| Summary table |
|---|
| Variable |
Value |
Source |
| GRB_name_Fermi |
GRB160101215 |
|
| T0 |
5:10:11 UTC |
GCN_circulars,Fermi LAT Det |
| ra |
1.4000° |
Fermi_LAT |
| decl |
55.2000° |
Fermi_LAT |
| pos_error |
1.40e+00° |
Fermi_LAT |
| T90 |
22.013 s |
Fermi_GBM |
| T90_error |
1.619 s |
Fermi_GBM |
| T90_start |
5:10:12.863 UTC |
Fermi_GBM |
| fluence |
1.87e-06 erg/cm² |
Fermi_GBM |
| fluence_error |
3.30e-08 erg/cm² |
Fermi_GBM |
| T100 |
23.876 s |
|
| GBM_located |
False |
|
| mjd |
57388.21540509259 |
GCN_circulars,Fermi LAT Det |
| Fermi GBM table |
|---|
| GRB_name_Fermi |
GRB160101215 |
| trigger_name |
bn160101215 |
| ra |
1.3600° |
| decl |
55.2300° |
| pos_error |
3.53e+00° |
| datum |
2016-01-01 |
| t_trigger |
5:10:12.860 UTC |
| T90 |
22.013 s |
| T90_error |
1.619 s |
| T90_start |
5:10:12.863 UTC |
| fluence |
1.87e-06 erg/cm² |
| fluence_error |
3.30e-08 erg/cm² |
| flux_1024 |
4.34e+00 erg/cm²/s |
| flux_1024_error |
2.84e-01 erg/cm²/s |
| flux_1024_time |
6.40e-02 erg/cm²/s |
| flux_64 |
6.42e+00 erg/cm²/s |
| flux_64_error |
1.31e+00 erg/cm²/s |
| Fermi LAT table |
|---|
| GRB_name_Fermi |
GRB160101215 |
| GRB_name |
GRB160101B |
| MET |
473317815.86 |
| datum |
2016-01-01 |
| t_trigger |
5:10:11.860 UTC |
| ra |
1.4000° |
| decl |
55.2000° |
| pos_error |
1.40e+00° |
| GCN 18798 table |
|---|
| GRB_name |
GRB160101B |
| GCN_number |
18798 |
| Detection_method |
Fermi GBM Det |
| t_trigger |
5:10:12.860 UTC |
| ra |
1.4000° |
| decl |
55.2000° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 18798
SUBJECT: GRB 160101B: Fermi GBM detection
DATE: 16/01/01 17:41:29 GMT
FROM: Adam Goldstein at Fermi-GBM/UAH
P Veres (UAH) and A. von Kienlin (MPE)
report on behalf of the Fermi GBM Team:
"At 05:10:12.86 UT on 01 January 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160101B (trigger 473317816 / 160101215).
The on-ground calculated location, using the GBM trigger
data, is RA = 1.4, DEC = 55.2 (J2000 degrees,
equivalent to 0 h 5 m, 55 d 14 '), with an uncertainty
of 1.4 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ).
The angle from the Fermi LAT boresight at the GBM trigger time is 9 degrees.
The GBM light curve consists of a single pulse
with a duration (T90) of about 6.9 s (50-300 keV).
The time-averaged spectrum from T0-0.5 s to T0+6.7 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.33 +/- 0.07 and
the cutoff energy, parameterized as Epeak, is 952 +/- 468 keV.
The event fluence (10-1000 keV) in this time interval is
(2.73 +/- 0.14)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.3 s in the 10-1000 keV band
is 2.1 +/- 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 18799 table |
|---|
| GRB_name |
GRB160101B |
| GCN_number |
18799 |
| Detection_method |
Fermi LAT Det |
| t_trigger |
5:10:11 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 18799
SUBJECT: GRB 160101B: Fermi-LAT detection
DATE: 16/01/01 17:43:46 GMT
FROM: Judith Racusin at GSFC
J. L. Racusin (NASA/GSFC), S. Razzaque (UJ, South Africa), and M. Axelsson (KTH, Sweden) report on behalf
of the Fermi-LAT team:
At 05:10:11 UT on January 1, 2016, Fermi-LAT detected high-energy emission from GRB 160101B, which was
also detected by Fermi-GBM (trigger 473317815/160101215).
The GBM location was initially inside the LAT field of view at an angle of 9 degrees to the LAT boresight, and
remained in the LAT field of view until ~T0+1500 s. No significant excess is seen using standard >100 MeV
likelihood analysis procedures.
Using the LAT Low Energy (LLE) data selection, over 100 counts above background were detected within a 10 s
interval coinciding with the time of the GBM emission. This data selection has insufficient spatial resolution to
provide a reliable LAT localization. Since an excess of events were not seen using the standard analysis
selection, this detection is likely due to low energy gamma-rays (below 100 MeV).
The Fermi-LAT point of contact for this burst is Judith Racusin (judith.racusin@nasa.gov).
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.
|