J/ApJ/893/46 The fourth Fermi-GBM GRB catalog: 10 years (von Kienlin+, 2020)
The fourth Fermi-GBM gamma-ray burst catalog: a decade of data.
von Kienlin A., Meegan C.A., Paciesas W.S., Bhat P.N., Bissaldi E.,
Briggs M.S., Burns E., Cleveland W.H., Gibby M.H., Giles M.M., Goldstein A.,
Hamburg R., Hui C.M., Kocevski D., Mailyan B., Malacaria C., Poolakkil S.,
Preece R.D., Roberts O.J., Veres P., Wilson-Hodge C.A.
<Astrophys. J., 893, 46 (2020)>
=2020ApJ...893...46V 2020ApJ...893...46V
ADC_Keywords: GRB
Mission_Name: Fermi
Keywords: Catalogs ; Gamma-ray bursts
Abstract:
We present the fourth in a series of catalogs of gamma-ray bursts
(GRBs) observed with Fermi's Gamma-ray Burst Monitor (Fermi-GBM). It
extends the six year catalog by four more years, now covering the 10yr
time period from trigger enabling on 2008 July 12 to 2018 July 11.
During this time period GBM triggered almost twice a day on transient
events, 2356 of which we identified as cosmic GRBs. Additional trigger
events were due to solar flare events, magnetar burst activities, and
terrestrial gamma-ray flashes. The intention of the GBM GRB catalog
series is to provide updated 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 GBM's low-energy detectors.
Furthermore, information is given on the settings of the triggering
criteria and exceptional operational conditions during years 7 to 10
in the mission. This fourth 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:
Fermi-GBM is one of two instruments on the Fermi Gamma-ray Space
Telescope, which was launched on 2008 June 11. GBM is made up of two
types of scintillation detectors, 12 NaI(Tl) detectors, sensitive from
8keV to ∼1MeV, and two BGO detectors, sensitive from 200keV to 40MeV.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 415 995 Trigger modification history
table4.dat 131 2360 GRB triggers: locations and trigger characteristics
table5.dat 76 2359 GRB durations (50-300keV)
table6.dat 76 2359 GRB fluence & peak flux (10-1000keV)
table7.dat 66 2359 GRB fluence & peak flux (50-300keV)
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See also:
J/ApJS/199/18 : The Fermi GBM catalog (Paciesas+, 2012)
J/ApJS/207/39 : IPN supplement to the Fermi GBM (Hurley+, 2013)
J/ApJS/211/13 : The second Fermi/GBM GRB catalog (4yr) (von Kienlin+, 2014)
J/MNRAS/448/2624 : List of isolated emission episodes in GRB (Charisi+, 2015)
J/ApJS/218/11 : The 5yr Fermi/GBM magnetar burst catalog (Collazzi+, 2015)
J/ApJS/216/32 : Localizations of GRBs with Fermi GBM (Connaughton+, 2015)
J/ApJS/223/28 : The third Fermi/GBM GRB catalog (6yr) (Bhat+, 2016)
J/ApJ/818/18 : Jet angle & gamma-ray energetic estimations (Goldstein+, 2016)
J/ApJ/826/37 : Fermi/GBM obs. of V404 Cygni 2015 outburst (Jenke+, 2016)
J/A+A/588/A135 : Fermi/GBM GRB time-resolved spectral catalog (Yu+, 2016)
J/ApJS/229/31 : IPN supplement to the 2nd Fermi GBM catalog (Hurley+, 2017)
J/ApJ/886/20 : Bayesian time-resolved spectra of Fermi GBM pulses (Yu+, 2019)
http://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigtrig.html : Fermi GBM Trigger
online catalog
http://fermi.gsfc.nasa.gov/ssc/observations/timeline/posting/arr/ : Fermi
Timeline posting
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 "M/D/Y" Date Observation date
10- 26 A17 --- Time Observation time; yyyy/DOY:hh:mm:ss UT
28-218 A191 --- Command Command
220-415 A196 --- Reason Reason
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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- 11 A11 --- Fermi Trigger identifier (bnYYMMDDddd)
13 A1 --- f_Fermi [A-Cb-z] Flag on Fermi (1)
15- 17 A3 --- --- [GRB]
19- 25 A7 --- GRB Gamma-ray burst identifier (YYMMDDA)
27- 36 A10 "Y/M/D" Obs.date UT date of the observation; date added by CDS
38- 50 A13 "h:m:s" Obs.time UT time of the observation
52- 56 F5.1 deg RAdeg Right Ascension in decimal degrees (J2000)
58- 62 F5.1 deg DEdeg Declination in decimal degrees (J2000)
64- 67 F4.1 deg Error [0/68.1] Position error
69- 82 A14 --- Loc Location source
84- 85 I2 --- Al [0/56] Algorithm (2)
87- 90 I4 ms Time [0/8192] Timescale
92- 97 A6 keV Energy Energy range
99-131 A33 --- Other Other detection(s) (3)
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Note (1): Flag as follows:
b = GRB091024A triggered GBM twice.
c = GRB120801 There is a delayed emission at T0 + ∼400s.
d = GRB121123A GBM did not trigger on pre-trigger which triggered
Swift; T90, is incorrect.
e = GRB121217A Swift triggered ∼12min before T0. This GRB has several
episodes well separated in time. Hence T90 is possibly incorrect.
f = GRB130206A Swift-BAT triggered at 07:17:20 UT on first emission period
of GRB130206A, GBM on the second pulse at Swift T0 +56s.
g = GRB130307A possible precursors of this trigger were unobservable
since it triggered soon after SAA exit.
h = GRB130604B Fermi enters SAA ∼105s after trigger.
i = GRB130907 Fermi enters SAA ∼130s after trigger.
j = GRB130909 Fermi enters SAA ∼53s after trigger.
k = GRB130925A triggered GBM twice.
l = GRB131028 This GRB triggered during a X-1.0 Solar Flare.
m = GRB131108 A second GRB131108A occurred ∼225s after this GRB triggered.
n = GRB131123 This GRB triggered during a M1.0 Solar Flare.
o = GRB140115 Fermi enters SAA ∼50s after trigger.
p = GRB140219 Fermi enters SAA ∼9s after trigger.
q = GRB140329A Fermi enters SAA ∼120s after trigger.
r = GRB140404 There is a precursor at T0 -70s.
s = GRB140430 Fermi enters SAA ∼155s after trigger.
t = GRB140501A Fermi enters SAA ∼60s after trigger
u = GRB140517 Fermi enters SAA ∼65s after trigger.
v = GRB140627 Fermi enters SAA ∼190s after trigger.
w = GRB141031 Swift sees another pulse at ∼900s after trigger.
Not seen by GBM.
x = GRB150201A triggered GBM twice.
y = GRB151023 Swift sees another pulse at ∼900s after trigger.
Not seen by GBM.
z = GRB160314B Trigger was 60s after SAA exit. Possibly occulted.
A = GRB160623A Known to be occulted (by Swift observation).
B = GRB160625B triggered GBM twice.
C = GRB161207 May be occulted before trigger.
Note (2): Trigger algorithms at the start of mission year 7 (Table 2):
----------------------------------------------------------------------------
Algorithm Timescale Offset Channels Energy Threshold (0.1σ)
Number (ms) (ms) (keV) 2014 Jul 12
----------------------------------------------------------------------------
1 16 0 3-4 50-300 75
2 32 0 3-4 50-300 75
3 32 16 3-4 50-300 75
4 64 0 3-4 50-300 50
5 64 32 3-4 50-300 50
6 128 0 3-4 50-300 50
7 128 64 3-4 50-300 50
8 256 0 3-4 50-300 45
9 256 128 3-4 50-300 45
10 512 0 3-4 50-300 45
11 512 256 3-4 50-300 45
12 1024 0 3-4 50-300 45
13 1024 512 3-4 50-300 45
14 2048 0 3-4 50-300 45
15 2048 1024 3-4 50-300 45
16 4096 0 3-4 50-300 45
17 4096 2048 3-4 50-300 45
18^b 8192 0 3-4 50-300 50
19^b 8192 4096 3-4 50-300 50
20^b 16384 0 3-4 50-300 50
21^b 16384 8192 3-4 50-300 50
22 16 0 2-2 25-50 80
23 32 0 2-2 25-50 80
24 32 16 2-2 25-50 80
25 64 0 2-2 25-50 55
26 64 32 2-2 25-50 55
27^b 128 0 2-2 25-50 55
28^b 128 64 2-2 25-50 55
29^b 256 0 2-2 25-50 55
30^b 256 128 2-2 25-50 55
31^b 512 0 2-2 25-50 55
32^b 512 256 2-2 25-50 55
33^b 1024 0 2-2 25-50 55
34^b 1024 512 2-2 25-50 55
35^b 2048 0 2-2 25-50 55
36^b 2048 1024 2-2 25-50 55
37^b 4096 0 2-2 25-50 65
38^b 4096 2048 2-2 25-50 65
39^b 8192 0 2-2 25-50 65
40^b 8192 4096 2-2 25-50 65
41^b 16384 0 2-2 25-50 65
42^b 16384 8192 2-2 25-50 65
43 16 0 5-7 >300 80
44^b 32 0 5-7 >300 80
45^b 32 16 5-7 >300 80
46^b 64 0 5-7 >300 60
47^b 64 32 5-7 >300 60
48^b 128 0 5-7 >300 55
49^b 128 64 5-7 >300 55
50 16 0 4-7 >100 80
51^b 32 0 4-7 >100 80
52^b 32 16 4-7 >100 80
53^b 64 0 4-7 >100 55
54^b 64 32 4-7 >100 55
55^b 128 0 4-7 >100 55
56^b 128 64 4-7 >100 55
57^b 256 0 4-7 >100 55
58^b 256 128 4-7 >100 55
59^b 512 0 4-7 >100 55
60^b 512 256 4-7 >100 55
61^b 1024 0 4-7 >100 55
62^b 1024 512 4-7 >100 55
63^b 2048 0 4-7 >100 55
64^b 2048 1024 4-7 >100 55
65^b 4096 0 4-7 >100 65
66^b 4096 2048 4-7 >100 65
116^a 16 0 5-7 >300 55
116^a 16 0 BGO/3-6 2-40MeV 55
117^a 16 0 5-7 >300 45
117^a 16 0 BGO/3-6 2-40MeV 45
118^a 16 0 5-7 >300 45
118^a 16 0 BGO/3-6 2-40MeV 45
119^a 16 0 BGO/3-6 2-40MeV 47
----------------------------------------------------------------------------
a: Trigger algorithms using the BGO detector count rates.
Algorithm 116 triggers when at least 2 NaI detectors and 1 BGO detector
exceed the trigger threshold.
Algorithm 117 is the 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
independently of the NaI detectors.
b: Those algorithms have been disabled during most of the mission.
------------------------------------------------------------------------------
Note (3): Instrument detection 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;
ARR = Autonomous Repoint Requests by GBM FSW.
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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- 11 A11 --- Fermi Trigger identifier
13- 14 A2 --- f_Fermi Flag on Fermi (1)
16- 28 A13 --- Det Detectors Used
30- 36 F7.3 s T90 [0.008/829] Duration between 5% and 95%
of maximum fluence
38- 43 F6.3 s e_T90 [0.02/54] Uncertainty in T90
45- 52 F8.3 s T90st [-808/189] Start of T90 burst duration
54- 60 F7.3 s T50 [0.008/737] Duration between 25% and 75%
of maximum fluence
62- 67 F6.3 s e_T50 [0.01/40] Uncertainty in T50
69- 76 F8.3 s T50st [-737/223] Start of T50 burst duration
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Note (1): 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 T0 +83s; durations are lower limits.
g = Used TTE binned at 16ms.
h = GRB 091024A triggered GBM twice (trigger IDs: bn091024372 and
bn091024380). The table lists two individual durations for each of
the triggers, since the determination of the overall duration,
covering both emission periods isn't possible. Despite the availability
of a CTIME file covering the entire burst emission of both triggers it
isn't usable, since the detector selections are not the same in the two
triggers and the background is highly variable that even a fourth order
polynomial does not give an acceptable fit. Combining the results of
both triggers done individually does give reasonable results.
Determining the fluence in the 50-300keV energy range for both
triggers, we find that the first trigger accounts for 20.0% of the
total fluence. This means that T50 for the entire event begins and
ends in the second trigger at the fluence levels of ∼6% (5% * 100/80)
and ∼69% (55% * 100/80). These points are at ∼4s and ∼310s, giving
T50 ∼306s. Similarly, T90 begins at the 25% (5% * 100/20) fluence
point in the first trigger and ends at the ∼94% (100% - 5% * 100/80)
fluence point in the second trigger These points are at ∼4s in the
first trigger, and ∼370s in the second trigger. The two trigger times
differ by 631s, giving a T90 of ∼997s. The error bars are no more
than 20s.
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, 64ms peak fluxes may not be correct.
q = GRB 130925A triggered GBM twice (trigger IDs: bn130925164 and
bn130925173). The fluence in the first trigger is <1% of the fluence
in the second: The durations for bn130925173 are therefore accurate
for the entire event.
r = Duration is only for first peak. Peak at 320s is cut off by SAA.
s = Used 64ms binning.
t = GRB 150201A triggered GBM twice (trigger IDs: bn150201574 and
bn150201590) The two triggers for this GRB are far apart (24 minutes)
to have the data in a single CTIME file, so it was not possible to
compute a total duration with our software. The fluence of the second
trigger is only about 3% of the fluence of the first trigger. This
implies that the durations for the first pulse alone are probably
valid for the entire burst, certainly for the T50.
t = Used 128ms binning.
u = Durations invalid; Swift sees later pulse that GBM does not;
probably occulted.
v = Highly uncertain due to low significance emission before & after.
w = Comptonized spectrum failed at times of significant burst emission.
Used a Band function seed spectrum.
x = Used 1.024ms binning.
y = GRB 160625B triggered GBM twice (trigger IDs: bn160625945 and
bn160625952). The CTIME data of the first trigger includes the GRB
emission of the second trigger. Thanks to a manageable overall
background the duration analysis of the entire GRB emission is
possible.
z = Used 8ms binning.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Fermi Trigger identifier
13- 20 E8.2 10-7J/cm2 Fluence [2.5e-8/0.0025] Fluence; erg/cm2
22- 29 E8.2 10-7J/cm2 e_Fluence [3.6e-9/1.5e-5] Uncertainty in Fluence
31- 37 F7.2 ph/cm2/s PF64 [1.4/3055] Peak flux on the 0.064s timescale
39- 45 F7.2 ph/cm2/s e_PF64 [0.3/4476] Uncertainty in PF64
47- 53 F7.2 ph/cm2/s PF256 [0.8/1211] Peak flux on the 0.256s timescale
55- 61 F7.2 ph/cm2/s e_PF256 [0.1/1119] Uncertainty in PF256
63- 69 F7.2 ph/cm2/s PF1024 [0.2/1052] Peak flux on the 1.024s timescale
71- 76 F6.2 ph/cm2/s e_PF1024 [0.09/280] Uncertainty in PF1024
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Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Fermi Trigger identifier
13- 20 E8.2 10-7J/cm2 Fluence [1.3e-8/0.00082] Fluence; erg/cm2
22- 29 E8.2 10-7J/cm2 e_Fluence [1.5e-9/1.4e-6] Uncertainty in Fluence
31- 36 F6.2 ph/cm2/s PF64 [0.08/577] Peak flux on the 0.064s timescale
38- 42 F5.2 ph/cm2/s e_PF64 [0.04/21] Uncertainty in PF64
44- 49 F6.2 ph/cm2/s PF256 [0.03/557] Peak flux on the 0.256s timescale
51- 54 F4.2 ph/cm2/s e_PF256 [0.02/7] Uncertainty in PF256
56- 61 F6.2 ph/cm2/s PF1024 [0.01/497] Peak flux on the 1.024s timescale
63- 66 F4.2 ph/cm2/s e_PF1024 [0.01/2.1] Uncertainty in PF1024
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-Mar-2021