NOVA SAGITTARII 2014
Sigeru Furuyama, Japan reports discovery of a possible magnitude 8.7 nova in
Sgr on two 10-s CCD frames (limiting magnitude 12.5) of 2014 Jan. 26.85UT
using a 200-mm f/2.8 camera lens + BJ-42L camera.
It is located at; RA 18h25m08s.60 DEC -22d 36' 02.4" (2000). Nothing was
visible on numerous patrol frames of the same field taken since 2012 August.


Additional CCD magnitudes: 2014 Jan. 27.847, 9.6 (Toshihide Noguchi, Japan;
0.23-m f/6.3 Schmidt-Cassegrain reflector, end figures 08s.76, 02".6; UCAC4
catalogue), 28.876, V = 10.19, R_c = 9.72, I_c = 9.15 (Seiichiro Kiyota,
Japan; 0.25-cm Schmidt-Cassegrain telescope); Feb. 2.862, 10.7 (Ken-ichi
Kadota, Japan; 0.25-m f/5 reflector, end figures 08s.74, 02".9; image posted
at http://members.jcom.home.ne.jp/kenic-k/i...gr-20140202.jpg
07.399, 11.172 +/-0.012 V (Hambsch); 08.300, 11.1 (Amorim); 09.399, 10.604
+/-0.012 V (Hambsch);

Andrew Pearce, Nedlands, Western Australia, reports the following visual
magnitude estimates Jan. 28.839, 10.5; Feb. 8.834, 10.9, 9.828, 10.8
(Pearce); 10.851, 9.8.

Akira Arai, Nishi-Harima Astronomical Observatory, University of Hyogo,
reports that a low-dispersion spectrogram was obtained on Jan. 30.87 UT
using the 2-m Nayuta telescope (+ MALLS). The spectrum shows emission lines
at H-alpha (FWHM about 1200 km/s; EW about -70 nm), H-beta (EW about -13
nm), Na D, Fe II (multiplets 42, 48, 49, 55, 74), [O I] (557.7- 630.0-, and
636.4-nm), O I (777.3- and 844.6-nm), and the Ca II infrared triplet on a
highly reddened continuum emission. Tiny absorption features are seen with
the H-alpha and O I lines at about -1200 and -700 km/s, respectively. These
results indicate that the object is a "Fe II"-type classical nova past
maximum.

V809 CEPHEI
Nick James reports it is just over a year since the discovery of the nova
V809 Cep. He imaged it again on 2014 Feb 13 in V, Rc, Ic. The estimated mag
is around Rc=18.2 using UCAC-4. The nova is also visible in the Ic frame but
not V which has an LM of around 18.3.
The nova is quite difficult to measure since it is only around 10 arcsec
from a V=16.6 star.