emission is still a debated issue. Relations between intrinsic properties of the prompt or afterglow emission can help to discriminate between plausible theoretical models of GRB production. Here we present an overview of the afterglow and prompt-afterglow two parameter relations, their physical interpretations, their use as redshift estimators and as possible cosmological tools. A similar task has already been correctly achieved for Supernovae (SNe) Ia by using the peak magnitude-stretch relation, known in the literature as the Phillips relation (Phillips 1993). The challenge today is to make GRBs, which are amongst the farthest objects ever observed, standardizable candles as the SNe Ia through well established and robust relations. Thus, the study of relations amongst the observable and physical properties of GRBs is highly relevant together with selection biases in their physical quantities. Therefore, we describe the state of the art of the existing GRB relations, their possible and debated interpretations in view of the current theoretical models and how relations are corrected for selection biases. We conclude that only after an appropriate evaluation and correction for selection effects can GRB relations be used to discriminate among the theoretical models responsible for the prompt and afterglow emission and to estimate cosmological parameters.

The Correlation between Isotropic Energy and Duration of Gamma-Ray Bursts

“…Because there are many models for interpreting the physical mechanism of GRBs, it is essential to statistically analyze basic properties of GRBs. Some empirical correlations have been found (Wang et al 2015;Dainotti & Del Vecchio 2017;Dainotti & Amati 2018;), e.g. the isotropic energy and spectral peak energy correlation E iso − E p (Amati et al 2002;Wang et al 2016), the correlation between E iso , spectral peak energy E p and rest-frame break time t b (Liang & Zhang 2005), X-ray luminosity L X and rest-frame time of plateau phase T * a (Dainotti et al 2015), lag-luminosity correlation τ lag − L iso (Norris et al 2000), and fundamental plane of GRBs (Dainotti et al 2016(Dainotti et al , 2017b.…”

A Study of the Gamma-Ray Burst Fundamental Plane

“…Isolating GRB categories allows us to derive tighter relations, thus increasing the accuracy with which cosmological parameters are inferred (e.g., Cardone et al 2009Cardone et al , 2010Dainotti et al 2013b;Postnikov et al 2014). For a review on GRB relations, see the following reviews: Dainotti et al (2016b and Dainotti & Del Vecchio (2017).…”

The key role of BeppoSAX in the GRB history

“…Other relations were later reported between prompt and afterglow emission or concerning only the afterglow. For a review see [19]. In spite of the more recent relations, the Amati relation remains the most robust and it is now confirmed by all long GRBs for which it has been possible to derive, along with z, their bolometric fluence and peak energy E p .…”