GRB 091127: The cooling break race on magnetic fuel

Filgas, R.; Greiner, J.; Schady, P.; Krühler, T.; Updike, A. C.; Klose, S.; Nardini, M.; Канн, Д. А.; Rossi, A.; Sudilovsky, V.; Afonso, P.; Clemens, C.; Elliott, J.; Guelbenzu, A. Nicuesa; Rau, A.

doi:10.1051/0004-6361/201117695

Cited by 64 publications

(81 citation statements)

References 76 publications

(102 reference statements)

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“…Flux calibration was therefore cross-checked by using photometric afterglow observations at (or near) the epoch in which the spectra were taken. We used light curves published by Wiersema et al (2012) and Filgas et al (2011) for GRBs 091018 and 091127, respectively. For GRB 071112C, the joint data sets of Huang et al (2012) and Covino et al (2013) were used.…”

Section: Flux Calibration Verificationmentioning

confidence: 99%

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

Japelj

Vergani

Salvaterra

et al. 2016

A&A

100

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Aims. Long gamma-ray bursts (LGRBs) are associated with the deaths of massive stars and might therefore be a potentially powerful tool for tracing cosmic star formation. However, especially at low redshifts (z < 1.5) LGRBs seem to prefer particular types of environment. Our aim is to study the host galaxies of a complete sample of bright LGRBs to investigate the effect of the environment on GRB formation. Methods. We studied host galaxy spectra of the Swift/BAT6 complete sample of 14 z < 1 bright LGRBs. We used the detected nebular emission lines to measure the dust extinction, star formation rate (SFR), and nebular metallicity (Z) of the hosts and supplemented the data set with previously measured stellar masses M . The distributions of the obtained properties and their interrelations (e.g. mass-metallicity and SFR-M relations) are compared to samples of field star-forming galaxies. Results. We find that LGRB hosts at z < 1 have on average lower SFRs than if they were direct star formation tracers. By directly comparing metallicity distributions of LGRB hosts and star-forming galaxies, we find a good match between the two populations up to 12 + log O H ∼ 8.4−8.5, after which the paucity of metal-rich LGRB hosts becomes apparent. The LGRB host galaxies of our complete sample are consistent with the mass-metallicity relation at similar mean redshift and stellar masses. The cutoff against high metallicities (and high masses) can explain the low SFR values of LGRB hosts. We find a hint of an increased incidence of starburst galaxies in the Swift/BAT6 z < 1 sample with respect to that of a field star-forming population. Given that the SFRs are low on average, the latter is ascribed to low stellar masses. Nevertheless, the limits on the completeness and metallicity availability of current surveys, coupled with the limited number of LGRB host galaxies, prevents us from investigating more quantitatively whether the starburst incidence is such as expected after taking into account the high-metallicity aversion of LGRB host galaxies.

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Section: Flux Calibration Verificationmentioning

confidence: 99%

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

Japelj

Vergani

Salvaterra

et al. 2016

A&A

100

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“…The optical AG was confirmed with GROND observations (Updike et al 2009) adding NIR detections. The full analysis of the GROND AG light curve was presented in Filgas et al (2011). The SN classification became official based on the photometric SN bump (Cobb et al 2010a,b) and spectroscopy was published later showing BL features (Berger et al 2011).…”

Section: Grb 081007/sn 2008hwmentioning

confidence: 99%

“…Obeying the fireball model for GRB AGs, the high-energy (β X ) and the low-energy (β opt ) spectral indexes are correlated by β X = β opt + 0.5 for E break ≈ E cooling , where the latter comes from the cooling frequency of the electrons, except in the case of GRB 091127 were β opt varies in the range 0.25-0.62. (a) The quoted values of β X , N H, host , and reduced χ 2 are computed from the simultaneous best fit to all eight GROND/XRT SEDs by Filgas et al (2011). The E break range comes from an observed evolution of β opt .…”

Section: Grb 101219b/sn 2010mamentioning

confidence: 99%

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Multiwavelength analysis of three supernovae associated with gamma-ray bursts observed by GROND

Greiner

Schady

Klose

et al. 2015

A&A

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Context. After the discovery of the first connection between γ-ray bursts (GRBs) and supernovae (SNe) almost two decades ago, tens of SN-like rebrightenings have been discovered and about seven solid associations have been spectroscopically confirmed to date. Aims. We determine the luminosity, evolution, and origin of three SN rebrightenings in GRB afterglow light curves at z ∼ 0.5 along with accurate determinations of the host-galaxy extinction. We estimate physical parameters of the SN explosions, such as synthesised 56 Ni mass, ejecta mass, and kinetic energy. Methods. We employ GROND optical/NIR data and Swift X-ray/UV data to estimate the host-galaxy extinction by modelling the afterglow spectral energy distribution, to determine the SN luminosity and evolution, and to construct quasi-bolometric light curves. The latter are corrected for the contribution of the NIR-bands using data available in the literature and black-body fits. We employ Arnett's analytic approach to obtain the physical parameters of the explosion. Conclusions. By means of a very comprehensive data set, we found that the luminosity and the 56 Ni mass of SNe 2008hw, 2009nz, and 2010ma resembles those of other known GRB-associated SNe. These findings strengthens previous claims of GRB-SNe being brighter than stripped-envelope SNe unaccompanied by GRBs.

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“…Some of the rebrightenings and bumps (Panaitescu et al 1998;Granot et al 2003;Guetta et al 2007) are attributed to refreshed shocks Panaitescu et al 1998), the others to density variations (Ramirez-Ruiz et al 2001;Dai & Lu 2002;Dai & Wu 2003;Panaitescu & Kumar 2004) or two-component jets (Berger et al 2003;Huang et al 2004;Peng et al 2005;Granot et al 2006;Racusin et al 2008;Filgas et al 2011b). However, with the latest generation of GRB instruments capable of high sampling in both time and energy domains, the modifications made to the standard model still fall short to explaining the observed afterglows consistently (e.g., Nardini et al 2011;Filgas et al 2011a).…”

Section: Introductionmentioning

confidence: 99%

GRB 091029: at the limit of the fireball scenario

Filgas

Greiner

Schady

et al. 2012

A&A

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Aims. Using high-quality, broad-band afterglow data for GRB 091029, we test the validity of the forward-shock model for gamma-ray burst afterglows. Methods. We used multi-wavelength (NIR to X-ray) follow-up observations obtained with the GROND, BOOTES-3/YA and Stardome optical ground-based telescopes, and the UVOT and the XRT onboard the Swift satellite. The resulting data of excellent accuracy allow us to construct a multi-wavelength light curve with relative photometric errors as low as 1%, as well as the well-sampled spectral energy distribution covering 5 decades in energy. Results. The optical/NIR and the X-ray light curves of the afterglow of GRB 091029 are almost totally decoupled. The X-ray light curve shows a shallow rise with a peak at ∼7 ks and a decay slope of α ∼ 1.2 afterwards, while the optical/NIR light curve shows a much steeper early rise with a peak around 400 s, followed by a shallow decay with temporal index of α ∼ 0.6, a bump and a steepening of the decay afterwards. The optical/NIR spectral index decreases gradually by over 0.3 before this bump, and then slowly increases again, while the X-ray spectral index remains constant throughout the observations. Conclusions. To explain the decoupled light curves in the X-ray and optical/NIR domains, a two-component outflow is proposed. Several models are tested, including continuous energy injection, components with different electron energy indices and components in two different stages of spectral evolution. Only the last model can explain both the decoupled light curves with asynchronous peaks and the peculiar SED evolution. However, this model has so many unknown free parameters that we are unable to reliably confirm or disprove its validity, making the afterglow of GRB 091029 difficult to explain in the framework of the simplest fireball model. This conclusion provides evidence that a scenario beyond the simplistic assumptions is needed to be able to model the growing number of well-sampled afterglow light curves.

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GRB 091127: The cooling break race on magnetic fuel

Cited by 64 publications

References 76 publications

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

Multiwavelength analysis of three supernovae associated with gamma-ray bursts observed by GROND

GRB 091029: at the limit of the fireball scenario

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