Gamma-Ray Burst Prompt Correlations

Dainotti, Maria Giovanna; Vecchio, R. Del; Tarnopolski, Mariusz

doi:10.1155/2018/4969503

Cited by 58 publications

(21 citation statements)

References 270 publications

(387 reference statements)

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“…The rest frame times are the observed times divided by the cosmic time expansion, for example, T . Right panel: the observed light curve for GRB 061121 with the best-fit W07 model superimposed from Dainotti et al (2016a). The red dot marks the end of the flat plateau phase in the X-ray afterglow (T X,a , F X,a ).…”

Section: Notationsmentioning

confidence: 99%

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Gamma Ray Burst afterglow and prompt-afterglow relations: An overview

Dainotti

Vecchio

2017

New Astronomy Reviews

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The mechanism responsible for the afterglow emission of Gamma Ray Bursts (GRBs) and its connection to the prompt γ-ray emission is still a debated issue. Relations between intrinsic properties of the prompt or afterglow emission can help to discriminate between plausible theoretical models of GRB production. Here we present an overview of the afterglow and prompt-afterglow two parameter relations, their physical interpretations, their use as redshift estimators and as possible cosmological tools. A similar task has already been correctly achieved for Supernovae (SNe) Ia by using the peak magnitude-stretch relation, known in the literature as the Phillips relation (Phillips 1993). The challenge today is to make GRBs, which are amongst the farthest objects ever observed, standardizable candles as the SNe Ia through well established and robust relations. Thus, the study of relations amongst the observable and physical properties of GRBs is highly relevant together with selection biases in their physical quantities. Therefore, we describe the state of the art of the existing GRB relations, their possible and debated interpretations in view of the current theoretical models and how relations are corrected for selection biases. We conclude that only after an appropriate evaluation and correction for selection effects can GRB relations be used to discriminate among the theoretical models responsible for the prompt and afterglow emission and to estimate cosmological parameters.

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Section: Notationsmentioning

confidence: 99%

“…The interpretation of this discrepancy between the slopes opens a new perspective in the theoretical understanding of these observational facts, see the next section for details. As a further step, Dainotti et al (2016a) analyzed this relation adding as a third parameter T X,a with a sample of 122…”

Section: E4 E0095mentioning

confidence: 99%

Gamma Ray Burst afterglow and prompt-afterglow relations: An overview

Dainotti

Vecchio

2017

New Astronomy Reviews

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“…In addition, there are many correlations present among observed and fitted GRB variables (e.g. see the recent review by Dainotti et al (2018)), which may help to elucidate the underlying progenitor. with redshift, even when accounting for Malmquist-type biases and selection effects in the observed data.…”

Section: Introductionmentioning

confidence: 99%

The evolution of gamma-ray burst jet opening angle through cosmic time

Lloyd-Ronning

Hurtado

Aykutalp

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Jet opening angles of long gamma-ray bursts (lGRBs) appear to evolve in cosmic time, with lGRBs at higher redshifts being on average more narrowly beamed than those at lower redshifts. We examine the nature of this anti-correlation in the context of collimation by the progenitor stellar envelope. First, we show that the data indicate a strong correlation between gamma-ray luminosity and jet opening angle, and suggest this is a natural selection effect -only the most luminous GRBs are able to successfully launch jets with large opening angles. Then, by considering progenitor properties expected to evolve through cosmic time, we show that denser stars lead to more collimated jets, and argue that the observed anti-correlation between opening angle and redshift can be accounted for if lGRB massive star progenitors at high redshifts have higher average density compared to those at lower redshifts. This may be viable for an evolving IMF, and under the assumption that average density scales directly with mass, this relationship is consistent with the form of the IMF characteristic mass evolution suggested in the literature. The jet angle-redshift anti-correlation may also be explained if the lGRB progenitor population is dominated by massive stars at high redshift, while lower redshift lGRBs allow for a greater diversity of progenitor systems. Overall, however, we find both the jet angle-redshift anti-correlation and jet angle-luminosity correlation are consistent with the conditions of jet launch through, and collimation by, the envelope of a massive star progenitor.In this paper, we consider how different progenitor systems connect to GRB observables over cosmic time. We are motivated by the results of Lloyd-Ronning et al. (2019b) who found that certain intrinsic long gamma-ray burst (lGRB) properties appear to evolve

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“…Isolating GRB categories allows us to derive tighter relations, thus increasing the accuracy with which cosmological parameters are inferred (e.g., Cardone et al 2009Cardone et al , 2010Dainotti et al 2013b;Postnikov et al 2014). For a review on GRB relations, see the following reviews: Dainotti et al (2016b and Dainotti & Del Vecchio (2017).…”

Section: Introductionmentioning

confidence: 99%

A Study of the Gamma-Ray Burst Fundamental Plane

Dainotti

Hernández

Postnikov

et al. 2017

ApJ

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Long gamma-ray bursts (GRBs) with a plateau phase in their X-ray afterglows obey a 3D relation, between the rest-frame time at the end of the plateau, T a , its corresponding X-ray luminosity, L a , and the peak luminosity in the prompt emission, L peak . This 3D relation identifies a GRB fundamental plane whose existence we here confirm. Here we include the most recent GRBs observed by Swift to define a "gold sample" (45 GRBs) and obtain an intrinsic scatter about the plane compatible within 1σ with the previous result. We compare GRB categories, such as short GRBs with extended emission (SEE), X-ray flashes, GRBs associated with supernovae, a sample of only long-duration GRBs (132), selected from the total sample by excluding GRBs of the previous categories, and the gold sample, composed by GRBs with light curves with good data coverage and relatively flat plateaus. We find that the relation planes for each of these categories are not statistically different from the gold fundamental plane, with the exception of the SSE, which are hence identified as a physically distinct class. The gold fundamental plane has an intrinsic scatter smaller than any plane derived from the other sample categories. Thus, the distance of any particular GRB category from this plane becomes a key parameter. We computed the several category planes with T a as a dependent parameter obtaining for each category smaller intrinsic scatters (reaching a reduction of 24% for the long GRBs). The fundamental plane is independent from several prompt and afterglow parameters.

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Gamma-Ray Burst Prompt Correlations

Cited by 58 publications

References 270 publications

Gamma Ray Burst afterglow and prompt-afterglow relations: An overview

Gamma Ray Burst afterglow and prompt-afterglow relations: An overview

The evolution of gamma-ray burst jet opening angle through cosmic time

A Study of the Gamma-Ray Burst Fundamental Plane

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