H_2 Absorption and Fluorescence for Gamma Ray Bursts in Molecular Clouds

TL;DR

This paper explores how gamma-ray bursts in molecular clouds excite H2 molecules, leading to observable UV absorption features and fluorescent emission, which can provide insights into the burst's environment and redshift.

Contribution

It introduces a model predicting UV absorption and fluorescence signatures from H2 in molecular clouds affected by GRBs, aiding in redshift estimation and environmental analysis.

Findings

UV absorption features can indicate GRB location within molecular clouds.

Fluorescent UV emission from H2 can last days to months after the burst.

Spectroscopy can distinguish H2 fluorescence from other transient sources.

Abstract

If a gamma ray burst with strong UV emission occurs in a molecular cloud, there will be observable consequences resulting from excitation of the surrounding H2. The UV pulse from the GRB will pump H2 into vibrationally-excited levels which produce strong absorption at wavelengths < 1650 A. As a result, both the prompt flash and later afterglow will exhibit strong absorption shortward of 1650 A, with specific spectroscopic features. Such a cutoff in the emission from GRB 980329 may already have been observed by Fruchter et al.; if so, GRB 980329 was at redshift 3.0 < z < 4.4 . BVRI photometry of GRB 990510 could also be explained by H2 absorption if GRB 990510 is at redshift 1.6 < z < 2.3. The fluorescence accompanying the UV pumping of the H2 will result in UV emission from the GRB which can extend over days or months, depending on parameters of the ambient medium and beaming of the GRB flash. The 7.5-13.6 eV fluorescent luminosity is \sim 10^{41.7} erg/s for standard estimates of the parameters of the GRB and the ambient medium. Spectroscopy can distinguish this fluorescent emission from other possible sources of transient optical emission, such as a supernova.