来自 ATLAS 望远镜的去势近地天体群

IF 2.5 2区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
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引用次数: 0

摘要

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除杂。ATLAS 由四台不同的望远镜组成。我们首先分别分析了所有四台望远镜的观测数据,然后将其合并。我们的结果凸显了CSS和ATLAS的主要区别,例如天空覆盖范围和在去除近地天体群方面的观测能力。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 ≲ 19 的近地天体数量方面比 CSS 更强大。由于 CSS 本身具有更高的灵敏度,而且侧重于近对角观测,因此在对较小天体进行除杂方面表现出色。而 ATLAS 作为一个旨在寻找即将出现的危险天体的全天空巡天观测系统,必然要花费大量的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的除杂能力。据我们估计,H <17.75的近地天体总数完整率≈88%-2%+3%,H <22.25的近地天体总数完整率≈36%-1%+1%。这些数字与之前来自 CSS 的估计值相似(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ν6世俗共振是H = 28处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处较大和较明亮近地天体的主要来源。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
The debiased Near-Earth object population from ATLAS telescopes
This work is dedicated to debias the Near-Earth Object (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 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 88%2%+3% for H < 17.75 and 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 ν6 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.
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来源期刊
Icarus
Icarus 地学天文-天文与天体物理
CiteScore
6.30
自引率
18.80%
发文量
356
审稿时长
2-4 weeks
期刊介绍: Icarus is devoted to the publication of original contributions in the field of Solar System studies. Manuscripts reporting the results of new research - observational, experimental, or theoretical - concerning the astronomy, geology, meteorology, physics, chemistry, biology, and other scientific aspects of our Solar System or extrasolar systems are welcome. The journal generally does not publish papers devoted exclusively to the Sun, the Earth, celestial mechanics, meteoritics, or astrophysics. Icarus does not publish papers that provide "improved" versions of Bode''s law, or other numerical relations, without a sound physical basis. Icarus does not publish meeting announcements or general notices. Reviews, historical papers, and manuscripts describing spacecraft instrumentation may be considered, but only with prior approval of the editor. An entire issue of the journal is occasionally devoted to a single subject, usually arising from a conference on the same topic. The language of publication is English. American or British usage is accepted, but not a mixture of these.
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