Prospects of Searching for Type Ia Supernovae with 2.5-m Wide Field Survey Telescope
Prospects of Searching for Type Ia Supernovae with 2.5-m Wide Field Survey Telescope
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DOI：
10.3390/universe9010007
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发表时间：
2022-12
期刊：
影响因子：
2.9
通讯作者：
Maokai Hu;L. Hu;Jiachen Jiang;Lin Xiao;L. Fan;Jun-Jie Wei;Xuefeng Wu
中科院分区：
文献类型：
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作者：
Maokai Hu;L. Hu;Jiachen Jiang;Lin Xiao;L. Fan;Jun-Jie Wei;Xuefeng Wu
Ia型超新星（SNe Ia）是碳 - 氧白矮星（WDs）的热核爆炸，是众所周知的距离指示物。然而，白矮星如何在钱德拉塞卡极限附近增加质量以及热核失控是如何发生的，仍然不清楚。与这些未解决的问题相关的观测线索，例如爆炸后数小时到数天内的光度数据，是稀缺的。因此，一个重要的方法是通过优化的观测在特定时期发现Ia型超新星。2.5米口径的广角巡天望远镜（WFST）是一台即将在中国西部部署的观测设备。在本文中，我们通过对WFST的模拟观测来评估Ia型超新星的可探测性。根据体视率，我们基于一个基于数据的模型生成了Ia型超新星的光谱系列，并引入视线消光来计算从观测者角度看到的亮度。通过与受观测条件影响的WFST探测极限进行比较，我们可以计算出通过模拟WFST观测所发现的Ia型超新星的数量。我们预计WFST在运行一年的时间内能够发现超过3.0×10⁴颗极大前的Ia型超新星。特别是，WFST在假设的宽、深或中模式下，分别能够发现约45颗明亮的Ia型超新星、99颗早期的Ia型超新星或1.1×10⁴颗观测良好的Ia型超新星，这表明WFST将是时域天文学中一个具有影响力的设备。
Type Ia supernovae (SNe Ia) are thermonuclear explosions of carbon-oxygen white dwarfs (WDs) and are well-known as a distance indicator. However, it is still unclear how WDs increase their mass near the Chandrasekhar limit and how the thermonuclear runaway happens. The observational clues associated with these open questions, such as the photometric data within hours to days since the explosion, are scarce. Thus, an essential way is to discover SNe Ia at specific epochs with optimal surveys. The 2.5 m Wide Field Survey Telescope (WFST) is an upcoming survey facility deployed in western China. In this paper, we assess the detectability of SNe Ia with mock observations of the WFST. Followed by the volumetric rate, we generate a spectral series of SNe Ia based on a data-based model and introduce the line-of-sight extinction to calculate the brightness from the observer. By comparing with the detection limit of the WFST, which is affected by the observing conditions, we can count the number of SNe Ia discovered by mock WFST observations. We expect that the WFST can find more than 3.0×104 pre-maximum SNe Ia within one year of running. In particular, the WFST could discover about 45 bright SNe Ia, 99 early phase SNe Ia, or 1.1×104 well-observed SNe Ia with the hypothesized Wide, Deep, or Medium modes, respectively, suggesting that the WFST will be an influential facility in time-domain astronomy.