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IAUC 6237: 1995ab; 1995ac; 1995Y

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                                                  Circular No. 6237
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)

SUPERNOVA 1995ab IN NGC 7663
     C. Pollas, Observatoire de la Cote d'Azur (OCA), reports his
discovery of an apparent supernova (V = 17.7) on a technical pan
film obtained on Sept. 22.97 UT with the 0.9-m OCA Schmidt
telescope; the supernova is located at R.A. = 23h26m44s.46, Decl. =
-4o57'45".9 (equinox 2000.0), which is 11".3 west and 14".1 north
of the spiral galaxy's center.  SN 1995ab is not visible at this
location on the Palomar Sky Survey prints.  A nearby star (V about
13.5) has position end figures 47s.77, 45".5.
     A. V. Filippenko and D. C. Leonard, University of California
at Berkeley, report that CCD spectra (range 310-1000 nm, resolution
0.7-1.4 nm) obtained on Sept. 26 UT with the 3-m Shane reflector
at Lick Observatory show that this supernova is of type II.  The
prominent, broad hydrogen Balmer lines have P-Cyg profiles.  The
narrow emission lines of a superposed H II region yield a redshift
of 0.019.

     Pollas also reports his discovery, on an OCA technical pan
film taken on Sept. 22.91 UT, of a supernova (V about 18.5) located
2".5 west and 4".2 south of the center of an edge-on spiral galaxy
(mag about 16.5) at R.A. = 22h45m41s, Decl. = -8o45'.2 (equinox
2000.0).  Nothing is visible at this location on the PSS.
     Filippenko and Leonard report that CCD spectra obtained as
above (range 350-1030 nm) show that SN 1995ac closely resembles
the peculiar type-Ia supernova 1991T (e.g., Filippenko et al. 1992,
Ap.J. 384, L15), within a week prior to maximum brightness.  The
deep Si II absorption trough normally seen at 615 nm is absent;
instead, there are blends (probably of Fe III) near rest
wavelengths of 420 and 490 nm.  The likely redshift of the parent
galaxy, 0.05, was determined from the weak H-alpha emission line in
the galaxy disk.

     P. Garnavich, A. Riess, P. Challis, and R. Kirshner, Center
for Astrophysics, report:  "Spectra obtained by J. Huchra with the
1.5-m Tillinghast telescope on Sept. 22 show that this is a type-Ia
supernova, 5-7 weeks after maximum.  This is significantly younger
than the age reported on IAUC 6221 and implies the discovery by
Mueller was made soon after maximum.  Photometry from CCD images
obtained by B. McLean with the F.L. Whipple Observatory 1.2-m
telescope yields:  Sept. 14.4 UT, V = 16.96 +/- 0.08; 19.4, V =
17.21 +/- 0.05, B-V = +1.22 +/- 0.07."

1995 September 26              (6237)            Daniel W. E. Green

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