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RSSGRBAG - Radio-Selected Gamma-Ray Burst Afterglow Catalog |
HEASARC Archive |
Overview
This table contains a catalog of radio afterglow observations of gamma-ray bursts (GRBs) over a 14 year period from 1997 to 2011. This sample of 304 afterglows consists of 2,995 flux density measurements (including upper limits) at frequencies between 0.6 GHz and 660 GHz, with the majority of data taken in the 8.5-GHz frequency band (1,539 measurements). The authors use this dataset to carry out a statistical analysis of the radio-selected sample. The detection rate of radio afterglows 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, the authors find few significant correlations between these same GRB and afterglow properties and the peak radio flux density. In their paper, they also produce synthetic light curves at centimeter and millimeter bands using a range of blast wave and microphysics parameters derived from multi-wavelength afterglow modeling, and use them to compare with the radio sample. Finding agreement, the authors extrapolate this behavior to predict the centimeter and millimeter behavior of GRBs which will observed by the Expanded Very Large Array and the Atacama Large Millimeter Array.The compiled sample consists of 304 GRBs observed with 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 2,995 flux density measurements taken in the frequency range from 0.6 to 660 GHz and spanning a time range from 0.026 to 1,339 days. Most of the afterglows (270 in total) in this sample were observed as part of VLA radio afterglow programs, whereas 15 bursts were observed by the Expanded VLA (EVLA), and 19 southern bursts with the Australia Telescope Compact Array (ATCA). This catalog describes the radio, optical and X-ray afterglow detections (see Section 2.2 of the reference paper): 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 (the post-Swift epoch).
Out of the 95 radio-detected afterglows (see Section 2.2 of the reference paper), 63 had radio lightcurves (i.e., three or more detections in a single radio band), whereas 32 bursts had less than three detections. For the GRBs for which the light curves were available, the authors determined the peak flux density and the time of the peak in the VLA frequency bands (i.e., 1.4 GHz, 4.9 GHz, 8.5 GHz, 15 GHz, and 22.5 GHz bands) by fitting the data with forward shock formula of the form (Frail 2005, IAU Coll. 192, p. 451) given in equation (1) of the reference paper. This formula may not accurately represent the full complexity of the radio lightcurve evolution. However, it is good enough to determine the approximate values for the peak flux density Fm and the time of the peak tm. See the discussion in Section 3.5 of the reference paper for more details and some caveats. For the remaining bursts, the flux density values were taken directly from the data, and hence do not have the best-fit errors for the peak flux, peak time and rest-frame peak time parameters Fm, tm and tm/(1+z), respectively.
Catalog Bibcode
2012ApJ...746..156CReferences
A radio-selected sample of gamma-ray burst afterglows.
Chandra P., Frail D.A.
<Astrophys. J., 746, 156 (2012)>
=2012ApJ...746..156C (SIMBAD/NED BibCode)
Provenance
This table was created by the HEASARC in November 2013 based on CDS catalog J/ApJ/746/156 files table1.dat and table4.dat.Parameters
Name
The gamma-ray burst designation in the standard date-based YY-MM-DD
format, e.g., 'GRB 970228[N]' for a burst which occurred in 1997 on Feb 28.
For dates on which more than one GRB was detected, suffices 'A', 'B', etc.,
are added.
Source_Flag
This source flag parameter contains codes indicating notes
concerning specific GRBs with the following meanings:
m = Double jet break.
n = SN/GRB (GRB with possible SN association). See section 2.1 of ref.
o = SHB (short-hard burst).
p = XRF (X-ray flash).
q = Galactic transient?
r = Also observed with WSRT (Westerbork Synthesis Radio Telescope).
The HEASARC notes that the value of 'r' occurs for only one GRB (090423) and likely should have been used for the radio_telescope_flag parameter value then for the source_flag value.
Instrument_Code
This flag parameter indicates the mission or instrument
which discovered the GRB, coded as follows:
A = ASM;
B = BeppoSAX;
F = Fermi;
H = HETE;
I = INTEGRAL,
P = PCA;
S = Swift;
sA = superAGILE,
T = IPN Triangulation.
RA
The Right Ascension of the GRB in the selected equinox. This was given in
J2000.0 equatorial coordinates to a precision of 0.1 seconds of time for GRBs
which occurred in the period 1997 from 2001 inclusive, and to 0.01 seconds of
time for GRBs which occurred in the period 2002 to 2011 inclusive, with a few
exceptions, viz., GRB 031111 (precision of 1 s), GRB 090328 (precision of 0.1
s) and GRB 090902B (precision of 0.1 s).
Dec
The Declination of the GRB in the selected equinox. This was given in
J2000.0 equatorial coordinates to a precision of 1 arcseconds for GRBs
which occurred in the period 1997 from 2001 inclusive, and to 0.1 arcseconds
for GRBs which occurred in the period 2002 to 2011 inclusive.
LII
The Galactic Longitude of the GRB.
BII
The Galactic Latitude of the GRB.
Xray_Ag_Flag
This flag parameter indicates the detection ('Y') or not ('N')
of the GRB afterglow in the X-ray band; 'X' means that the burst was not
observed in this band, while 'Y?' means that the observation was made but that
the detection could not be confirmed.
Opt_Ag_Flag
This flag parameter indicates the detection ('Y') or not ('N')
of the GRB afterglow in the optical band; 'X' means that the burst was not
observed in this band, while 'Y?' means that the observation was made but that
the detection could not be confirmed.
Radio_Ag_Flag
This flag parameter indicates the detection ('Y') or not
('N') of the GRB afterglow in the radio band; 'X' means that the burst was not
observed in this band, while 'Y?' means that the observation was made but that
the detection could not be confirmed.
Radio_Telescope
The (primary) radio telescope used to observe the
corresponding burst: ATCA, EVLA or VLA.
Radio_Telescope_Flag
This flag parameter indicates additional radio
telescope(s) used to observe the burst in addition to the one specified by'
the radio_telescope parameter, coded as follows:
l = Observed with WSRT, VLBA, Ryle, ATCA and GMRT in addition to VLA/EVLA;
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).
T90
The T90, duration of the burst, viz., the time interval over which
90% of the total background-subtracted counts are observed within the the
time interval starting at 5% of the total counts having been observed and
ending with 95% of the total counts having been observed (Koshut et al. 1995,
BAAS, 27, 886) in the observer's frame and in the energy band of the specific
detector of the burst: thus, for example, for Swift bursts, the T90
durations are in the 15-350 keV energy range.
Redshift_Limit
This limit parameter is set to '<' if the corresponding
redshift value is an upper limit rather than an actual value.
Redshift
The redshift z of the burst or, if a value is given for the
maximum redshift (redshift_max parameter), the minimum allowed redshift of the
burst.
Redshift_Max
If populated, the maximum allowed redshift of the burst.
Fluence_15_150_keV
The GRB fluence of the burst in the 15-150 keV energy
range, in erg cm-2.
Iso_Bol_Energy
The k-corrected bolometric gamma-ray energy in the
1-10,000 keV rest-frame energy range if it were isotropic, in erg.
Xray_Flux_11h_Limit
This limit parameter is set to '<' if the corresponding
parameter value is an upper limit rather than an actual value.
Xray_Flux_11h
The X-ray flux of the burst at 11 hours, FX11, in the
0.3-10 keV energy range (except if the flux comes from BeppoSAX as indicated
by a value of instrument_code = 'B', in which case it is in the 1.6-10 keV
energy range), in erg s-1 cm-2.
Opt_Flux_11h_Limit
This limit parameter is set to '<' if the corresponding
parameter value is an upper limit rather than an actual value.
Opt_Flux_11h
The optical R-band (0.7 micron) flux density of the burst at
11 hours, FX11, in microJansky (µJy).
Jet_Break_Time_Limit
This limit parameter is set to '<' if the corresponding
parameter value is an upper limit rather than an actual value, or to '>'
if the corresponding parameter value is a lower limit
Jet_Break_Time
The jet break time, tj, in days, in cases where a clear
jet break is seen.
Jet_Break_Time_Flag
This flag parameter is set to '?' to indicates that
there is uncertainty in the jet break time value.
Cbm_Number_Density
The inferred or assumed number density n of the
circumburst medium, in cm-3.
Cbm_Number_Density_Flag
This flag parameter is set to 'i' to indicate
cases where the number density is not known, and has been assumed to be
1 cm-3.
Coll_Angle_Limit
This limit parameter is set to '<' if the corresponding
parameter value is an upper limit rather than an actual value, or to '>'
if the corresponding parameter value is a lower limit .
Coll_Angle
The collimation angle, Thetaj, of the burst, in degrees.
This was estimated for GRBs with observed tj values using Frail et al.
(2001, ApJ, 562, L55) and Bloom et al. (2003, ApJ, 594, 674).
True_Bol_Energy_Limit
This limit parameter is set to '<' if the
corresponding parameter value is an upper limit rather than an actual value,
or to '>' if the corresponding parameter value is a lower limit.
True_Bol_Energy
The beaming (collimated) corrected energy, Etruebol,
of the burst, in erg. This was estimated for GRBs with observed tj values
using Frail et al. (2001, ApJ, 562, L55) and Bloom et al. (2003, ApJ, 594,
674).
Ref_Codes
The coded references for the properties of the GRB in the
following order: T90, z, fluence, bolometric isotropic energy, X-ray flux
at 11 hr, optical flux density at 11 hr, jet break time tj and density n.
If a particular parameter value is empty, then the ref_code has been given a
value of '[]'. However, a ref_code value of '[]' for a non-empty
corresponding parameter value means that the authors have estimated the
values themselves using GCN circulars, and that this paper itself is the
reference source. The numerical reference codes are as follows:
Code Bibcode Authors URL or CDS Catalog 1 2010A&A...517A...5A Aleksic et al. 2 2010ApJ...712L..31C Chandra et al. 3 2006MNRAS.372..233A Amati 4 2000ApJ...545L..39A Antonelli et al. 5 2005Natur.438..988B Berger et al. 6 2007ApJ...660..496B Berger et al. 7 2001AJ....121.2879B Bloom et al. 8 2007ApJ...671..656B Butler et al. 9 2009MNRAS.400..775C Cardone et al. 10 2006ApJ...652..490C Cenko et al. 11 2008ApJ...683..924C Chandra et al. 12 2010ApJ...708L.112D Dado & Dar 13 2006A&A...455..813D de Pasquale et al. CDS Cat. J/A+A/455/813 14 2006MNRAS.370..185F Firmani et al. 16 2000ApJ...537..191F Frail et al. 17 2001ApJ...562L..55F Frail et al. 18 2006ApJ...646L..99F Frail et al. 19 2009ApJS..180..192F Frontera et al. CDS Cat. J/ApJS/180/192 20 2009ApJS..185..526F Fynbo et al. 21 2008ApJ...689.1161G Gehrels et al. 22 2004ApJ...616..331G Ghirlanda et al. 23 2010A&A...511A..43G Ghirlanda et al. 24 2005A&A...437..411G Gorosabel et al. 25 2009ApJ...698.1620G Graham et al. 26 GCN Circulars Archive http://gcn.gsfc.nasa.gov/gcn3_archive.html 27 2012grbu.book..169H Hjorth & Bloom 28 1997IAUC.6683....1C Connaughton et al. 29 1997IAUC.6718....1S Smith et al. 30 1999IAUC.7174....1G Gandolfi et al. 31 2004ApJ...617L..21J Jakobsson et al. 32 2011ApJ...734...96K Kann et al. 33 2010ApJ...720.1513K Kann et al. CDS Cat. J/ApJ/720/1513 34 2009MNRAS.395L..21K Kuin et al. 35 2001ApJ...556..471L Lazzati et al. 36 2007ApJ...670..565L Liang et al. 37 2009ApJ...701..824N Nysewander et al. CDS Cat. J/ApJ/701/824 38 2009MNRAS.395..490O Oates et al. 39 2010ApJ...714..799P Pandey et al. 40 2008A&A...491..157P Pelangeon et al. 41 2011AN....332..297D de Ugarte Postigo et al. 42 2009ApJ...698...43R Racusin et al. 43 2011ApJ...728...42R Rao et al. 44 2005ApJ...629..311S Sakamoto et al. 45 2008ApJS..175..179S Sakamoto et al. CDS Cat. J/ApJS/175/179 46 2011ApJS..195....2S Sakamoto et al. CDS Cat. J/ApJS/195/2 47 2004Natur.430..648S Soderberg et al. 48 2005ApJ...627..877S Soderberg et al. 49 2006ApJ...650..261S Soderberg et al. 50 2006Natur.442.1014S Soderberg et al. 51 2010ApJ...725..625T Tanvir et al. 52 2009Natur.461.1254T Tanvir et al. 53 2004ApJ...609..935Y Yonetoku et al. CDS Cat. J/ApJ/609/935 54 http://www.raunvis.hi.is/~pja/GRBsample.html 55 INTEGRAL Trigger info http://gcn.gsfc.nasa.gov/integral_grbs.html 56 http://www.ssl.berkeley.edu/ipn3/ 57 http://www.grbhosts.org/ 58 http://space.mit.edu/HETE/Bursts/ 59 http://www.swift.ac.uk/xrt_curves/ 60 2001grba.conf...26B Bradt et al. 61 2003ApJ...594..674B Bloom et al. 62 2011ApJ...732...29C Cenko et al. 63 2010A&A...516A..71M McBreen et al. 64 2011ApJ...736....7C Cucchiara et al. 65 2003Natur.426..154B Berger et al. 66 2003ApJ...599.1223G Greiner et al. 67 2005ApJ...631L..29C Christensen et al. 68 2010GCN..11089...1O O'Meara et al. 69 2010GCN..11164...1C Chornock et al. 70 2010GCN..11230...1T Tanvir et al.
Radio_Freq_1
The radio frequency of the GRB afterglow detection, in GHz.
If the afterglow was detected at multiple radio frequencies, this is the
lowest frequency at which it was detected.
Peak_Flux_Freq_1
The peak flux density of the GRB afterglow at the
corresponding frequency (given by the radio_freq_1 value), in uJy.
This is obtained as discussed in the Overview above.
Peak_Flux_Freq_1_Error
The error in the peak flux density at the
corresponding frequency, in uJy. This is not given for those bursts for which
the value was taken directly from the data rather than using a fit with the
forward shock formula.
Peak_Time_1
The time of the peak of the radio afterglow, tm, in days
since the GRB, in the observer's frame and at the corresponding frequency
radio_freq_1. This is obtained as discussed in the Overview above.
Peak_Time_1_Error
The error in the time of the peak of the radio
afterglow, tm, in days since the GRB, in the observer's frame and at the
corresponding frequency. This is not given for those bursts for which the
value was taken directly from the data rather than using a fit with the
forward shock formula.
RF_Peak_Time_1
The time of the peak of the radio afterglow, tm/(1+z), in
days since the GRB, corrected to the rest-frame as shown, for bursts with known
redshifts, at the corresponding frequency radio_freq_1. The authors
did not estimate the rest-frame peak time for bursts with unknown redshifts.
RF_Peak_Time_1_Error
The error in the rest-frame time of the peak of the
radio afterglow, tm/(1+z), in days since the GRB, at the corresponding
frequency. This is not given for those bursts for which the value was taken
directly from the data rather than using a fit with the forward shock
formula.
Radio_Freq_2
The radio frequency of the GRB afterglow detection, in GHz.
If the afterglow was detected at multiple radio frequencies, this is the
second lowest frequency at which it was detected.
Peak_Flux_Freq_2
The peak flux density of the GRB afterglow at the
corresponding frequency (given by the radio_freq_2 value), in uJy.
This is obtained as discussed in the Overview above.
Peak_Flux_Freq_2_Error
The error in the peak flux density at the
corresponding frequency, in uJy. This is not given for those bursts for
which the value was taken directly from the data rather than using a
fit with the forward shock formula.
Peak_Time_2
The time of the peak of the radio afterglow, tm, in days
since the GRB, in the observer's frame and at the corresponding frequency
radio_freq_2. This is obtained as discussed in the Overview above.
Peak_Time_2_Error
The error in the time of the peak of the radio
afterglow, tm, in days since the GRB, in the observer's frame and at the
corresponding frequency. This is not given for those bursts for which the
value was taken directly from the data rather than using a fit with the
forward shock formula.
RF_Peak_Time_2
The time of the peak of the radio afterglow, tm/(1+z), in
days since the GRB, corrected to the rest-frame as shown, for bursts with known
redshifts, at the corresponding frequency radio_freq_2. The authors
did not estimate the rest-frame peak time for bursts with unknown redshifts.
RF_Peak_Time_2_Error
The error in the rest-frame time of the peak of the
radio afterglow, tm/(1+z), in days since the GRB, at the corresponding
frequency. This is not given for those bursts for which the value was taken
directly from the data rather than using a fit with the forward shock
formula.
Radio_Freq_3
The radio frequency of the GRB afterglow detection, in GHz.
If the afterglow was detected at multiple radio frequencies, this is the
third lowest frequency at which it was detected.
Peak_Flux_Freq_3
The peak flux density of the GRB afterglow at the
corresponding frequency (given by the radio_freq_3 value), in uJy.
This is obtained as discussed in the Overview above.
Peak_Flux_Freq_3_Error
The error in the peak flux density at the
corresponding frequency, in uJy. This is not given for those bursts for
which the value was taken directly from the data rather than using a
fit with the forward shock formula.
Peak_Time_3
The time of the peak of the radio afterglow, tm, in days
since the GRB, in the observer's frame and at the corresponding frequency
radio_freq_3. This is obtained as discussed in the Overview above.
Peak_Time_3_Error
The error in the time of the peak of the radio afterglow,
tm, in days since the GRB, in the observer's frame and at the
corresponding frequency. This is not given for those bursts for
which the value was taken directly from the data rather than using a
fit with the forward shock formula.
RF_Peak_Time_3
The time of the peak of the radio afterglow, tm/(1+z), in
days since the GRB, corrected to the rest-frame as shown, for bursts with
known redshifts, at the corresponding frequency radio_freq_3. The authors did
not estimate the rest-frame peak time for bursts with unknown redshifts.
RF_Peak_Time_3_Error
The error in the rest-frame time of the peak of the
radio afterglow, tm/(1+z), in days since the GRB, at the corresponding
frequency. This is not given for those bursts for which the value was taken
directly from the data rather than using a fit with the forward shock
formula.
Radio_Freq_4
The radio frequency of the GRB afterglow detection, in GHz.
If the afterglow was detected at multiple radio frequencies, this is the
fourth lowest frequency at which it was detected.
Peak_Flux_Freq_4
The peak flux density of the GRB afterglow at the
corresponding frequency (given by the radio_freq_4 value), in uJy.
This is obtained as discussed in the Overview above.
Peak_Flux_Freq_4_Error
The error in the peak flux density at the
corresponding frequency, in uJy. This is not given for those bursts for
which the value was taken directly from the data rather than using a
fit with the forward shock formula.
Peak_Time_4
The time of the peak of the radio afterglow, tm, in days
since the GRB, in the observer's frame and at the corresponding frequency
radio_freq_4. This is obtained as discussed in the Overview above.
Peak_Time_4_Error
The error in the time of the peak of the radio afterglow,
tm, in days since the GRB, in the observer's frame and at the
corresponding frequency. This is not given for those bursts for
which the value was taken directly from the data rather than using a
fit with the forward shock formula.
RF_Peak_Time_4
The time of the peak of the radio afterglow, tm/(1+z), in
days since the GRB, corrected to the rest-frame as shown, for bursts with known
redshifts, at the corresponding frequency radio_freq_4. The authors
did not estimate the rest-frame peak time for bursts with unknown redshifts.
RF_Peak_Time_4_Error
The error in the rest-frame time of the peak of the
radio afterglow, tm/(1+z), in days since the GRB,
at the corresponding frequency. This is not given for
those bursts for which the value was taken directly from the data rather than
using a fit with the forward shock formula.
Radio_Freq_5
The radio frequency of the GRB afterglow detection, in GHz.
If the afterglow was detected at multiple radio frequencies, this is the
fifth lowest frequency at which it was detected.
Peak_Flux_Freq_5
The peak flux density of the GRB afterglow at the
corresponding frequency (given by the radio_freq_5 value), in uJy.
This is obtained as discussed in the Overview above.
Peak_Flux_Freq_5_Error
The error in the peak flux density at the
corresponding frequency, in uJy. This is not given for those bursts for
which the value was taken directly from the data rather than using a
fit with the forward shock formula.
Peak_Time_5
The time of the peak of the radio afterglow, tm, in days
since the GRB, in the observer's frame and at the corresponding frequency
radio_freq_5. This is obtained as discussed in the Overview above.
Peak_Time_5_Error
The error in the time of the peak of the radio
afterglow, tm, in days since the GRB, in the observer's frame and at the
corresponding frequency. This is not given for those bursts for which the
value was taken directly from the data rather than using a fit with the
forward shock formula.
RF_Peak_Time_5
The time of the peak of the radio afterglow, tm/(1+z), in
days since the GRB, corrected to the rest-frame as shown, for bursts with
known redshifts, at the corresponding frequency radio_freq_5. The authors did
not estimate the rest-frame peak time for bursts with unknown redshifts.
RF_Peak_Time_5_Error
The error in the rest-frame time of the peak of the
radio afterglow, tm/(1+z), in days since the GRB, at the corresponding
frequency. This is not given for those bursts for which the value was taken
directly from the data rather than using a fit with the forward shock
formula.
Radio_Freq_6
The radio frequency of the GRB afterglow detection, in GHz.
If the afterglow was detected at multiple radio frequencies, this is the
sixth lowest frequency at which it was detected.
Peak_Flux_Freq_6
The peak flux density of the GRB afterglow at the
corresponding frequency (given by the radio_freq_6 value), in uJy.
This is obtained as discussed in the Overview above.
Peak_Flux_Freq_6_Error
The error in the peak flux density at the
corresponding frequency, in uJy. This is not given for those bursts for
which the value was taken directly from the data rather than using a
fit with the forward shock formula.
Peak_Time_6
The time of the peak of the radio afterglow, tm, in days
since the GRB, in the observer's frame and at the corresponding frequency
radio_freq_6. This is obtained as discussed in the Overview above.
Peak_Time_6_Error
The error in the time of the peak of the radio
afterglow, tm, in days since the GRB, in the observer's frame and at the
corresponding frequency. This is not given for those bursts for which the
value was taken directly from the data rather than using a fit with the
forward shock formula.
RF_Peak_Time_6
The time of the peak of the radio afterglow, tm/(1+z), in
days since the GRB, corrected to the rest-frame as shown, for bursts with
known redshifts, at the corresponding frequency radio_freq_6. The authors did
not estimate the rest-frame peak time for bursts with unknown redshifts.
RF_Peak_Time_6_Error
The error in the rest-frame time of the peak of the
radio afterglow, tm/(1+z), in days since the GRB, at the corresponding
frequency. This is not given for those bursts for which the value was taken
directly from the data rather than using a fit with the forward shock
formula.
Contact Person
Questions regarding the RSSGRBAG database table can be addressed to the HEASARC Help Desk.Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:34:12 EDT
- HEASARC Director: Dr. Andy Ptak
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- Last Modified: 16-Sep-2024