------------------------------------------------------------------- THE ASTRONOMER Electronic Circular No 2782 2011 Nov 26 14.45UT 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 ------------------------------------------------------------------- PI OF THE SKY NORTH OUTBURST, 2011 NOV 24 M. Sokolowski et. al., University of Warsaw and others report on The Astronomer's Telegram 3781 the outburst of an uncatalogued object recorded on 2011 November 24 at 23h 28m 38sUT in the wide field 'Pi of the Sky North' in BOOTES-1 apparatus. It is located at: RA 04h 13m 27.15s DEC -01 39'29" (2000). The following V magnitudes were recorded: Mag Start time (10s exposure) 12.02 23:28:26 11.80 23:28:38 12.01 23:28:51 11.89 23:29:04 12.24 23:29:16 12.28 23:29:29 No object was visible at this position at earlier times. The limit from 20 co-added frames was 12.5 mag. The measured position coincides within estimated position error of about 10 arcsec with 2MASS J04132663-0139211. Images of the optical transient: http://grb.fuw.edu.pl/piinta1/event_desc_public.php?night=20111124&ev ent=20&frame=01228 SUPERNOVA 2011ht IN UGC 5460 Tom Boles discovered this object which was reported on TA E-Circular 2770 under the temporary designation of: PSN J10081059+5150570 J. L. Prieto, Princeton University and others report that they obtained a spectrum (range 350-960 nm; resolution 0.7 nm) with the APO 3.5-m telescope on 2011 Nov. 11.5 UT. It shows substantial evolution with respect to the initial classification spectrum reported by Pastorello et al. It has a blue continuum with strong Balmer lines and weaker He I and Fe II lines in emission. The H-alpha line profile is asymmetric and can be relatively well-fitted using two Gaussian components with FWHM = 1300 km/s and 5400 km/s. The Balmer lines also show a narrow P-Cyg absorption through on top of the broader profiles, with the minimum at -700 km/s with respect to the central wavelength at rest (obtained after correcting for the recession velocity of the host galaxy, UGC 5460, of 1093 km/s from de Vaucouleurs et al. 1991, RC3 catalogue, via NED). These emission-line profiles are characteristic of the spectra of some type-IIn supernovae (e.g., Kiewe et al. 2010, http://lanl.arxiv.org/abs/1010.2689). This classification is consistent with the current absolute magnitude of the object of M_V = -17 (approximately 2.5 mag brighter than at discovery; Prieto et al. 2011, http://www.astronomerstelegram.org/?read=3749), which is too luminous compared with supernova impostors (e.g., Smith et al. 2011, MNRAS 415, 773). Note also that the blue continuum observed in the spectrum is consistent with the unusual ultraviolet brightening detected in Swift UVOT follow-up observations (as communicated by Roming et al. at website URL http://www.astronomerstelegram.org/?read=3690 and by Prieto et al., loc.cit.). The latest measure by Guy Hurst using the Sierra Stars 0.61-m Cassegrain telescope is: 2011 Nov 22.561UT, 14.1V. Guy M Hurst