GRB 030217

K. Hurley and T. Cline, on behalf of the Ulysses and HETE GRB teams,

G. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R.
Vanderspek, J. Villasenor, G. Crew, G. Monnelly, N. Butler, J.G.
Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, J. Braga, R.
Manchanda, G. Pizzichini, Y. Shirasaki, C. Graziani, M. Matsuoka, T.
Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi,
T. Tavenner, T. Donaghy, M. Boer, J-F Olive, and J-P Dezalay, on behalf
of the HETE GRB team, and

A. von Kienlin, G. Lichti, and A. Rau, on behalf of the INTEGRAL
SPI-ACS GRB team, report:

Ulysses, HETE-FREGATE, and INTEGRAL (SPI-ACS)  observed this GRB at
09942 seconds.  As observed by Ulysses, it had a duration of
approximately  50 seconds, a 25-100 keV fluence of approximately
1.2E-05 erg/cm2, and a peak flux of approximately  1.2E-06 erg/cm2 s
over 0.50 seconds.

We have triangulated it to a preliminary annulus centered  at RA,
Decl(2000)= 171.644, +41.752 degrees, whose radius is 55.349 +/-  0.035
degrees (3 sigma ).

This annulus may be constrained and/or improved, but it is not known at
this point whether this event was observed by Mars Odyssey, and thus
whether a small error box can be derived for it.

K. Hurley and T. Cline, on behalf of the Ulysses, HETE, and Mars Odyssey GRB teams,

I. Mitrofanov, D. Anfimov, A. Kozyrev, M. Litvak and A. Sanin,
on behalf of the HEND/Odyssey GRB team,

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr,
on behalf of the GRS/Odyssey GRB team,

G. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R. Vanderspek, 
J. Villasenor, G. Crew, G. Monnelly, N. Butler, J.G. Jernigan, A. Levine, 
F. Martel, E. Morgan, G. Prigozhin, J. Braga, R. Manchanda, G. Pizzichini,
Y. Shirasaki, C. Graziani, M. Matsuoka, T. Tamagawa, K. Torii,
T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, T. Donaghy,
M. Boer, J-F Olive, and J-P Dezalay, on behalf of the HETE GRB team, 

D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, and

A. von Kienlin, G. Lichti, and A. Rau, on behalf of the INTEGRAL
SPI-ACS GRB team, report:

This event (GCN 1870
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 ) was also observed by Mars Odyssey and
RHESSI.

We have triangulated it to a preliminary, 3 sigma error box 
with approximate area  68 square arcminutes whose coordinates are:

    RA(2000)                              DEC(2000)
 ERROR BOX CENTER:  12 h 26 m 22.80 s    -11 o 51 '  24.23 " 
 ERROR BOX CORNER 1: 12 h 26 m 30.37 s    -11 o 53 '  08.09 " 
 ERROR BOX CORNER 2: 12 h 25 m 27.01 s    -11 o 56 '  50.21 " 
 ERROR BOX CORNER 3: 12 h 27 m 18.75 s    -11 o 45 '  54.28 " 
 ERROR BOX CORNER 4: 12 h 26 m 15.24 s    -11 o 49 '  40.33 " 

This error box may be improved.

A. Guarnieri, S.Bernabei, C.Bartolini, A.Piccioni, I.Bruni, (Bologna 
University and Bologna Astronomical Observatory), and G. Pizzichini (IASF-CNR, 
Sezione di Bologna) report: 

On 2003, February 20, 00h38m23s UT we started observations of the error box 
of GRB030217 (GCN 1872
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 ) with the 152 cm telescope in Loiano, (R band, 
300 sec exposures). Coverage of the entire error box was performed in bright 
sky conditions because of the full moon. 
By comparison with the DssII, in our frames there is no new source brighter 
than 18.0 mag.


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S. T. Holland, P. M. Garnavich (Notre Dame),
A. Hornstrup (Danish Space Research Institute),
Barbara Mochejska, K. Z. Stanek (Harvard-Smithsonian CfA), and
H. Pedersen (Copenhagen) report

     We have obtained Rc-band images of most of the IPN error region
for GRB 030217 (GCN 1872
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 ) using the 2.56-meter Nordic Optical
Telescope on La Palma on 2003 Feb. 22 UT, and using the Fred Lawrence
Whipple Observatory 1.2m telescope on Mt Hopkins, Arizona on
2003 Feb. 20, 21 and 22 UT.  Our data cover approximately 80% of the
IPN error region and are centred on the centre of the error region.
No optical afterglow is visible in our images to the detection limit
of the second generation Digital Sky Survey.

     The galaxy LCRS B122355.6-113041 is located at R.A. = 12:26:30.91,
Dec. = -11:47:17.3 (J2000), which is just outside the northeast edge
of the IPN error region.  This galaxy has a magnitude of 17 and a
redshift of 0.14 (Shectman et al., 1996, ApJ, 470, 172).  We find no
evidence for a variable source in or near this galaxy, but we urge
observers with earlier data to check for a possible transient near
this location.


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