ePESSTO spectroscopic classification of optical transients
ATel #12485; R. Carini (INAF-OAR), E. Palazzi (INAF-OAS Bologna), E. Cappellaro, A. Fiore (INAF-OAPd), N. Elias-Rosa (ICE-CSIC), M. Gromadzki (Univ. Warsaw), C. Inserra (Univ. Cardiff), E. Kankare (Univ. Turku), K. Maguire, S. J. Smartt (QUB), O. Yaron (Weizmann), D. R. Young (QUB), I. Manulis (Weizmann), J. Tonry, L. Denneau, A. Heinze, H. Weiland (IfA, Univ. of Hawaii), B. Stalder (LSST), A. Rest (STScI), K. W. Smith, O. McBrien (QUB), D. E. Wright (Univ. of Minnesota), D. E. Wright (Univ. of Minnesota), K. C. Chambers, H. Flewelling, M. Huber, T. Lowe, E. Magnier, A. Schultz, C. Waters, R. J. Wainscoat, M. Willman (IfA, Univ. of Hawaii).
on 8 Feb 2019; 16:37 UT
Distributed as an Instant Email Notice Transients
Credential Certification: Enrico Cappellaro (enrico.cappellaro@oapd.inaf.it)
Subjects: Optical, Supernovae
ePESSTO, the extended Public ESO Spectroscopic Survey for Transient Objects (see Smartt et al. 2015, A&A, 579, 40 http://www.pessto.org ), reports the following supernova classifications. The targets were supplied by the ATLAS survey, see Tonry et al. (2011, PASP, 123, 58) and Tonry et al. (ATel 8680), Pan-STARRS Survey for Transients (see Chambers et al. 2016, arXiv:1612.05560, and http://pswww.ifa.hawaii.edu ), All Sky Automated Survey for SuperNovae ASAS-SN (see Shappee et al. 2014, ApJ, 788, 48 and http://www.astronomy.ohio-state.edu/~assassin/index.shtml ), ESA Gaia Photometric Science Alerts Team and DPAC (http://gsaweb.ast.cam.ac.uk/alerts) and the Zwicky Transient Facility (https://www.ztf.caltech.edu/; Kulkarni et al. 2018, ATel 11266), data stream processed through the Lasair broker (http://lasair.roe.ac.uk/). Observations were performed on the ESO New Technology Telescope at La Silla on 2019-02-07, using EFOSC2 and Grism 13 (3685-9315, 21.2A resolution).
Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and GELATO (Harutyunyan et al.,
2008, A&A, 488, 383). Classification spectra and additional details can be obtained
from http://www.pessto.org (via WISeREP) and the IAU Transient Name Server.
Survey Name | IAU Name | RA (J2000) | Dec (J2000) | Disc. Date | Source | Disc Mag | z | Type | Phase | Notes
Gaia19afw | SN2019xj | 11 10 50.26 | +07 50 59.6 | 20190116 | Gaia | 19.79 | 0.075 | Ia | +10 | (1)
ZTF18aajffcx | AT2019aht | 09 30 16.99 | +29 32 23.7 | 20190130 | ZTF | 16.26 | 0.00567 | Gal | | (2)
ATLAS19dcc | SN2019amr | 14 16 27.68 | -45 25 13.3 | 20190205 | ATLAS | 17.40 | 0.036 | Ia | +1 | (3)
ASASSN-19co | SN2019aos | 13 12 38 53 | -30 01 23.5 | 20190206 | ASAN-SN | 17.5 | 0.030 |Ia-91T| -5 | (4)
PS19mq | SN2019ape | 10 51 42.53 | +18 28 52.7 | 20190205 | Pan-STARRS | 18.57 | 0.020 | Ic | +5 | (5)
ATLAS19bus | SN2019zi | 11 08 44.64 | -13 52 34.9 | 20190123 | ATLAS | 18.77 | 0.048 | Ia | +8 | (6)
(1) The expansion velocity deduced from the Si II 635.5nm minimum is about 9000 km/s. The redshift has been deduced from the SN spectral fitting.
(2) The spectrum shows no variations with respect to that of the host galaxy (NGC2893) nucleus published in Moustakas, J. and Kennicutt, R.C., Jr. 2006, ApJS, 164, 81 (retrieved from NED).
(3) The expansion velocity deduced from the Si II 635.5nm minimum is about 11000 km/s. The redshift has been deduced from the SN spectral fitting
(4) The spectrum shows a blue continuum with broad P-Cygni absorptions of FeIII at 420 and 490 nm matching the spectrum of the bright SN Ia 1991T few days before maximum. No signature of SiII 635.5nm absorption is still visible. A good match is also obtained with the peculiar SN Ia 2000cx. The redshift has been deduced from the SN spectral fitting
(5) The spectrum matches that of various SNe Ic at different phases. Considering the photometric constrain from the ATLAS non-detection at MJD 58507, the best match is with the broad line SN1997ef at 5 days. The redshift of the host galaxy NGC 3426 was retrieved from SDSS DR12
(6) The expansion velocity deduced from the Si II 635.5nm minimum is about 9800 km/s. The redshift has been deduced from the SN spectral fitting
