发表机构
University of Texas Rio Grande Valley; South Texas Space Science Institute, University of Texas Rio Grande Valley; Universidad de La Laguna; Instituto de Astrofísica de Canarias (IAC); Texas Tech University; Universidad Nacional Autónoma de México, Instituto de Astronomía; Durham University; Institute of Space Sciences (ICE, CSIC)（德克萨斯大学里奥格兰德河谷分校; 南德克萨斯空间科学研究所，德克萨斯大学里奥格兰德河谷分校; 拉帕鲁纳大学; 加那利群岛天体物理研究所; 德克萨斯理工大学; 墨西哥国立自治大学，天文研究所; 杜伦大学; 空间科学研究所（ICE，CSIC））
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
COPAS巡天利用TESS高频率观测，从2054个CV候选体中识别出11个周期低于83分钟的吸积双星，其中7个为AM CVn型，并首次测量了6个系统的周期，强调了持续监测的重要性。
AI 中文摘要
我们展示了致密天体与吸积物理巡天（COPAS）的首批结果，这是一个利用TESS卫星通过爆发事件主要探测吸积白矮星双星的高频光度巡天。在TESS第6和第7周期观测到的2,054个激变变星（CV）候选体的初始样本中，我们识别出11个周期低于83分钟的系统，其中包括7个AM CVn型双星和4个CV。我们的双子座光谱数据确认ZTF18aaxuusk和ASASSN-21eo为AM CVn型双星，而Gaia21akb被确认为CV。我们为11个系统中的6个提供了首次周期测量。将TESS数据与地面观测相结合，我们测得AM CVn系统ASASSN-21in和ZTF18aaxuusk的超爆发复发时间约为一年，而短周期CV ASASSN-18rd和ASASSN-15ev的复发时间为1.8至2.0年。利用TESS数据，我们还估算了ASASSN-19ct的质量比（q = 0.05 +/- 0.02），这与高度演化的低质量伴星一致。尽管在总样本中探测到的超致密系统数量较低（0.54%），且这可能是观测偏差和固有群体稀有性的结果，但5个系统被重新分类为AM CVn型双星，凸显了持续监测以通过其爆发和短周期识别更多系统的重要性。
英文摘要
We present the first results from the Compact Objects and the Physics of Accretion Survey (COPAS), a high-cadence photometric survey focused on the detection of accreting white dwarf binaries mainly through their outbursts using TESS. From an initial sample of 2,054 cataclysmic variable (CV) candidates observed during TESS Cycle 6 and 7, we identify 11 systems with periods below 83 minutes. This includes 7 AM CVns and 4 CVs. Our Gemini spectroscopic data confirm ZTF18aaxuusk and ASASSN-21eo as AM CVns, while Gaia21akb is confirmed as a CV. We provide the first period measurements for 6 out of the 11 systems. Complementing our TESS data with ground-based observations, we measured superoutburst recurrence times of approximately one year for the AM CVn systems ASASSN-21in and ZTF18aaxuusk, and 1.8-2.0 years for the short-period CVs ASASSN-18rd and ASASSN-15ev. Using TESS, we also estimate the mass-ratio for ASASSN-19ct (q = 0.05 +/- 0.02), which is consistent with a highly evolved low-mass donor star. Though the number of ultracompact systems detected among the total sample is low (0.54%), and likely the result of observational biases and intrinsic population rareness, the reclassification of 5 systems as AM CVns highlights the importance of continuous monitoring to identify more systems through their outbursts and short periods.
Comments44 figures, 25 pages, and 4 tables; submitted to Publication of the Astronomical Society of Australia (PASA)
