------------------------------------------------------------------- THE ASTRONOMER Electronic Circular No 2989 2014 Mar 14 18.58UT 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 ------------------------------------------------------------------- NOVA CEPHEI 2014 Koichi Nishiyama, Japan; and Fujio Kabashima, also of Japan, report the discovery of a magnitude 11.7 nova in Cepheus on two 40-s unfiltered CCD frames (limiting magnitude 13.7) taken around 2014 Mar. 8.79UT using a 105-mm f/4 camera lens + CCD. It was confirmed immediately on five 5-s unfiltered CCD frames of Mar. 8.79UT (limiting magnitude 18.3) using a Meade 0.40-m f/9.8 reflector + CCD. It is located at: RA 20h 54m 23.86s DEC +60d 17' 07.7" (2000). Additional magnitudes obtained via CCD (except as stated) Mar. 7.781UT, 12.9 (Nishiyama and Kabashima; pre-discovery; limit mag 13.8); 8.922, V = 11.90 (Arto Oksanen, Finland; 0.40-m reflector + CCD + V filter; position end figures 22s.60, 08".9) U. Munari, INAF Astronomical Observatory of Padova and others write that it is a classical nova. On Mar. 9.792 UT, they obtained a low-resolution spectrogram with the Multi-Mode Spectrograph attached to the Varese 0.61-m telescope. The spectrum shows a red continuum with superimposed strong emission lines from the Balmer series, O I 777.4- and 844.6-nm, Ca II 849.8-nm, and Fe II multiplets 42, 48, and 49. All emission lines shows strong P-Cyg absorptions that are blue-shifted by 660 km/s for the Balmer lines, 780 km/s for the Fe II lines, and 900 km/s for the O I lines. The emission lines have a width of about 800 km/s. The intensity of the O I 844.6-nm emission line is about twice that of O I 777.4-nm, indicating that fluorescent pumping from hydrogen Lyman-beta is already taking place. On Mar. 10.094 UT, they obtained with an "ANS Collaboration" 0.4-m telescope the following photometric magnitudes, fully reduced for colour equations: B = 13.21, V = 11.94, R_c = 11.04, I_c = 10.13. The colour B-V = +1.27 agrees well with the red slope of the continuum observed in the low-resolution spectrum. Overall, the object appears as a highly reddened "Fe II-type" nova observed close to maximum brightness. SUPERNOVA 2014M CHINESE ANTARTIC SURVEY COLLABORATION) 2014M Jan 18.66 15 15 17.21 +75 29 09.5 17.0 18.3"E 2.9"N Discovery using the 0.5-m AST3-2 telescope at Mohe, China. H.-N. Sai: spectrum Jan 27 type-Ia and closely matches SN 1994ae at +9 days. SUPERNOVA 2014N IN ESO 246-G22 (STUART PARKER) 2014N Jan 27.46 02 30 58.91 -44 25 22.3 18.5r 13 "W 13 "N M. R. Drout: spectrum Feb 2 type-IIP about 30-40 days after maximum SUPERNOVA 2014O IN ESO 263-G4 (STUART PARKER) 2014O Feb 2.52 10 06 47.53 -47 41 28.5 16.0r 14 "E 18 "N D. Milisavljevic: spectrum Feb 4 type-IIP similar to 2004et near maximum E-CIRCULAR 2988 This circular was inadvertently dated Mar 19 which should have read Mar. 10. Guy M Hurst