[vsnet-grb-info 20311] GRB 180210A: Fermi GBM detection

[GCN Circulars]

TITLE:   GCN CIRCULAR
NUMBER:  22407
SUBJECT: GRB 180210A: Fermi GBM detection
DATE:    18/02/10 17:28:41 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi at ba.infn.it>

E. Bissaldi (Politecnico & INFN Bari)
reports on behalf of the Fermi GBM Team:


"At 12:24:38.55 UT on 10 February 2018, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 180210A (trigger 539958283 / 180210517).
The on-ground calculated location, using the GBM trigger data, is

RA = 3.33, DEC = 21.01 (J2000 degrees),

with an uncertainty of 1.5 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 trigger resulted in an Autonomous Repoint Request (ARR)
by the GBM Flight Software owing to the high peak flux of the GRB.
This ARR was accepted and the spacecraft slewed to the GBM in-flight
location. The initial angle from the Fermi LAT boresight to
the GBM ground location is 31 degrees.

The GBM light curve consists of a multi-peaked
emission episode with a duration (T90) of about 40 s (50-300 keV).
The time-averaged spectrum from T0 to T0+31 s is best fit by
a Band function with Epeak = 145 +/- 3 keV,
alpha = -0.45 +/- 0.02, and beta = -2.60 +/- 0.06.

The event fluence (10-1000 keV) in this time interval is
(4.21 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+24 s in the 10-1000 keV band
is 16.7 +/- 0.3 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."