A COMPREHENSIVE ANALYSIS OFFERMIGAMMA-RAY BURST DATA. III. ENERGY-DEPENDENTT90DISTRIBUTIONS OF GBM GRBs AND INSTRUMENTAL SELECTION EFFECT ON DURATION CLASSIFICATION

Qin, Ying; Liang, En‐Wei; Liang, Yun-Feng; Yi, Shuang-Xi; Lin, Lin; Zhang, Bin-Bin; Zhang, Jin; Lü, Hou-Jun; Lu, Rui-Jing; Lu, Liying; Zhang, Bing

doi:10.1088/0004-637x/763/1/15

Cited by 102 publications

(86 citation statements)

References 105 publications

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“…For display purposes, histograms are plotted using the Knuth rule for bin width. Up to date, to the best of the author's knowledge, only Horváth et al (2012) and Qin et al (2013) conducted research on a Fermi subsample, consisting of 425 GRBs from the first release of the catalog.…”

Section: Datasets and Methodsmentioning

confidence: 99%

On the limit between short and long GRBs

Tarnopolski

2015

Astrophys Space Sci

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Two classes of GRBs have been identified thus far without doubt and are prescribed to different physical scenarios-NS-NS or NS-BH mergers, and collapse of massive stars, for short and long GRBs, respectively. The existence of two distinct populations was inferred through a bimodal distribution of the observed durations T 90 , and the commonly applied 2 s limit between short and long GRBs was obtained by fitting a parabola between the two peaks in binned data from BATSE 1B. Herein, by means of a maximum likelihood (ML) method a mixture of two Gaussians is fitted to the datasets from BATSE, Swift, BeppoSAX, and Fermi in search for a local minimum that might serve as a new, more proper, limit for the two GRB classes. It is found that Swift and BeppoSAX distributions are unimodal, hence no local minimum is present, Fermi is consistent with the conventional limit, whereas BATSE gives the limit significantly longer (equal to 3.38 ± 0.27 s) than 2 s. These new values change the fractions of short and long GRBs in the samples examined, and imply that the observed T 90 durations are detector dependent, hence no universal limiting value may be applied to all satellites due to their different instrument specifications. Because of this, and due to the strong overlap of the two-Gaussian components, the straightforward association of short GRBs to mergers and long ones to collapsars is ambiguous.

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Section: Datasets and Methodsmentioning

confidence: 99%

On the limit between short and long GRBs

Tarnopolski

2015

Astrophys Space Sci

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“…In addition to the short and long categories using the burst durations, previous studies from GRBs detected by multiple instruments, including BATSE, Fermi, and Swift, have found that short bursts tend to be harder than long GRBs (e.g., Kouveliotou et al 1993;Qin et al 2000;Řípa et al 2009;Sakamoto et al 2011b;Qin et al 2013;von Kienlin et al 2014). Figure 8 shows an updated version of the hardness ratio (i.e., the fluence in 50-100 keV divided by fluence in 25-50 keV) versus T 90 to include all the new BAT-detected GRBs since the BAT2 catalog.…”

Section: Spectral Analyses 431 Time-averaged Spectramentioning

confidence: 99%

The Third Swift Burst Alert Telescope Gamma-Ray Burst Catalog

Lien

Sakamoto

Barthelmy

et al. 2016

ApJ

300

320

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To date, the Burst Alert Telescope (BAT) onboard Swift has detected ∼1000 gamma-ray bursts (GRBs), of which ∼360 GRBs have redshift measurements, ranging from z=0.03 to z=9.38. We present the analyses of the BATdetected GRBs for the past ∼11 years up through GRB151027B. We report summaries of both the temporal and spectral analyses of the GRB characteristics using event data (i.e., data for each photon within approximately 250 s before and 950 s after the BAT trigger time), and discuss the instrumental sensitivity and selection effects of GRB detections. We also explore the GRB properties with redshift when possible. The result summaries and data products are available at http://swift.gsfc.nasa.gov/results/batgrbcat/index.html. In addition, we perform searches for GRB emissions before or after the event data using the BAT survey data. We estimate the false detection rate to be only one false detection in this sample. There are 15 ultra-long GRBs (∼2% of the BAT GRBs) in this search with confirmed emission beyond ∼1000 s of event data, and only two GRBs (GRB100316D and GRB101024A) with detections in the survey data prior to the starting of event data.

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“…Their sample consists of the radio observed GRBs is the BAT6 sample (BAT6 being the brightest Swift-BAT-detected long GRBs that are considered complete with respect to the flux limit, Salvaterra et al 2012), thus it can be argued that they represent an unbiased sample of GRB radio afterglow properties (for details on Swift GRB selection effects and comparisons to GRBs detected with other instruments see Qin et al 2013;Lien et al 2016).…”

Section: Radio Grb Detection Ratesmentioning

confidence: 99%

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

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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.

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A COMPREHENSIVE ANALYSIS OFFERMIGAMMA-RAY BURST DATA. III. ENERGY-DEPENDENTT₉₀DISTRIBUTIONS OF GBM GRBs AND INSTRUMENTAL SELECTION EFFECT ON DURATION CLASSIFICATION

Cited by 102 publications

References 105 publications

On the limit between short and long GRBs

On the limit between short and long GRBs

The Third Swift Burst Alert Telescope Gamma-Ray Burst Catalog

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

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