The nature of HI absorbers in GRB afterglows: clues from hydrodynamic simulations

Details The nature of HI absorbers in GRB afterglows: clues from hydrodynamic simulations The nature of HI absorbers in GRB afterglows: clues from hydrodynamic simulations

2009-09-07

arxiv.org/abs/0909.1321v2

Mon. Not. Roy. Astron. Soc. 402 (2010) 1523-1535

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

Typos fixed; minor clarifications. 13 pages, 7 figures, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2009.16017.x

In recent work, we have shown that it is possible to link quantitatively many aspects of damped Lyman alpha (DLA) absorbers in the spectra of quasars to high resolution simulations of galaxy formation. Using runs from the same series of hydrodynamic numerical studies, we consider the expected properties of Lyman alpha absorbers seen in the spectra of high redshift (z>2) gamma ray burst afterglows (GRB-DLAs). If GRBs are associated with the death of massive stars, their afterglows provide insights into otherwise unprobed regions of protogalactic objects, but detailed physical interpretations are currently embryonic. We find that median impact parameters (measured from the potential minimum) are approximately 1 kpc for GRBs compared with 4 kpc for QSO-DLAs. However, an equally important difference is that GRB-DLAs are predominantly associated with halos of mass 10^1010^19 cm^-2, but they somewhat underpredict the incidence of low column densities N_HI<10^19 cm^-2. Line-of-sight neutral gas metallicities predicted by our simulations (10^-2 < Z/Z_sol < 1) are consistent with the modest observational constraints. Because of large internal dispersions in gas metallicities, this agreement is not significantly compromised by imposing a cut-off on the metallicity of stars able to launch GRBs (Z_star

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