Spectroscopic and photometric observations of dwarf nova superoutbursts by the 3.8 m telescope Seimei and the Variable Star Network

Tampo, Y.; Isogai, K.; Pavlenko, E.P.; Antonyuk, K.A.; Pit, N.V.; Antonyuk, O.I.; Babina, J.V.; Baklanov, A.V.; Sosnovskij, A.A.; Shugarov, S.Y.; Katysheva, N.; Chochol, D.; Zubareva, A.M.; Belinski, A.A.; Ikonnikova, N.P.; Burlak, M.A.; et al.

Авторы: Tampo Yusuke, Isogai Keisuke, Pavlenko Elena P., Antonyuk Kirill A., Pit Nikolaj V., Antonyuk Oksana I., Babina Julia V., Baklanov Aleksei V., Sosnovskij Aleksei A., Shugarov Sergey Yu, Katysheva Nataly, Chochol Drahomír, Zubareva Alexandra M., Belinski Alexandr A., Ikonnikova Natalia P., Burlak Marina A., et al.
Журнал: Publications of the Astronomical Society of Japan
Том: 73
Номер: 3
Год издания: 2021
Издательство: Astronomical Society of Japan
Местоположение издательства: Japan
Первая страница: 753
Последняя страница: 771
DOI: 10.1093/pasj/psab036
Аннотация: We present spectroscopic and photometric observations of 17 dwarf-nova superoutbursts obtained by KOOLS-IFU mounted on the 3.8 m telescope Seimei at the Okayama Observatory of Kyoto University and through the Variable Star Network collaboration (VSNET). Our spectroscopic observations for six outbursts were performed within 1 d of their optical peak. 11 objects (TCP J00590972+3438357, ASASSN-19ado, TCP J06073081−0101501, ZTF20aavnpug, ASASSN-19ady, MASTER OT J061642.05+435617.9, TCP J20034647+1335125, ASASSN-20kv, ASASSN-20kw, MASTER OT J213908.79+161240.2, and ASASSN-20mf) were previously unknown systems, and our observations enabled quick classification of their transient type. These results illustrate that the Seimei telescope has the capability to conduct quick follow-up observations of unknown transients. Our photometric observations yielded that 11 of the objects are WZ Sge-type dwarf novae and their candidates, and the other six are SU UMa-type dwarf novae and their candidates. The He ii 4686 Å emission line was clearly detected among ASASSN-19ado, TCP J06073081−0101501 and MASTER OT J213908.79+161240.2, the association of which with a spiral arm structure in an accretion disk has been suggested in previous studies. Our result suggests that a higher-inclination system shows a stronger emission line of He ii 4686 Å, as well as larger-amplitude early superhumps.
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Spectroscopic and photometric observations of dwarf nova superoutbursts by the 3.8 m telescope Seimei and the Variable Star Networkстатья

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