Afterglow light curves, viewing angle and the jet structure of  -ray bursts

Rossi, Elena M.; Lazzati, Davide; Rees, M. J.

doi:10.1046/j.1365-8711.2002.05363.x

Cited by 435 publications

(492 citation statements)

References 22 publications

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“…Several modifications have been suggested to explain some of the observed fluctuations, flares, bumps and wiggles. Such modifications may include different density profiles and fluctuations (Wang & Loeb 2000;Ramirez-Ruiz et al 2001;Dai & Lu 2002;, energy injections (Rees & Meszaros 1998;Sari & Mészáros 2000;Granot et al 2003;Björnsson et al 2004;Jóhannesson et al 2006), jets with complex structure (Mészáros et al 1998;Kumar & Piran 2000;Rossi et al 2002), late engine activity (Dai & Lu 1998;Zhang & Mészáros 2002;Ramirez-Ruiz 2004), microlensing (Loeb & Perna 1998;Garnavich et al 2000;Ioka & Nakamura 2001) or dust echoes (Esin & Blandford 2000;Mészáros & Gruzinov 2000;Reichart 2001). Discerning the different scenarios is only possible through the analysis of the SEDs obtained with multiwavelength observations (see Sect.…”

Section: The Physics Of Grbs and Their Environmentsmentioning

confidence: 99%

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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Section: The Physics Of Grbs and Their Environmentsmentioning

confidence: 99%

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

Postigo

Lundgren

Martín

et al. 2012

A&A

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“…In particular, we assume an opening angle that varies between min 0:05 and max 0:5 (with a power law distribution of the form / 1 ÿ cos s where the index is s ÿ1:5) and an absolute gamma-ray energy per GRB of 5 10 51 erg released in t 10 s, all of which are well within the reasonable ranges of these parameters [57] assuming a uniform jet (see Ref. [58] for alternative jet models).…”

Section: Metals and The Predicted Grb Ratementioning

confidence: 99%

Enhanced cosmological GRB rates and implications for cosmogenic neutrinos

Yüksel

Kistler

2007

Phys. Rev. D

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Gamma-ray bursts, which are among the most violent events in the Universe, are one of the few viable candidates to produce ultra high-energy cosmic rays. Recently, observations have revealed that GRBs generally originate from metal-poor, low-luminosity galaxies and do not directly trace cosmic star formation, as might have been assumed from their association with core-collapse supernovae. Several implications follow from these findings. The redshift distribution of observed GRBs is expected to peak at higher redshift (compared to cosmic star formation), which is supported by the mean redshift of the Swift GRB sample, hzi 3. If GRBs are, in fact, the source of the observed UHECR, then cosmic-ray production would evolve with redshift in a stronger fashion than has been previously suggested. This necessarily leads, through the GZK process, to an enhancement in the flux of cosmogenic neutrinos, providing a near-term approach for testing the gamma-ray burst-cosmic-ray connection with ongoing and proposed UHE neutrino experiments.

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“…Originally E ¼ 2 was suggested ( Rossi et al 2002;Zhang & Meszaros 2002) for a surface energy density that is a power law in the jet off-axis angle, while a Gaussian surface -Scatter plot of E iso vs. E iso; min . On the dotted line E iso ¼ E iso; min .…”

Section: Power-law E Iso Distributionmentioning

confidence: 99%

“…On the other hand, in the universal jet profile model (Rossi et al 2002;Zhang & Meszaros 2002) all jets have the same surface energy density as a function of off-axis angle (the angle from the jet axis), and thus the observed differences in L B or E iso result from the angle v between the jet axis and the line of sight. This model predicts that the energy probability distribution is a power law with index E , where Rossi et al (2002) and Zhang & Meszaros (2002) suggested k ¼ À2, resulting in E ¼ 2, to reproduce the distributions observed by Frail et al (2001), although this was not a firm prediction. A Gaussian surface energy density profile results in E ¼ 1 (Lloyd-Ronning et al 2004).…”

Section: Introductionmentioning

confidence: 99%

Gamma‐Ray Burst Intensity Distributions

Band

Norris

Bonnell³

2004

ApJ

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We use the lag-luminosity relation to calculate self-consistently the redshifts, apparent peak bolometric luminosities L B , and isotropic energies E iso for a large sample of BATSE gamma-ray bursts. We consider two different forms of the lag-luminosity relation; for both forms the median redshift for our burst database is 1.6. We model the resulting E iso sample with power-law and Gaussian probability distributions without redshift evolution, both of which are reasonable models. The power-law model has an index of E ¼ 1:76 AE 0:05 (95% confidence), where p(E iso ) / E À E iso . The simple universal jet profile model suggested but did not require E ¼ 2, and subsequent physically reasonable refinements to this model permit greater diversity in E , as well as deviations from a power law; therefore, our observed E iso probability distribution does not disprove the universal jet model.

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Afterglow light curves, viewing angle and the jet structure of -ray bursts

Cited by 435 publications

References 22 publications

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

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

Enhanced cosmological GRB rates and implications for cosmogenic neutrinos

Gamma‐Ray Burst Intensity Distributions

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