Padova-Asiago Supernova Group
The Asiago Transient Classification Program

Presentation
The program started in 2011 with the aim to classify all transients that are accessible from Asiago and are bright enough for our telescope/instrumentation. We use mainly the 1.82m Copernico telescope of Cima Ekar and, if not available, the 1.22m Galileo telescope of the Pennar station. A few cases of transients classified by our group with other facilities (eg. TNG) are included in the database.
Transient classification information and spectra (fits format) are made immediately available at our site. The spectra are semi-automatic reduction with archive calibration data. Please keep this in mind when using them.
For SN classification we compare the output of two automatic SN classification codes: Gelato (Harutyunyan et al. 2008, A&A 488, 383) and SNID (Blondin and Tonry 2007, Ap.J. 666, 1024).
If you use some of the information posted in these pages please make a reference to the paper Tomasella etal. 2014, A.N. 335, 841.

Latest classifications
sn galaxy RA DEC discoverer type redshift ref class fits
SDSS J175740.70+5001 17:57:40.36 +50:02:19.72 ASASSN Ia Pec 0.017 ATEL
fits
2MASX J14433925+1852 14:43:39.05 +18:52:12.65 ASASSN Ia Pec 0.031 ATEL
fits
GALEXASC J114845.20- 11:48:45.10 -18:24:34.31 ASASSN Ia 0.07 ATEL
fits
  09:41:10.63 +24:01:20.51 ASASSN Ia Pec 0.070 ATEL
fits
SDSS J130026.83+1837 13:00:26.55 +18:37:10.09 ASASSN Ia 0.053 ATEL
fits


2018aye in SDSS J175740.70+5001
2018aye in SDSS J175740.70+5001
Discovered by: ASASSN

The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic classification of ASASSN-18ii,ASASSN-18it, ASASSN-18iv, ASASN=18iw, ASASSN-18iu discovered during the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014) (Atel #11178).

The observations were performed with the Asiago 1.82 m Copernico Telescope equipped with AFOSC (range 340-820 nm; resolution 1.4 nm).

Survey Name   | IAI Name      | Discovery date (UT)  | Discovery mag    | Observation (UT)    |  Type     | z         | Notes|
ASASSN-18ii   | SN2018avp     |  2018-04-16.25       | 17.9             |2018-04-21.81        |   Ia      | 0.053     | (1)  |
ASASSN-18it   | SN2018awt     |  2018-04-19.92       | 18.1             |2018-04-21.91        |   Ia      | 0.07      | (2)  |
ASASSN-18iv   | SN2018ayf     |  2018-04-19.97       | 17.2             |2018-04-21.86        |   Ia pec   | 0.070     | (3)  | 
ASASSN-18iw   | SN2018ayg     |  2018-04-21.27       | 18.1             |2018-04-21.95        |   Ia      | 0.031     | (4)  | 
ASASSN-18iu   | SN2018aye     |  2018-04-21.31       | 18.0             |2018-04-21.99        |   Ia      | 0.017     | (5)  |                   

(1) Type Ia SN about one week after maximum light. The velocity of the ejecta, as measured from SiII 635.5 nm, is 11700 km/s, assuming a redshift of 0.052717 for the host galaxy SDSS J130026.83+183711.1 (Almeida et al. 2011, ApJ 735, via NED).

(2) The very noisy spectrum is consistent with that of Type Ia SNe around maximum light at redshift 0.07.

(3) the noisy spectrum matches those of peculiar SNe Ia, eg. SN1991T but also SN2000cx, around maximum light. The redshift of the host galaxy SDSS J094110.41+240122.2 is from SDSS-DR12.

(4) The spectrum, after subtracting the strong contamination from the host galaxy nucleus, matches Type Ia SN 6-10 days before maximum. The redshift of the host galaxy, 2MASX J14433925+1852124, is from SDSS-DR12. >/p>

(5) Best match with Type Ia SN about ten days before maximum light. The velocity of the ejecta, as measured from SiII 635.5 nm, is around 12600 km/s, assuming a redshift of 0.017 as derived from SNID SN template fitting.