[Iaude] CBET 4492: 20180312 : NEW NOVA IN OPHIUCHUS = TCP J17140253-2849233 = PNV J17140261-2849237

quai at eps.harvard.edu quai at eps.harvard.edu
Mon Mar 12 16:14:44 EDT 2018


                                                  Electronic Telegram No. 4492
Central Bureau for Astronomical Telegrams
Mailing address:  Hoffman Lab 209; Harvard University;
 20 Oxford St.; Cambridge, MA  02138; U.S.A.
e-mail:  cbatiau at eps.harvard.edu (alternate cbat at iau.org)
URL http://www.cbat.eps.harvard.edu/index.html
Prepared using the Tamkin Foundation Computer Network


NEW NOVA IN OPHIUCHUS = TCP J17140253-2849233 = PNV J17140261-2849237
     Several observers have independently discovered a new nova in Ophiuchus.
S. Nakano, Sumoto, Japan, reports the discovery by Hideo Nishimura
(Kakegawa, Shizuoka-ken, Japan) of the variable at mag 9.5 on three unfiltered
CCD images obtained on Mar. 10.805 UT with a Canon EOS 6D digital camera (+
200-mm-f.l. f/3.2 lens, the position given as R.A. = 17h14m02s.61, Decl. =
-28d49'23".7 (equinox J2000.0).  Nakano also forwards the discovery of the
variable at mag 9.5 by Tadashi Kojima (Tsumagoi, Gunma-ken, Japan) on six
images taken on Mar. 10.807 using an identical camera and lens system,
providing position end figures 02s.50, 23".5.  Nishimura's image was posted
at website URL http://www.oaa.gr.jp/~oaacs/image/PNVinOph2018.jpg.  The
designation PNV J17140261-2849237 was given the variable when Nakano posted
the report at the Central Bureau's TOCP webpage.
     Koichi Nishiyama and Fujio Kabashima report their discovery of the
apparent nova at mag 9.5 on two 40-s unfiltered CCD frames (limiting magnitude
13.3) taken around Mar. 10.814 UT using a 120-mm-f.l. f/4 camera lens (+ FLI
09000 camera); they confirmed the presence of the new variable on five 10-s
unfiltered CCD frames (limiting magnitude 18.3) taken around Mar. 10.830
using a 0.50-m f/6.8 reflector (+ FLI 1001E camera), providing precise
position end figures 02s.53, 23".3 (reference stars from Hipparcos and
GSC-ACT catalogues).  They add that nothing is visible at this position
on the Digitized Sky Survey.  The designation TCP J17140253-2849233 was given
the variable when their report was posted at the Central Bureau's TOCP
webpage, prior to Nakano's posting the discovery by Nishimura and Kojima.
     Additional CCD magnitudes for TCP J17140253-2849233 = PNV
J17140261-2849237:  Mar. 2.836 UT, [14.7 (Nishimura); 3.812, [12.0 (Kojima);
3.815, [13.3 (Nishiyama and Kabashima); 9.813, 10.9 (Nishiyama and Kabashima;
limiting mag 13.2); 11.827, B = 10.22, V = 9.54, R_c = 9.09, I_c = 8.66 (K.
Yoshimoto, Yamaguchi-ken, Japan, 0.20-m Ritchey-Chretien reflector; position
end figures 02s.55, 23".7; communicated by Nakano; image posted at website
URL http://orange.zero.jp/k-yoshimoto/TCP_J17140253-2849233.jpg); 10.753, 9.5
(A. Takao, Kitakyusgu, Japan; unfiltered images); 11.676, B = 10.06 (S.
O'Connor, St. George, Bermuda; communicated by E. O. Waagen, AAVSO); 11.677,
V = 9.42 (O'Connor); 11.678, I = 8.45 (O'Connor); 11.696, B = 10.05, V = 9.53,
R_c = 9.32, I_c = 8.99 (S. Kiyota, Kamagaya, Japan, using an iTelescope
0.43-m f/6.8 CDK astrograph at Siding Spring Observatory, NSW; image posted at
http://meineko.sakura.ne.jp/ccd/TCP_J17140253-2849233.jpg).  Visual magnitudes
for PNV J17140261-2849237 by A. Amorim, Florianapolis, Brazil, as communicated
by Waagen:  Mar. 11.228, 9.5; 11.297, 9.4; 12.324, 9.3.
     P. Schmeer notes that TCP J17140253-2849233 = PNV J17140261-2849237 is
in a crowded star field, adding that the most recent ASAS-SN Sky Patrol
Observation (cf. Shappee et al. 2014, Ap.J. 788, 48; Kochanek et al. 2017,
PASP 129, 4502) shows nothing at the position of the variable on 2018 Mar.
6.362 UT (thus fainter than mag 15.5), and no previous outbursts/eruptions
detected by ASAS since 2016 March.
     H. Yamaoka, National Astronomical Observatory of Japan, informs the
Central Bureau that TCP J17140253-2849233 = PNV J17140261-2849237 has been
confirmed as a Galactic nova by S. C. Williams et al. (as posted at website
URL http://www.astronomerstelegram.org/?read=11398); their spectroscopy (range
390-510 and 590-800 nm; resolution about 5400) obtained with the 2-m
Liverpool Telescope at the Observatorio del Roque de Los Muchachos, Spain,
shows strong Balmer lines exhibiting P-Cyg profiles (maximum velocity of
-1200 km/s from the H_alpha absorption component).  Among the numerous
spectral lines, there are several Fe II lines seen mainly in absorption,
suggesting that this is an "Fe II"-type nova in the early stages of eruption.
No date or time was given for the obsrvation, but their report was reportedly
posted on Mar. 11.46 UT.


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

                         (C) Copyright 2018 CBAT
2018 March 12                    (CBET 4492)              Daniel W. E. Green



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