Warner Brian D
Center for Solar System Studies-Palmer Divide Station 446 Sycamore Ave., Eaton, CO 80615 USA.
Minor Planet Bull. 2015 Jan-Mar;42(1):79-83.
Analysis of CCD photometry observations at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) made in 2014 June-October found four main-belt binary candidates. 2012 Tantalus is a binary that shows a strong second period but no . (68348) 2001 LO7 is a binary, also showing a strong second period and no confirmed , but is a close to an integral multiple to , which sometimes indicates a . (190208) 2006 AQ appears to be , showing a long period lightcurve superimposed by a short period, lower amplitude component. (276049) 2002 CE26 is a known binary (Shepard ., 2004). Pravec (2006) reported = 3.293 h with no indications of the satellite. The 2014 observations at CS3 initially led to = 3.088 h. After further analysis and confirmation of the longer period (Pravec, personal communications), a period of = 3.928 h was adopted. Unlike the earlier results, there were indications of a satellite with = 16.26 h, which agrees with estimates for the orbital period based on the discovery radar observations. The lightcurve data, however, indicate a considerably larger satellite than indicated by radar.
对太阳系研究中心-帕尔默分水岭站（CS3-PDS）在2014年6月至10月期间进行的电荷耦合器件测光观测分析发现了四颗主带双星候选体。2012年坦塔罗斯是一颗双星，显示出一个强烈的第二周期，但没有……（68348）2001 LO7是一颗双星，也显示出一个强烈的第二周期且没有得到确认的……，但……与……接近整数倍，这有时表明存在一个……（190208）2006 AQ似乎是……，显示出一条叠加有短周期、低振幅分量的长周期光变曲线。（276049）2002 CE26是一颗已知双星（谢泼德等人，2004年）。普拉韦克（2006年）报告其周期为3.293小时，未发现卫星迹象。2014年在CS3的观测最初得出周期为3.088小时。在对更长周期进行进一步分析和确认后（普拉韦克，私人通信），采用了3.928小时的周期。与早期结果不同的是，有迹象表明存在一颗周期为16.26小时的卫星，这与基于发现雷达观测的轨道周期估计相符。然而，光变曲线数据表明该卫星比雷达显示的要大得多。
