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IAUC 5766: N Oph 1993; 1993J; 1993e

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                                                  Circular No. 5766
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM     EASYLINK 62794505
MARSDEN@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)


NOVA OPHIUCHI 1993
     R. H. McNaught, Anglo-Australian Observatory, provides the
following position for N Oph 1993 from a film taken with the Uppsala
Southern Schmidt telescope on Apr. 17.5 UT:  R.A. = 17h22m04s.41,
Decl. = -23 08'32".2 (equinox 1950.0; uncertainty 0".3 in each
coordinate). This position does not correspond to any object on the
SERC J survey plate (limiting mag about 21.5) taken 1976 May 29, on
a UKST I plate taken 1980 Aug. 5, on an ESO B plate taken 1976 Apr.
5, or on an ESO R plate taken 1984 July 25.  The nearest star measured
from the J survey was at mag about 18.5 located 2".6 east and
3".2 south of the nova.  A star of mag about 12 is located at R.A.
= 17h21m58s.22, Decl. = -23 07'42".9.
     Photometry by A. C. Gilmore, Mt. John University Observatory,
obtained in poor conditions with the 0.6-m f/13 reflector (reference
star HR 6473):  Apr. 18.49 UT, V = 9.66, B-V = +0.79, U-B =
-0.17.


SUPERNOVA 1993J IN NGC 3031
     H. U. Zimmermann, Max-Planck-Institut fur Extraterrestrische
Physik (MPE); W. Lewin and E. Magnier, Massachusetts Institute of
Technology; P. Predehl, G. Hasinger, W. Pietsch, B. Aschenbach, and
J. Trumper, MPE; G. Fabbiano, Center for Astrophysics; J. van
Paradijs, University of Amsterdam; L. Lubin, Princeton University;
and R. Petre, Goddard Space Flight Center, communicate:  "SN 1993J
has been observed with the ROSAT Observatory on six occasions
between Apr. 3 (IAUC 5748 and 5750) and Apr. 13.  The exposures were
made on Apr. 3, 7, 9, 10, 12, and 13 and lasted between 1000 and
3000 s each.  A linear fit to the count rates (0.1-2.4 keV) shows a
decrease of about 30 percent in 10 days.  Our observations are
inconsistent with a constant count rate at a confidence level higher
than 99.9 percent.  This seems to support models that predict a decay
in the x-ray intensity on timescales of a few weeks to months."


COMET SHOEMAKER-LEVY (1993e)
     Total visual magnitude estimates (cf. IAUC 5745):  Apr. 1.03
UT, 13.9 (H. Mikuz, Ljubljana, Slovenia, 0.20-m Baker-Schmidt camera
+ CCD + V filter); Apr. 1.73, 14.0 (A. Nakamura, Kuma, Ehime, Japan,
0.60-m reflector); 12.28, 13.3 (A. Hale, Las Cruces, NM, 0.41-m
reflector); 14.13, 12.8 (J. E. Bortle, Stormville, NY, 0.50-m
reflector); 14.59, 13.9 (Nakamura).


1993 April 18                  (5766)            Daniel W. E. Green

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