------------------------------------------------------------------- THE ASTRONOMER Electronic Circular No 2742 2011 Jun.02 16 34UT Ed:Guy M Hurst, 16,Westminster Close, Kempshott Rise, Basingstoke, Hants, RG22 4PP,England.Telephone/FAX(01256)471074Int:+441256471074 INTERNET: GUY@TAHQ.DEMON.CO.UK Backup: gmh@wdcc1.bnsc.rl.ac.uk WORLD WIDE WEB http://www.theastronomer.org ------------------------------------------------------------------- POSSIBLE NOVA IN SCORPIUS John Seach, Chatsworth Island, Australia has recorded a magnitude 9.5 transient object on three images with a digital SLR at the following position: 2011 June 1.40UT RA 16h 55m 11s DEC -38 38 12 (2000) There is apparently no obvious DSS candidate Shaun Dvorak captured B and V images of the transient and has confirm the presence of the object near the position listed that does not correspond to any bright object on DSS images. Approximate astrometry gives a J2000 position of: RA 16:55:09.4 DEC -38:38:04.6 (2000) using GSC 1.1. The object was measured to be quite red, with v=10.59(1), b=12.34(1) at JD 2455714.75 Ernesto Guido and Giovanni Sostero: Following the posting on the Central Bureau's Transient Object Confirmation Page about a possible nova in Sco, we performed some follow-up of this object remotely through GRAS network from Officer, Australia (MPC Code - E03) using a RCOS 12.5" - FL 1950 @ f/6.3. On our images taken on June 02.4, 2011 we can confirm the presence of an optical counterpart with unfiltered CCD magnitude about 9.4 (USNO-B1.0 Catalogue reference stars) at coordinates: RA 16 55 09.46, DEC -38 38 04.5 (2000) Masayuki Yamanaka and Ryosuke Itoh (Hiroshima University): We performed spectroscopic observation of the possible nova in Scorpius with the 1.5-m Kanata telescope at Higashi-Hiroshima Observatory (HHO). The spectrum exhibits the broad emission lines of H-alpha. This FWZI is roughly measured to be 4500 km/s. The emission line profile shows the triple-peaked line profile. On the other hand, H-beta is not seen because the object is highly reddened by interstellar material. We also identified OI emission lines. These OI emission lines exhibit the double-peaked profile. Their peak separations are roughly 20?. We cannot see HeI emission lines. http://kanatatmp.g.hatena.ne.jp/kanataobslog/?word=Sco Guy M Hurst