Central Bureau for Astronomical Telegrams
IAUC 5781: 1993L; GRO J0422+32; V351 Pup (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 5782
.dvi or
.ps format.
Circular No. 5781
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 1993L IN IC 5270
N. Suntzeff, Cerro Tololo Interamerican Observatory,
communicates: "CCD images taken with the CTIO 0.9-m telescope by G.
Williger on May 1.43 UT show SN 1993L to be 25" west and 1".4 north
of the galaxy's center. Reduction of the CCD frames by R. Aviles
yields the following magnitudes (R and I on the Kron-Cousins
system): B = 14.26, V = 13.60, Rc = 13.61, Ic = 13.71). The photometry
was performed with a 14"-diameter aperture and may be slightly
contaminated by the galaxian light at the 0.03-magnitude level.
The suspected supernova is in the disk of IC 5270 near a prominent
dust lane, and the red colors may indicate high reddening. IC 5270
is a particularly interesting galaxy because it is a member of the
Grus cluster and has been used in Tully-Fisher distance scale work,
and further observations are urged."
GRO J0422+32
B. A. Harmon and G. J. Fishman, Marshall Space Flight Center,
NASA; and W. S. Paciesas and M. S. Briggs, University of Alabama,
Huntsville, report for the BATSE/CGRO Experiment Team: "Hard x-ray
monitoring of GRO J0422+32 (cf. IAUC 5580, 5584, 5587, 5592, 5685,
etc.) using Earth occultation indicated that flux from the object
in the energy band 20-300 keV had decreased below the BATSE one-day
detection limit of about 100 mCrab (3 sigma) after 1993 Mar. 14.
The characteristic times for exponential decay of the light curve
(1/e) following the primary maximum (1992 mid-August; IAUC 5580,
5584) and the secondary maximum (1992 mid- to late-December; IAUC
5685) were similar (about 40 days). Spectral fits with an optically
thin thermal bremsstrahlung model have shown that the spectrum
hardened in the initial decay phase from kT about 90 keV near the
primary maximum in 1992 August to kT about 115 keV around 1992 mid-
September. No significant spectral changes were observed during
the subsequent decline through 1993 March, which includes the
secondary intensity maximum. Monitoring of GRO J0422+32 is
continuing."
V351 PUPPIS (NOVA PUPPIS 1991)
Photometry by A. C. Gilmore, Mt. John University Observatory:
Apr. 18.45 UT, V = 13.07 +/- 0.02, U-B = -1.53 +/- 0.04, B-V =
+0.24 +/- 0.00, V-R = +0.14 +/- 0.03.
1993 May 1 (5781) Daniel W. E. Green
Read IAUC 5782
.dvi or
.ps format.
Our Web policy. Index to the CBAT/MPC/ICQ pages.
