2006年Markarian 421多波长活动期间的MAGIC TeV Gamma-Ray观测
MAGIC TeV Gamma-Ray Observations of Markarian 421 during Multiwavelength Campaigns in 2006
摘要：
主要大气伽马成像切伦科夫（MAGIC）望远镜参与了三次多波长（MWL）活动，在2006年4月28日，29日和2006年6月14日的夜晚观测了耀变体Markarian（Mkn）421。我们分析了2006年4月22日至30日和2006年6月14日9个夜晚的MAGIC甚高能观测。我们推断光变曲线与亚白天的分辨率和夜间的能量谱。在所有的观测夜晚都从MKN 421探测到了强烈的伽马射线信号。2006年4月，通量（E > 250 GeV）在夜间变化，介于（0.92+-0.11 10 ^-10 cm^-2 s^-1（0.57蟹状单位）和（3.21+-0.15 10 ^-10 cm^-2 s^-1（2.0蟹状单位）之间。在2006年4月29日晚上，有一个明显的夜间变化的迹象，倍增时间为36+-10（统计）分钟，再次建立了这个物体的快速通量变化。对于所有的夜晚，都可以推断出伽马射线谱，幂律指数在1.66到2.47之间。我们没有发现统计上显着的光谱指数和通量状态之间的相关性为个人的夜晚。在2006年6月的活动中，大大低于惠普尔10米望远镜4天后测得的通量被发现。使用对数抛物线幂律拟合，我们推导出一些数据集的光谱峰值的位置在非常高的能量制度。我们的研究结果证实了峰值能量随着通量的增加而增加的迹象，正如轻子加速模型所预期的那样。
英文摘要：
The Major Atmospheric Gamma Imaging Cerenkov (MAGIC) telescope participated in three multiwavelength (MWL) campaigns, observing the blazar Markarian (Mkn) 421 during the nights of 2006 April 28, 29, and 2006 June 14. We analyzed the corresponding MAGIC very-high energy observations during 9 nights from 2006 April 22 to 30 and on 2006 June 14. We inferred light curves with sub-day resolution and night-by-night energy spectra. A strong gamma-ray signal was detected from Mkn 421 on all observation nights. The flux (E > 250 GeV) varied on night-by-night basis between (0.92+-0.11)10^-10 cm^-2 s^-1 (0.57 Crab units) and (3.21+-0.15)10^-10 cm^-2 s^-1 (2.0 Crab units) in 2006 April. There is a clear indication for intra-night variability with a doubling time of 36+-10(stat) minutes on the night of 2006 April 29, establishing once more rapid flux variability for this object. For all individual nights gamma-ray spectra could be inferred, with power-law indices ranging from 1.66 to 2.47. We did not find statistically significant correlations between the spectral index and the flux state for individual nights. During the June 2006 campaign, a flux substantially lower than the one measured by the Whipple 10-m telescope four days later was found. Using a log-parabolic power law fit we deduced for some data sets the location of the spectral peak in the very-high energy regime. Our results confirm the indications of rising peak energy with increasing flux, as expected in leptonic acceleration models.
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