The Debiased Near-Earth Object Population from ATLAS Telescopes

Rogerio Deienno, Larry Denneau, David Nesvorný, David Vokrouhlický, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Davide Farnocchia, Paul W. Chodas
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Abstract

This work is dedicated to debias the Near-Earth Objects (NEO) population based on observations from the Asteroid Terrestrial-impact Last Alert System (ATLAS) telescopes. We have applied similar methods used to develop the recently released NEO model generator (NEOMOD), once debiasing the NEO population using data from Catalina Sky Survey (CSS) G96 telescope. ATLAS is composed of four different telescopes. We first analyzed observational data from each of all four telescopes separately and later combined them. Our results highlight main differences between CSS and ATLAS, e.g., sky coverage and survey power at debiasing the NEO population. ATLAS has a much larger sky coverage than CSS, allowing it to find bright NEOs that would be constantly "hiding" from CSS. Consequently, ATLAS is more powerful than CSS at debiasing the NEO population for H $\lesssim$ 19. With its intrinsically greater sensitivity and emphasis on observing near opposition, CSS excels in the debiasing of smaller objects. ATLAS, as an all sky survey designed to find imminent hazardous objects, necessarily spends a significant fraction of time looking at places on the sky where objects do not appear, reducing its power for debiasing the population of small objects. We estimate a NEO population completeness of $\approx$ 88%$^{+3\%}_{-2\%}$ for H $<$ 17.75 and $\approx$ 36%$^{+1\%}_{-1\%}$ for H $<$ 22.25. Those numbers are similar to previous estimates (within error bars for H $<$ 17.75) from CSS, yet, around 3% and 8% smaller at their face values, respectively. We also confirm previous finding that the $\nu_6$ secular resonance is the main source of small and faint NEOs at H = 28, whereas the 3:1 mean motion resonance with Jupiter dominates for larger and brighter NEOs at H = 15.
来自 ATLAS 望远镜的衰减近地天体群
这项工作致力于根据小行星地球撞击最后警报系统(ATLAS)望远镜的观测结果,对近地天体(NEO)群进行除杂。我们采用了开发最近发布的近地天体模型生成器(NEOMOD)所使用的类似方法,利用卡塔琳娜巡天(Catalina Sky Survey,CSS)G96望远镜的数据对近地天体群进行了一次除杂。ATLAS 由四台不同的望远镜组成。我们首先分别分析了这四台望远镜的观测数据,然后将它们合并在一起。我们的结果凸显了CSS和ATLAS之间的主要差异,例如天空覆盖范围和对近地天体群的探测能力。ATLAS的天空覆盖范围比CSS大得多,因此它能够发现CSS经常 "隐藏 "的明亮近地天体。因此,ATLAS 在消除 H $lesssim$ 19 的近地天体群方面比 CSS 更强大。CSS 本身具有更高的灵敏度,而且侧重于观测近对角线,因此在消除较小天体方面表现出色。ATLAS作为一个旨在寻找微小危险天体的全天巡天观测系统,必然要花费相当一部分时间去观测天空中没有出现天体的地方,这就降低了它对小天体群进行去逆的能力。我们估计,对于H $<$ 17.75的近地天体,近地天体数量的完整率大约为$88%^{+3/%}_{-2/%}$;对于H $<$ 22.25的近地天体,近地天体数量的完整率大约为$36%^{+1/%}_{-1/%}$。这些数字与之前来自 CSS 的估计值相近(H $<$ 17.75 的误差在误差范围内),但在面值上分别小了约 3% 和 8%。我们还证实了之前的发现,即$\nu_6$世俗共振是H = 28时小型和暗淡近地天体的主要来源,而与木星的3:1平均运动共振则是H = 15时较大和较明亮近地天体的主要来源。
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