| Summary table |
|---|
| Variable |
Value |
Source |
| GRB_name_Fermi |
GRB141102536 |
|
| T0 |
12:51:36.656 UTC |
GCN_circulars,Konus-Wind Det |
| ra |
208.6140° |
Swift |
| decl |
-47.1000° |
Swift |
| pos_error |
3.11e-02° |
Swift |
| T90 |
2.624 s |
Fermi_GBM |
| T90_error |
0.326 s |
Fermi_GBM |
| T90_start |
12:51:39.199 UTC |
Fermi_GBM |
| fluence |
1.42e-06 erg/cm² |
Fermi_GBM |
| fluence_error |
4.12e-08 erg/cm² |
Fermi_GBM |
| T100 |
5.844 s |
|
| GBM_located |
False |
|
| mjd |
56963.53584092593 |
GCN_circulars,Konus-Wind Det |
| Fermi GBM table |
|---|
| GRB_name_Fermi |
GRB141102536 |
| trigger_name |
bn141102536 |
| ra |
208.6142° |
| decl |
-47.1000° |
| pos_error |
4.69e+00° |
| datum |
2014-11-02 |
| t_trigger |
12:51:39.263 UTC |
| T90 |
2.624 s |
| T90_error |
0.326 s |
| T90_start |
12:51:39.199 UTC |
| fluence |
1.42e-06 erg/cm² |
| fluence_error |
4.12e-08 erg/cm² |
| flux_1024 |
4.76e+00 erg/cm²/s |
| flux_1024_error |
2.14e-01 erg/cm²/s |
| flux_1024_time |
1.22e+00 erg/cm²/s |
| flux_64 |
1.56e+01 erg/cm²/s |
| flux_64_error |
1.24e+00 erg/cm²/s |
| IPN table |
|---|
| GRB_name |
GRB141102A |
| ra |
208.6125° |
| decl |
-47.1000° |
| pos_error |
6.67e-02° |
| Swift table |
|---|
| GRB_name |
GRB141102A |
| t_trigger |
12:51:40 UTC |
| ra |
208.6140° |
| decl |
-47.1000° |
| pos_error |
3.11e-02° |
| T90 |
2.5 s |
| Fermi LAT table |
|---|
| GRB_name_Fermi |
GRB141102536 |
| GRB_name |
GRB141102A |
| MET |
436625502.26 |
| datum |
2014-11-02 |
| t_trigger |
12:51:39.260 UTC |
| ra |
208.6140° |
| decl |
-47.1000° |
| pos_error |
6.70e-02° |
| GCN 17020 table |
|---|
| GRB_name |
GRB141102A |
| GCN_number |
17020 |
| Detection_method |
Swift-BAT Det |
| ra |
208.6140° |
| decl |
-47.1000° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 17020
SUBJECT: GRB 141102A found in ground analysis of BAT data
DATE: 14/11/02 21:48:26 GMT
FROM: Jay R. Cummings at NASA/GSFC/Swift
J. R. Cummings on behalf of the Swift science team:
A possibly short burst occurred at 12:51:40 UT (BAT trigger 617313). No source was found
onboard. Ground analysis shows a significant source at RA, Dec 208.614, -47.100 which is:
RA (J2000) 13h 54m 27.4s
Dec (J2000) -47d 06' 00"
with an estimated uncertainty of 4 arcmin radius, 90% containment.
There were multiple peaks, at about T-0.2, T+0.4, T+1.7, and T+2.3. The latter two
were stronger than the first two and resembled them in shape, the third was the largest.
T90 is estimated as 2.5 +- 0.4 sec.
The spectrum from T-0.3 to T+2.7 seconds is best fit by a simple powerlaw function with
a photon index of 1.3 +- 0.5. The fluence was 3.7 x 10 ^-7 ergs/cm^2.
A Swift TOO is not possible because the source is too close to the Sun for the next
39 days.
|
| GCN 17021 table |
|---|
| GRB_name |
GRB141102A |
| GCN_number |
17021 |
| Detection_method |
Fermi GBM Det |
| t_trigger |
12:51:39.260 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 17021
SUBJECT: GRB 141102A: Fermi GBM detection
DATE: 14/11/03 00:51:53 GMT
FROM: Binbin Zhang at UAH
Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:
"At 12:51:39.26 UT on the 2nd of November 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 141102A (trigger 436625502 / 141102536), which was also
detected by Swift (Cummings 2014, GCN 17020). The GBM on-ground location, using
the Fermi GBM trigger data, is consistent with the Swift location. The trigger resulted in
an Autonomous Repoint Request (ARR) that was accepted and the spacecraft slewed
to the GBM in-flight location. The angle from the Fermi LAT boresight is about 57 degrees.
The GBM light curve consists of two main peaks with a total duration (T90) of about
2.62 s (50–300 keV). The time-averaged spectrum from T0–0.064 s to T0+2.56 s is
well fit by a power law function with an exponential high-energy cutoff. The power law
index is –0.85 +/- 0.12 and the cutoff energy, parameterized as Epeak, is 770 +/- 243 keV.
The event fluence (10–1000 keV) in this time interval is (1.7 +/- 0.1)E–06 erg/cm^2. The
1-sec peak photon flux measured starting from T0+1.1 s in the 10–1000 keV band is
5.0 +/- 0.2 ph/s/cm2.
The spectral analysis results presented above are preliminary; final results will be published
in the GBM GRB Catalog."
|
| GCN 17022 table |
|---|
| GRB_name |
GRB141102A |
| GCN_number |
17022 |
| Detection_method |
Fermi LAT Det |
| t_trigger |
12:51:39.260 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 17022
SUBJECT: GRB 141102A: Fermi-LAT detection
DATE: 14/11/03 04:34:37 GMT
FROM: Giacomo Vianello at SLAC
G.Vianello (Stanford U.), D. Kocevski (NASA/GSFC),
V. Connaughton (UAH), M. Arimoto (Tokyo Tech), S. Guiriec (NASA/GSFC)
At 12:51:39.26 on November 2, 2014, Fermi-LAT detected faint high-energy
emission from the short GRB 141102A, which was also detected by Fermi-GBM
(Zhang et al., GCN 17021) and Swift/BAT (Cummings et al., GCN 17020)
and initiated an autonomous repoint of the spacecraft. The high-energy emission
was detected during the ~300 s interval following the GBM trigger.
The best LAT on-ground location is found to be
(RA, Dec.) = 208.6, -47.7 deg
with an error radius of 0.6 deg (90% containment, statistical error
only), which is compatible
with the position measured by Swift/BAT (Cummings et al., GCN 17020).
Further follow up is encouraged.
The Fermi-LAT point of contact for this burst is
Makoto Arimoto (arimoto@hp.phys.titech.ac.jp).
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 17024 table |
|---|
| GRB_name |
GRB141102A |
| GCN_number |
17024 |
| Detection_method |
Konus-Wind Det |
| t_trigger |
12:51:36.656 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 17024
SUBJECT: Konus-Wind observation of GRB 141102A
DATE: 14/11/03 17:30:19 GMT
FROM: Dmitry Svinkin at Ioffe Institute
S. Golenetskii, R. Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:
A long duration GRB 141102A (Swift-BAT detection: Cummings et al., GCN
17020; Fermi-GBM detection: Zhang, GCN Circ. 17021) triggered Konus-Wind
at T0=46296.656 s UT (12:51:36.656).
The KW triggered on the most intense episode with a duration of about
0.6 s. There is a possible precursor at ~T0-80 s.
The emission in this episode is seen up to ~1 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141102_T46296/
As observed by Konus-Wind, the episode
had a fluence of 1.43(-0.42,+1.28)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.022 s,
of 5.95(-2.53,+7.28)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the episode
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.58 (-0.61,+0.93)
and Ep = 444 (-192,+1246) keV (chi2 = 21/28 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.3
(chi2 = 21/27 dof)
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
|
| GCN 17025 table |
|---|
| GRB_name |
GRB141102A |
| GCN_number |
17025 |
| Detection_method |
Swift-BAT Det |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 17025
SUBJECT: GRB 141102A possible precursor was another, known source
DATE: 14/11/04 01:30:34 GMT
FROM: Jay R. Cummings at NASA/GSFC/Swift
J. R. Cummings reports on behalf of the Swift science team:
The emission at ~T-80 that was mentioned in Golenetskii et al. (GCN
Circ # 17024) as apossible precursor to GRB 141102A was observed by
BAT (trigger # 617315). It was not a precursor, but rather a soft
burst from GX 354-0.
|