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IAUC 4041: 1985E; 1982i; 1984k

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                                                  Circular No. 4041
Central Bureau for Astronomical Telegrams
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM    Telephone 617-495-7244/7440/7444

     L. Cameron and A. Spanhauer report their discovery with the
1-m telescope at Las Campanas Observatory of a supernova 11"8 west
and 17"3 south of the nucleus of the spiral galaxy ESO 510-G50 (R.A. =
14h02m13s3, Decl. = -26deg09'3 (equinox 1985.1).  The supernova, of B ~
17.5, was found on Mar. 2 and confirmed photographically on Mar. 3.

     T. Y. Brooke and R. Knacke report magnitudes (7"2 diaphragm)
obtained at the NASA Infrared Telescope Facility on Feb. 17.3 UT: J
= 18.53 +/- 0.20, H = 17.76 +/- 0.17, K = 17.82 +/- 0.29.  These do not
confirm the very blue color noted on IAUC 4034, and J-H and H-K are
comparable to those of RD objects and other comets.

     P. A. Wehinger, Arizona State University, reports: " Reticon
spectra (300-750 nm, 1.5 nm resolution) obtained on Feb. 17 with
the 4.5-m Multiple-Mirror Telescope by S. Wyckoff, C. Foltz and C.
Heller, in collaboration with Wehinger, M. Wagner, D. Schleicher
and M. Festou, show evidence for weak CN emission at 387.5 nm.
The observed band strength through a 5" diameter aperture was 1.9
+/- 1.4 x 10**-18 J m**-2 s**-1 after subtraction of the reflected solar
continuum.  The average CN column density centered on the nucleus
was 3.3 x 10**13 m**-2, and the CN production rate calculated from the
vectorial model Q = 6 x 10**25 s**-1.  When the spectrum of the comet
is ratioed with that of a G star, very marginal evidence is found
for the presence of several additional weak emission features in
the 320-700 nm region.  The magnitude and color (measured through
the 5" aperture) were V = 18.9, B-V = +0.66.  No significant
brightness variations > +/- 0.2 mag were observed in twelve successive
10-min integrations during 3.5 hr beginning on Feb. 17.12 UT."

     W. Wisniewski, University of Arizona; and T. Fay, McDonnell
Douglas Astronautics Corporation, report that they monitored this
comet with the 1.5-m reflector at the Catalina Station during a
total of eight nights (Jan. 17-21, Feb. 15-17 UT).  The range of
variability was 0.6 mag, and the observations are best represented
by a rotation period of 27h12m for the comet.  Since the 12"
diaphragm included a significant contribution from the coma, the
amplitude of true variability must be considerably larger.

1985 March 5                   (4041)              Brian G. Marsden

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