Electronic Telegram No. 2275 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION CBAT Director: Daniel W. E. Green; Room 209; Dept. of Earth and Planetary Sciences; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbat@iau.org; cbatiau@eps.harvard.edu URL http://www.cfa.harvard.edu/iau/cbat.html CATACLYSMIC VARIABLE IN PEGASUS [Editor's note: the following text replaces that on CBET 2274] S. Nakano, Sumoto, Japan, reports the independent discovery of the outburst of this variable (cf. CBET 2273) by Shizuo Kaneko (Kami-Yashiki, Kakegawa, Shizuoka-ken) at mag 9.0 on two 20-s exposures (limiting mag 12.4) taken on May 7.787 UT with a Contax 80-mm f/2.0 camera lens (+ Canon Kiss Digital X camera); nothing was visible at this position on a frame taken by Kaneko on May 1.742 with the same instrumentation. From Kaneko's discovery frame, Nakano measures mag 9.1 (limiting mag 13.2) and the following position for the variable: R.A. = 21h38m07s.03, Decl. = +26d20'03".0 (equinox 2000.0; probable error +/- 4"), adding that a faint star of mag around 14 is visible at position end figures 11s.5, 01". H. Yamaoka, Kyushu University, reports that the variable appears at mag about 15 (near the limiting magnitude) on a CCD survey image taken by K. Itagaki (Yamagata, Japan) on May 1.71 UT with a 0.21-m telescope, which suggests that the star was then at a quiesient phase; Itagaki provides position end figures 06s.66, 19'57".1 and mag about 8.8 from an image taken on May 8.657 UT with his 0.60-m telescope, indicating that the outbursting object is a southern component of a double star GSC 2197:866 (cf. CBET 2273). A. Henden, AAVSO, notes that Palomar Sky Survey (POSS) plates show a close pair of objects at the location of the outbursting variable: one is essentially stationary, while the other has a relatively high proper motion. On the POSS-I plates, the southwest component of the 3"-separated double is obviously blue, while on the POSS-II plates, it has moved east-northeast by about 3" and is now about 1" southeast of the stationary northeast component. At this motion rate, it would be expected to lie an arcsec or two east of the stationary component at this epoch. This rate of motion would imply something intrinsically faint but relatively close; adding in the color would imply a white dwarf -- suggesting that the moving object is the outbursting object and that it is a cataclysmic variable with an amplitude of about 6 magnitudes. P. Camilleri, Sydney, Australia, obtained two unfiltered CCD images of the variable remotely at the Tzec Maun Observatory in New Mexico using a Takahashi Epsilon 0.18-m f/2.8 corrected Newtonian reflector (May 8.371 UT, mag 9.3) and a 0.35-m Maksutov-Newtonian f/3.8 reflector (May 8.388, mag 8.9), yielding position end figures 06s.64 +/- 0s.02, 19'56".8 +/- 0".1. Tabulated summary of the available data from CBET 2273 and above: 2010 UT R.A. (2000.0) Decl. Mag. Observer May 1.71 15 : Itagaki 1.742 [13 : Kaneko (Nakano) 6.77 (21 38 06.6 +26 19 57) 10.8 Yi 7.76 8.4 Yi 7.787 21 38 07.03 +26 20 03.0 9.1 Kaneko (Nakano) 8.371 21 38 06.63 +26 19 56.7 9.3 Camilleri 8.388 21 38 06.66 +26 19 56.8 8.9 Camilleri 8.657 21 38 06.66 +26 19 57.1 8.8 Itagaki M. L. Graham, H. Broekhoven-Fiene, A. H. Parker, S. Sadavoy, and A. J. Maxwell, Department of Physics and Astronomy, University of Victoria; E. Y. Hsiao, Lawrence Berkeley Laboratory; and D. D. Balam, Dominion Astrophysical Observatory, National Research Council of Canada, report that a spectrum (range 390-703 nm, resolution 0.3 nm) of this variable (cf. CBET 2273), obtained on May 8.47 UT with the 1.82-m Plaskett Telescope of the National Research Council of Canada, shows strong H-alpha and H-beta in emission (HWFM 800 km/s), as well as He II (468.6 nm) and a broad emission feature centered at 465 nm that is interpreted as the Bowen complex of N III, C III, and C IV. All members of the Balmer series show shell-like profiles with both red and blue absorption components. A. Arai, Kyoto Sangyo University, reports that an optical spectrogram (resolution 500) of the variable was obtained using the 1.3-m ARAKI telescope on May 8.66 UT under poor sky conditions. The spectrum shows a blue continuum and a weak H-alpha emission line (EW about 0.4 nm), suggesting that the object would be classified as a dwarf nova. No other significant emission or absorption lines were seen in the low-S/N data. NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2010 CBAT 2010 May 8 (CBET 2275) Daniel W. E. Green