PESSTO spectroscopic classification of optical transients
ATel #5537; S. Spiro, M. Turatto, S. Benetti, E. Cappellaro, A. Pastorello (INAF - Padova Astronomical Observatory), N. Elias-Rosa (INAF - Padova Astronomical Observatory/ICE-IEEC/CSIC Barcelona), A. De Cia (Weizmann Institute of Science), M. T. Botticella (INAF - Naples), S. Valenti (LCOGT/UCSB), S. Taubenberger (MPA Garching), S. J. Smartt, K. Smith, D. Young, C. Inserra (Queen's University Belfast), M. Fraser (University of Cambridge), M. Sullivan (University of Southampton), A. Gal-Yam, O. Yaron, I. Manulis (Weizmann Institute of Science).
on 2 Nov 2013; 22:21 UT
Distributed as an Instant Email Notice Supernovae
Credential Certification: N. Elias-Rosa (nancy.elias@oapd.inaf.it)
Subjects: Optical, Supernovae
PESSTO, the Public ESO Spectroscopic Survey for Transient Objects (see Valenti et al., ATel #4037; http://www.pessto.org ),
reports the following supernova classifications. Targets were supplied by the OGLE-IV Transient Search (see Wyrzykowski et al., ATEL #4495). All observations were performed on the ESO New Technology Telescope at La Silla on 2013 Novembre 1, using EFOSC2 and Grism 13 (3985-9315A, 18A resolution).
Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and GELATO (Harutyunyan et al., 2008,
A&A, 488, 383). Classification spectra can be obtained from http://www.pessto.org (via WISeREP).
Name | RA (J2000) | Dec (J2000) | Disc. Date | Disc. Source | Disc Mag | z | Type | Phase | Notes
OGLE-2013-SN-090 | 04 08 38.84 | -65 45 59.5 | 20131006 | OGLE | 18.6 | 0.125 | AGN | -- | (1)
OGLE-2013-SN-109 | 01 46 09.34 | -67 28 00.0 | 20131030 | OGLE | 19.2 | 0.088 | Ia | a week before maximum | (2)
OGLE-2013-NOVA-02 | 05:57:58.38 | -74:54:09.4 | 20131016 | OGLE | 13.2 | 0.003 | FeII-Nova | -- | (3)
(1) According with NED (http://ned.ipac.caltech.edu/), it has been detected X-ray sources close to the position of this object.
(2) Good match with several normal type Ia SNe around a week before their maximum light.
(3) Halpha has a FWHM velocity of about 1000 km/s. In addition to Balmer emissions, many Fe II lines with P-Cygni profiles are seen.
