Pan-STARRS1探测到的H>13近地天体和ARM目标的大小-频率分布
The size-frequency distribution of H>13 NEOs and ARM targets detected by Pan-STARRS1
摘要：
我们确定绝对星等（H）分布（或尺寸频率分布，SFD; $N(H) \propto 10^{αH}$，其中$α$为分布斜率），适用于全景望远镜和快速反应系统-Pan-STARRS 1的1 \st巡天望远镜探测到的具有$13<H<30$的近地天体和具有$27<H<31$的小行星回收任务目标（例如，Kaiser等人，2002年，Kaiser 2004年，Hodapp等人，2004年）。使用Greenstreet等人（2012年）的近地天体轨道分布计算了近地天体和反辐射导弹目标的探测效率。去偏的Pan-STARRS 1近地天体绝对星等分布比单一斜率幂律更为复杂-它显示了两个转变-在H $\sim$ 16处从陡坡到浅坡，在$21<H<23$间隔中从浅坡到陡坡，这与最近的其他工作一致（例如，Mainzer等人，2011年c; Brown等人，2013年; Harris和D`Abramo，2015年）。我们用$α= 0.48\pm0.02$拟合了具有$13<H<16$的近地天体，用$α= 0.33\pm0.01$拟合了具有$16<H<22$的近地天体，用$α= 0.62\pm0.03$拟合了具有$H>22$的较小天体。在H=27附近，还有另一个斜率从陡变浅的变化。Pan-STARRS 1在一年的调查中探测到的三个ARM目标候选者具有斜率为$α= 0.40^{+0.33}_{-0.45}$的校正SFD。我们还表明，用美国航天局的国际辐射传递函数望远镜以及阿雷西博和戈德斯通雷达对小型（H $\gtrsim$ 22）近地天体进行后续观测的时间非常短-只有几天的时间，必须执行快速响应程序，以便测量接近地球的小型天体的物理特征。CFHT的MegaCam和Pan-STARRS 1具有较长的观测窗口，由于其极限星等更深，视野更广，因此能够跟踪更多的近地天体。
英文摘要：
We determine the absolute magnitude (H) distribution (or size-frequency distribution, SFD; $N(H) \propto 10^{αH}$ where $α$ is the slope of the distribution) for near-Earth objects (NEO) with $13<H<30$ and Asteroid Retrieval Mission (ARM) targets with $27<H<31$ that were detected by the 1\st\ telescope of the Panoramic Survey Telescope and Rapid Response System - Pan-STARRS1 (e.g. Kaiser et al. 2002, Kaiser 2004, Hodapp et al. 2004). The NEO and ARM target detection efficiencies were calculated using the Greenstreet et al. (2012) NEO orbit distribution. The debiased Pan-STARRS1 NEO absolute magnitude distribution is more complex than a single slope power law - it shows two transitions - at H$\sim$16 from steep to shallow slope, and in the $21<H<23$ interval from a shallow to steep slope, which is consistent with other recent works (e.g. Mainzer et al. 2011c, Brown et al. 2013, Harris and D`Abramo 2015). We fit $α= 0.48\pm0.02$ for NEOs with $13<H<16$, $α= 0.33\pm0.01$ for NEOs with $16<H<22$, and $α= 0.62\pm0.03$ for the smaller objects with $H>22$. There is also another change in slope from steep to shallow around H=27. The three ARM target candidates detected by Pan-STARRS1 in one year of surveying have a corrected SFD with slope $α= 0.40^{+0.33}_{-0.45}$. We also show that the window for follow up observations of small (H$\gtrsim$22) NEOs with the NASA IRTF telescope and Arecibo and Goldstone radars are extremely short - on order of days, and procedures for fast response must be implemented in order to measure physical characteristics of small Earth-approaching objects. CFHT's MegaCam and Pan-STARRS1 have longer observing windows and are capable of following-up more NEOs due to their deeper limiting magnitudes and wider fields of view.
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