[Iaude] CBET 4489: 20180225 : NOVA IN OPHIUCHUS = PNV J17244011-2421463

quai at eps.harvard.edu quai at eps.harvard.edu
Sat Feb 24 21:03:41 EST 2018


                                                  Electronic Telegram No. 4489
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


NOVA IN OPHIUCHUS = PNV J17244011-2421463
     S. Nakano, Sumoto, Japan, reports the discovery of a possible nova (mag
12.5) by Tadashi Kojima (Tsumagoi, Gunma-ken, Japan) on three 5-s exposures
(limiting mag 13.5) taken on Feb. 12.834 UT with a Canon EOS 6D digital
camera (+ 200-mm-f.l. f/3.2 lens), giving the position of the variable as
R.A. = 17h24m40s.11, Decl. = -24d21'46".3 (equinox J2000.0) and adding that a
nearby star (mag 15.6) has position end figures 39s.95, 47".0.  The variable
received the provisional designation PNV J17244011-2421463 when it was posted
at the Central Bureau's TOCP webpage.
     Additional magnitudes for PNV J17244011-2421463 reported to the Central
Bureau:  2017 Apr. 27 UT, [14.0 (Kojima); Feb. 8.844, [12.0 (Kojima); Feb. 13,
B = 14.05, V = 12.87, I = 10.87 (K. Yoshimoto, Yamaguchi-ken, Japan; remotely
with a 0.25-m f/3.4 reflector near Mayhill, NM, USA; I-band image posted at
URL http://orange.zero.jp/k-yoshimoto/PNV-J17244011-2421463_20180213.jpg;
position end figures 39s.93, 47".4; communicated by Nakano); 13.474, 11.9
(L. Shotter, Uniontown, PA, USA; visual; forwarded by E. O. Waagen, AAVSO);
13.72, B = 14.22, V = 12.86 ((S O'Connor, St. George, Bermuda; forwarded by
Waagen); 13.742, V = 12.84 (A. Pearce, Nedlands, W. Australia; remotely with
an iTelescope 0.43-m f/6.8 reflector at Siding Spring; position end figures
39s.92, 47".2); 13.840, 12.7 (Pearce; visual); 14.848, 12.6 (Pearce; visual);
15.8451, 13.0 (Pearce; communicated by Waagen); 16.744, V = 12.88 (Pearce;
communicated by Waagen); 16.745, B = 14.20 (Pearce; communicated by Waagen);
16.76, R = 11.82, I = 10.82 (O'Connor; communicated by Waagen); 21.842, 13.1
(Pearce; communicated by Waagen).
     H. Maehara, Okayama Observatory, Kyoto University, reports that CCD
images obtained in the course of Kamogata Wide-field Survey (KWS) with a
105-mm-f.l. f/2.0 lens (+ SBIG ST-8ME camera for V band and SBIG STT-1603ME
camera for I_c band) yield the following magnitudes for PNV J17244011-2421463:
2018 Feb. 5.868 UT, I_c = 11.7; 12.870, V = 12.9; 12.871, I_c = 11.7.  Maehara
add that, according to the ASAS-SN light curve, the outburst of this variable
started in 2017 September (light curve viewable via the following website URL:
https://asas-sn.osu.edu/light_curves/bd9f4922-8561-4b5c-a04c-fab2c03dfa94),
noting that the object is listed as an H-alpha emission-line star (KW 011
519-33) by Kohoutek and Wehmeyer (2003, AN 324, 437).
     Despite the above from Maehara, a report posted by E. Aydi et al. (at
website URL http://www.astronomerstelegram.org/?read=11338) states that a
spectrogram obtained of PNV J17244011-2421463 on Feb. 23.127 UT with the 11-m
South African Large Telescope (range 380-890 nm; resolution 14000) reveals
emission lines that are characteristic of a classical "Fe II"-type nova that
is possibly evolving toward the nebular phase.  They note FWZI around 1300
km/s for H-alpha and H_beta.
     M. Yamanaka, M. Kawabata, T. Nakaoka, Hiroshima University, write that
they performed spectroscopic observations (resolution 400; range 450-900 nm)
of PNV J17244011-2421463 using the 1.5-m Kanata telescope (+ Hiroshima
One-shot Wide-field Polarimetry at the Higashi-Hiroshima Astronomical
Obesrvatory on Feb. 21.8 UT.  The spectra exhibit the H-alpha line in strong
emission, with full-width-at-zero-intensity (FWZI) = 2200 km/s.  There are
no absorption lines in the spectra.  The slope of the continuum indicates a
red color.  These were possibly consistent with the outburst event of the
progenitor emission-line star (Kohoutek and Wehmeyer 2003, AN 324, 437).
The relatively narrow line width of H-alpha is consistent with this being
an "Fe II"-type classical nova.


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

                         (C) Copyright 2018 CBAT
2018 February 25                 (CBET 4489)              Daniel W. E. Green



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