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Klose, Andreas; Stähly, Paul; Delfmann, Werner; Stein, Andreas; Prockl, Günter G.; Klaus, Peter

doi:10.1007/978-3-322-96526-4_19

Cited by 17 publications

(22 citation statements)

References 3 publications

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“…The quick distribution of the position (Frontera et al 1998a, In 't Zand et al 1998) resulted in the detection of a variable radio counterpart that peaked about 3 days after the burst (Taylor et al 1998). Observations of the position of this radio source revealed a candidate host galaxy (Djorgovski et al 1998) and fading coincident counterparts in the I band (Klose et al 1998), K band (Larkin et al 1998, Metzger et al 1998) and R band (Palazzi et al 1998). The R-band counterpart decayed in a manner consistent with a power law decay with an index of −1.3.…”

Section: Introductionmentioning

confidence: 94%

Gamma-Ray Burst 980329 and Its X-Ray Afterglow

Zand

Amati²,

Antonelli

et al. 1998

The Astrophysical Journal

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Section: Introductionmentioning

confidence: 94%

Gamma-Ray Burst 980329 and Its X-Ray Afterglow

Zand

Amati²,

Antonelli

et al. 1998

The Astrophysical Journal

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“…Discovered by the BeppoSAX Gamma Ray Burst Monitor (Costa et al 1997a), GRB 970228 is the first gamma ray burst (GRB) for which non-gamma ray emission has been detected for a prolonged period of time after a gamma ray burst: Costa et al (1997b), Yoshida et al (1997), and Frontera et al (1997) report transient x-ray emission from ∼ 8 hours to ∼ 13 days after the GRB event; Groot et al (1997a,b), Metzger et al (1997a,b), Sahu et al (1997a,b), Margon et al (1997), van Paradijs et al (1997), and Pedichini et al (1997) report transient optical emission from ∼ 17 hours to ∼ 37 days after the GRB event; and Klose et al (1997) and Soifer et al (1997) report transient infrared emission from ∼ 17 days to ∼ 30 days after the GRB event. Previously, only x-ray emission has been detected after GRB events, and then, for no longer than several hundred seconds (Murakami et al 1992).…”

Section: Introductionmentioning

confidence: 98%

Observations and Theoretical Implications of GRB 970228

Reichart

1997

The Astrophysical Journal

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GRB 970228 is the first gamma ray burst for which prolonged post-burst transient x-ray, optical, and infrared emission has been detected. Recent Hubble Space Telescope observations show that the transient consists of two components: a point source, which is known to be fading, and an extended source, which is possibly fading. I fit standard fireball remnant models to the first month of x-ray, optical, and infrared measurements, which may be done without assuming a GRB distance scale. I show that its emission is consistent with that of the remnant of a relativistically expanding impulsive fireball in which a forward shock dominates the emission of the GRB event: the piston model. However, two discrepant measurements may indicate that the post-burst flux varies by factors of approximately 3 on timescales of days or weeks. Furthermore, using the HST observations and the fitted model, I show that the extended object probably is fading, which may place GRB 970228 at galactic halo distances.Comment: Accepted to the Astrophysical Journal Letters, 11 pages, LaTe

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“…being an X-ray flash (XRF), with the fluences satisfying (Frontera et al 2000). Despite intense optical and near-S 1 S X g infrared (IR) follow-up observations initiated 6.5 and 8.4 hr after the burst, respectively (Klose 1998;Castro-Tirado et al 1998), no optical counterpart was found (Galama et al 1998;Wozniak 1998;Rhoads et al 1998;Bloom et al 1998;Schaefer et al 1998). The deep R-band observations carried out by Lindgren et al (1999) showed mag at 9.9 hr after the GRB.…”

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confidence: 99%

Photometric Redshift of the GRB 981226 Host Galaxy

Christensen

Hjorth

Gorosabel³

2005

ApJ

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No optical afterglow was found for the dark burst GRB 981226, and hence no absorption redshift has been obtained. We here use ground-based and space imaging observations to analyze the spectral energy distribution (SED) of the host galaxy. By comparison with synthetic template spectra, we determine the photometric redshift of the GRB 981226 host to be (68% confidence level). While the age-metallicity degeneracy z p 1.11 ‫ע‬ 0.06 phot for the host SED complicates the determination of accurate age, metallicity, and extinction, the photometric redshift is robust. The inferred z phot value is also robust compared to a Bayesian redshift estimator, which gives . The characteristics for this host are similar to other gamma-ray burst (GRB) hosts previously z p 0.94 ‫ע‬ 0.13 phot examined. Available low-resolution spectra show no emission lines at the expected wavelengths. The photometric redshift estimate indicates an isotropic energy release consistent with the Amati relation for this GRB, which had a spectrum characteristic of an X-ray flash.

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S

Cited by 17 publications

References 3 publications

Gamma-Ray Burst 980329 and Its X-Ray Afterglow

Gamma-Ray Burst 980329 and Its X-Ray Afterglow

Observations and Theoretical Implications of GRB 970228

Photometric Redshift of the GRB 981226 Host Galaxy

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