An optical spectrum of the afterglow of a γ-ray burst at a redshift of z = 6.295

By N. Kawai, G. Kosugi, K. Aoki, T. Yamada, T. Totani, Kouji Ohta, M. Iye, Takashi Hattori, Wako Aoki, H. Furusawa and 18 more. Nature, 2006

233 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

CONNECTING THE GAMMA RAY BURST RATE AND THE COSMIC STAR FORMATION HISTORY: IMPLICATIONS FOR REIONIZATION AND GALAXY EVOLUTION (2011, methodology): “…et al. (2009), we use the GRB rate at 1< z < 4 (where the star formation rate density ρ̇⋆(z) is roughly constant) to estimate thėρ⋆(z) at z > 4 (including constraints from the highest redshift GRBs, e.g., Kawai et al. 2006; Tanvir et al. 2009; Salvaterra et al. 2009a; Cucchiara et al. 2011).”
The metallicity of the long GRB hosts and the fundamental metallicity relation of low-mass galaxies (2010, background): “Thank to they brightness, GRBs can be used as a background light to study the metal content of its parent galaxy even at very high-z as demonstrated by the case of GRB 050904 at z = 6.3 for which an estimate of the metallicity has been derived by Totani et al. (2006) and Kawai et al. (2006).”
The 2175 Å Dust Feature in a Gamma-Ray Burst Afterglow at Redshift 2.45 (2008, background): “The enormous energy release in -rays is unaffected by dust or gas absorption, so GRBs are detectable out to very high redshifts (e.g., Lamb & Reichart 2000; Kawai et al. 2006).”
A PHOTOMETRIC REDSHIFT OF z ∼ 9.4 FOR GRB 090429B (2011, background): “Follow-up spectroscopy of these candidates has proved several to be at very high redshift (e.g., Kawai et al. 2006; Greiner et al. 2009), culminating in GRB 090423 at z ≈ 8.2 (Tanvir et al. 2009; Salvaterra et al. 2009).”
The physics of gamma-ray bursts & relativistic jets (2014, background): “…absorption by neutral hydrogen (e.g. Ioka and Mészáros, 2005; Toma et al., 2011a; Ciardi et al., 2013) that would facilitate investigation of gas distribution at the dawn of galaxy formation, and for determining the reionization history of the universe (Kawai et al., 2006; Totani et al., 2006).”
THE OPTICALLY UNBIASED GAMMA-RAY BURST HOST (TOUGH) SURVEY. I. SURVEY DESIGN AND CATALOGS (2012, unknown): “…et al. 2007; (13) Krühler et al. 2012; (14) Prochaska et al. 2007; (15) Fox et al. 2008; (16) Jakobsson et al. 2012; (17) Sollerman et al. 2007; (18) Kawai et al. 2006; (19) Prochaska et al. 2005; (20) Jakobsson et al. 2006a; (21) Piranomonte et al. 2008; (22) Soderberg et al. 2005; (23) Mirabal…”
Gamma-Ray Bursts in the Swift Era (2007, background): “…burst (Cusumano et al. 2006a) prompted the IR follow-up observations which led to the identification of its redshiftz = 6.29 (Haislip et al. 2006; Kawai et al. 2006; Antonelli et al. 2005); – Feb. 18, 2006: Swift detected an extremely long, faint, low-uminosity GRB (Campana et al. 2006a) at…”
The Giant Gemini GMOS survey of zem > 4.4 quasars – I. Measuring the mean free path across cosmic time (2014, background): “These include the most distant quasars (Fan et al. 2006; Mortlock et al. 2011) and z > 8 gammaray bursts ‘revealed’ by their extremely faint optical fluxes (Kawai et al. 2006; Cucchiara et al. 2011; Chornock et al. 2013).”
GRB 080913 AT REDSHIFT 6.7 (2008, background): “The hitherto highest redshift burst, GRB 050904 at z = 6.29 (Kawai et al. 2006; Haislip et al. 2006), held the record for three years and in that time only GRB 060927 at z = 5.47 (Ruiz-Velasco et al. 2007) came close.”
LOW-RESOLUTION SPECTROSCOPY OF GAMMA-RAY BURST OPTICAL AFTERGLOWS: BIASES IN THE SWIFT SAMPLE AND CHARACTERIZATION OF THE ABSORBERS (2009, unknown): “…a 0.99 Jakobsson et al. (2006b)050922B 1.1 < 0.58 050915A < 15.0 a < 0.44 Bloom (2005)050908 3.34 a 1.14 Fugazza et al. (2005)050904 6.30 a < 0.41 Kawai et al. (2006)050824 0.83 ah 0.91 Sollerman et al. (2007)050822 0.6 050820A 2.61 a 0.77 Fox et al. (2008)050819 0 < 0.90 050814 5.3 p 0.51…”
Gamma-Ray Bursts in the Swift Era (2009, background): “Intriguingly, the “high redshift” GRB 050904 (Tagliaferri et al. 2005a, Cusumano et al. 2006) at z = 6.29 (Kawai et al. 2006) also had prompt optical emission observed (Boër et al. 2006, Haislip et al. 2006), with a brightness, single-pulse structure, and fast-fading behavior reminiscent of GRB…”