Central Bureau for Astronomical Telegrams
IAUC 7205: 1999co, 1999cp; V382 Vel
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Circular No. 7205
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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SUPERNOVAE 1999co AND 1999cp
J. Y. King and W. D. Li, University of California at Berkeley,
on behalf of the Lick Observatory Supernova Search (cf. IAUC 6627,
7126), report their discovery of two apparent supernovae on
unfiltered CCD images taken with the 0.8-m Katzman Automatic
Imaging Telescope (KAIT). SN 1999co was discovered on frames taken
on June 18.43 and 18.47 UT (mag about 17.4) and confirmed on an
earlier image taken on June 13.5 (mag about 17.8); an image of the
field taken on June 7.5 under poor seeing conditions already showed
a hint of the supernova, which is on the northeast shoulder of the
faint host galaxy at R.A. = 21h03m19s.12, Decl. = -14o32'49".0
(equinox 2000.0). KAIT images of the same field taken on May 29.5
(limiting mag about 18.0) and 19.6 (limiting mag about 19.0) show
nothing at the position of SN 1999co. SN 1999cp was found on CCD
frames taken on June 18.2 and 18.3 UT (mag about 18.2), and
confirmed on images taken on June 19.2 (mag about 17.2); it is
located at R.A. = 14h06m31s.3, Decl. = -5o26'49" (equinox 2000.0),
which is about 52" west and 23" north of the nucleus of NGC 5468.
KAIT images of the same field taken on June 13.2 (limiting mag
about 19.0) and May 14.3 (limiting mag about 19.5) show nothing
at the position of SN 1999cp.
V382 VELORUM
K. Mukai, NASA Goddard Space Flight Center and Universities
Space Research Association; and M. Ishida, Institute of Space and
Astronautical Sciences, report on behalf of the ASCA team: "ASCA
observed V382 Vel between June 9.578 and 10.667 UT (about 17 days
past optical maximum) for about 40~000 s on-source. We detect the
source at about 0.16 counts/s per sensor. The spectrum is
relatively hard and highly absorbed, with N_H about 9 x 10**22
cm**-2 and a bremsstrahlung temperature of about 15 keV. However,
no lines are detected (a plasma-model fit requires an abundance of
iron about 0.1 that of the sun). A non-thermal origin of (part of)
the x-ray flux or a non-ionization equilibrium are both possible
explanations for this. The flux in the band 2-10 keV is 2.2 x
10**-11 erg cm**-2 s**-1; the inferred unabsorbed flux is 3.9 x
10**-11 erg cm**-2 s**-1, corresponding to apparent and true
luminosities of 1.0 x 10**34 and 1.7 x 10**34 erg/s, respectively,
for an assumed distance of 2 kpc, significantly higher than the
BeppoSAX measurements reported by Orio et al. (IAUC 7196).
However, we do not observe significant variability within the about
1-day span of the ASCA observation."
(C) Copyright 1999 CBAT
1999 June 19 (7205) Daniel W. E. Green
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