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
Anonymous 21:12:23.35 +14:46:45.47 PS1 Ia 0.029 ATEL
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Anonymous 19:08:42.21 +49:44:17.2 PS1 CV 0 ATEL
 
galex 21:12:23.35 +14:46:45.1 MASTER Ia 0.029 ATEL
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anonymous 18:38:37.55 +41:31:40.37 PTSS Ia 0.069 ATEL
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UGC 11635 20:43:22.40 +80:09:14.6 V. Tinella Ia 0.016 ATEL
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SN 2016cxb in Anonymous
SN 2016cxb in Anonymous
Discovered by: PS1
The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic observations of AT 2016cxa and SN 2016cxb (discovered by Pan-STARRS1, aka PS16cvb and PS16cvc, respectively), obtained with the Asiago 1.82 m Copernico Telescope (+AFOSC; range 340-820 nm; resolution 1.4 nm). Name | Discovery UT | Obs. Date UT | z | Type | Phase |Notes AT 2016cxa | 20160619.60 | 20160623.01 | 0 | CV | | (1) SN 2016cxb | 20160619.51 | 20160623.07 | 0.029 | Ia | a few days before max | (2) 1) The spectrum shows a blue continuum with narrow Halpha, Hbeta and Hgamma in emission at the rest wavelength. The object is therefore not a supernova but most likely a cataclismic variable (CV). The Balmer decrement from the emission components, with the presence of a fairly strong Halpha and higher members of the series showing progressively stronger absorptions, confirms the classification as a dwarf nova. Also the He I emission at 587.6 nm is clearly visible. 2) A good match is obtained with the Type Ia SN 1998bu (Hernandez et al. 2000, MNRAS, 319, 223), a few days before maximum light. From the position of the minimum of the Si II 635nm feature, we infer an expansion velocity of 11100 km/s for the ejected material. Classification was performed using GELATO (Harutyunyan et al. 2008, A&A, 488, 383) and SNID (Blondin and Tonry 2007, ApJ, 666, 1024). The Asiago classification spectra are posted at the website http://sngroup.oapd.inaf.it.