高频率瞬变测量（HiTS）- I.巡天设计与超新星激波爆发约束
The High Cadence Transient Survey (HiTS) - I. Survey design and supernova shock breakout constraints
摘要：
我们提出的高节奏瞬态调查（HiTS），调查的目的是检测和跟踪光学瞬态的特征时间尺度从几个小时到几天，特别是最早的几个小时的超新星（SN）爆炸的第一个结果。HiTS使用暗能量相机（DECam）和定制的管道进行图像相减、候选过滤和候选可视化，该管道实时运行，以便能够对新的瞬变做出快速反应。我们讨论了调查设计，与这些大量数据的实时分析相关的技术挑战和我们的第一个结果。在2013年、2014年和2015年的活动中，我们探测到了120多个年轻的SN候选者，但我们没有发现来自红超巨星核心坍缩后产生的短暂SN冲击爆发（SBOs）的明确特征，这是这次调查的最初科学目标。使用我们的观测活动中极限星等的经验分布，我们测量了随机注入SN光变曲线的预期恢复分数，其中包括使用Tominaga等人（2011）和Nakar & Sari（2010）的模型产生的SBO光学峰。从这个分析中，我们不能排除Tominaga等人的模型。（2011）在任何合理的祖先质量分布下，但我们可以在我们最佳猜测的祖先质量分布下稍微排除Nakar & Sari（2010）的更亮和更长寿命的SBO模型。最后，我们强调了这项工作对未来天文观测站（如LSST）产生的大规模数据集的影响。
英文摘要：
We present the first results of the High cadence Transient Survey (HiTS), a survey whose objective is to detect and follow up optical transients with characteristic timescales from hours to days, especially the earliest hours of supernova (SN) explosions. HiTS uses the Dark Energy Camera (DECam) and a custom made pipeline for image subtraction, candidate filtering and candidate visualization, which runs in real-time to be able to react rapidly to the new transients. We discuss the survey design, the technical challenges associated with the real-time analysis of these large volumes of data and our first results. In our 2013, 2014 and 2015 campaigns we have detected more than 120 young SN candidates, but we did not find a clear signature from the short-lived SN shock breakouts (SBOs) originating after the core collapse of red supergiant stars, which was the initial science aim of this survey. Using the empirical distribution of limiting-magnitudes from our observational campaigns we measured the expected recovery fraction of randomly injected SN light curves which included SBO optical peaks produced with models from Tominaga et al. (2011) and Nakar & Sari (2010). From this analysis we cannot rule out the models from Tominaga et al. (2011) under any reasonable distributions of progenitor masses, but we can marginally rule out the brighter and longer-lived SBO models from Nakar & Sari (2010) under our best-guess distribution of progenitor masses. Finally, we highlight the implications of this work for future massive datasets produced by astronomical observatories such as LSST.
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