中红外和远红外精细结构线对精细结构常数假设变化的灵敏度
Mid- and far-infrared fine-structure line sensitivities to hypothetical variability of the fine-structure constant
摘要：
计算了Cl、Si I、Si I、Ti I、Fe I、N II、Fe II、O III、S III、Ar III、Fe III、Mg V、Ca V、Na VI、Fe VI、Mg VII、Si VII、Ca VII、Fe VII和Si IX的基态的精细结构（FS）子能级之间跃迁的精细结构常数α随时间变化的灵敏度系数。这些跃迁位于中红外和远红外区域，可以在高红移类星体和具有活动星系核的红外明亮星系的光谱中观察到。利用FS跃迁研究宇宙学时间尺度上的α变化，与同时期的光学观测（$|Δα/α| < 10^{-5}$）相比，可以使$|Δα/α|$的极限提高几倍，并且可以显著地抑制由多普勒噪声引起的径向速度测量的系统误差。此外，在红移z > 10处可以观察到远红外线，远远超出了光学观测的范围（z < 4）。我们已经推导出一个简单的解析表达式，它涉及的FS间隔和FS过渡的灵敏度的变化的α。
英文摘要：
Sensitivity coefficients to temporal variation of the fine-structure constant alpha for transitions between the fine-structure (FS) sub-levels of the ground states of C I, Si I, S I, Ti I, Fe I, N II, Fe II, O III, S III, Ar III, Fe III, Mg V, Ca V, Na VI, Fe VI, Mg VII, Si VII, Ca VII, Fe VII, and Si IX are calculated. These transitions lie in the mid- and far-infrared regions and can be observed in spectra of high-redshift quasars and infrared bright galaxies with active galactic nuclei. Using FS transitions to study alpha-variation over cosmological timescale allows to improve the limit on $|Δα/α|$ by several times as compared to contemporaneous optical observations ($|Δα/α| < 10^{-5}$), and to suppress considerably systematic errors of the radial velocity measurements caused by the Doppler noise. Moreover, the far infrared lines can be observed at redshifts z > 10, far beyond the range accessible to optical observations (z < 4). We have derived a simple analytical expression which relates the FS intervals and the sensitivity of the FS transitions to the change of alpha.
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