Central Bureau for Astronomical Telegrams
IAUC 5430: 1992A; OAO 1657-415; N Pup 1991
The following International Astronomical Union Circular may be linked-to from your own Web pages, but must not otherwise be redistributed (see these notes on the conditions under which circulars are made available on our WWW site).
Read IAUC 5431
Circular No. 5430
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 or GREEN@CFA.BITNET MARSDEN or GREEN@CFAPS2.SPAN
SUPERNOVA 1992A IN NGC 1380
G. Sonneborn, Goddard Space Flight Center; and R. P. Kirshner,
Center for Astrophysics, report: "Low-dispersion ultraviolet spectra
(200-335 nm, resolution 0.6 nm) of SN 1992A were obtained with
the International Ultraviolet Explorer satellite on Jan. 13.9-14.1
UT. The supernova's ultraviolet spectrum, detected longward of 260
nm at a resolution of 0.6 nm, has a double-peaked structure with
maxima at 290 and 320 nm, and peak fluxes of 3.6 and 4.5 x 10E-14
erg cmE-2 sE-1 AE-1, respectively. This spectral morphology is
similar to that seen in other type-Ia supernovae (e.g., 1980N, 1981B,
1990N). The visual magnitude of SN 1992A was about 13.0, as
measured by the IUE fine error sensor."
OAO 1657-415
M. H. Finger, Computer Sciences Corporation; D. Chakrabarty, J.
M. Grunsfeld, and T. A. Prince, California Institute of Technology;
R. B. Wilson, G. J. Fishman, and C. A. Meegan, Marshall Space Flight
Center, NASA; and W. S. Paciesas, University of Alabama at Huntsville,
report for the BATSE team: "As part of a joint MSFC/Caltech
pulsar detection and all-sky monitoring program, Fourier transform
analysis is performed daily on the Compton Observatory BATSE
discriminator rates (1.024-s resolution, 20-60 keV). OAO 1657-415 has
been detected repeatedly over the last 6 months in about 1-day
Fourier transforms. The resulting frequency history over this time
span shows a clear modulation due to binary orbital motion. Preliminary
analysis provides an orbital period of 10.4 +/- 0.1 days and
projected semimajor axis of 95 +/- 5 light seconds. The pulse
period in the pulsar frame is 37.667 +/- 0.005 s on 1991 Oct. 20 UT.
The pulsar is observed to be eclipsed by its binary companion and
analysis indicates that the orbit is eccentric. Further analysis
and observations are in progress."
NOVA PUPPIS 1991
Photometry by A. C. Gilmore with the 0.6-m Boller & Chivens
reflector at Mt. John Observatory: Jan. 9.502 UT, V = 8.66, U-B =
-0.48, B-V = +0.60, V-R = +1.08, V-I = +1.27 (uncertainties about
0.01 mag in all colors except U-B, which may be up to 0.06 more
negative).
1992 January 15 (5430) Daniel W. E. Green
Read IAUC 5431
Our Web policy. Index to the CBAT/MPC/ICQ pages.
