THE AFTERGLOW OF GRB 130427A FROM 1 TO 10<sup>16</sup>GHz

Perley, D.; Cenko, S. Bradley; Corsi, A.; Tanvir, N. R.; Levan, A. J.; Канн, Д. А.; Сонбас, Э.; Wiersema, K.; Zheng, W.; Zhao, Xiaoxia; Bai, J. M.; Bremer, M.; Castro-Tirado, A. J.; Chang, Liang; Clubb, K. I.; Frail, D. A.; Fruchter, A. S.; Göǧüş, E.; Greiner, J.; Güver, T.; Horesh, A.; Filippenko, A. V.; Klose, S.; Mao, J.; Morgan, A. N.; Pozanenko, A.; Schmidl, S.; Stecklum, B.; Tanga, M.; Volnova, A.; Volvach, A. E.; Wang, J.-G.; Winters, J. M.; Xin, Yu

doi:10.1088/0004-637x/781/1/37

Cited by 197 publications

(257 citation statements)

References 142 publications

(137 reference statements)

Supporting

Mentioning

226

Contrasting

Order By: Relevance

“…We have previously found strong RS signatures only in low density environments, which we attribute to the slow cooling RS SEDs expected in such environments (Laskar et al 2013(Laskar et al , 2016Perley et al 2014;Alexander et al 2017). Our best-fit model results in an afterglow SED in the fast cooling regime, increasing the likelihood that the RS SED is fast cooling as well.…”

Section: Summary and Discussionsupporting

confidence: 57%

“…Additionally, high-redshift GRBs have been speculated to possibly differ from lower redshift events in their energy scales, durations, and circumburst media (Fryer et al 2001;Bromm et al 2003;Heger et al 2003;Suwa & Ioka 2011;Toma et al 2011). Due to time dilation, high-redshift GRBs also afford an opportunity to capture rapidly evolving reverse shock emission, and thereby a means of probing the Lorentz factor and composition of the relativistic ejecta powering the afterglow (Piran 2005;Mészáros 2006;Laskar et al 2013Laskar et al , 2014Laskar et al , 2016Perley et al 2014;Alexander et al 2017).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Laskar

Berger

Chornock

et al. 2018

ApJ

View full text Add to dashboard Cite

We present the first results from a recently concluded study of GRBs at z  5 with the Karl G. Jansky Very Large Array (VLA). Spanning 1 to 85.5 GHz and 7 epochs from 1.5 to 82.3 days, our observations of GRB140311A are the most detailed joint radio and millimeter observations of a GRB afterglow at z  5 to date. In conjunction with optical/near-IR and X-ray data, the observations can be understood in the framework of radiation from a single blast wave shock with energy »É 8.5 10 K,iso 53 erg expanding into a constant density environment with density, » n 8 0 -cm 3 . The X-ray and radio observations require a jet break at » t 0.6 jet days, yielding an opening angle of q »  4 jet and a beaming-corrected blast wave kinetic energy of »É 2.2 10 K 50 erg. The results from our radio follow-up and multiwavelength modeling lend credence to the hypothesis that detected high-redshift GRBs may be more tightly beamed than events at lower redshift. We do not find compelling evidence for reverse shock emission, which may be related to fast cooling driven by the moderately high circumburst density.

show abstract

Section: Summary and Discussionsupporting

confidence: 57%

Section: Introductionmentioning

confidence: 99%

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Laskar

Berger

Chornock

et al. 2018

ApJ

View full text Add to dashboard Cite

show abstract

“…The only reported radio observation of GRB 140419A is a marginal radio detection of 1.5 mJy/beam at 93 GHz with CARMA, just 77 minutes post-burst (Perley 2014b). If real, this is the earliest ever reported radio detection of a GRB.…”

Section: C2 Grb 140419amentioning

confidence: 77%

“…However, based on the 15.7 GHz extrapolated light curve in Figure 6 of Veres et al (2015) it appears that our first AMI detection at 0.51 days post burst occurred around the peak in that radio band. This peak time is even earlier than the 15.7 GHz peak observed from GRB 130427A, which occurred around 0.6 − 0.9 days post-burst and was well described by a reverse-shock model component (Anderson et al 2014e;Perley 2014b), so such a scenario should not be ruled out.…”

Section: Grb 130907amentioning

confidence: 83%

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

Anderson

Staley

Horst

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the Arcminute Microkelvin Imager (AMI) Large Array catalogue of 139 gamma-ray bursts (GRBs). AMI observes at a central frequency of 15.7 GHz and is equipped with a fully automated rapid-response mode, which enables the telescope to respond to highenergy transients detected by Swift. On receiving a transient alert, AMI can be on-target within two minutes, scheduling later start times if the source is below the horizon. Further AMI observations are manually scheduled for several days following the trigger. The AMI GRB programme probes the early-time (< 1 day) radio properties of GRBs, and has obtained some of the earliest radio detections (GRB 130427A at 0.36 and GRB 130907A at 0.51 days post-burst). As all Swift GRBs visible to AMI are observed, this catalogue provides the first representative sample of GRB radio properties, unbiased by multi-wavelength selection criteria. We report the detection of six GRB radio afterglows that were not previously detected by other radio telescopes, increasing the rate of radio detections by 50% over an 18-month period. The AMI catalogue implies a Swift GRB radio detection rate of 15%, down to ∼ 0.2 mJy/beam. However, scaling this by the fraction of GRBs AMI would have detected in the Chandra & Frail sample (all radio-observed GRBs between 1997 − 2011), it is possible ∼ 44 − 56% of Swift GRBs are radio bright, down to ∼ 0.1 − 0.15 mJy/beam. This increase from the Chandra & Frail rate (∼ 30%) is likely due to the AMI rapid-response mode, which allows observations to begin while the reverse-shock is contributing to the radio afterglow.

show abstract

“…As mentioned earlier, for a wind environment the cooling frequency is expected to evolve as ν c ∝ t 1/2 . However, a non-evolving ν c can be found when k ∼ 1.5, suggesting that for GRB 120711A, ν c remains within the X-ray band for the entire observation (see also GRB 130427A, Perley et al 2014). The time evolution of ν c might also be modified if the microphysical parameters of the afterglow emission are time dependent (Panaitescu et al 2006;Filgas et al 2011).…”

Section: Segment Iii: Multi-wavelength Afterglow Emissionmentioning

confidence: 99%

GRB 120711A: an intense INTEGRAL burst with long-lasting softγ-ray emission and a powerful optical flash

Martín-Carrillo

Hanlon

Topinka

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

A long and intense γ-ray burst (GRB) was detected by INTEGRAL on 11 July 2012 with a duration of ∼115 s and fluence of 2.8 × 10 −4 erg cm −2 in the 20 keV−8 MeV energy range. GRB 120711A was at z ∼ 1.405 and produced soft γ-ray emission (>20 keV) for at least ∼10 ks after the trigger. The GRB was observed by several ground-based telescopes that detected a powerful optical flash peaking at an R-band brightness of ∼11.5 mag at ∼126 s after the trigger, or ∼9th magnitude when corrected for the host galaxy extinction (A V ∼ 0.85). The X-ray afterglow was monitored by the Swift, XMM-Newton, and Chandra observatories from 8 ks to 7 Ms and provides evidence for a jet break at ∼0.9 Ms. We present a comprehensive temporal and spectral analysis of the long-lasting soft γ-ray emission detected in the 20−200 keV band with INTEGRAL/IBIS, the Fermi/LAT post-GRB detection above 100 MeV, the soft X-ray afterglow and the optical/near-infrared detections from Watcher, Skynet/PROMPT, GROND, and REM. The prompt emission had a very hard spectrum (E peak ∼ 1 MeV) and yields an E γ,iso ∼ 10 54 erg (1 keV−10 MeV rest frame), making GRB 120711A one of the most energetic GRBs detected so far. We modelled the long-lasting soft γ-ray emission using the standard afterglow scenario, which indicates a forward shock origin. The combination of data extending from the near-infrared to GeV energies suggest that the emission is produced by a broken power-law spectrum consistent with synchrotron radiation. The afterglow is well modelled using a stratified wind-like environment with a density profile k ∼ 1.2, suggesting a massive star progenitor (i.e. Wolf-Rayet) with a mass-loss rate between ∼10 −5 −10 −6 M yr −1 depending on the value of the radiative efficiency (η γ = 0.2 or 0.5). The analysis of the reverse and forward shock emission reveals an initial Lorentz factor of ∼120−340, a jet half-opening angle of ∼2 • −5 • , and a baryon load of ∼10 −5 −10 −6 M consistent with the expectations of the fireball model when the emission is highly relativistic. Long-lasting soft γ-ray emission from other INTEGRAL GRBs with high peak fluxes, such as GRB 041219A, was not detected, suggesting that a combination of high Lorentz factor, emission above 100 MeV, and possibly a powerful reverse shock are required. Similar long-lasting soft γ-ray emission has recently been observed from the nearby and extremely bright Fermi/LAT burst GRB 130427A.

show abstract

THE AFTERGLOW OF GRB 130427A FROM 1 TO 10¹⁶GHz

Cited by 197 publications

References 142 publications

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

GRB 120711A: an intense INTEGRAL burst with long-lasting softγ-ray emission and a powerful optical flash

Contact Info

Product

Resources

About

THE AFTERGLOW OF GRB 130427A FROM 1 TO 1016GHz

Cited by 197 publications

References 142 publications

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

GRB 120711A: an intense INTEGRAL burst with long-lasting softγ-ray emission and a powerful optical flash

Contact Info

Product

Resources

About

THE AFTERGLOW OF GRB 130427A FROM 1 TO 10¹⁶GHz