S5 0716+714的同时MITSuME gRI监测
Simultaneous MITSuME gRI monitoring of S5 0716+714
摘要：
我们提出了我们的夜间光通量监测观测的S5 0716+714同时在gRI过滤器。这些观测是在2008年3月11日至2008年5月8日之间的30个夜晚，利用冈山天体物理观测站50厘米望远镜上的多色成像望远镜进行的。在这30个夜晚中，有22个夜晚具有持续时间为1至6小时的连续观测（没有任何中断），因此被认为是夜间光学变率（INOV）。我们总共有4888个数据点同时在gR和I滤波器中。在INOV考虑的22个夜晚中，该物体在19个夜晚显示出通量变化，I波段的变化幅度从~4%到~ 55%不等。因此发现INOV的占空比为83%。在大多数夜晚，不同波段之间没有时间滞后，除了3个夜晚，g的变化被发现领先于I波段0.3至1.5小时。在夜间的时间尺度上，没有滞后G和I波段之间。在大多数夜晚的夜间时间尺度和夜间时间尺度上，发现变化的幅度朝着较短的波长增加。不同波段的通量变化不是消色差的，耀变体在夜间和夜间时间尺度上都倾向于变得更蓝，这可能是由于在较短的波长下有较大的振幅变化。2008年4月1日发现了一个明显的3.3小时的周期性变化，2008年3月31日发现了另一个可能的4小时周期性变化的暗示。在我们两个月的30天观测期间，源的变化幅度高达~ 80%。
英文摘要：
We present results of our intra-night optical flux monitoring observations of S5 0716+714 done simultaneously in gRI filters. The observations were done using Multicolor Imaging Telescopes for Survey and Monstrous Explosions (MITSuME) instrument on the 50 cm telescope at the Okayama Astrophysical Observatory over 30 nights between 11 March 2008 and 8 May 2008. Of these 30 nights, 22 nights have continuous (without any break) observations with duration ranging from 1 to 6 hours and hence were considered for intra-night optical variability (INOV). In total we have 4888 datapoints which were simultaneous in gR and I filters. Of the 22 nights considered for INOV, the object showed flux variability on 19 nights with the amplitude of variability in the I-band ranging from ~4% to ~55%. The duty cycle for INOV was thus found to be 83%. No time lag between different bands was noticed on most of the nights, except for 3 nights where the variation in g was found to lead that of the I band by 0.3 to 1.5 hrs. On inter-night timescales, no lag was found between g and I bands. On inter-night timescales as well as intra-night timescales on most of the nights, the amplitude of variability was found to increase toward shorter wavelengths. The flux variations in the different bands were not achromatic, with the blazar tending to become bluer when brighter both on inter-night and intra-night timescales; and this might be attributed to the larger amplitude variation at shorter wavelengths. A clear periodic variation of 3.3 hrs was found on 1 April 2008 and a hint for another possible periodic variability of 4 hrs was found on 31 March 2008. During our 30 days of observations over a 2 month period the source has varied with an amplitude of variability as large as ~80%.
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