J/ApJS/211/13 The second Fermi/GBM GRB catalog (4yr) (von Kienlin+, 2014)
The second Fermi GBM gamma-ray burst catalog: the first four years.
von Kienlin A., Meegan C.A., Paciesas W.S., Bhat P.N., Bissaldi E.,
Briggs M.S., Burgess J.M., Byrne D., Chaplin V., Cleveland W.,
Connaughton V., Collazzi A.C., Fitzpatrick G., Foley S., Gibby M.,
Giles M., Goldstein A., Greiner J., Gruber D., Guiriec S.,
van der Horst A.J., Kouveliotou C., Layden E., McBreen S., McGlynn S.,
Pelassa V., Preece R.D., Rau A., Tierney D., Wilson-Hodge C.A., Xiong S.,
Younes G., Yu H.-F.
<Astrophys. J. Suppl. Ser., 211, 13 (2014)>
=2014ApJS..211...13V 2014ApJS..211...13V
ADC_Keywords: Gamma rays ; Surveys
Mission_Name: Fermi
Keywords: catalogs; gamma-ray burst: general
Abstract:
This is the second of a series of catalogs of gamma-ray bursts (GRBs)
observed with the Fermi Gamma-ray Burst Monitor (GBM). It extends the
first two-year catalog by two more years, resulting in an overall list
of 953 GBM triggered GRBs. The intention of the GBM GRB catalog is to
provide information to the community on the most important observables
of the GBM detected GRBs. For each GRB the location and main
characteristics of the prompt emission, the duration, peak flux and
fluence are derived. The latter two quantities are calculated for the
50-300keV energy band, where the maximum energy release of GRBs in the
instrument reference system is observed and also for a broader energy
band from 10-1000keV, exploiting the full energy range of GBMs
low-energy detectors. Furthermore, information is given on the
settings and modifications of the triggering criteria and exceptional
operational conditions during years three and four in the mission.
This second catalog is an official product of the Fermi GBM science
team, and the data files containing the complete results are available
from the High-Energy Astrophysics Science Archive Research Center.
Description:
The Fermi Gamma-ray Burst Monitor (GBM), the secondary instrument on
board the Fermi Gamma-ray Space Telescope, launched on 2008 June 11,
is now operating successfully in space since five years. The GBM
instrument extends the energy range of the main instrument, the Large
Area Telescope (LAT; 30MeV-300GeV) down to the soft gamma-ray and
X-ray energy range (8keV-40MeV). In the first four years of operation
since triggering was enabled on 2008 July 12, GBM has triggered 2126
times on a variety of transient events: 954 of these are classified as
GRBs (in one case the same GRB triggered GBM twice).
The location of a GRB is calculated by comparing the measured
individual detector counting rates with a lookup table (LUT),
containing a list of relative detector rates for a grid of simulated
sky locations. The on-board and on-ground LUTs have resolutions of
5° and 1°, respectively. With this method the limiting
accuracy is approximately 8° for on-board locations and
approximately 4° for on-ground locations. A detailed investigation
of the GBM location accuracy can be found in Connaughton, V., Briggs,
M. S., & Goldstein, A. et al. 2014 (ApJS, submitted).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 56 73 *Trigger criteria history
table6.dat 114 954 GRB triggers: locations and trigger characteristics
table7.dat 75 954 GRB durations (50-300keV)
table8.dat 74 954 GRB fluence and peak flux (10-1000keV)
table9.dat 74 954 GRB fluence and peak flux (50-300keV)
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Note on table2.dat: The GBM trigger algorithms implemented in the flight
software (FSW) monitor the background count rates of all NaI detectors for the
occurrence of a significant count rate increase in different energy ranges and
timescales with adjustable sensitivities. A trigger is only generated in case
of simultaneous exceedance of the trigger threshold of at least two detectors,
thus reducing the probability for false triggers. See section 2.2 for further
explanations.
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See also:
J/ApJS/208/21 : The BATSE 5B GRB spectral catalog (Goldstein+, 2013)
J/ApJS/207/39 : IPN supplement to the Fermi GBM (Hurley+, 2013)
J/A+A/553/A33 : AGILE Mini-Calorimeter GRB catalog (Galli+, 2013)
J/ApJ/756/112 : Fermi/GBM GRB time-resolved spectral analysis (Lu+, 2012)
J/ApJ/754/121 : GRBs from Fermi/GBM and LAT (The Fermi Team, 2012)
J/ApJS/199/18 : The Fermi GBM catalog (Paciesas+, 2012)
J/A+A/525/A53 : GBM parameters for detected FERMI bursts (Guetta+, 2011)
J/A+A/530/A21 : Spectral properties of 438 GRBs (Nava+, 2011)
J/ApJS/195/2 : The second Swift BAT GRB catalog (BAT2) (Sakamoto+, 2011)
J/ApJ/711/495 : Durations of Swift/BAT GRBs (Butler+, 2010)
J/A+A/438/1175 : First INTEGRAL SPI-ACS GRB Catalogue (Rau+, 2005)
J/ApJS/134/385 : Supplement to the BATSE GRB catalogs (Kommers+, 2001)
http://gcn.gsfc.nasa.gov/ : GCN home page
http://www.isdc.unige.ch/integral/science/grb#ISGRI : INTEGRAL Science data
centre
http://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html : Fermi GBM Burst
online catalog
http://heasarc.gsfc.nasa.gov/W3Browse/all/batsegrb.html : BATSE GRB catalog
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Alg [1/119] Algortithm number
5 A1 --- f_Alg [b] BGO detector used (1)
7- 11 I5 ms Time [16/16384]? Time scale
13- 16 I4 ms Off [0/8192]? Time offset
18- 24 A7 --- Ch Channels (2-2, 3-4, 4-7, 5-7 or BGO/3-6)
26- 32 A7 keV Erange Energy range
35- 36 A2 --- Th1 0.1σ threshold on 2008 Jul 11 (2)
38- 39 A2 --- Th2 0.1σ threshold on 2008 Jul 14 (2)
41- 42 A2 --- Th3 0.1σ threshold on 2008 Aug 1 (2)
44- 45 A2 --- Th4 0.1σ threshold on 2009 May 8 (2)
47 A1 --- Th5 0.1σ threshold on 2009 Oct 29 (2)
49- 50 A2 --- Th6 0.1σ threshold on 2009 Nov 10 (2)
52- 53 A2 --- Th7 0.1σ threshold on 2009 Dec 7 (2)
55- 56 A2 --- Th8 0.1σ threshold on 2010 Mar 26 (2)
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Note (1):
b = Trigger algorithms using the BGO detector count rates. Algorithm 116
triggers off when at least two NaI and one BGO detectors are exceeding
the trigger threshold. Algorithms 117 is same as 116, but impose the
additional requirement that the triggered detectors are on the +X side
of the spacecraft. Algorithm 118 is the same as 117, but requiring the
triggered detectors to be on the -X side of the spacecraft. Algorithm
119 requires a significant rate increase in both BGO detectors.
Note (2): Symbol as follows:
: = no change from previous setting
C = the algorithm is in compute mode
D = the algorithm is disabled
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [bn]
3- 11 I09 --- TID Trigger identifier (YYMMDDNNN)
13 A1 --- n_TID [ic] Remarks (1)
15- 17 A3 --- --- [GRB]
19- 25 A7 --- GRB GRB name (YYMMDDA)
27- 29 A3 --- f_GRB [ia-g, ] Flag on GRB (1)
31- 43 A13 "h:m:s" ObsTime Time of the Observation
45- 49 F5.1 deg RAdeg Right Ascension in decimal degrees (J2000)
51- 55 F5.1 deg DEdeg Declination in decimal degrees (J2000)
57- 60 F4.1 deg Err [0.1/50]?=0 Positional error
62- 70 A9 --- Loc Source of the coordinate localization used
for the trigger (Fermi, Swift, IPN...) (2)
72- 73 I2 --- Alg [1/56] Algorithm used
75- 78 I4 ms Time [16/8192] Timescale
80- 85 A6 keV Erange Energy range of detection
87-114 A28 --- OtherDet Other instrument detections (3)
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Note (1): Flag as follows:
i = Bursts with TID and Name both flagged have significant emission in
at least one BGO detector (see text).
a = The trigger bn100724029 should have the ID GRB 100724B (see GCN #10978).
GRB 100724B identifier validated by the author.
b = bn120222021 should have the ID GRB120222A and
bn120222119 the ID GRB120222B; identifiers verified by the author.
c = GRB091024A triggered GBM twice.
d = bn101214993 should have the ID GRB101214B.
e = bn110517573 should have the ID GRB110517B;
f = bn110517902 should have the ID GRB110517C.
g = bn110920546 should have the ID GRB110920B.
Note (2): The GRB locations are adopted from the BA analysis results,
uploaded to the GBM trigger catalog at the National Space Science and
Technology Center (NSSTC; with a copy at the FSSC). Non-GBM locations
are listed for bursts that were detected by an instrument providing a
better location accuracy, such as Swift Burst Alert Telescope (BAT)
(Barthelmy et al. 2005SSRv..120..143B 2005SSRv..120..143B) or X-ray Telescope (XRT)
(Burrows et al. 2005SSRv..120..165B 2005SSRv..120..165B), or were localized more precisely
by the Inter-Planetary Network (IPN; Hurley et al. 2013, J/ApJS/207/39).
Note (3): Instrument as follows:
Mo = Mars Observer;
K = Konus-Wind;
R = RHESSI;
IA = INTEGRAL SPI-ACS;
IS = INTEGRAL IBIS-ISGRI;
S = Swift;
Me = Messenger;
W = Suzaku;
A = AGILE;
M = MAXI;
L = Fermi LAT.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [bn]
3- 11 I09 --- TID Trigger identifier (YYMMDDNNN)
13 A1 --- Rem Remarks on detection (4)
15- 27 A13 --- Det Detectors used
29- 35 F7.3 s T90 [0.04/605]? The T90 burst duration measure
37- 42 F6.3 s e_T90 [0.03/36]? Uncertainty in T90
44- 51 F8.3 s T90st ? Start of T90 duration
53- 59 F7.3 s T50 ? The T50 burst duration measure
61- 66 F6.3 s e_T50 ? Uncertainty in T50
68- 75 F8.3 s T50st ? Start of T50 duration
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Note (4): Flag as follows:
a = Data problems precluded duration analysis.
b = Used TTE binned at 32ms.
c = Partial earth occultation is likely; durations are lower limits.
d = Possible precursor at ∼T0-120s.
e = Data cut off due to SAA entry while burst in progress;
durations are lower limits.
f = SAA entry at T_0+83 s; durations are lower limits.
g = Used TTE binned at 16ms.
h = GRB091024 triggered GBM twice.
i = Too weak to measure durations; visual duration is ∼0.025s.
j = Possible contamination due to emergence of Crab and
A0535+26 from Earth occultation.
k = Solar activity starting at T0+200s. Post burst background
interval was selected before.
l = Data cut off due to SAA entry while burst in progress;
it is not possible to determine durations.
m = Spacecraft in sun pointing mode, detector threshold raised,
location of burst nearly in z direction. The response, peak
fluxes and fluence in the 10-100keV energy range have large
errors. Fluence, peak fluxes and durations in BATSE energy
range (50-300keV) are reliable.
n = Localization of precursor at T0-120s is consistent with
burst location and was included in the duration analysis.
o = SAA entry at T0+100s; durations are lower limits.
p = TTE/CTTE data not available, 64ms peak fluxes may not be correct.
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [bn]
3- 11 I09 --- TID Trigger identifier (YYMMDDNNN)
13- 20 E8.3 mJ/m2 Fl.w ? Fluence on wide (10-1000keV) band;
in erg/cm2
22- 29 E8.3 mJ/m2 e_Fl.w ? Uncertainty in Fl.w
31- 37 F7.2 ph/cm2/s PF1.w [0.5/3055]? Peak flux with 64ms binning
39- 45 F7.2 ph/cm2/s e_PF1.w [0.1/4476]? Uncertainty in PF1.w
47- 52 F6.2 ph/cm2/s PF2.w ? Peak flux with 256ms binning
54- 60 F7.2 ph/cm2/s e_PF2.w ? Uncertainty in PF2.w
62- 67 F6.2 ph/cm2/s PF3.w ? Peak flux with 1024ms binning
69- 74 F6.2 ph/cm2/s e_PF3.w ? Uncertainty in PF3.w
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [bn]
3- 11 I09 --- TID Trigger identifier (YYMMDDNNN)
13- 20 E8.3 mJ/m2 Fl.n ? Fluence on narrow (50-300keV) band;
in erg/cm2
22- 29 E8.3 mJ/m2 e_Fl.n ? Uncertainty in Fl.n
31- 37 F7.2 ph/cm2/s PF1.n [0.5/3055]? Peak flux with 64ms binning
39- 45 F7.2 ph/cm2/s e_PF1.n [0.1/4476]? Uncertainty in PF1.n
47- 52 F6.2 ph/cm2/s PF2.n ? Peak flux with 256ms binning
54- 60 F7.2 ph/cm2/s e_PF2.n ? Uncertainty in PF2.n
62- 67 F6.2 ph/cm2/s PF3.n ? Peak flux with 1024ms binning
69- 74 F6.2 ph/cm2/s e_PF3.n ? Uncertainty in PF3.n
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History:
* 08-Apr-2014: From electronic version of the journal
* 05-Jun-2014: Insert into VizieR
* 02-Dec-2014: In table 6, 2 flags added to point out inconsistencies in GRB
identifiers 100724 and 120222. The CDS acknowledges Andreas von Kienlin
(Max Planck Institut Extraterrestrische Physik) for these precisions.
References:
Paciesas et al. Fermi GBM 2 years cat. 2012ApJS..199...18P 2012ApJS..199...18P
Cat. J/ApJS/199/18
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 08-Apr-2014