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IAUC 9140: V5586 Sgr = N Sgr 2010 No. 2

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                                                  Circular No. 9140
Central Bureau for Astronomical Telegrams
CBAT Director:  D. W. E. Green, Room 209; Department of
 Earth and Planetary Sciences; Harvard University;
 20 Oxford St.; Cambridge, MA  02138; U.S.A.
URL http://www.cfa.harvard.edu/iau/cbat.html  ISSN 0081-0304

     As first announced on CBET 2261, K. Nishiyama (Kurume, Japan)
and F. Kabashima (Miyaki, Japan) report their discovery of a
possible Milky Way nova (mag 11.2) on two unfiltered CCD frames
(limiting mag 13.2) taken around Apr. 23.782 UT using a 105-mm f/4
camera lens (+ SBIG STL6303E camera).  They used five deeper
unfiltered CCD frames taken around Apr. 23.791 with a Meade 0.40-m
reflector to measure the following precise position for the
variable:  R.A. = 17h53m02s.99 +/- 0s.01, Decl. = -28o12'19".4 +/-
0".1 (equinox 2000.0).  A USNO-B1.0-catalogue star of red mag 17.4
has position end figures 03s.11, 19".0.  Additional magnitudes for
the variable (via unfiltered CCD, and from Nishiyama and Kabashima,
unless noted otherwise):  1996 Sept. 12, [17.5 (Digitized Sky
Survey, red plate); 2010 Apr. 2.831, [12.9; 16.749, [13.1; 20.262,
[11.0 (W. Liller, Vina del Mar, Chile; Kodak TP film, orange filter,
85-mm camera lens); 24.660, 11.1 (T. Yusa, Osaki, Japan, 0.30-m
reflector; position end figures 02s.98, 19".3); 24.673, 11.6;
24.752, I_c = 10.21 (H. Maehara, Kwasan Observatory, Kyoto
University, 25-cm telescope + CCD); 24.754, R_c = 12.47 (Maehara);
24.755, V = 15.33 (Maehara).  Further observations appear on CBET
     L. A. Helton, T. Vonderharr, and C. E. Woodward, University of
Minnesota; and G. J. Schwarz, American Astronomical Society, report
on Boller-and-Chivens spectroscopic observations (range 380-930 nm;
resolution about 0.28 nm) of this object, obtained at the Steward
Observatory Bok 2.29-m telescope on Apr. 25.4 UT.  These
observations confirm that this is a post-maximum classical nova.
The spectra exhibit strong, broad H_alpha emission (FWHM about 4000
km/s) with a flux of F = 1.4 x 10**-11 erg/s/cm**2.  No other
emission lines are readily apparent blueward of H_alpha.  Permitted
emission from O I 844.6-nm (FWHM about 3350 km/s; F = 1.7 x 10**-11
erg/s/cm**2) and 777.3-nm (FWHM about 3400 km/s) dominates the red
spectrum.  H_alpha and O I 777.3-nm both have asymmetric line
profiles with a single blue peak.  The emission lines are
superimposed on a continuum that rises sharply to the red.  The
lack of any blue emission lines in the spectrum, along with the
climbing red continuum, suggests that this object is subjected to
an exceptionally high degree of extinction.  The red spectrum is
similar to that of Nova Pup 1991 (V351 Pup; Williams et al. 1994,
Ap.J. Suppl. 90, 297), which suggests that the remaining features
dominating the red spectrum are likely due to multiplet emission
from Mg II (1,7,8), N I (1,2,15), and Na I (19).
     E. Kazarovets, Russian Academy of Sciences, writes that the
permanent GCVS designation V5586 Sgr has been assigned to this nova.

                      (C) Copyright 2010 CBAT
2010 April 26                  (9140)            Daniel W. E. Green

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