The Host Galaxy of GRB 970508

Bloom, J.; Djorgovski, S. G.; Kulkarni, S. R.; Frail, D. A.

doi:10.1086/311682

Cited by 189 publications

(184 citation statements)

References 26 publications

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“…3). This power law is 2 p below the power law reported by Pian et al (1998b), but agrees well with that found by Bloom et al (1998a) and is within 2 p of that found by Zharikov et al (1998). (We note that the Pian et al Ðt was slightly contaminated by the then-unmeasured light from the host galaxy.…”

Section: Observations Image Analysis and Resultssupporting

confidence: 93%

“…The optical Ñux reached a peak at R D 19.8 2 days after the GRB, then began a power-law decay, t~b, with b \ 1.141^0.014, that continued for over 100 days (Pian et al 1998b ;Galama et al 1998c). At that point, the decay curve began to Ñatten (Pian et al 1998a ;Pedersen et al 1998 ;Bloom et al 1998a ;Zharikov, Sokolov, & Baryshev 1998 ;Sokolov et al 1999), as expected if the measured Ñux were becoming dominated by light from a host galaxy. GRB 970508 was also the Ðrst GRB for which a radio counterpart was detected Galama et al 1998b).…”

Section: Introductionmentioning

confidence: 74%

“…Although the estimated galactic magnitudes have changed with time (a point we return to below), all observers have found a blue host, and Sokolov et al (1999) suggest that the galaxy colors are best Ðtted by an object intermediate between an Scd and an irregular (Im) redshifted to z \ 0.83. Using either the measured galaxy colors, obtained by a rough averaging of the values obtained by previous observers (Bloom et al 1998a ;Zharikov et al 1998 ;Sokolov et al 1999), or an SED created by interpolating between FIG. 1.ÈSection of the STIS CCD image of the Ðeld around GRB 970508.…”

Section: Observations Image Analysis and Resultsmentioning

confidence: 99%

“…However, there has been a continuing trend among the ground-based estimates of the host magnitude. The later the data used to Ðt the host galaxy, the fainter the host was found to be (Bloom et al 1998a ;Zharikov et al 1998 ;Sokolov et al 1999). The di †erences are visible in all bands (B, V , R, and I), and are typically at the 2 p level.…”

Section: Observations Image Analysis and Resultsmentioning

confidence: 99%

“…Spectroscopy has revealed [O II] and [Ne III] emission features, and these, together with colors of the galaxy obtained by Ðtting observations of the combined light from the optical transient (OT) and the galaxy, have led to the suggestion that the host is an actively star forming dwarf galaxy (Bloom et al 1998a ;Sokolov et al 1999). However, attempts to resolve the host galaxy from the ground have proven fruitless.…”

Section: Introductionmentioning

confidence: 99%

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Hubble Space TelescopeObservations of the Host Galaxy of GRB 970508

Fruchter

Pian²,

Gibbons

et al. 2000

ApJ

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We report on observations of the Ðeld of GRB 970508 made in 1998 early August, 454 days after outburst, with the STIS CCD camera on board the Hubble Space T elescope (HST ). The images, taken in open Ðlter (50CCD) mode, clearly reveal the presence of a galaxy that was overwhelmed in earlier (1997 June) HST images by emission from the optical transient (OT). The galaxy is regular in shape : after correcting for the HST /STIS PSF, it is well Ðtted by an exponential disk with a scale length of 0A .046and an ellipticity of 0.70^0.07. All observations are marginally consistent with a continuouŝ 0A .006 decline in OT emission as t~1.3 beginning 2 days after outburst ; however, we Ðnd no direct evidence in the late-time HST image for emission from the OT, and the surface brightness proÐle of the galaxy is most regular if we assume that the OT emission is negligible, suggesting that the OT may have faded more rapidly at late times than is predicted by the power-law decay. Due to the wide bandwidth of the STIS clear mode, the estimated magnitude of the galaxy is dependent on the galaxy spectrum that is assumed. Using colors obtained from late-time ground-based observations to constrain the spectrum, we Ðnd V \ 25.4^0.15, a few tenths of a magnitude brighter than earlier ground-based estimates that were obtained by observing the total light of the galaxy and the OT and then subtracting the estimated OT brightness, assuming that it fades as a single power law. This again suggests that the OT may have faded faster at late time than the power law predicts. The position of the OT agrees with that of the isophotal center of the galaxy to which, at the galaxy redshift z \ 0.83, corresponds to an o †set from the 0A .01, center of the host of pc. This remarkable agreement raises the possibility that the gamma-ray burst [70 may have been associated with either an active galactic nucleus or a nuclear starburst.

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Section: Observations Image Analysis and Resultssupporting

confidence: 93%

Section: Introductionmentioning

confidence: 74%

Section: Observations Image Analysis and Resultsmentioning

confidence: 99%

Section: Observations Image Analysis and Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Hubble Space TelescopeObservations of the Host Galaxy of GRB 970508

Fruchter

Pian²,

Gibbons

et al. 2000

ApJ

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Theoretical Implications of the Gamma-Ray Burst-Supernova Connection

Chevalier¹

Gamma-Ray Bursts in the Afterglow Era

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Although observations of circumstellar shock interactions around supernovae are generally consistent with a ρ ∝ r −2 wind surrounding the progenitor star, this is not true for GRB (gamma-ray burst) afterglows. However, GRB 991208 and GRB 000301C may be consistent with wind interaction if the injection particle spectrum is a broken power law. Circumstellar dust echos can place constraints on supernova and GRB progenitors, but have been clearly observed only around SN 1987A. Excess emission observed in two GRB afterglows is more likely to have a supernova origin. An interstellar dust echo, causing the light curve to flatten out, is a possibility for GRB afterglows, but is not likely to be observable.

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The Multiband Photometry of GRB Host Galaxies: Comparison with the Spectral Energy Distributions of Nearby Galaxies and Theoretical Modeling

Соколов

Фатхуллин

Komarova

et al. 2003

Gamma-Ray Bursts in the Afterglow Era

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We present one of the results of BV RI photometry of the hosts of GRB for the host galaxy of GRB 970508 and the theoretical modeling of its continuum spectral energy distribution (SED) to show that it is important to take into account internal extinction in the host galaxies. We compared the BV RI broad-band flux spectrum of the host to template SEDs of local starburst galaxies and found that there is a significant internal extintion in this host. Moreover, this comparison allows us to derive the absolute magnitude (MB rest ) and rouhgly estimate reddening (AV ). Population synthesis modeling of the continuum SED for different reddening laws ([4] and [5]) demostrates that the observational data of the host galaxy of GRB 970508 are best fitted by the spectral properties of a model SED with extinction of AV ≈ 2.

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The Host Galaxy of GRB 970508

Cited by 189 publications

References 26 publications

Hubble Space TelescopeObservations of the Host Galaxy of GRB 970508

Hubble Space TelescopeObservations of the Host Galaxy of GRB 970508

Theoretical Implications of the Gamma-Ray Burst-Supernova Connection

The Multiband Photometry of GRB Host Galaxies: Comparison with the Spectral Energy Distributions of Nearby Galaxies and Theoretical Modeling

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