Circular No. 6533
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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Phone 617-495-7244/7440/7444 (for emergency use only)


GRB 970111
     E. Costa, M. Feroci, and L. Piro, Istituto Astrofisica
Spaziale, C.N.R., Frascati; F. Frontera and G. Zavattini,
Universita di Ferrara; L. Nicastro and E. Palazzi, Istituto
Tecnologie e Studio Radiazioni Extraterrestri, C.N.R., Bologna; G.
Gandolfi, M. Smith, A. Coletta, G. D'Andreta, and G. Spoliti,
BeppoSAX Science Operation Center, Roma; and R. Jager and J. Heise,
Space Research Organization of the Netherlands, Utrecht,
communicate:  "The BeppoSAX Gamma Ray Burst Monitor (GRBM) was
triggered on Jan. 11.405556 UT.  Quick-look analysis carried out at
the BeppoSAX Science Operation Center shows the following.  From
the GRBM lightcurve, we see an intense gamma-ray burst lasting
about 50 s, with two major peaks of similar intensity spaced 9 s
apart, and a third peak after 17 s.  The fluxes of the three peaks
are about 4500, 5500, and 700 counts/s.  The burst is in the field
of Wide Field Camera (WFC) number 2 with a peak countrate of about
300 counts/s.  Taking into account the off-axis position, the peak
flux corresponds to about 4 Crab.  From the WFC image, we have
derived a first estimation of the position at R.A. = 15h28m24s,
Decl. = +19o40'.0 (equinox 2000.0); we conservatively estimate a
10' error radius.  The procedure for a TOO pointing of BeppoSAX
Narrow Field Instruments has been started.  Observations in all
bands are solicited."


PSR 0656+14
    V. G. Kurt and B. V. Komberg, Astro Space Center, Russian
Academy of Sciences; V. V. Sokolov and S. V. Zharikov, Special
Astrophysical Observatory; and G. G. Pavlov, Pennsylvania State
University, report:  "The radio pulsar PSR 0656+14 was observed
with the 6-m telescope on Nov. 11-12.  Broadband BVRI CCD images
(field-of-view 2'.4 x 2'.6; pixel size 0".274; seeing about 1".5)
show the following magnitudes of the pulsar:  B = 24.85 (+0.19,
-0.16), V = 24.90 (+0.16, -0.14), R = 24.52 (+0.12, -0.11), I =
23.81 (+0.27, -0.21).  The optical-ultraviolet spectrum, including
the flux measured in the HST/FOC F130LP filter (cf. Pavlov,
Stringfellow, and Cordova 1996, Ap.J. 467, 370) can be interpreted
as a sum of the nonthermal power-law spectrum and thermal spectrum
emitted by the surface of the neutron-star."

                      (C) Copyright 1997 CBAT
1997 January 11                (6533)            Daniel W. E. Green