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IAUC 5799: 1993O, 1993P; 1993J

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                                                  Circular No. 5799
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. Hamuy, Cerro Tololo Interamerican Observatory; and J. Maza,
University of Chile, report the discovery of an apparent supernova
of mpg about 17.5 by R. Antezana (University of Chile), found on a
20-min unfiltered IIa-O plate taken on May 18.16 UT by G. Valladares
with the CTIO Curtis Schmidt telescope.  SN 1993O is located 14"
west and 8" north of the nucleus of an anonymous galaxy at R.A. =
13h28m19s, Decl. = -32 57'.6 (equinox 1950.0).  Confirmation of
this supernova was made by A. Layden (CTIO) on CCD B and V images
obtained on May 20.229 with the CTIO 0.9-m telescope.  M. M.
Phillips (CTIO) obtained a spectrogram on May 21.13 with the CTIO
1.5-m telescope, indicating that SN 1993O is a type-Ia event at
maximum light, or perhaps even a few days before maximum; a spectrum
of the host galaxy shows weak H-alpha emission at a redshift
of 0.051.
     Phillips, Hamuy, and Maza also report the discovery of another
supernova of mpg about 17.5 by Antezana on the same plate noted
above, SN 1993P being located in the nucleus of a spiral galaxy at
R.A. = 13h26m37s.4, Decl. = -30 09'18" (equinox 1950.0).  Confirmation
was again made by Layden from a CCD V image obtained on May
20.22.  A spectrogram acquired by Phillips on May 21.03 with the
CTIO 1.5-m telescope reveals SN 1993P to be a type-Ic event near
maximum light.  Weak H-alpha emission observed in the disk of the
galaxy yields a redshift of 0.048.

     D. A. Green and G. G. Pooley, Mullard Radio Astronomy Observatory,
Cambridge, communicate:  "Continued monitoring of SN 1993J
with the Ryle Telescope at 15.25 GHz (not 15 or 15.5 GHz, as we
incorrectly stated on IAUC 5751 and 5773) shows that its increase in
flux density at this frequency has recently slowed considerably.
We see an approximately linear rise to 53 mJy on May 3.7 UT from
its detection Apr. 5 (IAUC 5751; about 10 days after the supernova
event, taken to be Mar. 26.0), with a slower rise since then to 60
mJy by May 19.8.  These flux densities are preliminary, and are
based on an assumed flux density of 1.2 Jy for 0954+658.  The linear
increase in flux density seen at this frequency lasted about 30
days, which is about three times the delay in detection of the
supernova; this is difficult to reconcile with the available models
for radio supernovae."

1993 May 21                    (5799)            Daniel W. E. Green

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