The Third BATSE Gamma-Ray Burst Catalog

Meegan, C.; Pendleton, G. N.; Briggs, M. S.; Kouveliotou, C.; Koshut, T. M.; Lestrade, John Patrick; Pačiesas, W. S.; McCollough, Michael L.; Brainerd, J. J.; Horack, John M.; Hakkila, Jon; Henze, W.; Preece, R.; Mallozzi, Robert S.; Fishman, G. J.

doi:10.1086/192329

Cited by 218 publications

(201 citation statements)

References 15 publications

(17 reference statements)

Supporting

Mentioning

188

Contrasting

Unclassified

Order By: Relevance

“…The division line between the long-duration GRBs (LGRBs) and short-duration GRBs (SGRBs) is around 2 seconds in the BATSE 50 − 300 keV band. Although the significance of this bimodality and the division line depend on the sensitivity and energy band of the detectors (Richardson et al 1996;Bissaldi et al 2011;Zhang et al 2012;Qin et al 2013), the authenticity of the bimodal T 90 distribution is confirmed not only with a larger BATSE sample (Meegan et al 1996;Paciesas et al 1999), but also by GRB data collected from other instruments such as BeppoSAX ), INTEGRAL Savchenko et al 2012;Bošnjak et al 2014), Swift and Fermi (Paciesas et al 2012;von Kienlin et al 2014). The existence of two phenomenological classes of GRBs is firmly established.…”

Section: Introductionmentioning

confidence: 97%

A Comparative Study of Long and Short Grbs. I. Overlapping Properties

Li¹,

Zhang²,

Lü³

2016

ApJS

View full text Add to dashboard Cite

Gamma ray bursts (GRBs) are classified into long and short categories based on their durations. Broad band studies suggest that these two categories of objects roughly correspond to two different classes of progenitor systems, i.e. compact star mergers (Type I) vs. massive star core collapse (Type II). However, the duration criterion sometimes leads to mis-identification of the progenitor systems. We perform a comprehensive multi-wavelength comparative study between duration-defined long GRBs and short GRBs as well as the so-called "consensus" long GRBs and short GRBs (which are believed to be more closely related to the two types of progenitor systems). The parameters we study include two parts: the prompt emission properties including duration (T 90 ), spectral peak energy (E p ), low energy photon index (α), isotropic γ-ray energy (E γ,iso ), isotropic peak luminosity (L p,iso ), and the amplitude parameters (f and f eff ); and the host galaxy properties including stellar mass (M * ), star formation rate (SFR), metallicity ([X/H]), half light radius (R 50 ), angular and physical (R off ) offset of the afterglow from the center of the host galaxy, the normalized offset (r off = R off /R 50 ), and the brightness fraction F light . For most parameters, we find interesting overlapping properties between the two populations in both 1D and 2D distribution plots. The three best parameters for the classification purpose are T 90 , f eff , and F light . However, no single parameter alone is good enough to place a particular burst into the right physical category, suggesting a need of multiple criteria for physical classification.

show abstract

Section: Introductionmentioning

confidence: 97%

A Comparative Study of Long and Short Grbs. I. Overlapping Properties

Li¹,

Zhang²,

Lü³

2016

ApJS

View full text Add to dashboard Cite

show abstract

“…The bursts measured with the BATSE instrument on the Compton Gamma-Ray Observatory are usually characterized by 9 observational quantities, i.e. 2 durations, 4 fluences and 3 peak fluxes (Meegan et al 1996;Paciesas et al 1999;Meegan et al 2001). In a previous paper (Bagoly et al 1998) we used the principal components analysis (PCA) technique to show that these 9 quantities can be reduced to only two significant independent variables, or principal components (PCs).…”

Section: Introductionmentioning

confidence: 99%

On the difference between the short and long gamma-ray bursts

Balázs

Bagoly²,

Horváth³

et al. 2003

A&A

View full text Add to dashboard Cite

Abstract. We argue that the distributions of both the intrinsic fluence and the intrinsic duration of the γ-ray emission in gammaray bursts from the BATSE sample are well represented by log-normal distributions, in which the intrinsic dispersion is much larger than the cosmological time dilatation and redshift effects. We perform separate bivariate log-normal distribution fits to the BATSE short and long burst samples. The bivariate log-normal behaviour results in an ellipsoidal distribution, whose major axis determines an overall statistical relation between the fluence and the duration. We show that this fit provides evidence for a power-law dependence between the fluence and the duration, with a statistically significant different index for the long and short groups. We discuss possible biases, which might affect this result, and argue that the effect is probably real. This may provide a potentially useful constraint for models of long and short bursts.

show abstract

“…As for the brightest range of GRBs, this is more or less evident-in the cosmological scenario a transition to Euclidean scaling with a powerlaw index Ϫ3/2 should exist, and this is indicated by the data (e.g., Meegan et al 1996). The domination of intrinsically weak bursts in the weakest range would imply a less trivial turnover of the distance distribution toward larger distances.…”

Section: Brightness-dependent Properties Of G-ray Bursts L45mentioning

confidence: 86%

Brightness-dependent Properties of Gamma-Ray Bursts

Stern

Poutanen

Svensson

1997

The Astrophysical Journal

View full text Add to dashboard Cite

Brightness-dependent correlations have been conclusively detected in the average time profiles of gamma-ray bursts (GRBs). Determining the time constants of the stretched exponential slopes of the average peak-aligned time profile of GRBs as a function of the peak brightness, we find that the postpeak slope shows time dilation when comparing bright and dim bursts, while the prepeak slope hardly changes. Stronger bursts are thus more symmetric than weaker bursts at a high confidence level. The very weakest bursts have a different shape (i.e., a different stretched exponential index) of their average time profile as compared to brighter bursts. This difference is too large to be explained by trigger effects and Poisson noise. We interpret these correlations as being the result of an intrinsic positive correlation between brightness and complexity of GRBs. This interpretation is directly confirmed by simulations as well as by a morphological classification of bursts. The fact that such a correlation can be observed should impose new constraints on the distribution of GRBs over luminosity distance.

show abstract

The Third BATSE Gamma-Ray Burst Catalog

Cited by 218 publications

References 15 publications

A Comparative Study of Long and Short Grbs. I. Overlapping Properties

A Comparative Study of Long and Short Grbs. I. Overlapping Properties

On the difference between the short and long gamma-ray bursts

Brightness-dependent Properties of Gamma-Ray Bursts

Contact Info

Product

Resources

About