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.
<Astrophys. J. Suppl. Ser., 209, 20 (2013)>
=2013ApJS..209...20G 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 T90 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 2009ApJS..185..526F); Jakobsson et al.
(2012ApJ...752...62J 2012ApJ...752...62J) and Kruhler et al. (2012ApJ...758...46K 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 2007A&A...469..379E).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table9.dat 221 754 GRB catalog
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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 γ-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
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Bytes Format Units Label Explanations
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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 T90
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/cm2
56- 62 E7.2 mJ/m2 e_Flue ? Uncertainty in Flue
64- 67 F4.2 --- Gamma [0.4/5]? BAT 15-150keV photon index Γ
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
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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 1968ApJ...154...21O):
Fluencek = Fluenceobs * (1+z)(2-Γ).
Note (2): The excess absorption above the Galactic value is then given
by ΔNH = NH,fit-NH,gal.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 14-Jan-2014