2000ApJ...532..273D

If a gamma-ray burst (GRB) with strong UV emission occurs in a molecular cloud, excitation of the surrounding H₂ will have observable consequences. The UV will pump H₂ into vibrationally excited levels that produce strong absorption at wavelengths λ≲1650 Å. As a result, both the prompt flash and later afterglow will exhibit strong absorption shortward of 1650 Å, with specific spectroscopic features. Such a cutoff in the emission from GRB 980329 may have already been observed by Fruchter and coworkers; 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 was at redshift 1.6≲z≲2.3. Fluorescence accompanying the UV pumping of the H₂ will result in UV emission from the GRB which can extend over days or months, with 7.5-13.6 eV fluorescent luminosity ∼10⁴² ergs.s^–1. Spectroscopy can distinguish this fluorescence from other possible sources of transient optical emission, such as a supernova.