IAU Central Bureau for Astronomical Telegrams

Central Bureau for Astronomical Telegrams -- Image credits

CBAT "Transient Object Followup Reports"

PNV J16364440-4132340

PNV J16364440-4132340   2011 09 06.4313*  16 36 44.40 -41 32 34.0   9.7 C             Sco       0 8



2011 09 06.4313

Discovery Observation by Y. Nakamura, Kameyama, Mie, Japan, with CCD camera + f.l.135-mm lens. Position accuracy is about 30". Five images caught this object. Image taken on Aug. 29.451 UT does not detect the object (limiting mag 12.0).




2011 09 07.5046

We performed some follow-up of this object remotely through the 2.0-m f/10.0 Ritchey-Chretien + CCD of "Faulkes Telescope South" (MPC Code - E10). On our images taken on September 07.50, 2011 we can confirm the presence of an optical counterpart with filtered R-Bessel CCD magnitude 9.1 (USNO-B1.0 Catalogue reference stars) at coordinates: R.A. = 16 36 44.29, Decl.= -41 32 37.7 (equinox 2000.0; USNO-B1.0 catalogue reference stars). According to VIZIER there is a 15.08 R1 magnitude star at 0.060 arcseconds from the transient position (USNO-B1.0 0484-0459316). An animation showing a comparison between our confirmation image and the archive POSS2/UKSTU plate (R Filter - 1997): http://bit.ly/ojz76D Our BRV image: http://bit.ly/oKyFo6 Ernesto Guido, Nick Howes and Giovanni Sostero




2011 09 07.5256

I confirmed this possible nova using 31.7cm Ritchey-Chretien telescope(fl=1910mm)+SBIG ST-10 camera at Officer, Australia(Global-rent-a-scope). Photometric results are 11.88B, 10.73V, 9.75Rc and 8.77Ic on 7.5256-7.5288 Sep. 2011 UT. Position end figures are 44.28 and 37.58. (Seiichiro Kiyota, Tsukuba, Japan) http://meineko.sakura.ne.jp/ccd/PNV_J16364440-4132340-110907.jpg




2011 09 07.42

We performed low-resolution optical spectroscopic observations (R about 580) of PNV J16364440-4132340 on 2011 Sep. 7.42 using Araki telescope at Koyama Astronomical Observatory. The spectrum exhibits broad Balmer emissions and Fe II multiplet emissions on a highly reddened continuum light. The H-alpha emission line shows an asymmetric profiles with the FWZI about 6000 km/s. Other significant features are invisible in our spectrum. These results suggests that the object is an Fe II-type classical nova highly reddened by interstellar medium. ( http://www.cc.kyoto-su.ac.jp/~kao/blog/index.php/view/127 ) A. Arai, T. Kajikawa, C. Naka, Kyoto Sangyo University, Japan.




2011 09 09.406

Mag.= 10.3 U; 0.23-m Schmidt Cassegrain with 20-second exposure (limit mag.= 16.5); Position end figures 44s.26, 37".4; T. Noguchi, Japan.



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