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IAUC 5728: 1993f; 1993I; GRO J0422+32

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IAUC number

                                                  Circular No. 5728
Central Bureau for Astronomical Telegrams
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

     M. P. Candy, Perth Observatory, reports the recovery of this comet
from his measurements on plates taken by G. Lowe with the 0.33-m astrograph:

     1993 UT             R.A. (2000) Decl.        m1
     Mar. 21.84583   21 27 52.66   -18 45 17.1    14
          21.88750   21 27 59.93   -18 44 37.2
          27.85729   21 46 38.68   -16 58 02.3

On the first night the comet had a central condensation 5" across and a 1'
tail to the southwest.  The indicated correction to the prediction on MPC
16379 is delta T = +0.04 day.

SUPERNOVA 1993I IN MCG +02-32-144
     C. Pollas, Observatoire de la Cote d'Azur, reports his discovery
of a possible supernova of mag 18.0 at R.A. = 12h32m10s.50, Decl. =
+9D16'39".2 (equinox 1950.0), 13".8 west and 8".6 south of the center
of the S0 galaxy (B = 14.9) MCG +02-32-144.  The object was found on
films taken by D. Albanese and himself on Mar. 23.03 and 25.01 UT.  It
was also present at mag 21 on Mar. 17.02 UT but is not visible in the
Palomar Sky Survey.  SN 1960B also appeared in this galaxy.

GRO J0422+32
     E. T. Harlaftis, Royal Greenwich Observatory; and P. A. Charles,
University of Oxford, report: "CCD photometry of the GRO J0422+32 optical
counterpart (IAUC 5588) with the 1-m Kapteyn Telescope at La Palma
on Feb. 28.93 UT gave U = 15.5, B = 16.2, V = 15.3 and R = 14.8 (errors
0.2 mag) and on Mar. 19.92 UT gave V = 15.9 and R = 15.2, indicating a
decay rate in V of about 0.03 mag/day.  A 20-min optical spectrum on Feb.
19.92 with ISIS on the 4.2-m Herschel Telescope covered the ranges 420-500
and 600-700 nm at a resolution of 0.14 nm.  The main difference from the
spectrum reported on IAUC 5589 is the disappearance of the 464-465-nm
Bowen blend.  He II (468.6 nm) is still very strong (equivalent width
2 nm) and indicates that the source is probably still x-ray active.
H alpha, beta and gamma all show a narrow emission feature and other
complex structure, with H beta and gamma both being superposed on a broad,
shallow absorption feature (FWZI about 9 nm).  The 443-nm and 661.3-nm
diffuse interstellar features imply E(B-V) = 0.20."

1993 March 28                  (5728)              Brian G. Marsden

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