Spectroscopic and photometric observations of dwarf nova superoutbursts by the 3.8 m telescope Seimei and the Variable Star Network
Spectroscopic and photometric observations of dwarf nova superoutbursts by the 3.8 m telescope Seimei and the Variable Star Network
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DOI：
10.1093/pasj/psab036
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发表时间：
2021-04
影响因子：
2.3
通讯作者：
Y. Tampo;K. Isogai;N. Kojiguchi;H. Maehara;K. Taguchi;Taichi Kato;M. Kimura;Yasuyuki Wakamatsu
中科院分区：
文献类型：
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作者：
Y. Tampo;K. Isogai;N. Kojiguchi;H. Maehara;K. Taguchi;Taichi Kato;M. Kimura;Yasuyuki Wakamatsu
我们给出了由安装在京都大学冈山天文台3.8m望远镜Seimei上的Kools-IFU和变星网络合作(VSNET)获得的17个矮新星超暴的光谱和光度观测结果。我们对六次爆发的光谱观测是在它们的光学峰值的1天内完成的。11个对象(TCPJ00590972+3438357、ASASSN-19ADO、TCPJ06073081−0101501、ZTF20aavnpug、ASASSN-19ady、主OTJ061642.05+435617.9、TCPJ20034647+1335125、ASASSN-20KV、ASASSN-20kw、主OTJ13908.79+161240.2和ASASSN-20mf)是以前未知的系统，我们的观察使我们能够快速分类它们的瞬变类型。这些结果说明，清美望远镜有能力对未知瞬变进行快速后续观测。我们的光度观测结果表明，其中11个天体是WZSGE型矮新星及其候选星，另外6个天体是SU-UMA型矮新星及其候选星。在ASASSN-19ADO、TCPJ06073081−0101501和MASTER OTJ13908.79+161240.2中明显检测到He II 4686ä发射线，以前的研究表明它们与吸积盘中的螺旋臂结构有关。我们的结果表明，高倾角系统显示出更强的He II 4686ä发射线，以及更大幅度的早期超峰。
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.