SIMBAD references

E. Cappellaro, S. Benetti, A. Pastorello, L. Tomasella, and M. Turatto, Osservatorio Astronomico di Padova, Istituto Nazionale di Astrofisica (INAF); G. Pignata and F. Bufano, Universidad Andres Bello; M. T. Botticella, A. Grado, and L. Limatola, Osservatorio Astronomico di Capodimonte, INAF; M. Vaccari, University of the Western Cape, South Africa; and M. Capaccioli, G. Covone, and M. Paolillo, Universita Federico II, Napoli, on behalf of the SUDARE/VOICE collaboration, report the discovery of the first two supernovae on r-band images taken during their supernova search program with the European Southern Observatory (ESO) VLT Survey Telescope (+ Omegacam). The new objects were discovered in the VOICE-CDFS-2 field, an extended area centered on the Chandra Deep Field South.

---------------------------------------------------------------------------— SN 2012 UT R.A. (2000.0) Decl. Mag. Offset ---------------------------------------------------------------------------— 2012ez Sep. 8.30 3 35 16.368 -27 29 49.21 23.2 1".1 E, 0".1 S 2012fa Sep. 14.24 3 34 59.022 -27 51 55.43 23.4 – ---------------------------------------------------------------------------—

A spectrogram of 2012ez, obtained on Sept. 14.28 UT with the ESO Very Large Telescope Antu (+ FORS2; range 370-920 nm, resolution 10 nm), shows the typical features of a normal type-Ia supernova. Adopting a redshift z = 0.348, as measured from a number of narrow lines of the host galaxy, the best fit with the GELATO tool (Harutyuyan et al. 2008, A.Ap. 488, 383) in a library of supernova spectra is with SN 1995al at fourteen days past maximum (Anupama et al. 1997, A.J. 114, 2054). The ejecta expansion velocity, derived from the position of the Si II doublet, is 11300 km/s.

A spectrogram of 2012fa, which is located at the center of a very faint galaxy, was obtained on Sept. 15.27 as above. Cross-correlation with a library of supernova spectra using the Supernova Identification tool (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) shows that the object is very similar to the bright type-Ia supernova 1991T at ten days before maximum (Ruiz- Lapuente et al. 1992, Ap.J. 387, L33) when placed at a redshift, z, of about 0.4. As for SN 1991T at this phase, the Si II doublet is barely visible.