J/ApJS/223/28 The third Fermi/GBM GRB catalog (6yr) (Bhat+, 2016)
The third Fermi GBM gamma-ray burst catalog: the first six years.
Bhat P.N., Meegan C.A., von Kienlin A., Paciesas W.S., Briggs M.S.,
Burgess J.M., Burns E., Chaplin V., Cleveland W.H., Collazzi A.C.,
Connaughton V., Diekmann A.M., Fitzpatrick G., Gibby M.H., Giles M.M.,
Goldstein A.M., Greiner J., Jenke P.A., Kippen R.M., Kouveliotou C.,
Mailyan B., McBreen S., Pelassa V., Preece R.D., Roberts O.J., Sparke L.S.,
Stanbro M., Veres P., Wilson-Hodge C.A., Xiong S., Younes G., Yu H.-F.,
Zhang B.
<Astrophys. J. Suppl. Ser., 223, 28-28 (2016)>
=2016ApJS..223...28B 2016ApJS..223...28B (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; Surveys
Mission_Name: Fermi
Keywords: catalogs; gamma-ray burst: general
Abstract:
Since its launch in 2008, the Fermi Gamma-ray Burst Monitor (GBM) has
triggered and located on average approximately two γ-ray bursts
(GRBs) every three days. Here, we present the third of a series of
catalogs of GRBs detected by GBM, extending the second catalog by two
more years through the middle of 2014 July. The resulting list
includes 1405 triggers identified as 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 to 1000keV,
exploiting the full energy range of GBM's low-energy [NaI[Tl)]
detectors. Using statistical methods to assess clustering, we find
that the hardness and duration of GRBs are better fit by a
two-component model with short-hard and long-soft bursts than by a
model with three components. Furthermore, information is provided on
the settings and modifications of the triggering criteria and
exceptional operational conditions during years five and six in the
mission. This third 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 third GBM catalog comprises a list of 1403 cosmic GRBs that
triggered GBM between 2008 July 12 and 2014 July 11. The increased
sample of GRBs in this catalog confirms the conclusions of the earlier
two year (Paciesas+, 2012, J/ApJS/199/18) and four year (von Kienlin+,
2014, J/ApJS/211/13) catalogs.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 57 73 Trigger criteria history
table4.dat 72 283 Trigger modification history
table5.dat 118 1405 GRB triggers: locations and trigger characteristics
table6.dat 75 1405 GRB durations (50-300keV)
table7.dat 76 1405 GRB fluence & peak flux (10-1000keV)
table8.dat 76 1405 GRB fluence & peak flux (50-300keV)
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See also:
IX/20 : The Fourth BATSE Burst Revised Catalog (Paciesas+ 1999)
J/A+A/588/A135 : Fermi/GBM GRB time-resolved spectral catalog (Yu+, 2016)
J/ApJS/216/32 : Localizations of GRBs with Fermi GBM (Connaughton+, 2015)
J/ApJ/811/93 : Fermi/GBM GRB minimum timescales (Golkhou+, 2015)
J/A+A/568/A75 : GRB 130925A GROND light curves (Greiner+, 2014)
J/ApJS/211/13 : The second Fermi/GBM GRB catalog (4yr) (von Kienlin+, 2014)
J/ApJS/207/39 : IPN supplement to the Fermi GBM (Hurley+, 2013)
J/ApJ/763/15 : Fermi GRB analysis. III. T90 distributions (Qin+, 2013)
J/MNRAS/431/3608 : BeppoSAX/GRBM and Fermi/GBM long GRBs (Dichiara+, 2013)
J/ApJS/199/18 : The Fermi GBM catalog (Paciesas+, 2012)
J/ApJ/756/44 : Spectral lags and counts of the RHESSI GRBs (Ripa+, 2012)
J/ApJ/754/121 : GRBs from Fermi/GBM and LAT (The Fermi Team, 2012)
J/A+A/530/A21 : Spectral properties of 438 GRBs (Nava+, 2011)
J/ApJ/508/314 : Gamma-ray bursts types (Mukherjee+, 1998)
http://gcn.gsfc.nasa.gov/ : GCN archive access
http://gammaray.nsstc.nasa.gov/batse/grb/catalog/ : BATSE GRB catalog
http://www.ssl.berkeley.edu/ipn3/masterli.txt : List of detections
http://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html : Online Fermi
GBM burst 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] Trigger algorithm
5 A1 --- f_Alg [b] Flag on Algorithm number (1)
7- 11 I5 ms Time [16/16384]? Time scale
13- 16 I4 ms Off [0/8192]? Time offset
18- 24 A7 --- Ch Channels
26- 33 A8 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 24 (2)
47- 48 A2 --- Th5 0.1σ threshold on 2009 Oct 29 (2)
50- 51 I2 --- Th6 [24/60] 0.1σ threshold on 2009 Nov 10
53- 54 I2 --- Th7 [24/55] 0.1σ threshold on 2009 Dec 7
56- 57 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 Na I and one BGO detectors
are exceeding the trigger threshold.
Algorithm 117 is same as 116, but imposes the additional requirement that
the triggered detectors are on the +X side of the spacecraft.
Algorithm 118 is the same as 117, but requires 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): Symbols are:
: = 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: table4.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "M/D/Y" Trig.date Date of the trigger
12- 14 I3 d DOY Day of the year of the trigger
16- 23 A8 "h:m:s" Trig.time UT time of the trigger
25- 72 A48 --- Oper Operation description
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [bn]
3- 11 I09 --- Fermi Trigger identifier (YYMMDDddd)
13- 14 A2 --- f_Fermi Flag on Fermi (1)
16- 18 A3 --- --- [GRB]
20- 26 A7 --- GRB GRB name (YYMMDDA) (2)
28- 29 I2 h Trig.h UT Hour of the trigger
31- 32 I2 min Trig.m UT Minute of the trigger
34- 40 F7.4 s Trig.s UT Second of the trigger
42- 46 F5.1 deg RAdeg Right Ascension in decimal degrees (J2000)
48- 53 F6.2 deg DEdeg Declination in decimal degrees (J2000)
55- 59 F5.2 deg Err [0/50] Position error
61- 69 A9 --- Inst Instrument that determined the location
71- 72 I2 --- Alg [1/56] Trigger algorithm
74- 77 I4 ms Time [16/8192] Trigger timescale
79- 84 A6 keV Erange Trigger energy range (23-47, 47-291 or >100)
86-118 A33 --- Other Other information (3)
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Note (1): Flag as follows:
aa = GRB120801 There is a delayed emission at T0+∼400s.
b = GRB091024A triggered GBM twice.
bb = GRB121123A GBM did not trigger on pre-trigger which triggered Swift;
T90 is incorrect
c = GRB130307A possible precursors of this trigger were unobservable since
it triggered soon after South Atlantic Anomaly (SAA) exit.
cc = GRB121217A Swift triggered ∼12min before T0. This GRB has several
episodes well separated in time. Hence T90 is possibly incorrect
d = GRB130604B Fermi enters SAA ∼105s after trigger.
dd = GRB131028 This GRB triggrered during a X1.0 Solar Flare.
e = GRB130907 Fermi enters SAA ∼130s after trigger.
ee = GRB131108 A second GRB131108A occurred ∼225s after this GRB triggered.
f = GRB130909 Fermi enters SAA ∼53s after trigger.
ff = GRB131123 This GRB triggrered during a M1.0 Solar Flare.
g = GRB130925A triggered GBM twice.
h = GRB140115 Fermi enters SAA ∼50s after trigger.
i = GRB130206A Swift-BAT triggered at 07:17:20 UT on first emission
period of GRB1140206A, GBM on the second pulse at Swift T0+56s.
j = GRB140219 Fermi enters SAA ∼9s after trigger.
k = GRB140329A Fermi enters SAA ∼120s after trigger.
l = GRB140404 There is a precursor at T0-70s.
m = GRB140329 Fermi enters SAA ∼155s after trigger.
n = GRB140329A Fermi enters SAA ∼60s after trigger.
o = GRB140517 Fermi enters SAA ∼65s after trigger.
p = GRB140627 Fermi enters SAA ∼190s after trigger.
Note (2): Note that the table is consistent with the small change in the GRB
naming convention that became effective on 2010 January 1
(Barthelmy et al. 2009GCN..10251...1B 2009GCN..10251...1B): if for a given date no burst
has been "published" previously, then the first burst of the day
observed by GBM includes the "A" designation even if it is the only
one for that day.
Note (3): Other detections and/or ARRs. Instrument code 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;
Nu = NuSTAR;
iPTF = intermediate Palomar Transient Factory;
ARR = Autonomous Repoint Requests by GBM FSW.
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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 --- Fermi Trigger identifier (YYMMDDddd)
13 A1 --- n_Fermi Note on Fermi (4)
15- 27 A13 --- Det Detectors used
29- 35 F7.3 s T90 [0.04/829] The T90 duration
37- 42 F6.3 s e_T90 [0.03/36] The 1σ uncertainty in T90
44- 51 F8.3 s T90st The T90 start time
53- 59 F7.3 s T50 [0.01/737] The T50 duration
61- 66 F6.3 s e_T50 [0.02/40] The 1σ uncertainty in T50
68- 75 F8.3 s T50st The T50 start time
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Note (4): Note 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 T0+83s; durations are lower limits.
g = Used TTE binned at 16ms.
h = This GRB triggered GBM twice.
i = Too weak to measure durations; visual duration is ∼0.025s.
j = Possible contamination due to emergence of Crab & 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 - 100 keV 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, 64 ms peak fluxes may not be correct.
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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 --- Fermi Trigger identifier (YYMMDDddd)
13- 20 E8.2 mJ/m2 Fl.w [0/0.003] Fluence on wide (10-1000keV) band;
in erg/cm2
22- 29 E8.2 mJ/m2 e_Fl.w The 1σ uncertainty in Fl.w
31- 37 F7.2 ph/cm2/s PFl.w [1.4/3055] Peak flux at 64ms in photons/cm2/s
39- 45 F7.2 ph/cm2/s e_PFl.w [0.3/4476] The 1σ uncertainty in PF1.w
47- 53 F7.2 ph/cm2/s PF2.w [0.8/1211] Peak flux at 256ms in photons/cm2/s
55- 61 F7.2 ph/cm2/s e_PF2.w [0.1/1119] The 1σ uncertainty in PF2.w
63- 69 F7.2 ph/cm2/s PF3.w [0.3/1052] Peak flux at 1024ms
71- 76 F6.2 ph/cm2/s e_PF3.w [0.09/280] The 1σ uncertainty in PF3.w
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [bn]
3- 11 I09 --- Fermi Trigger identifier (YYMMDDddd)
13- 20 E8.2 mJ/m2 Fl.n [0/0.0009] Fluence on narrow (50-300keV) band;
in erg/cm2
22- 29 E8.2 mJ/m2 e_Fl.n The 1σ uncertainty in Fl.n
31- 37 F7.2 ph/cm2/s PF1.n [0.2/577] Peak flux at 64ms in photons/cm2/s
39- 45 F7.2 ph/cm2/s e_PF1.n [0.08/8] The 1σ uncertainty in PF1.n
47- 53 F7.2 ph/cm2/s PF2.n [0.1/557] Peak flux at 256ms in photons/cm2/s
55- 61 F7.2 ph/cm2/s e_PF2.n [0.04/4] The 1σ uncertainty in PF2.n
63- 69 F7.2 ph/cm2/s PF3.n [0.06/497] Peak flux at 1024ms
71- 76 F6.2 ph/cm2/s e_PF3.n [0.04/2] The 1σ uncertainty in PF3.n
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Nomenclature note:
GRBs are <Fermi bnYYMMDDddd> in Simbad.
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-Jun-2016