Electronic Telegram No. 2818
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
CBAT Director:  Daniel W. E. Green; Hoffman Lab 209; Harvard University;
 20 Oxford St.; Cambridge, MA  02138; U.S.A.
e-mail:  cbatiau@eps.harvard.edu (alternate cbat@iau.org)
URL http://www.cbat.eps.harvard.edu/index.html
Prepared using the Tamkin Foundation Computer Network


CATACLYSMIC VARIABLE STAR IN DRACO = PNV J18422792+4837425
     S. Nakano, Sumoto, Japan, reports the discovery by Hideo Nishimura
(Miyawaki, Kakegawa, Shizuoka-ken, Japan) of a possible nova (mag 11.8) on two
10-s CCD frames (limiting magnitude 14.0) taken on Sept. 5.529 UT with a Canon
EOS 5D digital camera (+ Canon 200-mm f/3.2 lens) mounted on a Takahashi EM100
equatorial telescope at Mt. Kogasayama, Kakegawa.  The variable, which was
designated PNV J18422792+4837425 when posted on the Central Bureau's TOCP
webpage, is located at R.A. = 18h42m27.92, Decl. = +48d37'42".5 (equinox
2000.0); Nakano measured position end figures 28s.11, 41".5 (+/- 2") for
the variable and limiting mag 15.6 from Nishimura's confirming frame taken on
Sept. 5.695 with the same instrument.  Additional magnitudes for PNV
J18422792+4837425:  2011 Aug. 11, [13.5 (Nishimura); 24, [13.5 (Nishimura);
Sept. 7.450, 12.4 (T. Noguchi, Katori, Chiba-ken, Japan; 0.23-m Schmidt-
Cassegrain reflector + unfiltered BITRAN BT-11E CCD camera; position end
figures 28s.01, 41".5; via Nakano).  Toru Yusa, Osaki, Japan, has posted an
image of PNV J18422792+4837425 at the following website URL:
http://space.geocities.jp/yusastar77/PNV_110906.htm.

     U. Munari, Istituto Nazionale di Astrofisica, Padova Astronomical
Observatory, reports that he acquired a spectrogram of PNV J18422792+4837425,
which is visible where the Palomar Sky Survey images show an empty field.
Munari's spectrogram (resolution 0.23 nm/pixel; range 320-780 nm) was taken
on Sept. 6.841 UT with the 1.22-m telescope of the Asiago Astrophysical
Observatory.  The spectrum is dominated by an absorption continuum similar
to that of an A-type star -- with H_alpha in emission, filling in the
corresponding absorption, and H_beta appearing as an emission core within
the absorption profile.  The H_alpha and H_beta emission lines are very sharp
(gaussian-like), not wider than the instrumental profile.  Overall, the
spectrum is very typical of a cataclismic variable close to maximum
brightness.


NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
      superseded by text appearing later in the printed IAU Circulars.

                         (C) Copyright 2011 CBAT
2011 September 11                (CBET 2818)              Daniel W. E. Green