Central Bureau for Astronomical Telegrams

IAUC 8369: N Sco 2004; UNUSUAL CATACLYSMIC Var IN Her

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 8368 Read IAUC 8370

View IAUC 8369 in .dvi or .ps format.

IAUC number

---

                                                  Circular No. 8369
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
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)


NOVA SCORPII 2004
     G. Pojmanski, Warsaw University Astronomical Observatory,
reports the discovery of a variable star on 'All Sky Automated
Survey' images obtained with a 65-mm-aperture (180-mm-focal-length
f/2.8) telephoto lens at Las Campanas on July 3.146 (at V = 11.98)
and 5.239 UT (V = 11.19), with the position of the variable given
as R.A. = 17h12m51s.3, Decl. = -30o56'39" (equinox 2000.0; CCD
pixel size 14".8).  Pojmanski reports that nothing was visible at
this location on an ASAS image taken on June 27.219 (limiting mag V
approximately 14.0).  H. Yamaoka, Kyushu University, reports his
measures for the new object from an image taken by G. Bolt
(Craigie, Australia), yielding position end figures 51s.28, 37".6
(82 UCAC-2 reference stars; fitting error about 0".15 for each
coordinate); Yamaoka adds that the nearest star visible in DSS
images (and listed in the GSC 2.2 and 2MASS catalogues) is about 1"
from this position.  D. Nogami, Hida Observatory, Kyoto University,
finds that there is no known x-ray source within 30" of the ASAS
position, which suggests that it is not a dwarf nova.  Nogami adds
that a spectrum of the new object, taken by M. Fujii (Bisei,
Okayama, Japan) on July 6.51, shows prominent Balmer emission lines
(FWHM about 500 km/s for H_alpha, with possible P-Cyg profile); Na
D absorption on a flat continuum is also clearly detected, which
suggests moderate reddening.  Nogami suggests that the spectrum
resembles that of the slow nova V723 Cas (= N Cas 1995) during the
pre-maximum halt phase (Iijima et al. 1998, A.Ap. 338, 1006).
Additional magnitude estimates (partially forwarded by Yamaoka;
visual unless noted otherwise):  July 4.985, [11.8 (W. Liller, Vina
del Mar, Chile, Technical Pan film + orange filter); 5.645, 11.3
(Bolt, unfiltered CCD; 0.06-mag rise in 2.7 hr); 6.052, R = 11.0
(P. Cacella, Brasilia, Brazil; CCD); 6.234, V = 10.92 (Pojmanski);
6.281, 11.1 (M. Linnolt, Honolulu, HI); 6.413, 10.8 (J. Bedient,
Honolulu, HI); 6.463, B = 11.62, V = 10.83, R_c = 10.41, I_c =
10.00 (S. Kiyota, Tsukuba, Japan); 6.567, 10.9 (Y. Maeda, Nagasaki,
Japan); 6.616, B = 11.44, V = 10.83, R_c = 10.33, I_c = 9.91 (H.
Maehara, Saitama, Japan).


UNUSUAL CATACLYSMIC VARIABLE IN HERCULES
     CCD magnitudes by B. E. Schaefer, Louisiana State University,
via the Cerro Tololo 1.0-m telescope, for the variable on IAUC
8363:  July 1.198 UT, U = 15.03, B = 15.87, V = 15.68, R = 15.24,
I = 14.37; 3.250, 15.46, 16.31, 16.03, 15.44, 14.48; July 5.183,
15.20, 15.96, 16.03, 15.54, 14.52.

                      (C) Copyright 2004 CBAT
2004 July 6                    (8369)            Daniel W. E. Green

---

Read IAUC 8368 Read IAUC 8370

View IAUC 8369 in .dvi or .ps format.

---

Our Web policy. Index to the CBAT/MPC/ICQ pages.