<i>Hubble Space Telescope</i>and Ground‐based Optical and Ultraviolet Observations of GRB 010222

Galama, T. J.; Reichart, D.; Brown, Thomas M.; Kimble, Randy A.; Price, P. A.; Berger, E.; Frail, D. A.; Kulkarni, S. R.; Yost, S. A.; Gal‐Yam, A.; Bloom, J.; Harrison, Fiona A.; Sari, Re’em; Fox, D. B.; Djorgovski, S. G.

doi:10.1086/368123

Cited by 38 publications

(41 citation statements)

References 44 publications

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“…Both mechanisms naturally lead to a dust size distribution skewed toward large grains, producing an extinction curve weakly dependent on wavelength. Nongray extinction has also been reported (e.g., for the host of GRB 010222 by Galama et al 2003). Our nongray, type II 7 Alternatively, these results can be explained by an intrinsically low dust content: a low metallicity and/or a low level of depletion of the dust-forming heavy elements in the burst environment (Fynbo et al 2003;Hjorth et al 2003;Vreeswijk et al 2004;Fruchter et al 2006).…”

Section: Discussionsupporting

confidence: 66%

Dust Extinction of Gamma-Ray Burst Host Galaxies: Identification of Two Classes?

Chen

Wei

2006

ApJ

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Dust in the host galaxies of gamma-ray bursts (GRBs) dims and reddens their afterglow spectra. Knowledge of the nature of this dust is crucial for correcting for extinction, providing clues to the nature of GRB progenitors, and probing the interstellar medium of high-redshift galaxies as well as the nature of cosmic dust when the universe was much younger and galaxies were much less evolved. The dust and extinction properties of GRB host galaxies are still poorly known. Unlike previous work, we derive in this Letter the extinction curves for 10 GRB host galaxies without a priori assumption of any specific extinction types (such as those of the Milky Way or Small/Large Magellanic Clouds). It is found that there appear to exist two different types of extinction curves: one is relatively flat and gray, and the other displays a steeper dependence on inverse wavelength, closely resembling that of the Milky Way but with the 2175 feature removed.

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Section: Discussionsupporting

confidence: 66%

Dust Extinction of Gamma-Ray Burst Host Galaxies: Identification of Two Classes?

Chen

Wei

2006

ApJ

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“…The situation is similar for GRB 010222, where at least four nearby galaxies surround its host (e.g. Mirabal et al 2002;Frail et al 2002;Galama et al 2003). Two galaxies are located 2.…”

Section: The Intervening Absorption Galaxymentioning

confidence: 83%

The line-of-sight towards GRB 030429 at z $\mathsf{=2.66}$: Probing the matter at stellar, galactic and intergalactic scales

Jakobsson

Hjorth²,

Fynbo

et al. 2004

A&A

108

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Abstract. We report the discovery of the optical afterglow (OA) of the long-duration gamma-ray burst GRB 030429, and present a comprehensive optical/near-infrared dataset used to probe the matter at different distance scales, i.e. in the burst environment, in the host galaxy and in an intervening absorber. A break in the afterglow light curve is seen approximately 1 day from the onset of the burst. The light curve displays a significant deviation from a simple broken power-law with a bright 1.5 mag bump with a duration of 2-3 days. The optical/near-infrared spectral energy distribution is best fit with a power-law with index β = −0.36 ± 0.12 reddened by an SMC-like extinction law with (a modest) A V = 0.34 ± 0.04. In addition, we present deep spectroscopic observations obtained with the Very Large Telescope. The redshift measured via metal absorption lines in the OA is z = 2.658 ± 0.004. Based on the damped Lyα absorption line in the OA spectrum we measure the H  column density to be log N(H i) = 21.6 ± 0.2. This confirms the trend that GRBs tend to be located behind very large H  column densities.The resulting dust-to-gas ratio is consistent with that found in the SMC, indicating a low metallicity and/or a low dust-to-metal ratio in the burst environment. We find that a neighbouring galaxy, at a separation of only 1. 2, has z = 0.841 ± 0.001, ruling it out as the host of GRB 030429. The small impact parameter of this nearby galaxy, which is responsible for Mg  absorption in the OA spectrum, is in contrast to previous identifications of most QSO absorption-selected galaxy counterparts. Finally, we demonstrate that the OA was not affected by strong gravitational lensing via the nearby galaxy.

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“…With these data we can constrain the position of ν a < 2 × 10 11 Hz and 2 × 10 11 < ν c < 10 13 Hz. significant amounts of dust, these GRB hosts exhibit properties consistent with the rest of the GRB host population, namely blue optical colours, low extinction and low optical star formation rates (Gorosabel et al 2003a,b;Galama et al 2003;Berger et al 2003;Savaglio et al 2003Savaglio et al , 2009Christensen et al 2004;Castro Cerón et al 2006Kann et al 2006). This discrepancy was explained by Michałowski et al (2008) by invoking very young stellar population with optical emission completely extinguished by dust.…”

Section: Grb Host Galaxies With Almamentioning

confidence: 94%

Pre-ALMA observations of GRBs in the mm/submm range

Postigo

Lundgren

Martín

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) generate an afterglow emission that can be detected from radio to X-rays during days, or even weeks after the initial explosion. The peak of this emission crosses the millimeter and submillimeter range during the first hours to days, making their study in this range crucial for constraining the models. Observations have been limited until now due to the low sensitivity of the observatories in this range. This situation will be greatly improved with the start of scientific operations of the Atacama Large Millimeter/submillimeter Array (ALMA). Aims. In this work we do a statistical analysis of the complete sample of mm/submm observations of GRB afterglows obtained before the beginning of scientific operations at ALMA. Methods. We present observations of 11 GRB afterglows obtained from the Atacama Pathfinder Experiment (APEX) and the SubMillimeter Array (SMA), as well as the first detection of a GRB with ALMA, still in the commissioning phase, and put them into context with a catalogue of all the observations that have been published until now in the spectral range that is covered by ALMA.Results. The catalogue of mm/submm observations collected here is the largest to date and is composed of 102 GRBs, of which 88 have afterglow observations, whereas the rest are host galaxy searches. With our programmes, we contributed with data of 11 GRBs and the discovery of 2 submm counterparts. In total, the full sample, including data from the literature, has 22 afterglow detections with redshifts ranging from 0.168 to 8.2. GRBs have been detected in mm/submm wavelengths with peak luminosities spanning 2.5 orders of magnitude, the most luminous reaching 10 33 erg s −1 Hz −1 . We observe a correlation between the X-ray brightness at 0.5 days and the mm/submm peak brightness. Finally we give a rough estimate of the distribution of peak flux densities of GRB afterglows, based on the current mm/submm sample. Conclusions. Observations in the mm/submm bands have been shown to be crucial for our understanding of the physics of GRBs, but have until now been limited by the sensitivity of the observatories. With the start of the operations at ALMA, the sensitivity has improved by more than an order of magnitude, opening a new era in the study of GRB afterglows and their host galaxies. Our estimates predict that, once completed, ALMA will detect up to ∼98% of the afterglows if observed during the passage of the peak synchrotron emission.

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Hubble Space Telescopeand Ground‐based Optical and Ultraviolet Observations of GRB 010222

Cited by 38 publications

References 44 publications

Dust Extinction of Gamma-Ray Burst Host Galaxies: Identification of Two Classes?

Dust Extinction of Gamma-Ray Burst Host Galaxies: Identification of Two Classes?

The line-of-sight towards GRB 030429 at z $\mathsf{=2.66}$: Probing the matter at stellar, galactic and intergalactic scales

Pre-ALMA observations of GRBs in the mm/submm range

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