Central Bureau for Astronomical Telegrams

Central Bureau for Astronomical Telegrams -- Image credits

IAUC 3734: OPTICAL CANDIDATES FOR THE 1978 Nov. 19 gamma-RAY BURST; N Sgr 1982; N Aql 1982; R Aqr

The following International Astronomical Union Circular may be linked-to from your own Web pages, but must not otherwise be redistributed (see these notes on the conditions under which circulars are made available on our WWW site).


Read IAUC 3733  SEARCH Read IAUC 3735
IAUC number


                                                  Circular No. 3734
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM     Telephone 617-864-5758


OPTICAL CANDIDATES FOR THE 1978 NOVEMBER 19 gamma-RAY BURST
     H. Pedersen and C. Motch, European Southern Observatory,
communicate: "We have made two observations further to those mentioned
on IAUC 3711.  The telescope and detector were unchanged.
The first observation was made on 1981 Nov. 26, 27 and 28.  A
total of 120-min exposure time (60 min Gunn R, 614-710 nm and 60
min Gunn I, 724-884 nm) gave magnitudes for candidates A and B in
agreement with those on IAUC 3711, which refer to a broader band
(665-1000 nm).  The average Johnson R magnitude determined from
all observations made in the period 1981 July 10 to 1982 July 6 is
23.15 +/- 0.35 for A, 23.70 +/- 0.60 for B.  The second observation
was made on 1982 Sept. 19, 20 and 21.  A total of 390-min exposure
time in the 665-1000-nm band did not reveal any significant change
in the brightness of source A (R = 23.10), while source B disappeared
completely (R >= 24.7), even though the exposure goes deeper
than both the ones reported on IAUC 3711 and the one of 1981 Nov.
The variability of B increases the likelihood that it is the optical
counterpart of the gamma-ray burst source.  If this can be proven,
then models involving very-low-mass binaries would be favored,
while lone-neutron-star models would seem excluded."


NOVA SAGITTARII 1982
     A. P. Cowley, University of Michigan, reports that a spectrogram
obtained by J. Sowell at the McGraw-Hill Observatory on Oct. 12.1 UT
shows strong emission due to H, Ca II and Fe II, accompanied by weak,
shallow, single absorptions corresponding to a velocity of about
900 km/s and suggesting that the nova is in a very early
post-maximum stage.


NOVA AQUILAE 1982
     Visual magnitude estimates by M. Verdenet, Bourbon-Lancy,
France: Sept. 6, 14.6; 9, 14.8: 10, 15.0; 11, 15.0.


R AQUARII
     With reference to his remarks on IAUC 3729, S. Tapia, Steward
Observatory, notes that the jet of R Aqr was clearly described by
G. H. Herbig in 1980 (see IAUC 3535).


1982 October 15                (3734)              Brian G. Marsden

Read IAUC 3733  SEARCH Read IAUC 3735


Our Web policy. Index to the CBAT/MPC/ICQ pages.


Valid HTML 4.01!