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IAUC 6058: 1994Y; 1993J; 1994W

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                                                  Circular No. 6058
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

     William Wren, McDonald Observatory, reports his visual
discovery of an apparent supernova in NGC 5371 (R.A. = 13h55m.7,
Decl. = +40o28', equinox 2000.0), located about 28" west and 14"
north of the galaxy's nucleus.  Wren provides the following
magnitude estimates as seen through a 0.9-m telescope:  July 31.18
UT, [16.5; Aug. 19.15, 15.0.
     Y. Paik, A. V. Filippenko, R. R. Treffers, and S. D. Van Dyk,
University of California at Berkeley; and M. W. Richmond, Princeton
University, report that R-band images of NGC 5371 were obtained in
August as part of the Leuschner Observatory Supernova Search.  On
Aug. 12, SN 1994Y is 2.7 mag fainter than the comparison star 61"
west and 5" south of it, barely below the threshold for automatic
detection.  On Aug. 16, it is perhaps 2 mag fainter than the
comparison star, but the image quality is very poor.  Images obtained
on Aug. 3, 6, and 9 show little or nothing due to clouds.  SN 1994Y
is measured as 34" west and 11" north of the galaxy's nucleus.

     R. W. Hanuschik, University of Tubingen; and M. Werger,
University of Bochum, report:  "We have performed optical spectroscopy
(dispersion 20.0 nm/mm) of SN 1993J on June 6-8 and Aug. 1-3 with
the 2.2-m telescope (+ CAFOS Faint Object Spectrograph) of the
German-Spanish Observatory at Calar Alto.  We confirm the outburst
of broad H-alpha emission as reported on IAUC 6005; if due to pure
H-alpha emission, its total base width is about 20000 km/s.  We do
not exclude, however, the alternative possibility of blended H-alpha
and He I 667.8-nm emission, in which case the half base width of
each line is about 5000 km/s.  The intensity of the emission feature
is approximately the same as that of [O I] at 630.0 and 636.3 nm in
June, and higher than that in August; it is also substantially
higher than [Ca II] at 729.1 and 732.3 nm for June and August.  If
this feature is a blend of H-alpha and He I, then both lines show
about the same intensity for each date.  The emission feature is
likely to be the result of the interaction of the expanding ejecta
with a dense shell in the progenitor's circumstellar wind."

     Visual magnitude estimates by L. Szentasko, Veresegyhaz,
Hungary:  Aug. 8.83 UT, 13.5; 10.84, 14.0; 12.83, 13.9; 16.83,
14.0; 18.83, 13.8.

1994 August 19                 (6058)            Daniel W. E. Green

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