Central Bureau for Astronomical Telegrams
IAUC 5823: 1993S; V1357 Cyg; RX Pup
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Circular No. 5823
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
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
MARSDEN@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)
SUPERNOVA 1993S IN ANONYMOUS GALAXY
M. Hamuy, Cerro Tololo Interamerican Observatory, reports that
a spectrogram of SN 1993S (cf. IAUC 5812) obtained on June 26.27 UT
with the CTIO 1.5-m telescope telescope shows broad H-alpha emission
with the characteristic P-Cyg profile of type-II supernovae.
The spectrum of the underlying galaxy shows narrow H-alpha emission
yielding a redshift z = 0.032.
V1357 CYGNI
M. D. Leising, Clemson University; and M. S. Strickman, W. N.
Johnson, J. D. Kurfess, and J. E. Grove, Naval Research Laboratory,
report for the Compton Observatory/OSSE Team: "OSSE observed V1357
Cyg (Cygnus X-1) during two intervals, May 13-14 and May 31-June 3,
during the period when it was reported to be in a low hard x-ray
state (IAUC 5813). We confirm that the 45- to 140-keV flux was low
during these periods: 0.08 and 0.06 photon cmE-2 sE-1, respectively.
We find no evidence for MeV emission in either observation,
with 99-percent confidence upper limits on the integral flux from
0.6 to 1.5 MeV of 2.8 and 1.9 x 10E-3 photon cmE-2 sE-1. These
limits are factors of 4 and 6, respectively, below the flux observed
by Ling et al. (1987, Ap.J. 321, L117), when the hard x-ray
flux was similarly low."
RX PUPPIS
R. J. Ivison and E. R. Seaquist, University of Toronto,
report: "Continuum measurements obtained with the James Clerk
Maxwell Telescope and the Very Large Array during 1992 October and
1993 May, respectively, suggest that the symbiotic binary RX Pup
has returned to a state of low excitation after more than a decade
of activity. The centimeter spectral index is -0.1 +/- 0.1, with a
flux density of 13.3 +/- 0.7 mJy at 3.6 cm. Spectra obtained with
the International Ultraviolet Explorer and the Anglo-Australian
Telescope during 1993 April and May confirm that high-excitation
emission lines seen during the 1980s have disappeared, leaving only
the Balmer series, He I, Fe II, O I, and weak, residual [O III] in
emission. The IUE Fine Error Sensor magnitude remains at 11.5, but
a weak, red continuum has replaced the emission lines of N IV], C
IV, and He II usually seen in the SWP and LWP cameras."
1993 June 28 (5823) Daniel W. E. Green
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