The Bright Gamma‐Ray Burst of 2000 February 10: A Case Study of an Optically Dark Gamma‐Ray Burst

Piro, L.; Frail, D. A.; Gorosabel, J.; Garmire, Gordon; Soffitta, P.; Amati, L.; Andersen, M. I.; Antonelli, L. A.; Berger, E.; Frontera, F.; Fynbo, J.; Gandolfi, G.; Garcia, M. R.; Hjorth, J.; Zand, J. in’t; Jensen, B. L.; Masetti, N.; Møller, Per; Pedersen, H.; Pian, E.; Wieringa, M.

doi:10.1086/342226

Cited by 113 publications

(102 citation statements)

References 61 publications

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“…Moreover, small extinction values do not exclude the possibility that the GRBs themselves are located in more dusty and higher density environments, such as embedded in molecular clouds which has been suggested through analyses of X-ray afterglows. This was discussed for the case of the GRB 000210 host galaxy, where a large N H was inferred (Piro et al 2002), while the galaxy itself shows a small global extinction (see Table 2; and Gorosabel et al 2003a). However, if the regions of star formation where GRBs occur are small and not numerous, this will not have a large effect on the overall SEDs of the hosts.…”

Section: Discussionmentioning

confidence: 90%

UV star-formation rates of GRB host galaxies

Christensen¹,

Hjorth²,

Gorosabel

2004

A&A

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Abstract. We study a magnitude-limited sample of 10 gamma-ray burst (GRB) host galaxies with known spectroscopic redshifts (0.43 < z < 2.04). From an analysis of the spectral energy distributions (SEDs), based on published broad-band optical and near-infrared photometry, we derive photometric redshifts, galaxy types, ages of the dominant stellar populations, internal extinctions, and ultraviolet (UV) star-formation rates (SFRs) of the host galaxies. The photometric redshifts are quite accurate despite the heterogeneous nature of the sample: the rms errors are σ(z) = 0.21 and σ(∆z/(1 + z spec )) = 0.16 with no significant systematic offsets. All the host galaxies have SEDs similar to young starburst galaxies with moderate to low extinction. A comparison of specific SFRs with those of high-redshift galaxies in the Hubble Deep Fields shows that GRB hosts are most likely similar to the field galaxies with the largest specific SFRs. On the other hand, GRB hosts are not significantly younger than starburst field galaxies at similar redshifts, but are found to be younger than a sample of all types of field galaxies.

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Section: Discussionmentioning

confidence: 90%

UV star-formation rates of GRB host galaxies

Christensen¹,

Hjorth²,

Gorosabel

2004

A&A

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302

357

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“…Since GRB 990506 is one of only a handful of well-studied dark bursts (also including GRB 000210, Piro et al 2002;and GRB 970828, Djorgovski et al 2001) the measurement of a redshift near the median of other long-duration bursts may suggest a common progenitor population. This emerging trend of similar redshift distributions will almost certainly be testable with the advent of systematic absorption redshift determinations for Swift bursts.…”

Section: Discussionmentioning

confidence: 99%

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

Bloom

Berger

Kulkarni

et al. 2003

The Astronomical Journal

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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 AE 0.00004 and 1.1181 AE 0.0001, respectively. Thanks to the excellent spectral resolution of ESI ( /D = 13000), we resolved the [O ii] 3727 doublet in both cases. The measured redshift of GRB 990506 is the highest known for a darkburst 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 H 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 À1 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.

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“…After a putative host has been identified, the observations can constrain not only the redshift but may also help to explain the optical dimness of the afterglow Several studies of individual events have already found that dust extinction in the corresponding GRBHs was the main reason for the optical dimness of some events (e.g., Piro et al 2002;Gorosabel et al 2003;Levan et al 2006;Berger et al 2007;Küpcü Yoldaş et al 2010;Krühler et al 2011). This conclusion then naturally leads to the question of whether extinction by cosmic dust can explain the entire ensemble of optically dark bursts or whether their high redshifts (seen as Lyman dropouts) is also an important factor.…”

Section: Bursts With Optically Undetected Afterglowsmentioning

confidence: 99%

A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

Rossi

Klose

Ferrero

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) can provide information about star formation at high redshifts. Even in the absence of a bright optical/nearinfrared/radio afterglow, the high detection rate of X-ray afterglows by Swift/XRT and its localization precision of 2-3 arcsec facilitates the identification and the study of GRB host galaxies. Aims. We focus on the search for the host galaxies of 17 bursts with arcsec-sized XRT error circles but no detected long-wavelength afterglow, in spite of their deep and rapid follow-up observations. Three of these events can also be classified as truly dark bursts, i.e., the observed upper limit on the optical flux of the afterglow was less than expected based on the measured X-ray flux. Our goals are to identify the GRB host galaxy candidates and characterize their phenomenological parameters. Methods. Our study is based on deep R C and K s -band observations performed with FORS1, FORS2, VIMOS, ISAAC, and HAWK-I at the ESO/VLT, partly supported by observations with the seven-channel imager GROND at the 2.2-m telescope on La Silla, and supplemented by observations with NEWFIRM at the 4-m telescope on Kitt Peak. To be conservative, we searched for host galaxy candidates within an area of twice the radius of each associated 90% c.l. Swift/XRT error circle. Results. For 15 of the 17 bursts, we find at least one galaxy within the searching area, and in the remaining two cases only a deep upper limit to R C and K s can be provided. In seven cases, we discover extremely red objects in the error circles, at least four of which might be dust-enshrouded galaxies. The most remarkable case is the host of GRB 080207, which has a color of (R C − K s ) AB ∼ 4.7 mag, and is one of the reddest galaxies ever associated with a GRB. As a by-product of our study we identify the optical afterglow of GRB 070517. Conclusions. Only a minority of optically dim afterglows are due to Lyman dropout ( 1/3). Extinction by dust in the host galaxies might explain all other events. Thereby, a seemingly non-negligible fraction of these hosts are globally dust-enshrouded, extremely red galaxies. This suggests that at least a fraction of GRB afterglows trace a subpopulation of massive starburst galaxies, which are markedly different from the main body of the GRB host galaxy population, namely the blue, subluminous, compact galaxies.

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The Bright Gamma‐Ray Burst of 2000 February 10: A Case Study of an Optically Dark Gamma‐Ray Burst

Cited by 113 publications

References 61 publications

UV star-formation rates of GRB host galaxies

UV star-formation rates of GRB host galaxies

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

A deep search for the host galaxies of gamma-ray bursts with no detected optical afterglow

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