[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:
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

More information about the Iaude mailing list