| Summary table |
|---|
| Variable |
Value |
Source |
| GRB_name_Fermi |
GRB140206275 |
|
| T0 |
6:36:09.061 UTC |
GCN_circulars,Konus-Wind Det |
| ra |
315.2600° |
Fermi_LAT |
| decl |
-8.5100° |
Fermi_LAT |
| pos_error |
2.30e-01° |
Fermi_LAT |
| T90 |
146.69 s |
Fermi_GBM |
| T90_error |
4.419 s |
Fermi_GBM |
| T90_start |
6:36:20.331 UTC |
Fermi_GBM |
| fluence |
1.23e-04 erg/cm² |
Fermi_GBM |
| fluence_error |
2.78e-07 erg/cm² |
Fermi_GBM |
| T100 |
157.96 s |
|
| GBM_located |
False |
|
| mjd |
56694.275104872686 |
GCN_circulars,Konus-Wind Det |
| Fermi GBM table |
|---|
| GRB_name_Fermi |
GRB140206275 |
| trigger_name |
bn140206275 |
| ra |
315.2600° |
| decl |
-8.5200° |
| pos_error |
2.47e+00° |
| datum |
2014-02-06 |
| t_trigger |
6:36:12.843 UTC |
| T90 |
146.69 s |
| T90_error |
4.419 s |
| T90_start |
6:36:20.331 UTC |
| fluence |
1.23e-04 erg/cm² |
| fluence_error |
2.78e-07 erg/cm² |
| flux_1024 |
4.32e+01 erg/cm²/s |
| flux_1024_error |
3.90e-01 erg/cm²/s |
| flux_1024_time |
1.34e+01 erg/cm²/s |
| flux_64 |
4.64e+01 erg/cm²/s |
| flux_64_error |
1.57e+00 erg/cm²/s |
| Fermi LAT table |
|---|
| GRB_name_Fermi |
GRB140206275 |
| GRB_name |
GRB140206B |
| MET |
413361375.0 |
| datum |
2014-02-06 |
| t_trigger |
6:36:12 UTC |
| ra |
315.2600° |
| decl |
-8.5100° |
| pos_error |
2.30e-01° |
| GCN 15790 table |
|---|
| GRB_name |
GRB140206B |
| GCN_number |
15790 |
| Detection_method |
Fermi GBM Det |
| t_trigger |
6:36:12.840 UTC |
| ra |
314.6000° |
| decl |
-6.6000° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 15790
SUBJECT: GRB 140206B: Fermi GBM detection
DATE: 14/02/06 14:09:48 GMT
FROM: Andreas von Kienlin at MPE
A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team:
"At 06:36:12.84 UT on 06 February 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140206B (trigger 413361375 / 140206275).
The on-ground calculated location, using the GBM trigger data, is RA =
314.6,
DEC = -6.6 (J2000 degrees, equivalent to 20 h 58 m, -6 d 36 '),
with an uncertainty of 1.9 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The trigger resulted in an Autonomous Repoint Request (ARR)
that was accepted and the spacecraft slewed to the GBM in-flight location.
The initial angle from the LAT boresight was 46 deg from the Fermi/GBM
position.
The GBM light curve is multi-peaked with a duration (T90) of about 120 s
(50-300 keV).
The time-averaged spectrum from T0+0.003 s to T0+44.993 s is well fit by a
Band function
with Epeak = 296.6 +/- 7.3 keV, alpha = -0.97 +/-0.01 and beta = -2.14
+/-0.03
The event fluence (10-1000 keV) in this time interval is
(0.993 +/- 0.005)E-04 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+13.44 s in the 10-1000 keV band
is 42.4 +/- 0.4 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
|
| GCN 15791 table |
|---|
| GRB_name |
GRB140206B |
| GCN_number |
15791 |
| Detection_method |
Fermi LAT Det |
| t_trigger |
6:36:12.840 UTC |
| ra |
315.2600° |
| decl |
-8.5100° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 15791
SUBJECT: GRB 140206B: Fermi-LAT detection
DATE: 14/02/06 14:31:50 GMT
FROM: Elisabetta Bissaldi at U.Innsbruk/IAPP
E. Bissaldi (University & INFN Trieste), G. Vianello (Stanford University),
F. Longo (University & INFN Trieste), R. Desiante (Udine University &
INFN Trieste),
J. Racusin (NASA/GSFC) report on behalf of the Fermi-LAT team:
On February 6th, 2014, Fermi LAT detected high-energy emission
from GRB 140206B, which triggered GBM at 06:36:12.84 UT
(trigger 413361375/140206275, von Kienlin et al., GCN 15790).
GBM also initiated an autonomous repoint of Fermi at 06:36:25 UT
due to high peak flux.
The best LAT on-ground location is found to be:
(RA, Dec) = 315.26, -8.51 (J2000)
with an error radius of 0.23 deg (90% containment, statistical error only).
This was 45 deg from the LAT boresight at the time of the trigger.
More than 25 photons above 100 MeV and 2 photons above 1 GeV are observed
within 600 seconds. The highest-energy photon is a 3.5 GeV event,
which is observed 460 seconds after the GBM trigger.
Unfortunately, the GRB position is too close to the Sun (8.2 deg)
for Swift to conduct follow-up observations.
The Fermi LAT point of contact for this burst is
Elisabetta Bissaldi (Elisabetta.Bissaldi@ts.infn.it
).
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 15804 table |
|---|
| GRB_name |
GRB140206B |
| GCN_number |
15804 |
| Detection_method |
Konus-Wind Det |
| t_trigger |
6:36:09.061 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 15804
SUBJECT: Konus-Wind observation of GRB 140206B
DATE: 14/02/07 08:29:36 GMT
FROM: Dmitry Frederiks at Ioffe Institute
S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:
The long-duration intense GRB 140206B
(Fermi-GBM detection: von Kienlin, GCN 15790;
Fermi-LAT detection: Bissaldi et al., GCN 15791)
triggered Konus-Wind at T0=23769.061 s UT (06:36:09.061).
The light curve consists of two major multi-peaked emission
episodes in the time interval from ~T0-3 s to ~T0+155 s.
The emission is seen up to ~12 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140206_T23769/
As observed by Konus-Wind, the burst
had a fluence of (1.52 0.09)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+7.488 s,
of (1.73 0.09)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum (measured from T0 to T0+154.368 s)
is best fit in the 25 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.07 0.08,
the high energy photon index beta = -2.28 0.09,
the peak energy Ep = 227 18 keV,
chi2 = 93.8/96 dof.
The spectrum near the maximum count rate
(measured from T0+8.448 s to T0+16.384 s)
is best fit in the 35 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.59 0.08,
the high energy photon index beta = -2.18 0.04,
the peak energy Ep = 278 16 keV,
chi2 = 84.3/93 dof.
All the quoted results are preliminary.
|
| GCN 17421 table |
|---|
| GRB_name |
GRB140206B |
| GCN_number |
17421 |
| Detection_method |
Optical |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 17421
SUBJECT: GRB 140206B: Continued iPTF Observations
DATE: 15/02/07 09:02:26 GMT
FROM: Leo Singer at GSFC/iPTF
L. P. Singer (NASA/GSFC), M. M. Kasliwal (Carnegie Observatories/Princeton),
and S. B. Cenko (NASA/GSFC) report on behalf of the intermediate Palomar
Transient Factory (iPTF) collaboration:
Using the Palomar 48-inch Oschin telescope (P48) and the robotic 60-inch
telescope (P60), we have continued observing the optical transients that
we reported (Singer et al., GCN 17415) in connection with GRB 140206B
(Burns & Yu, GCN 17417). At about 20 hours after the burst, all three of
the candidates (iPTF15gz, iPTF15hb, and iPTF15gv) are still clearly
detected in host-subtracted images, despite relatively coarse 3" seeing.
They show no statistically significant fading. We therefore dismiss them
as counterparts of the GRB.
|