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

Gorosabel, J.; Fynbo, J.; Hjorth, J.; Wolf, Christian; Andersen, M. I.; Pedersen, H.; Christensen, L.; Jensen, B. L.; Møller, Per; Afonso, J.; Treyer, Marie; Mallén‐Ornelas, G.; Castro‐Tirado, A. J.; Fruchter, A. S.; Greiner, J.; Pian, E.; Vreeswijk, P. M.; Frontera, F.; Kaper, L.; Klose, S.; Kouveliotou, C.; Masetti, N.; Palazzi, E.; Rol, E.; Salamanca, I.; Tanvir, N. R.; Wijers, R. A. M. J.; Heuvel, E. van den

doi:10.1051/0004-6361:20011598

Cited by 17 publications

(9 citation statements)

References 54 publications

(74 reference statements)

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“…These colors are consistent with the ones expected of a GRB afterglow (see the shaded region of the color-color diagram in Fig. 2 of Gorosabel et al (2002a)).…”

Section: Optical/near-infrared Sedsupporting

confidence: 88%

Very High Column Density and Small Reddening toward GRB 020124 atz = 3.20

Hjorth

Møller

Gorosabel

et al. 2003

ApJ

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102

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We present optical and near-infrared observations of the dim afterglow of GRB 020124, obtained between 2 and 68 hours after the gamma-ray burst. The burst occurred in a very faint (R 29.5) Damped Lyα Absorber (DLA) at a redshift of z = 3.198±0.004. The derived column density of neutral hydrogen is log(N HI ) = 21.7 ± 0.2 and the rest-frame reddening is constrained to be E(B − V) < 0.065, i.e., A V < 0.20 for standard extinction laws with R V ≈ 3. The resulting dust-togas ratio is less than 11% of that found in the Milky Way, but consistent with the SMC and high-redshift QSO DLAs, indicating a low metallicity and/or a low dust-to-metals ratio in the burst environment. A grey extinction law (large R V ), produced through preferential destruction of small dust grains by the GRB, could increase the derived A V and dust-to-gas ratio. The dimness of the afterglow is however fully accounted for by the high redshift: If GRB 020124 had been at z = 1 it would have been approximately 1.8 mag brighter-in the range of typical bright afterglows.

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“…These colors are consistent with the ones expected of a GRB afterglow (see the shaded region of the color-color diagram in Fig. 2 of Gorosabel et al (2002a)).…”

Section: Optical/near-infrared Sedsupporting

confidence: 88%

Very High Column Density and Small Reddening toward GRB 020124 atz = 3.20

Hjorth

Møller

Gorosabel

et al. 2003

ApJ

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102

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“…The optical and NIR colors of the OT of GRB 000911 during the first 10 days after the high-energy event fall in the loci populated by GRB afterglows in the color−color diagrams as illustrated by Šimon et al (2001) and by Gorosabel et al (2002).…”

Section: Grb 000911 Optical-nir Afterglow Light Curvesmentioning

confidence: 85%

Late-epoch optical and near-infrared observations of the GRB 000911 afterglow and its host galaxy

Masetti¹,

Palazzi²,

Pian

et al. 2005

A&A

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Abstract. We present the results of an optical and near-infrared (NIR) monitoring campaign of the counterpart of Gamma-Ray Burst (GRB) 000911, located at redshift z = 1.06, from 5 days to more than 13 months after explosion. Our extensive dataset is a factor of 2 larger and spans a time interval ∼4 times longer than the ones considered previously for this GRB afterglow; this allows a more thorough analysis of its light curve and of the GRB host galaxy properties. The afterglow light curves show a single power-law temporal decline, modified at late times by light from a host galaxy with moderate intrinsic extinction, and possibly by an emerging supernova (SN). The afterglow evolution is interpreted within the classical "fireball" scenario as a weakly collimated adiabatic shock propagating in the interstellar medium. The presence of a SN light curve superimposed on the non-thermal afterglow emission is investigated: while in the optical bands no significant contribution to the total light is found from a SN, the NIR J-band data show an excess which is consistent with a SN as bright as the known hypernova SN1998bw. If the SN interpretation is true, this would be the farthest GRB-associated SN, as well as the farthest core-collapse SN, discovered to date. However, other possible explanations of this NIR excess are also investigated. Finally, we studied the photometric properties of the host, and found that it is likely to be a slightly reddened, subluminous, extreme starburst compact galaxy, with luminosity ∼0.1 L , an age of ∼0.5 Gyr and a specific Star Formation Rate (SFR) of ≈30 M yr −1 (L/L ) −1 . This is the highest specific SFR value for a GRB host inferred from optical/NIR data.

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“…Optical/NIR spectroscopy will discriminate extragalactic transients (e.g. Gorosabel et al 2002), low-frequency (mm and radio bands) observations 6 could be used (as shown in Fig. 4) to distinguish among possible competing transients sources.…”

Section: Discussionmentioning

confidence: 99%

Unveiling the population of orphanγ-ray bursts

Ghirlanda

Salvaterra

Campana

et al. 2015

A&A

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Gamma-ray bursts (GRBs) are detectable in the γ-ray band if their jets are oriented toward the observer. However, for each GRB with a typical θ jet , there should be ∼2/θ 2 jet bursts whose emission cone is oriented elsewhere in space. These off-axis bursts can eventually be detected when, due to the deceleration of their relativistic jets, the beaming angle becomes comparable to the viewing angle. Orphan afterglows (OAs) should outnumber the current population of bursts detected in the γ-ray band even if they have not been conclusively observed so far at any frequency. We compute the expected flux of the population of orphan afterglows in the mm, optical, and X-ray bands through a population synthesis code of GRBs and the standard afterglow emission model. We estimate the detection rate of OAs with ongoing and forthcoming surveys. The average duration of OAs as transients above a given limiting flux is derived and described with analytical expressions: in general OAs should appear as daily transients in optical surveys and as monthly/yearly transients in the mm/radio band. We find that ∼2 OA yr −1 could already be detected by Gaia and up to 20 OA yr −1 could be observed by the ZTF survey. A larger number of 50 OA yr −1 should be detected by LSST in the optical band. For the X-ray band, ∼26 OA yr −1 could be detected by the eROSITA. For the large population of OA detectable by LSST, the X-ray and optical follow up of the light curve (for the brightest cases) and/or the extensive follow up of their emission in the mm and radio band could be the key to disentangling their GRB nature from other extragalactic transients of comparable flux density.

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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

Cited by 17 publications

References 54 publications

Very High Column Density and Small Reddening toward GRB 020124 atz = 3.20

Very High Column Density and Small Reddening toward GRB 020124 atz = 3.20

Late-epoch optical and near-infrared observations of the GRB 000911 afterglow and its host galaxy

Unveiling the population of orphanγ-ray bursts

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