Abstract
Gamma-ray Bursts (GRBs) are highly energetic events that can be observed at extremely high redshift. However, inherent bias in GRB data due to selection effects and redshift evolution can significantly skew any subsequent analysis. We correct for important variables related to the GRB emission, such as the burst duration, T90*, the prompt isotropic energy, Eiso, the rest-frame end time of the plateau emission, Ta,radio*, and its correspondent luminosity La,radio, for radio afterglow. In particular, we use the Efron–Petrosian method presented in 1992 for the correction of our variables of interest. Specifically, we correct Eiso and T90* for 80 GRBs, and La,radio and Ta,radio* for a subsample of 18 GRBs that present a plateau-like flattening in their light curve. Upon application of this method, we find strong evolution with redshift in most variables, particularly in La,radio, with values similar to those found in past and current literature in radio, X-ray and optical wavelengths, indicating that these variables are susceptible to observational bias. This analysis emphasizes the necessity of correcting observational data for evolutionary effects to obtain the intrinsic behavior of correlations to use them as discriminators among the most plausible theoretical models and as reliable cosmological tools.
Highlights
Gamma-ray bursts (GRBs) can be observed at extremely high redshift, making them a valuable tool for studies of the early Universe
GRBs are characterized by the main event, called the prompt emission, which is usually observed in gamma-rays, hard X-rays and sometimes in optical, while the afterglow is the counterpart in soft X-rays (≈66% of observed GRBs), in optical
We here clarify that the purpose of our analysis is to show how similar our results are, compared to other ones in the literature given that our sample size differs from other
Summary
Gamma-ray bursts (GRBs) can be observed at extremely high redshift, making them a valuable tool for studies of the early Universe. Observations of GRBs have shown a very diverse population with few common characteristics. GRBs are characterized by the main event, called the prompt emission, which is usually observed in gamma-rays, hard X-rays and sometimes in optical, while the afterglow is the counterpart in soft X-rays (≈66% of observed GRBs), in optical (≈38% of observed GRBs) and sometimes in radio (≈6.6% of observed GRBs). GRB radio afterglows are very difficult to observe, similar to the X-ray observations which are characterized by the detector limits, and additional difficulties rise due to the limited allocated time for the follow-up observations in the radio band after the GRB trigger.
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
