[Iaude] CBET 4320: 20160909 : NOVA SCORPII 2016 No. 2 = PNV J17225112-3158349

quai at eps.harvard.edu quai at eps.harvard.edu
Fri Sep 9 14:27:45 EDT 2016

                                                  Electronic Telegram No. 4320
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)
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Prepared using the Tamkin Foundation Computer Network

NOVA SCORPII 2016 No. 2 = PNV J17225112-3158349
[Editor's note:  this text replaces that on CBET 4319]
     M. Soma, National Astronomical Observatory of Japan, Mitaka, Tokyo,
reports the discovery by Shigehisa Fujikawa (Kan'onji, Kagawa, Japan) of an
apparent nova (mag 11.6) on unfiltered images obtained on Sept. 6.481 UT with
a 120-mm-f.l. f/3.5 camera lens; the variable's position was given as R.A. =
17h22m51s.12, Decl. = -31d58'34".9 (equinox 2000.0).  The variable was
designated PNV J17225112-3158349 when it was posted at the Central Bureau's
TOCP webpage.
     Laura Chomiuk, Department of Physics and Astronomy, Michigan State
University (MSU), reports the independent discovery of this apparent nova
(at magnitude V = 12.1) by a team of astronomers (including K. Z. Stanek,
C. S. Kochanek, J. S. Brown, T. W.-S. Holoien, J. Shields, and G. Simonian,
Ohio State University; B. J. Shappee, Hubble Fellow, Carnegie Observatories;
J. L. Prieto, Universidad Diego Portales, Santiago, and Millennium Institute
of Astrophysics; D. Bersier, Liverpool John Moores University; S. Dong, S.
Bose, and P. Chen, Kavli Institute for Astronomy and Astrophysics, Peking
University; L. Chomiuk and J. Strader, MSU; and J. Brimacombe, Cairns,
Australia) on Sept. 6.0 UT in the course of the V-band All-Sky Automated
Survey for Supernova (ASAS-SN) using the robotic 14-cm telescopes.  The
object was measured to be located at R.A. = 17h22m51s.43, Decl. =
-31d58'36".3 (equinox 2000.0).
     Additional CCD magnitudes for PNV J17225112-3158349:  Sept. 3.0 UT, [17.5
(ASAS-SN); 5, [12.9 (Fujikawa); 7.6, V = 11.4 (ASAS-SN); 8.062, V = 11.79,
I_c = 9.33 (S. Kiyota, Kamagaya, Japan; remotely with an iTelescope 0.61-m
f/6.5 CDK astrograph at the Sierra Remote Observatory, Auberry, CA, USA).
Visual magnitude estimates forwarded by E. O. Waagen, AAVSO:  Sept. 7.938,
11.8 (A. Amorim, Florianopolis, Brazil); 8.042, 11.9 (L. Camargo da Silva,
Brazil); 8.917, 11.9 (Amorim); 9.042, [11.6 (L. Shotter, Uniontown, PA, USA).
     A. Arai, Koyama Astronomical Observatory, Kyoto Sangyo University; and
S. Honda, Nishi-Harima Astronomical Observatory, University of Hyogo, obtained
low-resolution (R about 600) optical spectra (exposure time 1200 s) of PNV
J17225112-3158349 using the 2-m Nayuta telescope (+ MALLS spectrograph) on
Sept. 8.43 UT at the Nishi-Harima Astronomical Observatory.  The spectra show
significant emission lines at H-alpha, H-beta, H-gamma, Fe II (multiplets 41,
42, 49, 74), and O I (777.4, 844.6 nm), which are accompanied with P-Cyg
profiles, as well as the Ca II infrared triplets.  Emission lines at H-alpha
and O I (777.4-nm) have broad wings, with FWHM being about 1700 and 2000 km/s,
respectively.  The absorption minimum of the P-Cyg profiles in H-alpha and O I
(777.4-nm) are located at velocities of about -870 and -890 km/s,
respectively.  Furthermore, two weak absorption components are seen at
H-alpha at velocities of -1470 and -2270 km/s.  H-delta and Na I D lines
show only absorption features around the rest wavelength (equivalent width
about 0.13 and 0.08 nm, respectively), suggesting that the envelope gas of
the object is in an optically thick phase.  No helium lines were detected in
the spectra.  These results indicate that PNV J17225112-3158349 is an "Fe II"-
type classical nova around maximum light.

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

                         (C) Copyright 2016 CBAT
2016 September 9                 (CBET 4320)              Daniel W. E. Green

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