估计“标准速射枪”距离的可行性
Estimating the feasibility of `standard speed-gun' distances
摘要：
在以前的论文中，我们展示了一种测量活动星系核（AGN）宇宙学距离的单梯级方法，该方法可以从低红移（z < 0.1）到高红移（z > 3）使用。这种方法依赖于这样的假设，即在活动星系核中看到的变化是由耀斑事件期间的光速约束，因此可以用来估计发射区域的大小。这种方法的局限性在于，以前需要知道多普勒因子。在本文中，我们推导出一个扩展的“标准的速度枪”的方法来测量宇宙学的距离，取决于最大的固有亮度温度的源可以达到，而不是多普勒因子。如果内禀亮度温度的精确值不随红移而变化，并且耀斑在统计上是独立的，那么我们原则上可以在统计上改善宇宙物质含量测量的误差（在平坦的Lambda CDM模型中）。然后，我们探讨了未来的观测计划将如何约束宇宙学参数。我们发现，恢复输入的宇宙学关键取决于不确定性的内在亮度温度和观测到的耀斑的数量。
英文摘要：
In a previous paper, we demonstrated a single-rung method for measuring cosmological distances in active galactic nuclei (AGN) that can be used from low redshift (z < 0.1) to high redshift (z > 3). This method relies on the assumption that the variability seen in AGN is constrained by the speed of light during a flare event and can therefore be used to estimate the size of an emitting region. A limitation of this method is that previously, the Doppler factor was required to be known. In this paper, we derive an extension of the `standard speed-gun' method for measuring cosmological distances that depends on the maximum intrinsic brightness temperature that a source can reach, rather than the Doppler factor. If the precise value of the intrinsic brightness temperature does not evolve with redshift and flares are statistically independent, we can in principle improve the errors in measurements of the matter content of the universe (in a flat LambdaCDM model) statistically. We then explored how well a future observing program would constrain cosmological parameters. We found that recovering the input cosmology depends critically on the uncertainty of the intrinsic brightness temperature and the number of flares observed.
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