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THE ASTRONOMER Electronic Circular No 1518      2000 Apr 30 11.36UT
Ed:Guy M Hurst, 16,Westminster Close, Kempshott Rise,  Basingstoke,
Hants, RG22 4PP,England.Telephone/FAX(01256)471074Int:+441256471074
INTERNET: GUY@TAHQ.DEMON.CO.UK             GMH at AST.STAR.RL.AC.UK
WORLD WIDE WEB                    http://www.demon.co.uk/astronomer
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CI AQUILAE (Q2000/256)
Kesao Takamizawa, Saku-machi, Nagano, Japan, reports his
discovery of an apparent nova (mag 10.0) on unfiltered 5-min T-Max
400 film exposures taken on Apr. 28.669 and 28.673 UT with twin
0.10-m f/4 patrol cameras, giving the star's position as:
R.A. = 18h52m02s.0, Decl. = -1 28'14" (equinox 2000.0).  Nothing
appears on Takamizawa's earlier patrol films from 1994 May 12 to
2000 Apr.11 (limiting mag 13.5-15.0).  T. Kato, Kyoto University,
reports that Minoru Yamamoto, Aichi, independently discovered this
object at mag 9.8 on a T-Max 400 exposure taken on Apr. 28.694.
Visual magnitude estimates forwarded by Kato: Apr. 29.654, 9.8 (S.
Takahashi, Shiga); 29.708, 10.0 (H. Hirosawa, Aichi); 29.731, 9.3
(H. Maehara, Saitama).  It is uncertain if this star is identical
with the suspected 1917 nova (peak m_pg about 11) and eclipsing
binary (IBVS 4232, 4338) CI Aql, which has position end figures
03s.66, 38".7 (via Reinmuth 1925, A.N. 225, 385) and appears
identical with an R about 15.7 red star that is present in the
USNO-A2.0 star catalogue (position end figures 03s.56, 38".9).

M. Uemura and T. Kato, Kyoto University, report that they
obtained low-dispersion spectra (range 430-730 nm) of the new star
on Apr. 29.6 UT with the Okayama Astrophysical Observatory 1.88-m
telescope.  H-alpha emission, whose FWHM is about 2300 km/s, is
prominent and H-beta is also detected.  The spectrum is similar to
those of fast novae a few weeks after maximum.  The Balmer lines
show no P-Cyg profiles.  These spectral features indicate that the
outbursting object is a fast nova at a slightly evolved stage.
IAUC 7409

Editor:
Following issue of the above IAUC, H. Yamaoka, Kyushu University,
reports the accurate position of the object measured with the
unfiltered CCD image taken with Bisei 1.01-m telescope by K. Ayani,
Bisei Astronomical Observatory, and K. Shirakami, Okayama, Japan,
as R.A. = 18h52m03s.55, Decl. = -01o28'38".9 (equinox 2000.0,
uncertainty around 0".2).

Given the end figures from this measurement agree closely with
those for CI Aquilae it seems likely the present event is a
recurrence of the 1917 object.

Please note the Internet has a considerable number of messages
referring to this object as Nova Aquilae 2000. To our knowledge
this designation was not assigned in IAUCs and should not be
used.

Guy M Hurst