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THE ASTRONOMER Electronic Circular No 2834      2012 Jun 30 16.48UT
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      Backup: gmh@wdcc1.bnsc.rl.ac.uk
WORLD WIDE WEB                         http://www.theastronomer.org
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NOVA SAGITTARII 2012 No. 3
K. Itagaki , Japan reports discovery of a possible mag 10.3 nova on an 
unfiltered CCD image taken on 2012 June 26.5494 UT with a 0.21-m 
reflector, located at:
RA 17h 52m 25.79s DEC -21 26' 21.5" (2000); which he confirmed on June 
26.565 at mag 10.2 (0.60-m reflector).

Additional CCD magnitudes: June 25.666, [16.0 (Itagaki); 26.540, 9.9 
(Sakurai, Japan; independent discovery on four 20-s frames taken with a 
Fuji FinePix S2 Digital Camera + Nikon 180-mm f/2.8 lens; position end 
figures 25s.59, 22".9); 26.640, 10.0 (Itagaki); June 27.192, 9.0 
(Jacques and Pimentel, 0.25-m f/3.4 astrograph + clear filter at the RAS 
Observatory Mayhill).

L. Kiss et. al., Konkoly Observatory, Hungary, report an optical 
spectrogram of June 26.95 UT does not contain any strong emission lines, 
with a clearly identifiable H-beta line in absorption and a strong 
interstellar absorption of the sodium D doublet.  The H-alpha line is 
possibly seen in absorption.  Two narrow emission lines are also visible 
around 575.0 nm, each with FWZI about 60 km/s.  The spectrum apparently 
excludes the nova nature of the object, which is presumably a dwarf nova 
in outburst phase.  The estimated visual brightness of the target was 
about mag 9.5, based on the guider image.

Kazuyoshi Imamura reports a low-resolution spectrum of June 28.593 UT 
shows broad and prominent emission lines of the Balmer series, He I 
(706.5-nm), O I (777.3-nm), and Mg II (788.0-nm) can be seen. The Balmer 
lines show asymmetrical profiles; the FWHM of H-alpha is approximately 
4100 km/s.  From this result, the variable is thought to be a classical 
nova with a large expansion velocity.

Hiroyuki Maehara reports a spectrum of June 28 suggests the object is a 
classical nova. Christian Buil reports a spectrogram of June 28.864 UT 
reveals it to have a nova-like nature

Ulisse Munari, Padova Astronomical Observatory, using the 1.22-m Asiago 
telescope on June 28.95 UT finds the spectrum to be that of a nova of 
the He/N type, with hydrogen Balmer and He I in strong emission.  The 
FWHM of the emission lines is 4500 km/s.  The object appears to be 
heavily reddened, with strong interstellar Na I lines visible in 
absorption.

SUPERNOVA 2012ce (MCNAUGHT ET. AL.)
2012ce  May 14.49   11 13 49.46  -29 55 32.0  16.6   7.0"E    2.2"S
G. H. Marion: spectrum May 15 type-Ia about one week after maximum
A good fit is found to the template of supernova 1995D at +6 days.

SUPERNOVA 2012cf IN PGC 48432 (L. COX ET. AL.)
2012cf  May 14.17   13 41 10.49  +30 22 37.2  17.3   8.7"W    4.8"S
G. H. Marion: spectrum May 17 type-Ia a few days before maximum.
A good fit is found to SN 2002er at 4 days before maximum.

SUPERNOVA 2012cg IN NGC 4424 (LOSS)
2012cg  May 17.22   12 27 12.83  +09 25 13.2  16.9  17.3"E    1.5"S
S. B. Cenko: spectrum May 18 shows that 2012cg is probably a very young 
type-Ia supernova.
Guy Hurst, using the 0.61-m Cassegrain of Sierra Stars measures the 
following V magnitudes: May 24, 13.0; May 28, 12.4; June 15, 12.3; June 
20, 12.5; June 23, 12.9 (sequence AAVSO AA7546AY).

Guy M Hurst