J/ApJS/209/20 Swift GRB catalog with X-ray data (Grupe+, 2013) ================================================================================ Evidence for new relations between gamma-ray burst prompt and X-ray afterglow emission from 9 years of Swift. Grupe D., Nousek J.A., Veres P., Zhang B.-B., Gehrels N. =2013ApJS..209...20G ================================================================================ ADC_Keywords: Gamma rays ; Redshifts ; X-ray sources Keywords: catalogs, gamma-ray burst: general Abstract: When a massive star explodes as a gamma-ray burst (GRB), information about the explosion is retained in the properties of the prompt and afterglow emission. We report on new relations between the prompt and X-ray afterglow emission of Swift-detected GRBs found from Burst Alert Telescope (BAT) and X-Ray Telescope data covering 2004 December to 2013 August (754 in total). These relations suggest that the prompt and afterglow emission are closely linked. In particular, we find very strong correlations between the BAT 15-150keV T_90_ and the break times before and after the plateau phase in the 0.3-10keV X-ray afterglow light curves. We also find a strong anticorrelation between the photon index of the GRB prompt emission and the X-ray spectral slope of the afterglow. Moreover, anticorrelations exist between the rest-frame peak energy in the prompt emission E_peak, z_and the X-ray afterglow decay slope during the plateau phase and the break times after the plateau phase. The rest-frame break times before and after the plateau phase are also anticorrelated with the rest-frame 15-150keV luminosity and the isotropic energy during the prompt emission. A principal component analysis suggests that the GRB properties are primarily driven by the luminosity/energy release in the 15-150keV band. Luminosity functions derived at different redshifts from a log N-log S analysis indicate that the density of bright bursts is significantly lower in the local universe than in the universe at z~3, where the density of bright GRBs peaks. Using cluster analysis, we find that the duration of BAT-detected short GRBs is less than 1s. Description: By the end of 2013 August, Swift had discovered 804 bursts. Of these, 40 GRBs were discovered through ground processing, and nine through the BAT Slew Survey. There is also one burst with no data available. Excluding these 50 bursts from the initial sample leaves a total of 754 Swift-discovered, onboard-triggered bursts, given in table 9. In 663 cases, XRT observed the field of the GRB, and 607 X-ray afterglows were detected (91%). Of the 754 GRBs in our sample, 63 are short-duration and 690 are long-duration bursts (one early GRB did not have a T90 measurement). Through 2013 August, 232 of the 754 GRBs in our sample or their host galaxies had spectroscopic redshift measurements (about 31%). Burst redshifts were taken from GCN Circulars and the GRB redshift catalogs by Fynbo et al. (2009ApJS..185..526F); Jakobsson et al. (2012ApJ...752...62J) and Kruhler et al. (2012ApJ...758...46K). The 0.3-10keV X-ray count rate light curves and spectra were derived from the University of Leicester GRB repository Web site (Evans et al. 2007A&A...469..379E). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table9.dat 221 754 GRB catalog -------------------------------------------------------------------------------- See also: J/MNRAS/428/729 : GRB Swift X-ray light curves analysis (Margutti+, 2013) J/ApJ/746/170 : Follow-up resources for high-redshift GRBs (Morgan+, 2012) J/A+A/528/A122 : SwiftFT catalog (Puccetti+, 2011) J/MNRAS/418/2202 : Analysis of {gamma}-ray bursts (Dainotti+, 2011) J/ApJ/731/103 : Redshift catalog for Swift long GRBs (Xiao+, 2011) J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010) J/PAZh/35/10 : Gamma-ray bursts with known redshifts (Badjin+, 2009) J/ApJ/701/824 : Afterglows of short & long-duration GRBs (Nysewander+, 2009) J/ApJ/690/163 : The first Swift UV-Opt GRB afterglow catalog (Roming+, 2009) J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009) http://www.swift.ac.uk/xrt_curves : Swift-XRT light curve repository http://swift.gsfc.nasa.gov/archive/grb_table : Swift GRB table Byte-by-byte Description of file: table9.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- Seq [1/754] Running index number 5- 11 A7 --- GRB GRB Name (YYMMDDA) 14- 19 I6 --- TID BAT trigger number 22- 27 F6.4 --- z [0.03/8.2]? Redshift of the GRB 30- 37 F8.3 s T90 [0.03/2100]? Observed BAT 15-150keV T_90_ 40- 46 F7.3 s e_T90 ? Uncertainty in T90 48- 54 E7.2 mJ/m2 Flue ? Fluence in 15-150 keV BAT band; erg/cm^2^ 56- 62 E7.2 mJ/m2 e_Flue ? Uncertainty in Flue 64- 67 F4.2 --- Gamma [0.4/5]? BAT 15-150keV photon index {Gamma} 69- 72 F4.2 --- e_Gamma ? Uncertainty in Gamma 74- 79 F6.1 keV Epeak [19/4250]? Peak beak energy in keV at high energies 81- 86 F6.2 keV e_Epeak ? Uncertainty in ePeak 88- 94 F7.4 [10-7J] logE [46/56]? Log of k-corrected BAT 15-150keV energy; erg (1) 97-103 F7.4 [10-7W] logL [45/55]? Log of k-corrected BAT 15-150keV luminosity; erg/s (1) 105-110 F6.2 10+20/cm2 NHgal [0.5/150]? Galactic absorption column density 112-117 F6.2 10+20/cm2 NHfit [0.3/873]? Free fit absorption column density (2) 120-125 F6.2 10+20/cm2 e_NHfit [0.02/428]? Negative uncertainty in NHfit 127-134 F8.4 10+20/cm2 E_NHfit [0.02/505]? Positive uncertainty in NHfit 136-141 F6.3 10+20/cm2 NHz [0/37]? Absorption column density at burst redshift 143-148 F6.3 10+20/cm2 e_NHz [0/23]? Negative uncertainty in NHz 150-155 F6.3 10+20/cm2 E_NHz [0/26]? Positive uncertainty in NHz 156-160 F5.2 --- bx [-0.2/4]? The 0.3-10keV energy spectral index 162-166 F5.2 --- e_bx ? Negative uncertainty in bx 168-172 F5.2 --- E_bx ? Positive uncertainty in bx 175-179 I5 s Tbr1 [80/44300]? X-ray light curve break time before plateau phase 181-185 I5 s e_Tbr1 ? Uncertainty in Tbreak1 188-193 I6 s Tbr2 [111/780000]? X-ray light curve break time after plateau phase 195-200 I6 s e_Tbr2 ? Uncertainty in Tbreak2 202-206 F5.2 --- ax2 [-1.5/2]? X-ray light curve decay slope during plateau phase 208-211 F4.2 --- e_ax2 ? Uncertainty in ax2 213-216 F4.2 --- ax3 [0.6/8]? X-ray light curve decay slope during plateau phase 218-221 F4.2 --- e_ax3 ? Uncertainty in ax3 -------------------------------------------------------------------------------- Note (1): The k-corrected energy and luminosity were based on the k-corrected fluence following the standard k-correction by Oke & Sandage (1968ApJ...154...21O): Fluence_k_ = Fluence_obs_ * (1+z)^(2-{Gamma})^. Note (2): The excess absorption above the Galactic value is then given by {Delta}_NH_ = N_H,fit_-N_H,gal_. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 14-Jan-2014