IAU Central Bureau for Astronomical Telegrams

Central Bureau for Astronomical Telegrams -- Image credits

CBAT "Transient Object Followup Reports"

TCP J18001854-3533149

TCP J18001854-3533149   2016 03 16.8449*  18 00 18.54 -35 33 14.9  12.2 U             Sgr       N 0

2016 03 16.8449*

Koichi Nishiyama, Kurume,Japan and Fujio Kabashima, Miyaki,Japan report a discovery of TCPobject (mag.= 12.2) in Sgr on two 40-s unfiltered CCD frames taken around 2016 Mar. 16.84493 UT ( limiting magnitude=13.5 ), using a 135-mm f/4 camera lens (+FLI 09000 camera). We have confirmed immediately the appearance of our discovery this TCPobject on five 3-s unfiltered CCD frames taken around 2016 Mar 16.85167 UT ( limiting magnitude=17.3 ), using a 0.50-m f/6.8 reflector (+FLI 1001E camera). (lens magnitude of referred catalogue Hipparcos, others reference catalogue GSC-ACT) Nothing is visible at this location on two past survey frames taken on 2016 Mar 02.858 UT(limiting mag.= 12.7 ) and 14.844 UT (limiting mag.= 13.2) nor on DSS, USNO-B1.0, We have checked in Minor Planets. nearest star in USNO B1.0 has position end figures 18s322, 14"97, distance 2"7, magnitudes R1=16.12 I=15.95

2016 03 17.4747

I took confirmation image of this transient object with 0.50-m f/4.5 CDK astrograph + FLI-PL11002M CCD of iTelescope.NET at Mayhill, NM, USA, remotely. Photometry results were B=11.83, V=11.92, Rc=11.95 and Ic=12.06. Spectroscopy will be encourage to reveal nature of this object as it has blue color. It might be CVs rather than classical nova. My image is available at http://meineko.sakura.ne.jp/ccd/TCP_J18001854-3533149.jpg. Seiichiro Kiyota (Kamagaya, Japan)

2016 03 20.8

Kazuya Ayani, Bisei Astronomical Observatory (BAO), Ibara, Okayama, Japan, reports that a low-resolution spectrogram (range 400-800 nm; resolution 0.5 nm at H-alpha) of this TCP was obtained with the BAO 1.01-m telescope. It shows H-beta, H-gamma, H-delta absorption lines on a blue continuum. Presence of H-alpha line is not clear probably because the absortion is filled with the emission. These imply that it may be a dwarf nova rather than a classical nova. The spectrum can be viewed via website URL http://www.bao.city.ibara.okayama.jp/astro/2016/tcp/TCP_J18001854-3533149_Mar20.png.

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