J/ApJS/227/7 Long & short GRBs with host galaxies data (Li+, 2016)
A comparative study of long and short GRBs.
I. Overlapping properties.
Li Y., Zhang B., Lu H.-J.
<Astrophys. J. Suppl. Ser., 227, 7-7 (2016)>
=2016ApJS..227....7L 2016ApJS..227....7L (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; Redshifts ; References ; Extinction ; Abundances
Keywords: gamma-ray burst: general; methods: statistical
Abstract:
Gamma-ray bursts (GRBs) are classified into long and short categories
based on their durations. Broadband studies suggest that these two
categories of objects roughly correspond to two different classes of
progenitor systems, i.e., compact star mergers (Type I) versus massive
star core collapse (Type II). However, the duration criterion
sometimes leads to mis-identification of the progenitor systems. We
perform a comprehensive multi-wavelength comparative study between
duration-defined long GRBs and short GRBs as well as the so-called
"consensus" long GRBs and short GRBs (which are believed to be more
closely related to the two types of progenitor systems). The
parameters we study include two parts: the prompt emission properties
including duration (T90), spectral peak energy (Ep), low energy
photon index (α), isotropic γ-ray energy (Eγ,iso),
isotropic peak luminosity (Lp,iso), and the amplitude parameters (f
and feff); and the host galaxy properties including stellar mass
(M*), star formation rate, metallicity ([X/H]), half light radius
(R50), angular and physical (Roff) offset of the afterglow from
the center of the host galaxy, the normalized offset
(roff=Roff/R50), and the brightness fraction Flight. For most
parameters, we find interesting overlapping properties between the two
populations in both one-dimensional (1D) and 2D distribution plots.
The three best parameters for the purpose of classification are T90,
feff, and Flight. However, no single parameter alone is good
enough to place a particular burst into the right physical category,
suggesting the need for multiple criteria for physical classification.
Description:
Our main sample includes 375 GRBs with spectroscopic redshift
measurements in the literature before 2014 June 30. Also included are
32 GRBs with host galaxy information, even though no spectroscopic
redshifts have been reported for these bursts. Altogether we have 407
GRBs.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 112 407 Basic sample
table2.dat 189 407 Prompt emission properties sample
(see section 2.1)
table3.dat 197 407 Star Formation Rate (SFR) of host galaxies
(see section 2.2.1)
table4.dat 168 407 Offset of the GRB location from the center
of host galaxy (see section 2.2.2)
refs.dat 113 526 References
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See also:
IX/20 : The Fourth BATSE Burst Revised Catalog (Paciesas+ 1999)
J/ApJS/224/20 : 10yr of Swift/XRT obs. of GRBs (Yi+, 2016)
J/ApJ/802/103 : Model predictions for GRB host galaxies (Trenti+, 2015)
J/A+A/581/A125 : UV/Optical/NIR spectroscopy GRB hosts (Kruehler+, 2015)
J/A+A/568/A19 : Photometry of 3 γ-ray burst supernovae (Cano+, 2014)
J/ApJS/211/13 : The second Fermi/GBM GRB catalog (4yr) (von Kienlin+, 2014)
J/ApJ/778/128 : GRB-host galaxies photometry (Perley+, 2013)
J/ApJS/208/21 : The BATSE 5B GRB spectral catalog (Goldstein+, 2013)
J/ApJ/763/15 : Fermi GRB analysis. III. T90 distributions (Qin+, 2013)
J/A+A/557/A100 : Fermi and Swift GRBs Epeak-Eiso relation (Heussaff+, 2013)
J/ApJS/199/18 : The Fermi GBM catalog (Paciesas+, 2012)
J/ApJS/195/2 : The second Swift BAT GRB catalog (BAT2) (Sakamoto+, 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/ApJS/180/192 : BeppoSAX/GRBM γ-ray Burst Catalog (Frontera+, 2009)
J/ApJ/609/935 : Gamma-ray burst formation rate (Yonetoku+, 2004)
J/ApJS/126/19 : BATSE gamma-ray burst spectral catalog. I. (Preece+, 2000)
http://swift.gsfc.nasa.gov/archive/grb_table/ : Swift GRBs at NASA
http://www.mpe.mpg.de/~jcg/grbgen.html : List of GRBs
http://ibas.iasf-milano.inaf.it/IBAS_Results.html : GRBs localized with IBAS
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 1 A1 --- Type Type of GRB (L=long or S=short)
3- 9 A7 --- GRB GRB identifier
11- 11 A1 --- f_GRB [a] Flag on GRB (G1)
13- 13 A1 --- l_z Limit flag on z
14- 20 F7.5 --- z [0.008/8.3]? Redshift
22- 27 F6.4 --- E_z [0.001/0.6]? Upper uncertainty on z
29- 34 F6.4 --- e_z [0.001/0.6]? Lower uncertainty in z
36- 37 A2 --- n_z Method on z (1)
39- 42 I4 --- r_z ? Reference code for z (see refs.dat file)
44- 53 A10 --- n_T90 Observatory used to obtain T90
55- 55 A1 --- l_T90 Limit flag on T90
56- 64 F9.3 s T90 [0.02/25000] Timescale where 5-95% of total
γ-ray fluence is emitted
66- 71 F6.3 s e_T90 [0.05/23]? Uncertainty in T90
73- 75 I3 s T90ex [77/120]? T90 including the extended
emission (2)
77- 80 I4 --- r_T90 Reference code for T90 (see refs.dat file)
82- 88 E7.2 10-7J Eg_iso ? Isotropic 1-1e4keV energy; erg (3)
90- 96 E7.2 10-7W Lp_iso ? Isotropic peak 1-1e4keV
luminosity; erg/s (4)
98-102 F5.2 --- f [1/42.5]? Amplitude f parameter, Fp/Fb (5)
104-107 F4.2 --- feff [1/8]? Effective f parameter (6)
109-112 F4.2 --- e_feff [0.01/2]? Uncertainty in feff
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Note (1): The redshifts of GRBs are usually measured/estimated as follows:
E = via host galaxy emission lines,
A = afterglow absorption lines, or
P = broad band SED fitting based on photometric properties.
HA = For a few objects such as GRB 050509B, host galaxies spectra are
obtained and only absorption lines are detected.
Note (2): In these cases the T90 value is for the short-hard spike only.
Note (3): In rest frame 1-1e4keV. z=2.0 is assumed for long-duration GRBs
(LGRBs) without redshifts and z=0.5 is assumed for
short-duration GRBs (SGRBs) without redshifts.
Spectral parameters in Table 2 are used. Units are erg/cm2.
Note (4): In rest frame 1-1e4keV and units of erg/s/cm2.
Note (5): The f parameter is defined as the ratio between 1s peak flux and
background flux f=Fp/FB, which measures how bright the brightest
peak of a burst is above the background level. See section 2.1.4 for
further explanations.
Note (6): The effective amplitude parameter (feff=F'p/FB) by assuming
a background making T90 to be 2s. See section 2.1.4.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Type Type of GRB (L=long or S=short)
3- 9 A7 --- GRB GRB identifier
11- 24 A14 --- Det Detector used to obtain the data
26- 31 F6.3 --- Gamma [0.4/3.2]? Power law index
33- 37 F5.3 --- E_Gamma [0/0.8]? Upper uncertainty in Gamma
39- 43 F5.3 --- e_Gamma [0/0.8]? Lower uncertainty in Gamma
45- 50 F6.3 --- alpha [-1.9/-0.06]? Low energy photon index
52- 56 F5.3 --- E_alpha [0/2.3]? Upper uncertainty in alpha
58- 62 F5.3 --- e_alpha [0/2.2]? Lower uncertainty in alpha
64 A1 --- l_beta Limit flag on beta
65- 70 F6.2 --- beta [-22.1/-1.5]? High energy photon index
72- 76 F5.2 --- E_beta [0/11.1]? Upper uncertainty in beta
78- 82 F5.2 --- e_beta [0/11.1]? Lower uncertainty in beta
84 A1 --- l_Ep Limit flag on EP
85- 91 F7.2 keV Ep [2.6/4301]? Spectral peak energy
93- 99 F7.2 keV E_Ep [1/2398]? Upper uncertainty in Ep
101-106 F6.2 keV e_Ep [0.8/901]? Lower uncertainty in Ep
108 A1 --- l_Sg Limit flag on Sg
109-116 F8.2 10-10J/m2 Sg [0.07/24619] Energy fluence in SgBand;
1e-7erg/cm2
118-123 F6.2 10-10J/m2 E_Sg [0/610]? Upper uncertainty in Sg
125-130 F6.2 10-10J/m2 e_Sg [0/610]? Lower uncertainty in Sg
132-139 A8 keV SgBand Energy band range used for Sg
141 I1 --- KWFlag [1/8]? Konus-Wind flag (1)
143 A1 --- l_Fp Limit flag on Fp
144-151 F8.3 10-10W/m2 Fp [0.02/8700]? The 1 second peak flux
in FpBand; 1e-7erg/s/cm2
153-159 F7.3 10-10W/m2 E_Fp [0/400]? Upper uncertainty in Fp
161-167 F7.3 10-10W/m2 e_Fp [0/430]? Lower uncertainty in Fp
169 A1 --- f_Fp [p] p: Fp is a peak photon flux; ph/s/cm2
171-178 A8 keV FpBand Energy band range used for Fp
180-189 A10 --- Ref Reference(s) (see refs.dat file)
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Note (1): Fluxes from Konus-Wind are not 1 second peak flux but as follows:
1 = 0.004s;
2 = 0.016s;
3 = 0.064s;
4 = 0.128s;
5 = 0.256s;
6 = 0.5s;
7 = 2.944s;
8 = 3s.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Type Type of GRB (L=long or S=short)
3- 9 A7 --- GRB GRB identifier
11- 17 F7.5 --- z [0.008/8.3]? Spectroscopic redshift
19- 45 A27 --- Inst Instrument used to obtain the spectrum
47 A1 --- l_logM* Limit flag on logM*
49- 53 F5.2 [Msun] logM* [7.7/12.3]? Log stellar mass
55- 58 F4.2 [Msun] E_logM* [0.01/1.5]? Upper uncertainty in logM*
60- 63 F4.2 [Msun] e_logM* [0.01/1.5]? Lower uncertainty in logM*
65- 74 A10 --- n_logM* Method used to derive logM* (SED, IR or
line_width)
76 A1 --- l_SFR Limit flag on SFR
77- 83 F7.3 Msun/yr SFR [0.01/280]? Star Formation Rate
85- 92 F8.3 Msun/yr E_SFR [0.005/1563]? Upper uncertainty in SFR
94-100 F7.3 Msun/yr e_SFR [0.005/174]? Lower uncertainty in method
102-109 A8 --- n_SFR Method used to derive SFR
111-115 F5.2 Gyr-1 sSFR [0.01/58]? Specific Star Formation Rate
117 A1 --- l_[X/H] Limit flag on [X/H]
118-123 F6.3 [-] [X/H] [-2.2/0.7]? Metallicity
125-130 F6.3 --- [X/H]up [-0.6/0.04]? Upper branch of R23-[X/H]
relation (2)
132-135 F4.2 [-] E_[X/H] [0.07/0.6]? Upper uncertainty in [X/H]
137-140 F4.2 [-] e_[X/H] [0.07/0.6]? Lower uncertainty in [X/H]
142-150 A9 --- n_[X/H] Method used to derive [X/H]
153 A1 --- l_Av Limit flag on Av
155-162 F8.6 mag Av [0/4.4]? Extinction in the V band
164-167 F4.2 mag E_Av [0/3]? Upper uncertainty in Av
169-172 F4.2 mag e_Av [0/2]? Lower uncertainty in Av
174-181 A8 --- n_Av Method used to derive Av
183-197 A15 --- Ref Reference(s) (see refs.dat file)
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Note (2): The [X/H] value estimated from the R23 method (one of emission line
method) is double-valued. In these cases the [X/H] value is the lower
branch and [X/H]up is the upper branch of R23-[X/H] relation.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Type Type of GRB (L=long or S=short)
3- 9 A7 --- GRB GRB identifier
11 A1 --- f_GRB [a] Flag on GRB (G1)
13- 19 F7.5 --- z [0.008/8.3]? Spectroscopic redshift
21- 34 A14 --- Inst Instrument used to obtain the optical image
36- 40 F5.3 --- Pcc [0/0.32]? Probability of chance coincidence
42 A1 --- l_R50a Limit flag on R50a
43- 48 F6.3 arcsec R50a [0.04/19]? Angular half light radius
50 A1 --- f_R50a [*] Flag on R50a (1)
52- 56 F5.3 arcsec E_R50a [0/0.8]? Upper uncertainty in R50a
58- 62 F5.3 arcsec e_R50a [0/0.8]? Upper uncertainty in F50a
64 A1 --- l_R50p Limit flag on R50p
65- 70 F6.3 kpc R50p [0.3/21]? Physical half light radius
72- 75 F4.2 kpc E_R50p [0/1.4]? Upper uncertainty in R50p
77- 80 F4.2 kpc e_R50p [0/1.4]? Lower uncertainty in R50p
82- 85 F4.2 --- n [0.3/5.6]? Sersic index
87 A1 --- l_Roffa Limit flag on Roffa
88- 93 F6.3 arcsec Roffa [0.01/18]? Angular GRB offset from
host galaxy center
95 A1 --- f_Roffa [*] Flag on Roffa (1)
97-101 F5.3 arcsec E_Roffa [0/3.4]? Upper uncertainty in Roffa
103-107 F5.3 arcsec e_Roffa [0/3.4]? Lower uncertainty in Roffa
109 A1 --- l_Roffp Limit flag on Roffp
110-116 F7.3 kpc Roffp [0.07/86.2]? Physical GRB offset from
host galaxy center
118-123 F6.3 kpc E_Roffp [0/18.1]? Upper uncertainty in Roffp
125-130 F6.3 kpc e_Roffp [0/18.1]? Lower uncertainty in Roffp
132 A1 --- l_roff Limit flag on roff
133-138 F6.3 --- roff [0.04/15.5]? Normalized offset
(roff=Roff(a|p)/R50(a|p))
140-144 F5.3 --- E_roff [0/5.2]? Upper uncertainty in roff
146-150 F5.3 --- e_roff [0/5.2]? Lower uncertainty in roff
152-156 F5.3 --- Flight [0/1]? Fraction of host galaxy area brighter
than GRB region (2)
158-168 A11 --- Ref Reference(s) (see refs.dat file)
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Note (1):
* = Roughly estimated from the images in the references.
Note (2): A 1.0 indicates GRB is in the brightest region of the host and 0.0
indicates GRB is in the faintest region of the host.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- Ref Reference code
6- 24 A19 --- BibCode Bibcode
26- 49 A24 --- Auth First author's name(s)
51-113 A63 --- Comm Comment
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Global notes:
Note (G1):
a = A z equal 0.5 is assumed for LGRB 020410A, according to the possible
detection of SN in Levan et al. (2005ApJ...624..880L 2005ApJ...624..880L).
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 05-Jan-2017