Redshift Determination of GRB 990506 and GRB 000418 with the Echellete Spectrograph Imager on Keck

Creators: Bloom, J. S.; Berger, E.; Kulkarni, S. R.; Djorgovski, S. G.; Frail, D. A.

Abstract

Using the Echellete Spectrograph Imager (ESI) on the Keck II 10 m telescope we have measured the redshifts of the host galaxies of gamma-ray bursts GRB 990506 and GRB 000418, z = 1.30658 ± 0.00004 and 1.1181 ± 0.0001, respectively. Thanks to the excellent spectral resolution of ESI (λ/Δλ = 13000), we resolved the [O II] λ3727 doublet in both cases. The measured redshift of GRB 990506 is the highest known for a dark-burst GRB, though entirely consistent with the notion that dark and non–dark bursts have a common progenitor origin. The relative strengths of the [O II], He I, [Ne III], and Hγ emission lines suggest that the host of GRB 000418 is a starburst galaxy, rather than a LINER or Seyfert 2. Since the host of GRB 000418 has been detected at submillimeter wavelengths, these spectroscopic observations suggest that the submillimeter emission is due to star formation (as opposed to AGN) activity. The [O II]-derived unobscured star formation rates are 13 and 55 M_⊙ yr^(-1) for the hosts of GRB 990506 and GRB 000418, respectively. In contrast, the star formation rate of the host of GRB 000418 derived from submillimeter observations is 20 times larger.

Additional Information

© 2003 The American Astronomical Society. Received 2002 November 20; accepted 2002 December 4. The authors thank the generous support of the staff of the W. M. Keck Foundation. J. S. B. gratefully acknowledges the fellowship from the Fannie and John Hertz Foundation and a research grant from the Harvard-Smithsonian Center for Astrophysics. S. R. K.'s research in GRBs is supported by the NSF and NASA. S. G. D. acknowledges partial funding from the Bressler Foundation. We thank S. Castro for helpful discussions concerning ESI reductions. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. The authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, the observations presented herein would not have been possible.

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