[Iaude] CBET 4506: 20180411 : NOVA IN SAGITTARIUS = PNV J18040967-1803581

quai at eps.harvard.edu quai at eps.harvard.edu
Wed Apr 11 10:17:03 EDT 2018

                                                  Electronic Telegram No. 4506
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 IN SAGITTARIUS = PNV J18040967-1803581
[Editor's note:  This text replaces that on CBET 4505 (Nakamura's report).]
     S. Nakano, Sumoto, Japan, reports the independent discoveries of a
possible nova by T. Kojima (Tsumagoi, Gunma-ken, Japan) and H. Nishimura
(Kakegawa, Shizuoka-ken, Japan).  Kojima found the new variable at mag 11.2
on six unfiltered 5-s frames (limiting mag 12.5) taken on Apr. 8.723 UT with
a Canon EOS 6D digital camera (+ 200-mm-f.l. f/3.2 lens); he measured the
variable's position as R.A. = 18h04m09s.67, Decl. = -18d03'58".1 (equinox
J2000.0).  Kojima's discovery image has been posted at the following website
URL:  http://www.oaa.gr.jp/~oaacs/image/PNVSgr2018K.JPG.  Nishimura also
found this star at mag 11.2 on five 10-s frames (limiting mag 14.3) taken
on Apr. 8.728 with the same camera set-up; he provided position end figures
09s.46, 57".3.  Nishimura's discovery image has been posted at website URL
http://www.oaa.gr.jp/~oaacs/image/PNVSgr2018N.JPG.  The variable was given
the provisional designation PNV J18040967-1803581 when Nakano posted it at
the Central Bureau's TOCP webpage.  P. Schmeer, Saarbruecken-Bischmisheim,
Germany, writes that he has identified a Pan-STARRS DR1 source (magnitude g
= 20.95) at position end figures 09s.449, 55".85 as the possible progenitor,
adding that he found no previous outbursts or eruptions in images taken by
the ASAS-SN Sky Patrol since Feb. 2015, with the latest available exposure
taken on 2018 Mar. 29.605 (limiting V mag 16.1).
     Additional CCD magnitudes (unfiltered unless noted otherwise) for PNV
J18040967-1803581:  Mar. 27.767, [13.2 (Kojima); 30.786, [13 (Yuji Nakamura,
Kameyama, Mie, Japan; CCD camera with 135-mm-f.l. f/4.0 telephoto lens; Apr.
7.723, [14 (Nishimura); 8.788, 11.3 (Nakamura; reported as independent
discovery after initial TOCP posting by Nakano; limiting mag 13; position
end figures 09s.5, 04'01"; communicated by M. Soma, National Astronomical
Observatory of Japan); 8.927, V = 11.74, B = 13.63 (Vikrant Kumar Agnihotri,
Rawatbhata, India; communicated by R. Fidrich, Budapest, Hungary);
9.448, 9.5 (G. Masi and M. Schwartz, remotely using a 40.6-cm f/3.75 robotic
telescope at Tenagra Observatories near Nogales, AZ, USA; 5-s exposures;
position end figures 09s.46, 55".6); 9.644, B = 13.23, V = 11.01, R_c = 9.80,
I_c = 8.52 (S. Kiyota; remotely with an iTelescope 0.50-m f/4.5 CDK astrograph
at Siding Spring, NSW, Australia); 9.676, 9.7 (T. Noguchi, Chiba-ken, Japan;
0.23-m f/10 Schmidt-Cassegrain reflector; position end figures 09s.47, 55".9;
image posted at URL http://park8.wakwak.com/~ngc/images/PNVinSgr_20180409.jpg;
communicated by Nakano); 9.754, B = 12.99 (A. Pearce, Nedlands, W. Australia;
0.5-m f/6.8 telescope at Siding Spring); 9.756, V = 10.83 (Pearce; position
end figures 09s.46, 55".7); 9.757, I = 8.12 (Pearce); 9.803, V = 10.87, R_c =
9.62, I_c = 8.30 (K. Yoshimoto, Yamaguchi-ken, Japan; remotely with a 0.50-m
f/6.8 reflector at Siding Spring; position end figures 09s.46, 55".9;
communicated by Nakano; image posted at the following website URL:
     Visual magnitude estimates provided by E. O. Waagen, AAVSO:  Apr. 10.191
UT, [9.1 (C. Adib, Porto Alegre, Brazil); 10.360, 11.1 (A. Amorim,
Florianapolis, Brazil); 10.419, 11.0 (L. Shotter, Uniontown, PA, USA).
     H. Akazawa (Funao Astronomical Observatory, Kurashiki, Okayama, Japan)
reports that low-dispersion (resolution about 400) spectra taken on Apr. 9.827
UT with a 35-cm telescope show an H-alpha emission line with a P-Cyg profile.
K. Ayani (Bisei Astronomical Observatory) measured Akazawa's data and found
that the absorption trough of the H-alpha line is blueshifted about 1100 km/s
with respect to the emission peak.  The spectrum can be viewed at website URL

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

                         (C) Copyright 2018 CBAT
2018 April 11                    (CBET 4506)              Daniel W. E. Green

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