THE SECOND SWIFT BURST ALERT TELESCOPE GAMMA-RAY BURST CATALOG

By T. Sakamoto, S. Barthelmy, W. Baumgartner, J. Cummings, E. Fenimore, N. Gehrels, H. Krimm, C. Markwardt, D. Palmer, A. Parsons and 5 more. 2011

184 citations recorded by the source corpus.

We present the second Swift Burst Alert Telescope (BAT) catalog of gamma-ray bursts (GRBs), which contains 476 bursts detected by the BAT between 2004 December 19 and 2009 December 21. This catalog (hereafter the BAT2 catalog) presents burst trigger time, location, 90% error radius, duration, fluence, peak flux, time-averaged spectral parameters, and time-resolved spectral parameters measured by the BAT. In the correlation study of various observed parameters extracted from the BAT prompt emission data, we distinguish among long-duration GRBs (L-GRBs), short-duration GRBs (S-GRBs), and short-duration GRBs with extended emission (S-GRBs with E.E.) to investigate differences in the prompt emission properties. The fraction of L-GRBs, S-GRBs, and S-GRBs with E.E. in the catalog are 89%, 8%, and 2%, respectively. We compare the BAT prompt emission properties with the BATSE, BeppoSAX, and HETE-2 GRB samples. We also correlate the observed prompt emission properties with the redshifts for the GRBs with known redshift. The BAT T90 and T50 durations peak at 70 s and 30 s, respectively. We confirm that the spectra of the BAT S-GRBs are generally harder than those of the L-GRBs. The time-averaged spectra of the BAT S-GRBs with E.E. are similar to those of the L-GRBs. Whereas, the spectra of the initial short spikes of the S-GRBs with E.E. are similar to those of the S-GRBs. We show that the BAT GRB samples are significantly softer than the BATSE bright GRBs and that the time-averaged Eobspeak of the BAT GRBs peaks at 80 keV, which is significantly lower energy than those of the BATSE sample, which peak at 320 keV. The time-averaged spectral properties of the BAT GRB sample are similar to those of the HETE-2 GRB samples. By time-resolved spectral analysis, we find that only 10% of the BAT observed photon indices are outside the allowed region of the synchrotron shock model. We see no obvious observed trend in the BAT T90 and the observed spectra with redshifts. The T90 and T50 distributions measured at the 140–220 keV band in the GRB rest frame from the BAT known redshift GRBs peak at 19 s and 8 s, respectively. We also provide an update on the status of the on-orbit BAT calibrations.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b5e4ace14034387a31b290e2113ca1bd89504aae

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Citations in the corpus

• THE THIRD SWIFT BURST ALERT TELESCOPE GAMMA-RAY BURST CATALOG (2015, methodology): “Several catalogs related to the BAT-detected GRBs have been published, including the first and second BAT GRB catalog from the Swift/BAT team (Sakamoto et al. 2008; Sakamoto et al. 2011b, which will hereafter be referred as the BAT1 and BAT2 catalog, respectively).”
• CONNECTING THE GAMMA RAY BURST RATE AND THE COSMIC STAR FORMATION HISTORY: IMPLICATIONS FOR REIONIZATION AND GALAXY EVOLUTION (2011, methodology): “Of the 29 GRBs whose energies we compute asEiso = 4πd2LS, wheredL is the luminosity distance to a redshiftz andS is the fluence, 21 broad-band fluences are taken from Butler et al. (2007, 2010)and 8 10−150keV fluences (effectively lower limits) are taken from Sakamoto et al. (2011).”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “Long and short GRBs roughly comprise 3/4 and 1/4 of the total population of the BATSE sample, but the short GRB fraction is smaller for other detectors (Sakamoto et al., 2008a, 2011; Paciesas et al., 2012; Zhang et al., 2012c; Qin et al., 2013).”
• The prompt-afterglow connection in gamma-ray bursts: a comprehensive statistical analysis of Swift X-ray light curves (2012, methodology): “…and errors, break times (tb1, tb2, tb3) and errors, normalizations (N1, N2) and errors, smoothing parameters (s1, s2), prompt emission T90 (we refer to Sakamoto et al. 2011 for GRBs detected before December 2009, and to the refined BAT GCNs otherwise), power-law index of the first segment when t0…”
• THE MILLISECOND MAGNETAR CENTRAL ENGINE IN SHORT GRBs (2015, background): “About 20% of short GRBs detected with Swift have extended emission (EE) (Sakamoto et al. 2011) following the initial short, hard spike.”
• The rate, luminosity function and time delay of non-Collapsar short GRBs (2014, methodology): “…al. 2004) mission page.6 The 64-ms peak-flux of the bursts was estimated by correcting the 1 s peak-flux with the ratio of the 64-ms and 1024-ms peak-counts in the 64-ms binned light curve provided in Swift Burst GroundAnalysis Information page7 (Barthelmy et al. 2005; Sakamoto et al. 2008, 2011).”
• GIANT SPARKS AT COSMOLOGICAL DISTANCES? (2014, methodology): “A search through the BAT catalog (Sakamoto et al. 2011) would provide observational feedback to the coronal model.”