DRAFT
2019-07-26 08:06:27
Type: Object/s-Discovery/Classification
Bibcode: 2019TNSAN..53....1B
Asiago spectroscopic classification of optical transients
Authors: Marco Berton (FINCA, University of Turku) , Lina Tomasella (INAF OAPd), Irene Salmaso (DFA University of Padova, INAF OAPd), Stefano Benetti (INAF OAPd), Enrico Cappellaro (INAF OAPd), Massimo Turatto (INAF OAPd)
Source Group: Padova-Asiago
Keywords: Spectroscopy, Transient, AGN, Optical
Abstract:
We report the spectroscopic classifications of AT2019lrq as a type 1 AGN

The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841), in the framework of the ASYAGO School Program (Asiago School for Young Astronomers with Galileo Observations, attending students: Francesco Antonuccio, Giovanni Benetti, Alberto Fantini, Emily Pertile, Anna Rigoni; tutors: Alessandro Siviero, Costantino Sigismondi), reports the following spectroscopic observation.

The target was supplied by the All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014).

The observation was performed with the Asiago 1.82m Copernico Telescope (+AFOSC; range 340-820 nm; resolution 1.4 nm).

Show current TNS values
Catalog Name Reported RA Reported DEC Reported Obj-Type Reported Redshift Host Name Host Redshift Remarks TNS RA TNS DEC TNS Obj-Type TNS Redshift
TNS 2019lrq [ASASSN-19se] 16:18:01.310 +67:04:00.19 AGN 0.095 2MASX J16180075+6703563 AT2019lrq is a type 1 AGN at z = 0.095, as measured by the low ionization line [O II] 372.7 nm. The high ionization lines of [O III] are shifted with respect to the galaxy rest frame by more than 100 km/s, suggesting a disturbed kinematics of the gas. A similar behaviour is present in the Balmer lines. In particular, the Hbeta likely has three distinct kinematic components. The first has a FWHM of 1850 km/s and is blueshifted by 1680 km/s. The second component is in the same frame as the [O II] line, and has a FWHM of 1050 km/s. The last one, instead, is redshifted by 1360 km/s, and it has a FWHM of 2100 km/s. This behaviour is reminiscent of a candidate black hole binary (Bon et al. 2012, 2016). The optical image, indeed, shows possible signs of a recent merger, which could account for these peculiar properties. 16:18:01.310 +67:04:00.19 AGN 0.095

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