IAU Central Bureau for Astronomical Telegrams

Central Bureau for Astronomical Telegrams -- Image credits

CBAT "Transient Object Followup Reports"

PNV J18422792+4837425

PNV J18422792+4837425   2011 09 05.5293*  18 42 27.92 +48 37 42.5  11.8 U             Dra       9 0

2011 09 05.529

Discovered by Hideo Nishimura who has confirmed this star four hours later.

2011 09 05.695

Mag.= 11.8 U +/-0.3, Position end figures 28s.11, 41".5 +/- 2", from a BMP image by Nishimura on 2011 Sept. 5.69549 UT.

2011 09 06.1019

I confirmed this transient object on images taken with 25cm reflector (fl=850mm) and SBIG ST-8XE camera at Mayhill, NM, USA (Global-rent-a-scope). Position end figures are 28.03 and 41.77. Photometry results are 12.13V, 12.16Rc, 12.28Ic and 12.13B at 6.1019-6.1073 Sep 2011 UT. According to its blue color, it might be dwarf nova rather than classical nova. (Seiichiro Kiyota, Tsukuba, Japan) http://meineko.sakura.ne.jp/ccd/PNV_J18422792+4837425.jpg

2011 09 06.226

Object detected at position end figures 28.01, 41.7 (UCAC3). Magnitude 12.09 U +/- 0.02. Limiting magnitude 17.5. Object faintly visible in DSS image at these coordinates. Nothing listed at these coordinates in USNO-B1.0. Time series observations taken from approximately 0300 UT to 0800 UT. Observer: R. A. Koff, Bennett, Colorado USA (H09) Link to Image: http://antelopehillsobservatory.org/SNpictures/PNV18422792+4837425final.jpg Link to lightcurve: http://antelopehillsobservatory.org/SNpictures/PNV18422792+4837425LCfinal.jpg

2011 09 06.4879

I confirmed this PNV using 0.30-m f/7.0 Cassegrain + unfiltered CCD (SBIG STL-1001E). Mag.= 11.9 U, Position end figures 28s.03 and 41".5. Position and magnitude are measured on an image composed from 6-frames which were taken by each 60-seconds exposure under the limiting magnitude = 18.5. Position and magnitude was measured using USNO-B1.0 T. Yusa, Osaki Lifelong Learning Center, Japan.

2011 09 06.55

We performed low-resolution optical spectroscopic observations of PNV J18422792+4837425 on 2011 September 6.55 at Koyama Astronomical Observatory. The spectrum shows Balmer series lines on a blue continuum light. The H-alpha line clearly shows a strong emission feature (E.W. about -300) in its absoption component. The H-beta and the H-gamma were dominated by absorption components. These results suggests that the object would be a dwarf nova duirng its outburst. (http://www.cc.kyoto-su.ac.jp/~kao/blog/index.php/view/125) A. Arai, Kyoto Sangyo University, Japan.

2011 09 07.450

Mag.= 12.4 U; 0.23-m Schmidt Cassegrain + unfiltered CCD (BITRAN BT-11E); Position end figures 28s.01, 41".5, by 30-second exposure under the limiting magnitude = 17.5. T. Noguchi, Japan.

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