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IAUC 6706: 1997cy; SNR G327.6+14.6; C/1995 O1

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                                                 Circular No. 6706
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/cfa/ps/cbat.html
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     The Mount Stromlo Abell Cluster Supernova Search Team (cf.
IAUC 6639) reports the discovery of an apparent supernova (V = 17.4,
R = 16.8) on CCD images taken on July 16 by S. Sabine with the Mt.
Stromlo 1.27-m telescope (+ Macho Camera).  SN 1997cy is located on
a faint host galaxy near Abell 3266 at R.A. = 4h32m54s.86, Decl. =
-61o42'57".5 (equinox 2000.0).  A nearby star has position end
figures 59s.27, 43'06".6.  SN 1997cy is not visible on images taken
on Mar. 12 (limiting mag R = 20.5).  A V CCD frame taken on July 22
by D. Baines and J. Howard with the Mt. Stromlo 0.76-m telescope
shows that SN 1997cy had faded by 0.5 mag.

SNR G327.6+14.6
     T. Tanimori, Y. Hayami, and S. Kamei, Tokyo Institute of
Technology, Tokyo; and T. Kifune, ICRR, University of Tokyo, report
on behalf of the CANGAROO Collaboration:  "We have detected TeV
gamma-rays from the remnant of the supernova of 1006 (cf. Green
1984, MNRAS 209, 449) with a statistical significance of 5.5 sigma,
in data taken over 26 hr in April and June 1996 with the 3.8-m
imaging Air Cherenkov Telescope at Woomera.  It is the first
evidence of very-high-energy gamma-rays from an extended supernova
remnant.  We have an additional observation (6.0-sigma significance)
in March and April 1997 to confirm the result.  The TeV gamma-rays
are mainly from the northeast rim of the shell of the supernova
remnant, in accordance with the nonthermal x-rays (2-10 keV) that
the x-ray satellite ASCA has detected.  The gamma-ray signal
suggests extended emission along the ridge of the northeast rim.
However, by approximating the emission as from a single point
source at the rim, preliminary estimation of the integral flux for
the 1996 data is (3.0 +/- 0.54) x 10E-12 cmE-2 sE-1 (> 3 TeV).  The
flux will be increased by taking into account the extended emission
that is much wider than the point-spread function of our detection
(about 0.2 deg in FWHM)."

     Total visual magnitude estimates:  July 9.82 UT, 2.9 (D. A. J.
Seargent, The Entrance, N.S.W., 25x100 binoculars); 10.92, 3.3 (A.
Pearce, Subiaco, W. Australia, 20x80 binoculars); 11.92, 3.6
(Pearce); 14.92, 3.8 (Pearce); 16.82, 3.1 (Seargent, naked eye);
16.92, 3.9 (Pearce).

                      (C) Copyright 1997 CBAT
1997 July 23                   (6706)            Daniel W. E. Green

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