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IAUC 6158: 1995J; 1995I; V1974 Cyg

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                                                  Circular No. 6158
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

     A. V. Filippenko, University of California at Berkeley, reports
that T. Hurt (University of California, Santa Barbara) obtained CCD
spectra (range 340-800 nm) of SN 1995J (cf. IAUC 6157) on Apr. 9 UT
with the 3-m Shane reflector at Lick Observatory.  The partially-
calibrated data reveal very strong, broad P-Cyg profiles of hydrogen,
indicating that this is a normal type-II supernova less than or
approximately equal to 2 months past maximum brightness.
     S. Nakano, Sumoto, Japan, forwards the following precise
position measured by Y. Kushida from a CCD frame taken by R.
Kushida at Yatsugatake South Base Observatory on Apr. 7.659 UT:
R.A. = 12h32m38s.34, Decl. = +63o53'09".2 (equinox 2000.0); this
position corresponds to a point 29" east and 30" north of the
galaxy's center.  The unfiltered magnitude of SN 1995J was found to
be 16.1, using V GSC comparison-star magnitudes.  A measurement
obtained at Sormano from a CCD observation by P. Sicoli and V.
Giuliani on Apr. 7.944 UT gives position end figures 38s.31, 09".4.

     P. Garnavich, P. Challis, and R. Kirshner, Center for
Astrophysics, report that spectra obtained with the Multiple Mirror
Telescope on Mar. 31 indicate that SN 1995I (cf. IAUC 6153) is a
type-II supernova.  A broad emission feature with a weak P-Cyg
profile has developed at the rest wavelength of H-alpha.  Spectra
taken on Mar. 9 at the MMT showed only a blue continuum that peaked
at a rest wavelength of 400 nm.  The redshift is 0.075, based on
narrow emission lines from the host galaxy.

     A. Retter, E. O. Ofek, and E. M. Leibowitz, Wise Observatory,
Tel Aviv University, report:  "Photometry of V1974 Cyg (N Cyg 1992)
in the I band during seven nights in 1994 confirms the finding of
Semeniuk et al. (1994, Acta Astron. 44, 277) about the presence of
a periodicity of 0.08505 day in the light curve of the star.  This
period is 4.7 percent longer than a second period of 0.08127 day,
which is also clearly present in the light curve and which was
identified in 1993 as the binary periodicity of the system by
DeYoung and Schmidt (1994, Ap.J. 431, L47).  The two periods obey
exactly the linear relation of Stolz and Schoembs (1981, IBVS 2029)
for SU UMa stars."

1995 April 10                  (6158)            Daniel W. E. Green

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