Central Bureau for Astronomical Telegrams
IAUC 8176: 2003gw; 2003go; V4743 Sgr
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Circular No. 8176
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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CBAT@CFA.HARVARD.EDU (science)
URL http://cfa-www.harvard.edu/iau/cbat.html ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)
SUPERNOVA 2003gw IN UGC 3252
Further to IAUC 8173, M. Armstrong reports his discovery of an
apparent supernova on unfiltered CCD images taken on Aug. 7.114
(mag 17.1) and 7.945 UT (mag 17.3). SN 2003gw is located at R.A. =
5h11m47s.68, Decl. = +67o29'22".2, which is approximately 14" east
and 6" north of the center of UGC 3252. Nothing is visible at this
position on his images from 2000 Nov. 3 and 2003 Mar. 22 (limiting
mag 19.0) or on Palomar Sky Survey plates.
SUPERNOVA 2003go
Further to IAUC 8173, M. Hamuy, N. Morrell, J. Arias, and R.
Barba report that a spectrum (range 390-900 nm) of SN 2003go (cf.
IAUC 8168), obtained on July 30.30 UT with the Baade telescope,
shows it to be a type-IIn supernova with a blue continuum and
strong Balmer lines in emission, at a redshift of 0.051.
Superimposed, narrow, absorption-line components can be seen
blueshifted by about 600 km/s from the emission line cores of the
Balmer lines. A weak He I 587.6-nm emission is also present.
V4743 SAGITTARII
R. M. Wagner, LBT Observatory; S. G. Starrfield and J.
Rohrbach, Arizona State University; H. Bond, Space Telescope
Science Institute; A. Karam, University of Arizona; B. Monard,
Bronberg Observatory; G. Bolt, Craigie, Australia; and R. Ishioka,
M. Uemura, and T. Kato, Kyoto University, report: "A comparison of
optical photometry, obtained contemporaneously with Chandra x-ray
observations in April and July, reveals a substantial change in the
optical light curve of this classical nova and super-soft-x-ray
source. Unfiltered photometry obtained on July 18, 19, and 21 and
B-band photometry obtained at Cerro Tololo (1.3-m reflector +
AndiCam) on July 19 show a sinusoidal modulation of amplitude 0.2
mag with a period of 0.281 +/- 0.003 day, which is likely to be the
orbital period. Minimum light corresponds to JD 2452839.321.
Another variation with a period of 69 +/- 3 min is superposed on
the orbital modulation. Photometry obtained at Cerro Tololo with
the same equipment on seven nights between Apr. 5.3 and 20.4 UT
shows erratic variations that are not periodic or consistent with
the July results. No statistically significant variation is
detected near the x-ray period of 1325 s (Ness et al. 2003,
http://xxx.lanl.gov/abs/astro-ph/0308017) or at twice this period.
The recent photometric behavior is similar to some intermediate
polar cataclysmic variables. Additional observations are
encouraged."
(C) Copyright 2003 CBAT
2003 August 7 (8176) Daniel W. E. Green
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