PKS B1519-273和PKS B1622-253星际闪烁时标的年周期
Annual Cycles in the Interstellar Scintillation Timescales of PKS B1519-273 and PKS B1622-253
摘要：
我们使用塔斯马尼亚大学在南澳大利亚塞杜纳的30米射电望远镜定期监测一些南部耀变体的通量密度。我们报告检测的年度周期的变化时间尺度的厘米射电发射的PKS B1622 - 253。对PKS B1519 - 273近两年的观测证实了该源在变率时间尺度上存在年周期。这些观测结果证明，星际闪烁是这些源射电波长日间变化的主要原因。两个源的最佳拟合的年周期模型意味着在散射屏幕的各向异性程度很高，它有一个大的速度偏移相对于当地标准的休息。这与这些“慢”IDV源的屏幕距离比快速闪烁体（例如PKS B0405 - 385或J1819 + 3845）更大一致。
英文摘要：
We have used the University of Tasmania's 30 m radio telescope at Ceduna in South Australia to regularly monitor the flux density of a number of southern blazars. We report the detection of an annual cycle in the variability timescale of the centimetre radio emission of PKS B1622-253. Observations of PKS B1519-273 over a period of nearly two years confirm the presence of an annual cycle in the variability timescale in that source. These observations prove that interstellar scintillation is the principal cause of inter-day variability at radio wavelengths in these sources. The best-fit annual cycle model for both sources implies a high degree of anisotropy in the scattering screen and that it has a large velocity offset with respect to the Local Standard of Rest. This is consistent with a greater screen distance for these "slow'" IDV sources than for rapid scintillators such as PKS B0405-385 or J1819+3845.
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