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IAUC number

                                                  Circular No. 6198
Central Bureau for Astronomical Telegrams
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
Phone 617-495-7244/7440/7444 (for emergency use only)

    R. H. McNaught, Anglo-Australian Observatory, reports that he has
located an image of this comet on a 50-min U.K. Schmidt R survey
plate obtained by C. P. Cass on 1993 Apr. 27.  During the exposure
the comet, then 13.1 AU from the sun, would have moved 3".7 to
 the southwest, and the image is consistent with this.  It has
the appearance of a slightly diffuse and slightly elongated star image
within a very faint coma 0'.4 in diameter.  The total and nuclear
magnitudes are about 18 and 19, respectively, based on this being a
good-quality plate with a presumed limit of 21.  The position is 9'
from that given by the parabolic elements on MPEC 1995-P01
(and IAUC 6194), which are now improved on MPEC 1995-P02:

                    Epoch = 1995 Oct. 10.0 TT
     T = 1997 Apr.  1.3922 TT         Peri. = 130.4405
     e = 0.996348                     Node  = 282.4733  2000.0
     q = 0.916702 AU                  Incl. =  88.8797

                    Epoch = 1997 Mar. 13.0 TT
     T = 1997 Apr.  1.6416 TT         Peri. = 130.6678
     e = 0.994441                     Node  = 282.4729  2000.0
     q = 0.913023 AU                  Incl. =  89.4142

These orbital elements, satisfying 248 observations with mean residual
0".6, lead to (1/a)orig = +0.00456 +/- 0.00016 AU-1, indicating that the
comet is not on its first pass from the Oort Cloud.  However, McNaught
adds that he could not locate the comet on a plate taken on 1991 Sept. 1,
when an inverse-square law would have put the comet 1.0 mag fainter than
in 1993.

     I. de Pater and J. R. Graham, University of California at Berkeley;
J. J. Lissauer, State University of New York at Stony Brook; and M.
Showalter, NASA Ames Research Center, report: "Observations were made
of Saturn's rings on May 23 (1.3 days after the ring-plane crossing)
with the W. M. Keck telescope on Mauna Kea at a wavelength of 2.3 microns.
The E-ring is confined to within 2500 km from the ring plane; it extends
out to 5 Saturnian radii.  The peak brightness is about 19 mag per
linear arcsec at the orbit of Saturn II (Enceladus, 4 Saturnian radii).
The ring brightness is lower and drops off faster with distance than seen
at visible wavelengths.  We also report a tentative detection of the
G-ring at 2.8 Saturnian radii, similar in magnitude to the peak of the

1995 August 2                  (6198)              Brian G. Marsden

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