GRB 000214

For GRB lovers, on S. Valentine's day:
 
On Feb.14 at 01:01:01 a GRB (GRB000214)  has been detected by the GRBM and
WFC1 of BeppoSAX.

Preliminary coordinates from WFC are:

R.A.(2000)= 283.573
DEC(2000)= -66.455

The attitude configuration at the time of the GRB introduces a systematic
error in the position. At this stage of the analysis we estimate a total
error of about 8' in radius.

Luigi Piro
BeppoSAX Mission Scientist

GRB000214 refined BeppoSAX-WFC position
 
Refined  coordinates from WFC are:

R.A.(2000)= 283.576
DEC(2000)= -66.439

i.e. 1' off from the preliminary position
The error radius is 6.5'

A follow-up pointing with the Narrow Field Instruments of BeppoSAX is
being planned

Luigi Piro
BeppoSAX Mission Scientist

A BeppoSAX follow up of GRB000214 with the Narrow Field Instruments
started around Feb.14 at 13:11 UT, i.e. 12 hours after the GRB.

Preliminary analysis of the MECS (1.6-10 keV) data of the 1st orbit shows
a relatively strong, previously unknown source inside the WFC error box
at:

R.A.(2000)= 283.61
DEC(2000)= -66.477

with  an error radius of 1.5'.


Luigi Piro
BeppoSAX Mission Scientist

K. Hurley, on behalf of the Ulysses GRB team, and M. Feroci,
on behalf of the BeppoSAX GRBM team, report:

Ulysses and the BeppoSAX GRBM observed GRB000214 (GCN 551
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 , 552
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 ).
Triangulation gives an annulus centered at RA(2000)=153.560,
Decl(2000)=-41.892, with radius 65.114 +/- 0.021 degrees
(3 sigma).  This annulus intersects the refined WFC error
circle to make an ~30 sq. arcmin. error box whose corners
are at:

     RA(2000)           DEC(2000)
18 h 55 m 14.39 s    -66 o 29 ' 35 "
18 h 53 m 34.70 s    -66 o 21 ' 33 "
18 h 54 m 57.30 s    -66 o 31 ' 31 "
18 h 53 m 19.47 s    -66 o 23 ' 37 "

It also intersects the NFI error circle, reducing its
area by a factor of about 2, and making it likely that
this is indeed the counterpart to GRB000214.

Further refinement to this annulus is possible.
A map may be viewed at ssl.berkeley.edu/ipn3/000214.

A. Paolino, M. Stornelli, A. Coletta, Scientific Operation Centre, 
Telespazio, Roma, L.A. Antonelli, Osservatorio Astronomico di Roma, 
Roma, M.J.S. Smith, J. in 't Zand, Space Research Organization 
Netherlands (SRON), Utrecht, C. Guidorzi, Universita' di Ferrara, 
Ferrara, M. Feroci IAS/CNR, Roma, report:

"The BeppoSAX Gamma Ray Burst Monitor (GRBM) and Wide Field Camera
(WFC unit 1) observed a gamma-ray burst on February 14.042 UT. 
A preliminary analysis reveals a duration of about 9 s in the GRBM, 
with a peak photon countrate of 4.2E3 cts/s in the 40-700 keV energy 
band. In the WFC, the duration is about 115 s and the peak flux is 
2.9 Crab (2-26 keV). The position of the X-ray counterpart is 
R.A.= 18h 4m 18s Decl.= -66 26'.3" (equinox 2000.0) with a 99% 
error radius of 6.5'. An NFI follow-up is being carried on."

This message is citable.

L.A. Antonelli, reports:

the coordinate of the X-ray counterpart published in the GCN #557
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should be read: R.A.= 18h 54m 18s Decl.= -66 26'.3" (equinox 2000.0). 
Thanks to D. Frail for pointing out this error.

L.A. Antonelli, Osservatorio Astronomico di Roma, Rome; 
L. Piro, Istituto di Astrofisica Spaziale, CNR, Rome;
G. Tarei, G. Tassone, C. De Libero, M. Stornelli, D. Ricci, 
BeppoSAX Science Operations Center, Telespazio, Rome;  
M. Capalbi, M.R. Daniele, BeppoSAX Science Data Center, Rome; 
R.C. Butler, Agenzia Spaziale Italiana, Rome; J. Heise, Space 
Research Organization Netherlands, Utrecht; F. Frontera, 
Universita' di Ferrara, Ferrara; report: 

"GRB 000214 ``Valentine's Day Burst'' was observed with the Narrow 
Field Instruments (NFI) on board BeppoSAX from Feb. 14.5479 to 
15.0793 UT (starting about 12 hrs after the burst trigger time). 
In the 2-10 keV image of all data from both MECS units 2 and 3, a 
fading point source ( 1SAX J185427-6627.5 ) is detected within the 
WFC error box (Paolino et al., GCN #557
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  and #559
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 ). The source position 
is R.A. = 18h54m27.0s, Decl. = -66d27'30" (Eq. 2000) with 50" error 
radius. In the first 20,000 s the source had a 2-10 keV flux of 5E-13 
erg/cmE2/s and faded by a factor of two in the last 20,000 s. We conclude 
that 1SAX J185427-6627.5 is the X-ray afterglow of GRB 000214." 

This message may be cited.

R. Subrahmanyan, M.H. Wieringa, R.M. Wark, D. McConnell (ATNF),
D. A. Frail (NRAO) and S. R. Kulkarni (Caltech) report:

"We obtained a 8 hour integration with the Australia Telescope Compact
Array (ATCA) centered on February 17.92 UT at 4.8 GHz and 8.6 GHz.
Within the 50-arcsec radius of the NFI error circle (GCN 561
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 ), we find
no radio sources above a 4-sigma level of 235 microJy."

This message may be cited.

James Rhoads (STScI), Andrew Wilson (U Maryland), 
Thaisa Storchi-Bergmann (UFRGS), and Andrew Fruchter (STScI) report:

We observed the field of GRB 000214 in the K' (2.1 micron) filter on
February 15.392 and on February 17.410 using the CTIO 4m Blanco
Telescope + OSIRIS imager, with net integration times of 180 seconds
and 384 seconds respectively.  Both epochs covered the entire BeppoSAX
NFI error circle (Antonelli et al, GCNC 561).

We find no convincingly variable sources down to an approximate first
epoch 5 sigma limiting point source magnitude of K' = 18.15, or 34
microJansky (calibrated by observation of the standard star S071-D).
Assuming a normal, unobscured afterglow spectral index (in the 
range -0.65 to -1.25 for f_nu) implies a corresponding flux limit
of 8 to 17 microJansky at 0.7 micron, or roughly R=21.

The approximate 5 sigma point source limit for the second epoch is K' = 19.1.