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IAUC 8109: 2003cv; IGR J16358-4726; 2003cz

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                                                  Circular No. 8109
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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     Further to IAUC 8103, M. Hamuy reports that a spectrum (range
380-930 nm) of SN 2003cv (cf. IAUC 8104), obtained by J. Maza and
L. Huerta on Apr. 6.15 UT with the Dupont telescope, shows it to be
a peculiar type-II supernova.  H_alpha and H_beta lines exhibit
very broad P-Cyg profiles; their minima yield expansion velocities
of -14000 and -11300 km/s (based on a redshift of 0.028, derived
for the host galaxy from superimposed narrow Balmer lines), which
are unusually high for type-II events.  The spectrum has a broad
trough centered at 589.1 nm, probably due to Na I D 589.3-nm, and a
P-Cyg profile due to the near-infrared Ca II triplet.  This
spectrum is very similar to that of the H-rich 'hypernova' SN
2003bg (IAUC 8084, 8088) taken on Apr. 4.04 by Maza and Huerta, and
this suggests that SN 2003cv is at least least one month old.

IGR J16358-4726
     C. Kouveliotou, Marshall Space Flight Center (MSFC) and
Universities Space Research Association (USRA); S. Patel, National
Research Council; A. Tennant, MSFC; P. Woods and M. Finger, USRA;
and S. Wachter, SIRTF Science Center, California Institute of
Technology, report that IGR J16358-4726 (cf. IAUC 8097) was
observed for 25700 s serendipitously with the Chandra X-ray
Observatory during a scheduled observation of SGR 1627-41 starting
on Mar. 24.17 UT.  The source was approximately 9'.7 off axis.  A
fit to the off-axis image was found to be consistent with the
point-spread function and put the transient at R.A. = 16h35m53s.8,
Decl. = -47o25'41".1 (equinox 2000.0; error radius 0".6).  The
spectrum of the source is hard and highly absorbed, consistent with
a power law of index 0.5(1) plus a line feature at 6.4 keV and a
column density of N_H = 3.3 x 10**23 cm**-2.  The source flux
(unabsorbed) is 1.7 x 10**-10 (2-10 keV).  Pulsations with a period
of 5850(50) s are directly visible in the x-ray light curve with an
energy-dependent amplitude; the pulse fraction between 2 and 10 keV
is 63(6) percent, peak-to-peak.  It is unclear whether these
pulsations reflect a spin or orbital period, or a high-coherence
quasiperiodic oscillation.  A search for an infrared counterpart in
the 2MASS All Sky Catalog reveals a relatively bright source 1".7
from the Chandra position of IGR J16358-4726 (2MASS
J16355369-4725398, with J = 15.41, H = 13.44, K = 12.59).  Further
observations are encouraged.

     Corrigendum.  On IAUC 8106, line 5, FOR  Apr. 2.14  READ
Apr. 2.21

                      (C) Copyright 2003 CBAT
2003 April 8                   (8109)            Daniel W. E. Green

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