Signatures of Extragalactic Dust in Pre‐<i>Swift</i>GRB Afterglows

Канн, Д. А.; Klose, S.; Zeh, A.

doi:10.1086/500652

Cited by 304 publications

(605 citation statements)

References 128 publications

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“…Despite the low amount of energy that was promptly released, this is among the most luminous afterglows ever detected (Kann et al 2006), even compared to a much larger Swift-era sample (Kann et al 2010). The multiwavelength temporal evolution of the GRB 021004 afterglow can be explained by multiple energy injections (Björnsson et al 2004;de Ugarte Postigo et al 2005), although other scenarios cannot be discarded (Lazzati et al 2002).…”

Section: Introductionmentioning

confidence: 87%

“…The isotropic energy release during the prompt emission of this GRB was modest, with log E iso = 52.65 +0.12 −0.17 (Kann et al 2010), and the dust extinction for this somehow reddish afterglow (R − K ∼ 3) was also low as is typical of many wellobserved afterglows (Kann et al 2006). Despite the low amount of energy that was promptly released, this is among the most luminous afterglows ever detected (Kann et al 2006), even compared to a much larger Swift-era sample (Kann et al 2010).…”

Section: Introductionmentioning

confidence: 93%

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GRB 021004: Tomography of a gamma-ray burst progenitor and its host galaxy

Castro-Tirado¹,

Møller

Garcı́a-Segura³

et al. 2010

A&A

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Aims. We analyse the distribution of matter around the progenitor star of gamma-ray burst GRB 021004 and the properties of its host galaxy with high-resolution echelle and near-infrared spectroscopy. Methods. Observations were taken by the 8.2 m Very Large Telescope with the Ultraviolet and Visual Echelle spectrograph (UVES) and the Infrared Spectrometer And Array Camera (ISAAC) between 10 and 14 h after the onset of the event.Results. We report the first detection of emission lines from a GRB host galaxy in the near-infrared, detecting Hα and the [O III] doublet. These allow us to independently measure the systemic redshift (z = 2.3304 ± 0.0005), which is not contaminated by absorption as the Lyα line is, and infer the host galaxy properties. From the visual echelle spectroscopy, we find several absorptionline groups spanning a range of about 3000 km s −1 in velocity relative to the redshift of the host galaxy. The absorption profiles are very complex with both velocity-broadened components extending over several 100 km s −1 and narrow lines with velocity widths of only ∼20 km s −1 . By analogy with QSO absorption line studies, the relative velocities, widths, and degrees of ionization of the lines ("line-locking", "ionization-velocity correlation") show that the progenitor had both an extremely strong radiation field and several distinct mass-loss phases (winds). Conclusions. These results are consistent with GRB progenitors being massive stars, such as luminous blue variables (LBVs) or Wolf-Rayet stars, providing a detailed picture of the spatial and velocity structure of the GRB progenitor star at the time of explosion. The host galaxy is a prolific star-forming galaxy with a SFR of ∼40 M yr −1 .

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Section: Introductionmentioning

confidence: 87%

Section: Introductionmentioning

confidence: 93%

GRB 021004: Tomography of a gamma-ray burst progenitor and its host galaxy

Castro-Tirado¹,

Møller

Garcı́a-Segura³

et al. 2010

A&A

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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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“…With knowledge of the distance from the redshift determination and the local dust extinction from the SED fitting, we are able to compare the afterglows of our sample of LAT-detected GRBs (where we also include GRB 080916C, Greiner et al 2009a) with a large sample of well observed GRB afterglows presented in Kann et al (2006) (pre-Swift long GRBs), Kann et al (2009a) (Swift-era long GRBs) and Kann et al (2008) (Swift-era short GRBs). Using the method detailed in Kann et al (2006), the afterglows are corrected for host-galaxy extinction and all shifted to a common redshift of z = 1, so they can be compared directly both in terms of temporal evolution as well as luminosity.…”

Section: Optical Afterglows Of Lat-detected Grbs In Comparison With Tmentioning

confidence: 99%

Optical and near-infrared follow-up observations of fourFermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies

McBreen

Krühler

Rau

et al. 2010

A&A

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100

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Aims. Fermi can measure the spectral properties of gamma-ray bursts over a very large energy range and is opening a new window on the prompt emission of these energetic events. Localizations by the instruments on Fermi in combination with follow-up by Swift provide accurate positions for observations at longer wavelengths leading to the determination of redshifts, the true energy budget, host galaxy properties and facilitate comparison with pre-Fermi bursts. Methods. Multi-wavelength follow-up observations were performed on the afterglows of four bursts with high energy emission detected by Fermi/LAT: GRB 090323, GRB 090328, GRB 090510 and GRB 090902B. They were obtained in the optical/near-infrared bands with GROND mounted at the MPG/ESO 2.2 m telescope and additionally of GRB 090323 in the optical with the 2 m telescope in Tautenburg, Germany. Three of the events are classified as long bursts while GRB 090510 is a well localized short GRB with GeV emission. In addition, host galaxies were detected for three of the four bursts. Spectroscopic follow-up was initiated with the VLT for GRB 090328 and GRB 090510. Results. The afterglow observations in 7 bands are presented for all bursts and their host galaxies are investigated. Knowledge of the distance and the local dust extinction enables comparison of the afterglows of LAT-detected GRBs with the general sample. The spectroscopic redshifts of GRB 090328 and GRB 090510 were determined to be z = 0.7354 ± 0.0003 and z = 0.903 ± 0.001 and dust corrected star-formation rates of 4.8 M yr −1 and 0.60 M yr −1 were derived for their host galaxies, respectively. Conclusions. The afterglows of long bursts exhibit power-law decay indices (α) from less than 1 to ∼2.3 and spectral indices (β opt ) values from 0.65 to ∼1.2 which are fairly standard for GRB afterglows. Constraints are placed on the jet half opening angles of < ∼ 2.1 • to > ∼ 6.4 • , which allows limits to be placed on the beaming corrected energies. These range from < ∼ 5 × 10 50 erg to the one of the highest values ever recorded, > ∼ 2.2 × 10 52 erg for GRB 090902B, and are not consistent with a standard candle. The extremely energetic long Fermi bursts have optical afterglows which lie in the top half of the brightness distribution of all optical afterglows detected in the Swift era or even in the top 5% if incompleteness is considered. The properties of the host galaxies of these LAT detected bursts in terms of extinction, star formation rates and masses do not appear to differ from previous samples.

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Signatures of Extragalactic Dust in Pre‐SwiftGRB Afterglows

Cited by 304 publications

References 128 publications

GRB 021004: Tomography of a gamma-ray burst progenitor and its host galaxy

GRB 021004: Tomography of a gamma-ray burst progenitor and its host galaxy

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

Optical and near-infrared follow-up observations of fourFermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies

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