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IAUC 6110: 1994af; 1994ae; OJ 287

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                                                  Circular No. 6110
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     TWX 710-320-6842 ASTROGRAM CAM

     R. H. McNaught, Anglo-Australian Observatory, reports his
discovery of an apparent supernova (mag about 18) at R.A. =
3h02m57s.97, Decl. = -12o22'54".9 (equinox 1950.0, uncertainty 0".4
in each coordinate), or about 3" due east of the center of the host
spiral galaxy.  SN 1994af was found on an R plate taken on Nov. 27
by C. P. Cass with the U.K. Schmidt Telescope.  No image appears at
this position on another R plate taken on 1993 Sept. 23 or on the
SERC J survey.  A nearby star (about 0.5 mag fainter than SN 1994af)
has position end figures 3m05s.52, 8".6.
     B. Schmidt, P. Challis, and R. Kirshner, Harvard-Smithsonian
Center for Astrophysics (CfA), report that a spectrogram (380-740
nm) of SN 1994af taken by P. Berlind (CfA) with the Tillinghast
1.5-m reflector (+ FAST spectrograph) on Dec. 1.25 UT shows this
object to be a relatively young type-II supernova, as indicated by
broad P-Cyg profiles of H-alpha and He I (587.6 nm).  The velocity
of the host galaxy, measured from narrow H-alpha emission, is 3750

SUPERNOVA 1994ae IN NGC 3370
     S. Nakano, Sumoto, Japan, forwards the following accurate
position from Y. Kushida and R. Kushida at Yatsugatake South Base
Observatory (from a CCD image taken on Nov. 30.842 UT, when the
supernova was at unfiltered mag 12.5):  R.A. = 10h44m21s.52, Decl.
= +17o32'20".7 (equinox 1950.0).

OJ 287
     H. Inoue, F. Nagase, F. Makino, C. Otani, R. Fujimoto, and Y.
Ueda, Institute of Space and Astronautical Science; and M. Tashiro,
T. Takahashi, and E. Idesawa, University of Tokyo, communicate on
behalf of the ASCA Team:  "We observed OJ 287 with ASCA between Nov.
18.42 and 19.62 UT, with an exposure time of about 40~000 s, and
detected significant x-ray emission from the source.  The flux was
then (4.2 +/- 0.2) x 10E-12 erg cmE-2 sE-1 in the range 2-10 keV,
which is smaller by about a factor of two than when seen with the
Einstein Observatory in 1979 and 1980 (Madjeski and Schwartz 1988,
Ap.J. 330, 776), in spite of the current high luminosity at optical
bands (IAUC 6095).  The intensity variation during our observation
was < 30 percent on time scales from 100 min to a day.  The 0.5- to
10-keV spectrum is fit by a power-law spectrum with photon index
1.7 +/- 0.1 and with interstellar-absorption column density < 1 x
10E21 cmE-2."

1994 December 3                (6110)            Daniel W. E. Green

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