GRB 071112c: A Case Study of Different Mechanisms in X-Ray and Optical Temporal Evolution

Huang, K. Y.; Urata, Y.; Tung, Yu-Hsin; Lin, Hsiu Mei; Xin, L. P.; Yoshida, Michitoshi; Zheng, W.; Akerlof, C.; Wang, S. Y.; Ip, W.-H.; Lehner, M. J.; Bianco, Federica; Kawai, N.; Kuroda, D.; Marshall, Stuart; Schwamb, Megan E.; Qiu, Y.; Wang, J. H.; Wen, C. Y.; Wei, J. Y.; Yanagisawa, K.; Zhang, Z. W.

doi:10.1088/0004-637x/748/1/44

Cited by 12 publications

(5 citation statements)

References 41 publications

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“…A less intense flare was observed in the GRB 071112C X-ray afterglow. The fact that no corresponding flare was detected in the optical was used by Huang et al (2012) to argue that different mechanisms were responsible for the time evolution of the X-ray and optical afterglows. The simple power-law structure of the optical light curve was shown to be consistent with the external shock model, whereas late injection and internal shocks inside the jet itself were invoked to explain the excess X-ray emission.…”

Section: Discussionmentioning

confidence: 99%

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Gamma-Ray Bursts in Circumstellar Shells: A Possible Explanation for Flares

Mesler

Whalen

Lloyd-Ronning

et al. 2012

ApJ

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It is now generally accepted that long-duration gamma-ray bursts (GRBs) are due to the collapse of massive rotating stars. The precise collapse process itself, however, is not yet fully understood. Strong winds, outbursts, and intense ionizing UV radiation from single stars or strongly interacting binaries are expected to destroy the molecular cloud cores that give birth to them and create highly complex circumburst environments for the explosion. Such environments might imprint features on GRB light curves that uniquely identify the nature of the progenitor and its collapse. We have performed numerical simulations of realistic environments for a variety of long-duration GRB progenitors with ZEUS-MP and have developed an analytical method for calculating GRB light curves in these profiles. Though a full, three-dimensional, relativistic magnetohydrodynamical computational model is required to precisely describe the light curve from a GRB in complex environments, our method can provide a qualitative understanding of these phenomena. We find that, in the context of the standard afterglow model, massive shells around GRBs produce strong signatures in their light curves, and that this can distinguish them from those occurring in uniform media or steady winds. These features can constrain the mass of the shell and the properties of the wind before and after the ejection. Moreover, the interaction of the GRB with the circumburst shell is seen to produce features that are consistent with observed X-ray flares that are often attributed to delayed energy injection by the central engine. Our algorithm for computing light curves is also applicable to GRBs in a variety of environments such as those in high-redshift cosmological halos or protogalaxies, both of which will soon be targets of future surveys such as the Joint Astrophysics Nascent Satellite or Lobster.

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Section: Discussionmentioning

confidence: 99%

“…et al 2011), GRB 071112C (Huang et al 2012), GRB 050502B (Falcone et al 2006), GRB 060607A (Ziaeepour et al 2008), and GRB 050421 (Godet et al 2006). It is generally accepted that these flares are a product of late-time injections of energy into the system by the GRB's central engine, but this is not the only possible scenario.…”

Section: Introductionmentioning

confidence: 99%

Gamma-Ray Bursts in Circumstellar Shells: A Possible Explanation for Flares

Mesler

Whalen

Lloyd-Ronning

et al. 2012

ApJ

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“…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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“…The onset process were reported in some bursts (e.g., Molinari et al, 2007;Huang et al, 2012) , thanks to the fast slew capability of Swif t satellite and quick multi-wavelength follow-up observations by ground-based telescopes. In those reports, other radiations from reverse shock or internal shock or others were detected in optical or X-ray light curves.…”

Section: Introductionmentioning

confidence: 99%

“…For example, the variation in the optical light curve of GRB 060607 (Molinari et al, 2007) at the later phase was detected. During X-ray observations, flares (e.g., Burrows et al, 2005) or emission in steep decay phase which is related with internal-shock process were detected (e.g., Zhang 2007;Huang et al, 2012). Recently, Li et al,(2015) found that in 87 well sampled and simultaneously observed GRBs, only 9 GRBs match the prediction of the standard fireball model, and have a single power law decay in both energy bands during their entire observations.…”

Section: Introductionmentioning

confidence: 99%

Optical light curve of GRB 121011A: a textbook for the onset of GRB afterglow in a mixture of ISM and wind-type medium

Xin

Wei

Qiu

et al. 2016

Res. Astron. Astrophys.

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We reported the optical observations of GRB 121011A by 0.8-m TNT telescope at Xinglong observatory, China. The light curve of optical afterglow shows a smooth and featureless bump during the epoch of ∼130 sec and ∼5000 sec with a rising index of 1.57 ± 0.28 before the break time of 539 ± 44 sec, and a decaying index of about 1.29 ± 0.07 up to the end of our observations. Meanwhile, the X-ray light curve decays in a single power-law with a slop of about 1.51 ± 0.03 observed by XRT onboard Swif t from 100 sec to about 10000 sec after the burst trigger. The featureless optical light curve could be understood as an onset process under the external-shock model. The typical frequency has been below or near the optical one before the deceleration time, and the cooling frequency is located between the optical and X-ray wavelengths. The external medium density has a transition from a mixed stage of ISM and wind-type medium before the peak time to the ISM at the later phase. The joint-analysis of X-ray and optical light curves shows that the emission from both frequencies are consistent with the prediction of the standard afterglow model without any energy injections, indicating that the central engine has stopped its activity and does not restart anymore after the prompt phase.

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GRB 071112c: A Case Study of Different Mechanisms in X-Ray and Optical Temporal Evolution

Cited by 12 publications

References 41 publications

Gamma-Ray Bursts in Circumstellar Shells: A Possible Explanation for Flares

Gamma-Ray Bursts in Circumstellar Shells: A Possible Explanation for Flares

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

Optical light curve of GRB 121011A: a textbook for the onset of GRB afterglow in a mixture of ISM and wind-type medium

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