A Large Catalogue of Multi-wavelength GRB Afterglows I: Color Evolution And Its Physical Implication

TL;DR

This study compiles a large catalog of 70 GRB afterglows to analyze their color evolution over time, revealing that most colors remain constant and supporting the external forward shock model, with some variations explained by specific physical processes.

Contribution

It provides the first comprehensive analysis of color index evolution in a large sample of GRB afterglows, linking observed variations to physical mechanisms.

Findings

95% of color indices do not vary over time.

Color variations are mainly due to cooling frequency crossing, dust extinction, shock transition, or supernova emission.

Most colors (86%) are constant between episodes, supporting simple external shock models.

Abstract

The spectrum of gamma-ray burst (GRB) afterglows can be studied with color indices. Here we present a large comprehensive catalogue of 70 GRBs with multi-wavelength optical transient data on which we perform a systematic study to find the temporal evolution of color indices. We categorize them into two samples based on how well the color indices are evaluated. The Golden sample includes 25 bursts mostly observed by GROND, and the Silver sample includes 45 bursts observed by other telescopes. For the Golden sample, we find that 95\% of the color indices do not vary over time. However, the color indices do vary during short periods in most bursts. The observed variations are consistent with effects of (i) the cooling frequency crossing the studied energy bands in a wind medium (43\%) and in a constant density medium (30\%), (ii) early dust extinction (12\%), (iii) transition from reverse shock to forward shock emission (5\%), or (iv) an emergent supernova emission (10\%). We also study the evolutionary properties of the mean color indices for different emission episodes. We find that 86\% of the color indices in the 70 bursts show constancy between consecutive ones. The color index variations occur mainly during the late GRB-SN bump, the flare and early reversed-shock emission components. We further perform a statistical analysis of various observational properties and model parameters (spectral index $\beta_{o}^{\rm CI}$, electron spectral indices $p^{\rm CI}$, etc.) using color indices. Overall, we conclude that $\sim$ 90\% of colors are constant in time and can be accounted for by the simplest external forward shock model, while the varying color indices call for more detailed modeling.