------------------------------------------------------------------- THE ASTRONOMER Electronic Circular No 2604 2009 Dec 19 19.56UT 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 AQUILAE 2009 K. Kinugasa et. al., Gunma Astronomical Observatory, report on CBET 2076 that a low-resolution spectrum (range 420-800 nm; resolution 1.0 nm), obtained with the 1.5-m telescope on 2009 on Dec. 15.4UT, confirms that the object referred to on TA E-Circular 2603 is a nova. Its spectrum shows H_alpha emission (FWHM about 1000 km/s) with a P-Cyg profile, its absorption minimum being blue-shifted by 1000 km/s with respect to the emission peak. H_beta, H_gamma, and Fe II (multiplet 42) lines also have P-Cyg profiles. U. Munari, Istituto Nazionale di Astrofisica, Padova Astronomical Observatory and others report that their spectroscopy (range 390-860 nm, dispersion 0.22 nm/pixel; range 544-704 nm at 0.072 nm/pixel) with the Varese 0.6-m telescope on 2009 Dec. 15.8UT shows that this object is a nova, of the Fe II type, with Balmer and Fe II lines in emission and displaying P-Cyg profiles. Strong interstellar lines and diffuse interstellar bands suggest a high reddening. The absorption component of the Balmer P-Cyg line profiles has a FWHM of 560 km/s and is displaced by -620 km/s with respect to the emission component, whose FWHM is 1025 km/s. Fe II multiplets 42 and 49 are in emission with P-Cyg profiles, too. The H_alpha/H_beta flux ratio is 5.7, and H_alpha has an equivalent width of 0.69 nm. The continuum is characterised by the deep absorption lines characteristic of novae close to maximum. The AAVSO advise that finder charts may be plotted by entering 'Nova Aql 2009' at the URL: http://www.aavso.org/observing/charts/vsp/ By calling a smaller field, say of 30 arc minutes with limiting magnitude of 13 should ensure some comparison star values are suited to the current brightness of the nova. SUPERNOVA 2009jq IN UGC 1919 Discovery by LOSS of a possible supernova (CBET 1963): SN 2009 UT R.A. (2000.0) Decl. Mag. Offset 2009jq Oct 9.38 02 27 39.82 +36 09 28.6 17.9 19.0"E,24.7"N SUPERNOVA 2009js IN NGC 918 Independent discoveries of a supernova in NGC 918 have been reported by KAIT (Oct 11.44UT) and Itagaki, Japan (Oct 11.69UT) 2009 UT R.A. (2000.0) Decl. Mag. Offset Oct. 11.44 2 25 48.28 +18 29 25.8 17.2 35".5 W, 20.7"S KAIT Oct. 11.689 2 25 48.30 +18 29 26.2 17.2 35" W, 20.5"S Itagaki J. M. Silverman et. al., University of California, Berkeley, report that inspection of CCD spectra of Oct. 12 UT with the 3-m Shane reflector (+ Kast) at Lick Observatory, shows that SN 2009js is a type-II supernova about two days after maximum brightness. Guy Hurst, using the Bradford Robotic Telescope reports the following photometry based on unfiltered exposures with comparison stars converted from A2 to V : 2009 Oct 18.169UT, 17.4, 20.158, 17.4; Nov 9.123, 17.6, Nov 24.054, 17.6. SUPERNOVA 2009jt Discovery by CRTS of a possible supernova (CBET 1970): SN 2009 UT R.A. (2000.0) Decl. Mag. Offset 2009jt Sep 29.39 03 41 10.67 -09 35 46.9 18.6 1.4"E, 1.5"S Guy M Hurst