Detection of the optical afterglow of GRB 000630: Implications for dark bursts

Fynbo, J. P. U.; Jensen, B. L.; Gorosabel, J.; Hjorth, J.; Pedersen, H.; Møller, P.; Abbott, T. M. C.; Castro‐Tirado, A. J.; Delgado, David Martínez; Greiner, J.; Henden, A. A.; Magazzù, A.; Masetti, N.; Merlino, Silvia; Masegosa, J.; Østensen, R. H.; Palazzi, E.; Pian, E.; Schwarz, H. E.; Cline, T.; Guidorzi, C.; Goldsten, J.; Hurley, K.; Mazets, E.; McClanahan, T. P.; Montanari, E.; Starr, R.; Trombka, J. I.

doi:10.1051/0004-6361:20010112

Cited by 129 publications

(121 citation statements)

References 27 publications

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“…However, with 8 m class telescopes the technique can easily be used for bursts as faint as R = 24. Hopefully this technique will therefore facilitate the detection of optical and/or near-IR afterglows from a larger fraction of well localised GRBs than the ≈30% during the latest 3-4 years (Fynbo et al 2001b).…”

Section: Discussionmentioning

confidence: 99%

“…This demonstrates that, besides the colour, the magnitude of the source is an important parameter that together with the colour shows the unusual nature of a source. However, we do not wish to exclude faint candidates since one of the important quests for future searches is to extend the detection sensitivity to fainter magnitudes (Fynbo et al 2001b). …”

Section: Rejection Of Non-transient Sources With Similar Colours As Oasmentioning

confidence: 99%

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Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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Abstract.We report the discovery of the optical and near-infrared counterparts to GRB 001011. The GRB 001011 error box determined by Beppo-SAX was simultaneously imaged in the near-infrared by the 3.58-m New Technology Telescope and in the optical by the 1.54-m Danish Telescope ∼8 hr after the gamma-ray event. Here we implement the colour-colour discrimination technique proposed by Rhoads (2001) and extend it using near-IR data as well. We present the results provided by an automatic colour-colour discrimination pipe-line developed to discern the different populations of objects present in the GRB 001011 error box. Our software revealed three candidates based on single-epoch images. Second-epoch observations carried out ∼3.2 days after the burst revealed that the most likely candidate had faded, thus identifying it with the counterpart to the GRB. In deep R-band images obtained 7 months after the burst a faint (R = 25.38 ± 0.25) elongated object, presumably the host galaxy of GRB 001011, was detected at the position of the afterglow. The GRB 001011 afterglow is the first discovered with the assistance of colour-colour diagram techniques. We discuss the advantages of using this method and its application to error boxes determined by future missions.

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Section: Discussionmentioning

confidence: 99%

Section: Rejection Of Non-transient Sources With Similar Colours As Oasmentioning

confidence: 99%

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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“…While many of these non-detections are simply due to the lack of rapid and deep optical follow-up observations, some events (after correction for Galactic extinction) are truly optically dark (e.g., Fynbo et al 2001;De Pasquale et al 2003;Castro-Tirado et al 2007;Rol et al 2007;Hashimoto et al 2010;Holland et al 2010).…”

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

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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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“…However, the properties of an unbiased sample of long GRBs hosts are still largely unknown, and selection effects due Article published by EDP Sciences A8, page 1 of 11 to optically-dark bursts (Groot et al 1998;Fynbo et al 2001;Perley et al 2009) arguably play a crucial role (e.g., Krühler et al 2011;Perley et al 2011a). Consequently, the conditions for the formation of GRBs, the relation between GRB hosts and field galaxies and the extent to which GRBs trace the cosmic star-formation rate (SFR) remain highly debated (e.g., Jakobsson et al 2005;Fruchter et al 2006;Kocevski et al 2009;Campisi et al 2011;Kocevski & West 2011).…”

Section: Introductionmentioning

confidence: 99%

The metal-enriched host of an energeticγ-ray burst atz ≈ 1.6

Krühler¹,

Fynbo²,

Geier³

et al. 2012

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Context. The star-forming nature of long γ-ray burst (GRB) host galaxies provides invaluable constraints on the progenitors of GRBs and might open a short-cut to the characteristics of typical star-forming galaxies throughout the history of the Universe. Due to the absence of near-infrared (NIR) spectroscopy, however, detailed investigations, specifically a determination of the gas-phase metallicity of gamma-ray burst hosts, was largely limited to redshifts z < 1 to date. Aims. We observed the galaxy hosting GRB 080605 at z = 1.64 using optical/NIR spectroscopy and high-resolution HST/WFC3 imaging in the rest-frame wavelength range between 1150 and 8700 Å. These data allow us to study a z > 1 GRB host in unprecedented detail and investigate the relation between GRB hosts and field galaxies. Methods. We availed of VLT/X-shooter optical/NIR spectroscopy to measure the metallicity, electron density, star-formation rate (SFR), and reddening of the host of GRB 080605. Specifically, we used different strong-line diagnostics to robustly measure the gas-phase metallicity within the interstellar medium (ISM) for the first time based on [N ii] at this redshift.Results. The host of the energetic (E γ,iso ∼ 2 × 10 53 erg) GRB 080605 at z ∼ 1.64 is a morphologically complex, vigorously starforming galaxy with an Hα-derived SFR of 31 +12 −6 M yr −1 . Its ISM is significantly enriched with metals. Specifically, [N ii]/Hα = 0.14 ± 0.02, which yields an oxygen abundance 12 + log(O/H) between 8.3 and 8.6 depending on the adopted strong-line calibrator. This corresponds to values in the range of 0.4−0.8 Z . For its measured stellar mass (M * = 8.0 +1.3 −1.6 × 10 9 M ) and SFR, this value is consistent with the fundamental metallicity relation defined by star-forming field galaxies. The absence of strong Lyα emission constrains the escape fraction of resonantly-scattered Lyα photons to f esc < ∼ 0.08. Conclusions. Our observations provide a detailed picture of the conditions in the ISM of a highly star-forming galaxy with irregular morphology at z ∼ 1.6. They include the first robust metallicity measurement based on [N ii] for a GRB host at z > 1 and directly illustrate that GRB hosts are not necessarily metal-poor, both on absolute scales as well as relative to their stellar mass and SFR. GRB hosts could thus be fair tracers of the population of ordinary star-forming galaxies at high redshift.

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Detection of the optical afterglow of GRB 000630: Implications for dark bursts

Cited by 129 publications

References 27 publications

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

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

The metal-enriched host of an energeticγ-ray burst atz ≈ 1.6

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