| Summary table |
|---|
| Variable |
Value |
Source |
| GRB_name_Fermi |
GRB170329387 |
|
| T0 |
9:17:03.095 UTC |
GCN_circulars,Konus-Wind Det |
| ra |
356.0000° |
Fermi_LAT |
| decl |
23.7900° |
Fermi_LAT |
| pos_error |
6.00e-01° |
Fermi_LAT |
| T90 |
33.536 s |
Fermi_GBM |
| T90_error |
6.149 s |
Fermi_GBM |
| T90_start |
9:17:07.195 UTC |
Fermi_GBM |
| fluence |
1.11e-05 erg/cm² |
Fermi_GBM |
| fluence_error |
3.84e-08 erg/cm² |
Fermi_GBM |
| T100 |
37.636 s |
|
| GBM_located |
False |
|
| mjd |
57841.386841377316 |
GCN_circulars,Konus-Wind Det |
| Fermi GBM table |
|---|
| GRB_name_Fermi |
GRB170329387 |
| trigger_name |
bn170329387 |
| ra |
356.6000° |
| decl |
9.8000° |
| pos_error |
2.94e+00° |
| datum |
2017-03-29 |
| t_trigger |
9:17:06.939 UTC |
| T90 |
33.536 s |
| T90_error |
6.149 s |
| T90_start |
9:17:07.195 UTC |
| fluence |
1.11e-05 erg/cm² |
| fluence_error |
3.84e-08 erg/cm² |
| flux_1024 |
5.16e+00 erg/cm²/s |
| flux_1024_error |
1.96e-01 erg/cm²/s |
| flux_1024_time |
1.34e+00 erg/cm²/s |
| flux_64 |
6.68e+00 erg/cm²/s |
| flux_64_error |
9.28e-01 erg/cm²/s |
| IPN table |
|---|
| GRB_name |
GRB170329A |
| ra |
356.6000° |
| decl |
9.8000° |
| pos_error |
6.00e-01° |
| Fermi LAT table |
|---|
| GRB_name_Fermi |
GRB170329387 |
| GRB_name |
GRB170329A |
| MET |
512471829.94 |
| datum |
2017-03-29 |
| t_trigger |
9:17:04.940 UTC |
| ra |
356.0000° |
| decl |
23.7900° |
| pos_error |
6.00e-01° |
| GCN 20942 table |
|---|
| GRB_name |
GRB170329A |
| GCN_number |
20942 |
| Detection_method |
Fermi LAT Det |
| t_trigger |
9:17:06.940 UTC |
| ra |
356.6000° |
| decl |
9.8000° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20942
SUBJECT: GRB 170329A: Fermi-LAT detection
DATE: 17/03/29 15:31:29 GMT
FROM: Manal Yassine at IN2P3/LUPM/CNRS
M. Yassine (LUPM, Montpellier) ,E. Bissaldi (Politecnico & INFN Bari),
G. Vianello (Stanford), J. L. Racusin (NASA/GSFC),
F. Longo (University and INFN, Trieste) and N. Omodei (Stanford) report
on behalf of the Fermi-LAT team:
At 09:17:06.94 UT on March 29, 2017, Fermi-LAT detected high-energy
emission from GRB 170329A, which was also detected by Fermi-GBM
(170329387/512471831).
The best LAT on-ground location is found to be RA, Dec 356.6, 9.8
(degrees, J2000) with an error radius of 0.6 deg (90% containment,
statistical error only).
This was 33 deg from the LAT boresight at the time of the trigger.
The data from the Fermi-LAT show a significant increase in the event
rate that is spatially and temporally consistent with the GBM emission.
More than 37 photons above 100 MeV observed within 1 ks.
The highest-energy photon is a 0.8 GeV event which is observed 4 seconds
after the GBM trigger.
The Fermi-LAT point of contact for this burst is Manal Yassine
(manal.yassine@lupm.in2p3.fr).
The Fermi-LAT is a pair conversion telescope designed to cover the
energy band from 20 MeV to greater than 300 GeV.
It is the product of an international collaboration between NASA and DOE
in the U.S. and many scientific institutions across France, Italy, Japan
and Sweden.
|
| GCN 20943 table |
|---|
| GRB_name |
GRB170329A |
| GCN_number |
20943 |
| Detection_method |
Fermi GBM Det |
| t_trigger |
9:17:06.940 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20943
SUBJECT: GRB 170329A: Fermi GBM detection
DATE: 17/03/30 04:07:55 GMT
FROM: Oliver J Roberts at USRA/NASA
E.Bissaldi (Politecnico & INFN Bari), O.J.Roberts (USRA/MSFC)
and C.Meegan (UAH) report on behalf of the Fermi GBM Team:
"At 09:17:06.94 UT on 29 March 2017, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 170329A (trigger 512471831 / 170329387),
which was also detected by the LAT (Yassine et al. 2017, GCN 20942)
The GBM on-ground location is consistent with the LAT position.
The angle from the Fermi LAT boresight at the GBM trigger time is 33 degrees.
The GBM light curve consists of a bright peak
with a duration (T90) of 33.5 s (50-300 keV).
The time-averaged spectrum from T0+0 s to T0+33.5 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.61 +/- 0.06 and
the cutoff energy, parameterized as Epeak, is 799 +/- 86 keV
The event fluence (10-1000 keV) in this time interval is
(1.45 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.3 s in the 10-1000 keV band
is 5.2 +/- 0.2 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
|
| GCN 20951 table |
|---|
| GRB_name |
GRB170329A |
| GCN_number |
20951 |
| Detection_method |
AstroSat CZTI |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20951
SUBJECT: GRB 170329A: AstroSat CZTI detection
DATE: 17/03/31 09:31:04 GMT
FROM: Vidushi Sharma at IUCAA
V. Sharma(IUCAA), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data showed clear detection of GRB170329A (Fermi GBM detection: E.Bissaldi et al., GCN Circ. 20943) in the 40-200 keV energy range. The light curve shows single peak emission with peak counts at 09:17:08.940 UT, 2 s after the Fermi trigger. The measured peak count rate is 161.1 counts/s above the background in combined data of four quadrants, with a total 879 counts. The local mean background count rate was 387.9 counts/s. Using cumulative rates, we measure a T90 of 14.1 s.
It was clearly detected in the CsI anticoincidence detector (Veto) also in the 100-500 keV energy range.
CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.
|
| GCN 20952 table |
|---|
| GRB_name |
GRB170329A |
| GCN_number |
20952 |
| Detection_method |
Konus-Wind Det |
| t_trigger |
9:17:03.095 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20952
SUBJECT: Konus-Wind observation of GRB 170329A
DATE: 17/03/31 10:56:46 GMT
FROM: Anna Kozlova at Ioffe Institute
A.Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 170329A (Fermi-LAT detection: Yassine et al., GCN
20942; Fermi-GBM detection: Bissaldi et al., GCN 20943)
triggered Konus-Wind at T0=33423.095 s UT (09:17:03.095).
The burst light curve shows a single multi-peaked pulse
with a total duration of ~7 s. The emission is seen up to ~6 MeV.
As observed by Konus-Wind, the burst
had a fluence of 1.47(-0.18,+0.22)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.346 s,
of 4.74(-1.61,+1.66)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 6 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.30(-0.25,+0.30)
and Ep = 688(-109,+153) keV (chi2 = 63/81 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.3
(chi2 = 63/80 dof)
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB170329_T33423/
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
|