Central Bureau for Astronomical Telegrams
IAUC 8105: 2003cx; 2003cp; IGR J17464-3213 = XTE J17464-3213
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Circular No. 8105
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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SUPERNOVA 2003cx
Further to IAUC 8104, W. M. Wood-Vasey, G. Aldering, and P.
Nugent report the discovery of an apparent supernova (mag 19.1) on
unfiltered NEAT images taken with the Palomar 1.2-m Schmidt
telescope on Mar. 31.42, 31.46, and 31.48 UT. The new object is
located at R.A. = 13h57m06s.46, Decl. = -17o02'22".6 (equinox
2000.0), which is 1".0 west and 2".6 south of the center of the
apparent host galaxy. Additional magnitudes from NEAT observations
with the Palomar 1.2-m and Haleakala 1.2-m telescopes: 2002 May
17.29, [21.0; 2003 Feb. 12.61, [20.3; Mar. 23.44, 19.4.
SUPERNOVA 2003cp IN MCG +10-12-78
T. Matheson, P. Challis, and R. Kirshner, Harvard-Smithsonian
Center for Astrophysics, report that a spectrum (range 370-750 nm)
of SN 2003cp (cf. IAUC 8103), obtained by P. Berlind on Apr. 1.18
UT with the F. L. Whipple Observatory 1.5-m telescope (+ FAST
spectrograph), shows it to resemble a type-Ia supernova, two to
three weeks past maximum, but some of the line strengths appear
unusual.
IGR J17464-3213 = XTE J17464-3213
M. P. Rupen, A. J. Mioduszewski, and V. Dhawan, National Radio
Astronomy Observatory (NRAO), report the detection of a probable
radio counterpart to the the x-ray transient and blackhole
candidate IGR J17464-3213 = XTE J17464-3213 (Revnivtsev et al. 2003,
http://atel.caltech.edu/?read=132; Markwardt and Swank 2003,
http://atel.caltech.edu/?read=133). Observations with the Very
Large Array (VLA) on Mar. 30 and Apr. 1 UT show a compact, variable
source at R.A. = 17h46m15s.61 +/- 0s.01, Decl. = -32o13'59".9 +/-
1" (equinox 2000.0), roughly 2' from the original INTEGRAL position
and consistent with the position of H1743-322 (Gursky et al. 1978,
Ap.J. 223, 973). The flux densities on Mar. 30 (after correcting
for primary beam attenuation) were 3.5 +/- 0.2 mJy at 4.9 GHz and
4.6 +/- 0.2 mJy at 8.5 GHz. By Apr. 1, the source had brightened
by about 50 percent, while retaining a flat or somewhat rising
spectrum: 1.4 GHz, 7.8 +/- 1.5 mJy; 4.9 GHz, 6.0 +/- 0.3 mJy; 8.5
GHz, 6.6 +/- 0.2 mJy; 14.9 GHz, 6.9 +/- 0.6 mJy. The NRAO VLA Sky
Survey (NVSS; Condon et al. 1998, A.J. 115, 1693) shows no source
at 1.4 GHz in 1995, in an image with an rms noise of 0.45 mJy/beam.
Further radio observations are planned, and observations at other
wavelengths are urgently requested.
(C) Copyright 2003 CBAT
2003 April 2 (8105) Daniel W. E. Green
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