Published January 1, 2021
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Spectroscopic and photometric observations of dwarf nova superoutbursts by the 3.8 m telescope Seimei and the Variable Star Network
Creators
- Tampo, Yusuke1
- Isogai, Keisuke
- Kojiguchi, Naoto1
- Maehara, Hiroyuki
- Taguchi, Kenta1
- Kato, Taichi1
- Kimura, Mariko
- Wakamatsu, Yasuyuki1
- Shibata, Masaaki1
- Nogami, Daisaku1
- Kawabata, Miho
- Maeda, Keiichi1
- Namekata, Kosuke
- Okamoto, Soshi1
- Otsuka, Masaaki
- Burgaz, Umut
- Nagoshi, Shumpei1
- Itoh, Hiroshi2
- Vanmunster, Tonny
- Tordai, Tamas3
- Tordai, Tamas3
- 1. Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Oiwakecho, Kyoto, Kyoto 6068502, Japan
- 2. Variable Star Observers League Japan VSOLJ, 1001-105 Nishiterakata, Hachioji, Tokyo 1920153, Japan
- 3. Hungarian Astron Assoc, Polaris Observ, Laborc Utca 2-C, H-1037 Budapest, Hungary
Description
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 1d 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 Heii 4686 angstrom 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 Heii 4686 angstrom, as well as larger-amplitude early superhumps.
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