J/ApJ/746/156 Radio afterglow observations of GRBs (Chandra+, 2012)
A radio-selected sample of gamma-ray burst afterglows.
Chandra P., Frail D.A.
<Astrophys. J., 746, 156 (2012)>
=2012ApJ...746..156C 2012ApJ...746..156C
ADC_Keywords: Gamma rays ; Radio continuum
Keywords: cosmology: observations - gamma-ray burst: general - hydrodynamics -
radio continuum: general
Abstract:
We present a catalog of radio afterglow observations of gamma-ray
bursts (GRBs) over a 14 year period from 1997 to 2011. Our sample of
304 afterglows consists of 2995 flux density measurements (including
upper limits) at frequencies between 0.6 GHz and 660 GHz, with the
majority of data taken at 8.5 GHz frequency band (1539 measurements).
We use this data set to carry out a statistical analysis of the
radio-selected sample. The detection rate of radio afterglows has
stayed unchanged almost at 31% before and after the launch of the
Swift satellite. The canonical long-duration GRB radio light curve at
8.5 GHz peaks at three to six days in the source rest frame, with a
median peak luminosity of 1031 erg/s/Hz. The peak radio luminosities
for short-hard bursts, X-ray flashes, and the supernova-GRB classes
are an order of magnitude or more fainter than this value. There are
clear relationships between the detectability of a radio afterglow and
the fluence or energy of a GRB, and the X-ray or optical brightness of
the afterglow. However, we find few significant correlations between
these same GRB and afterglow properties and the peak radio flux
density. We also produce synthetic light curves at centimeter and
millimeter bands using a range of blast wave and microphysics
parameters derived from multiwavelength afterglow modeling, and we use
them to compare to the radio sample. Finding agreement, we extrapolate
this behavior to predict the centimeter and millimeter behavior of
GRBs observed by the Expanded Very Large Array and the Atacama Large
Millimeter Array.
Description:
Our compiled sample consists of 304 GRBs observed with the radio
telescopes between 1997 January and 2011 January, along with the 2011
April 28 Fermi burst, GRB 110428A. The sample consists of a total of
2995 flux density measurements taken between the frequencies
0.6-660GHz bands spanning a time range from 0.026 to 1339 days.
Most of the afterglows (270 in total) in our sample were observed as
part of the VLA radio afterglow programs, whereas 15 bursts were
observed by EVLA, and 19 southern bursts with the Australia Telescope
Compact Array (ATCA).
Radio, optical and X-ray afterglows detections (section 2.2): out of
the 304 bursts, 123 bursts were observed in the pre-Swift epoch from
1997 until 2004. The remaining 181 bursts were observed between 2005
and 2011 April (post-Swift epoch).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 186 304 Master table
table4.dat 43 140 The radio peak flux densities and the time of
peak for radio afterglows
refs.dat 122 70 References
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See also:
J/ApJ/727/73 : S/N composite spectrum of GRB afterglows (Christensen+, 2011)
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/701/824 : Afterglows of short and long-duration GRBs (Nysewander+, 2009)
J/ApJ/690/163 : The first Swift UV-Opt GRB afterglow catalog (Roming+, 2009)
J/ApJS/180/192 : BeppoSAX/GRBM γ-ray Burst Catalog (Frontera+, 2009)
J/ApJS/175/179 : The BAT1 gamma-ray burst catalog (Sakamoto+, 2008)
J/ApJ/686/1209 : Optical properties of GRB afterglows (Melandri+, 2008)
J/A+A/455/813 : BeppoSAX catalog of GRB X-ray afterglows (De Pasquale+, 2006)
J/ApJ/609/935 : Gamma-ray burst formation rate (Yonetoku+, 2004)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- GRB GRB name (YYMMDD)
9- 11 A3 --- n_GRB [m-r, ] Note(s) on GRB (1)
13- 17 A5 --- Inst [A-T, sA] Instrument code (2)
19- 20 I2 h RAh [0,23] Hour of right ascension (J2000)
22- 23 I2 min RAm Minute of right ascension (J2000)
25- 29 F5.2 s RAs Second of right ascension (J2000)
31 A1 --- DE- Sign of declination (J2000)
32- 33 I2 deg DEd [0,83] Degreee of declination (J2000)
35- 36 I2 arcmin DEm Arcminute of declination (J2000)
38- 41 F4.1 arcsec DEs Arcsecond of declination (J2000)
43- 44 A2 --- X? [XYN? ] X-ray afterglow detection? (3)
46- 47 A2 --- O? [XYN? ] Optical afterglow detection? (3)
49- 50 A2 --- R? [YN? ] Radio afterglow detection? (3)
52- 55 A4 --- Tel Radio telescope (ATCA, EVLA or VLA)
57- 61 A5 --- n_Tel [lr-v, ] Multiple observations (1)
63- 70 F8.2 s T90 [0.07,1800]? Duration in the energy band of
the specific detector (T90)
72 A1 --- l_z Limit flag on z
74- 79 F6.3 --- z [0.009/20]? Redshift
81- 83 F3.1 --- z2 ? Upper range of redshift (if filled,
"Redshift" is the lower range)
85- 92 E8.3 mJ/m2 S15 [6e-09,0.000283]? GRB fluences in 15-150keV
range (in erg/cm-2) (4)
94-101 E8.3 10-7J Ebol [1e+40,4.1e+54]? k-corrected bolometric
isotropic energy in 1-10000keV range (in erg)
103 A1 --- l_FX Limit flag on FX
105-111 F7.2 10-16W/m2 FX [0,548.6]? X-ray flux (0.3-10keV or 1.6-10keV)
at 11hr in 10-13erg/cm2/s (5)
113 A1 --- l_FR Limit flag on FR
115-122 F8.2 uJy FR [0.08,4328]? Optical R-band (0.7um) flux density
at 11hr in µJy
124 A1 --- l_Tj Limit flag on Tj
126-131 F6.3 d Tj [0.004/47.7]? Jet break time (tj)
133 A1 --- u_Tj [?] Uncertainty flag on Tj
135-141 F7.3 cm-3 n [0.001,680]? Number density (n) of the
circumburst medium
143 A1 --- f_n [i] assumed value of n (6)
145 A1 --- l_theta Limit flag on theta
147-151 F5.2 deg theta [0.45,80.26]? Collimation angle (θj) (7)
153 A1 --- l_Ebolt Limit flag on Ebolt
155-162 E8.3 10-7J Ebolt [1e+40,1.38e+52]? Beaming-corrected (true)
bolometric energy (in erg) (7)
164-186 A23 --- Ref References (see refs.dat file) (8)
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Note (1): Flag as follows:
l = Observed with WSRT, VLBA, Ryle, ATCA and GMRT in addition to VLA/EVLA.
m = Double jet break.
n = SN/GRB (GRB with possible SN association). See section 2.1.
o = SHB (short-hard burst).
p = XRF (X-ray flash).
q = Galactic transient?
r = Also observed with WSRT (Westerbork Synthesis Radio Telescope).
s = Also observed with VLBA (Very Long Baseline Array).
t = Also observed with the Ryle telescope.
u = Also observed with ATCA (Australia Telescope Compact Array).
v = Also observed with GMRT (Giant Metrewave Radio Telescope).
Note (2): Instrument code as follows:
A = ASM;
B = BeppoSAX;
F = Fermi;
H = HETE;
I = INTEGRAL,
P = PCA;
S = Swift;
sA = superAGILE,
T = IPN Triangulation
Note (3): Symbol "Y" indicates a detection, while "N" indicates a non-detection.
The symbol "X" means the burst was not observed in that particular
band, whereas "Y?" indicates that the observation was made but a
detection could not be confirmed.
Note (4): For non Swift fluences, the available fluences have been extrapolated
to this energy range using formulation of Nysewander et al. (2009,
Cat. J/ApJ/701/824).
Note (5): The fluxes are mentioned in 0.3-10keV energy range. However, the
fluxes for the BeppoSAX bursts are quoted in the energy range of
1.6-10 keV.
Note (6):
i = The GRBs for which number densities are not available; we assume a number
density of 1cm-3.
Note (7): We estimate the collimation angle θj (deg) and the
beaming-corrected bolometric energy (Eboltrue) of GRBs with
observed tj using Frail et al. (2001ApJ...562L..55F 2001ApJ...562L..55F) and Bloom
et al. (2003ApJ...594..674B 2003ApJ...594..674B).
Note (8): References are in the following order: T90, z, fluence, bolometric
isotropic energy, X-ray flux at 11hr, Optical flux density at 11hr,
jet break time and density. If a particular cell is empty, then the
reference has value "[]". However, a reference value of "[]" for a
non-empty corresponding cell means that we have estimated the values
ourselves using GCN circulars.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- GRB GRB name (YYMMDDA)
9- 13 F5.2 GHz Freq [1.38,43] Frequency of the observation
15- 19 I5 uJy Fm [50,59318] Peak flux density (Fm) (1)
21- 23 I3 uJy e_Fm [9,557]? Fm uncertainty
25- 29 F5.1 d tm [1.3,179.1] Peak time (1)
31- 34 F4.1 d e_tm [0.1,11.3]? tm uncertainty
36- 39 F4.1 d tm/(1+z) [0.6,97.6]? Rest-frame peak time (1)
41- 43 F3.1 d e_tm/(1+z) [0.1,5]? tm/(1+z) uncertainty
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Note (1): See section 3.5 and equation (1) for further details.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Ref Reference code
4- 22 A19 --- BibCode Bibcode
24- 47 A24 --- Aut Author's name(s)
49-122 A74 --- Comm Comment
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 12-Sep-2013