Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/731/103         Redshift catalog for Swift long GRBs         (Xiao+, 2011)

Redshift catalog for Swift long gamma-ray bursts. Xiao L., Schaefer B.E. <Astrophys. J., 731, 103 (2011)> =2011ApJ...731..103X
ADC_Keywords: Gamma rays ; Redshifts ; Spectroscopy Keywords: gamma-ray burst: general Abstract: We present a catalog of the redshifts for most long-duration gamma-ray bursts (GRBs) by Swift from 2004 December 20 to 2008 July 23 (258 bursts in total). All available information is collected, including spectroscopic redshifts, photometric redshift limits, and redshifts calculated from various luminosity relations. Error bars for the redshifts derived from the luminosity relations are asymmetric, with tails extended to the high-redshift end, and this effect is evaluated by looking at the 30% of Swift bursts with spectroscopic redshifts. A simulation is performed to eliminate this asymmetric effect, and the resultant redshift distribution is deconvolved. We test and confirm this simulation on the sample of bursts with known spectroscopic redshifts and then apply it to the 70% of Swift bursts that do not have spectroscopic measures. A final intrinsic redshift distribution is then made for almost all Swift bursts, and the efficiency of the spectroscopic detections is evaluated. The efficiency of spectroscopic redshifts varies from near unity at low redshift to 0.5 at z=1, to near 0.3 at z=4, and to 0.1 at z=6. We also find that the fraction of GRBs with z>5 is ∼10%, and this fraction is compared with simulations from a cosmological model. Description: We collect all the Swift GRBs from 2004 December 20 (GRB041220) to 2008 July 23 (GRB080723A). Most of the data are downloaded from the Legacy ftp site (ftp://legacy.gsfc.nasa.gov/swift/data/obs). Swift is a multi-wavelength GRB detection satellite that has three instruments on board. The wide-field BAT, which covers a 15-150keV energy band, can position a burst to 1'-4' accuracy. The narrow X-ray telescope (XRT) and UV/Optical telescope (UVOT) start observing the GRB within ∼100s after the trigger time and position it within the arcsec level. With the analysis of the spectroscopic features (e.g., absorption lines) of the afterglows, redshifts of the GRBs are measured with relatively high accuracy. We collected all the reported spectroscopic redshift from GCN Circulars archive and the literature. GRBs with multiple or conflicting reported redshifts are excluded from our catalog. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 34 76 Bursts not included in our catalog table3.dat 136 258 Luminosity indicators table5.dat 72 263 Our redshifts and spectroscopic redshifts refs.dat 86 282 References
See also: J/ApJS/195/2 : The second Swift BAT GRB catalog (BAT2) (Sakamoto+, 2011) J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010) J/ApJ/690/163 : The first Swift UV-Opt GRB afterglow catalog (Roming+, 2009) J/ApJ/704/1405 : Testing the Epeak-Eiso relation for GRBs (Krimm+, 2009) J/ApJS/175/179 : The BAT1 gamma-ray burst catalog (Sakamoto+, 2008) J/ApJ/642/L99 : R-band photometry of GRB 060206 (Wozniak+, 2006) J/A+A/427/87 : List of GRBs (Gorosabel+, 2004) http://swift.gsfc.nasa.gov/docs/swift/archive/grb_table/ : Swift GRB table Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 A7 --- GRB GRB identification (YYMMDDA) 9- 33 A25 --- rej Rejection cause 34 A1 --- n_rej [a-e] Additional note (1)
Note (1): Note as follows: a = Suggested a probable Soft Gamma-Ray Repeater. b = Possible incomplete light curve. c = Swift BAT slew survey discovery. d = Short-hard burst with long extended emissions. e = Below Swift threshold.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 7 A7 --- GRB GRB identification (YYMMDDA) 9- 13 F5.2 s tauLag ? Spectral lag 15- 18 F4.2 s e_tauLag ? Uncertainty in tauLag 20- 25 F6.3 --- Var ? Variability indicator (4) 27- 31 F5.3 --- e_Var ? Uncertainty in Var 33- 37 F5.2 s tauRT ? Minimum rise time in the light curve 39- 42 F4.2 s e_tauRT ? Uncertainty in tauRT 45 A1 --- l_Np Limit flag on Npeak 46- 47 I2 --- Np ? Number of peaks in the light curve 49- 52 I4 keV Epeak Photon energy spectrum is brightest 54- 57 I4 keV E_Epeak Upper limit uncertainty in Epeak 59- 61 I3 keV e_Epeak Lower limit uncertainty in Epeak 63 A1 --- f_Epeak [c] conservative estimation of uncertainty (1) 65- 70 F6.3 --- alpha [-5/1] The α power law index (see refs) 72- 75 F4.2 --- E_alpha ? Upper limit uncertainty in alpha 77- 80 F4.2 --- e_alpha Uncertainty in alpha (2) 82 A1 --- f_alpha [c] conservative estimation of uncertainty (1) 84- 88 F5.2 --- beta [-4/2.1] The β power law index (see refs) 90- 93 F4.2 --- E_beta ? Upper limit uncertainty in beta 95- 98 F4.2 --- e_beta Uncertainty in beta (2) 100 A1 --- f_beta [c] conservative estimation of uncertainty (1) 102-106 A5 --- refs Reference(s) for the power law indices (see refs.dat file) 108 A1 --- l_tJet Limit flag on tJet 109-115 F7.4 d tJet ? Optical jet break time 117-122 F6.4 d e_tJet ? Uncertainty in tJet 124-125 A2 --- n_tJet Individual notes on tJet (3) 127-136 A10 --- r_tJet Reference(s) for tJet (see refs.dat file)
Note (1): Indicates a conservative estimation of uncertainty not reported in the original paper. Note (2): This is a lower limit when the upper limit in the previous column is provided otherwise it is the symmetric uncertainty. Note (3): Flag as follows: b = Jet break time reported from X-ray data only, not being used in this work. c = Multi-values for jet break reported, due to the confusing condition of the afterglow light curve, not using any of these values in this work. d = Grupe et al. (2006ApJ...645..464G) shows no break between 0.4-2.5day, with the slope of the light curve suggesting a break before 0.4day, while both Ghirlanda et al. (2007A&A...466..127G) and Campana et al. (2007A&A...472..395C) suggest a break after 2.5day, based on Ghirlanda's relation. e = Value obtained from Liang et al. (2008ApJ...675..528L ) figure and text, table 4 misreported it. f = With a pre-break slope too shallow for the forward shock model, not being used as a jet break time. g = Only one post-break data reported. h = Optical break not restrictive. i = Break not detected in X-ray data. j = Optical data confusing, not able to make decision where the jet break lies. k = Only taking R band jet break, as later data is lacked in V band. Note (4): the variability indicator V measures whether a light curve is spiky (large V) or smooth; see Fennimore and Ramirez-Ruiz 2000, astro-ph:0004176
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 7 A7 --- GRB GRB identification (YYMMDDA) 9 A1 --- l_zsp Limit flag on zsp 11- 16 F6.3 --- zsp ? Spectroscopic redshift 18- 20 F3.1 --- e_zsp ? Uncertainty in zsp 22- 24 A3 --- r_zsp Reference for zsp (see refs.dat file) 26 A1 --- l_zbest Limit flag on zbest 28- 33 F6.3 --- zbest ? Best estimated redshift 35- 38 F4.2 --- e_zbest ? The 1σ lower limit on zbest 40- 45 F6.3 --- E_zbest ? The 1σ upper limit on zbest 47- 50 F4.2 --- zph ? Upper limit from photometric redshift 52- 60 A9 --- r_zph Reference for zph (see refs.dat file) 62 A1 --- l_z Limit flag on z 64- 68 F5.2 --- z Final redshift 70- 72 F3.1 --- e_z ? Uncertainty in z
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Ref Reference code 6- 24 A19 --- BibCode Bibcode 26- 49 A24 --- Aut Author's name(s) 51- 86 A36 --- Comm Comment
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 22-Oct-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact