arXivDaily arXiv每日学术速递 周一至周五更新
北美退伍军人节（Veterans Day），12 日无更新
arXiv 2001.10958astro-ph.IMastro-ph.CO
收藏

钠层Laser激发的精确光度比I：使用342.78 nm光的单光子激发

A Precise Photometric Ratio via Laser Excitation of the Sodium Layer I: One-photon Excitation Using 342.78 nm Light

J. Albert, D. Budker, K. Chance, I. E. Gordon, F. Pedreros Bustos, M. Pospelov, S. M. Rochester, H. R. Sadeghpour

备注：
The second article in this pair of articles is at arXiv:2010.08683 . This article has 14 pages & 7 figures. Both articles are published in MNRAS. This most recent arXiv version fixes a minor error in the caption of Figure 4
发表信息：
MNRAS 508, 4399 (2021)
阅读 PDF
arXiv 页面 ↗HTML 原文 ↗

摘要：

使用Ia型超新星测量暗能量的最大不确定性目前是由于光度学的系统性;特别是光度学作为光谱中波长的函数的相对不确定性。我们表明，在即将到来的调查（如在LSST在维拉C。鲁宾天文台）通过一个位于山顶的激光源调谐到342.78 nm的真空激发波长的中性钠原子。使用从激光导星研究中改进的高功率（500 W）激光，这种激发将在中间层中产生一个去激发光的人造星（我们称之为“激光光度比星”，或LPRS），从地面可以观察到大约20星等（即，完全在LSST的预期单图像幅度限制内），真空中的波长为589.16 nm、589.76 nm、818.55 nm和819.70 nm，该过程产生的589.16 nm和589.76 nm光子数量之和等于818.55 nm和819.70 nm光子数量之和，建立例如LSST r和z滤波器之间的精确校准比率。因此，这种技术可以提供一种新的机制，建立一个前所未有的精度，从上面的大部分地球的大气，即将到来的天文学和大气物理望远镜观测分光光度计校准比。本文是关于此主题的两篇文章中的第一篇。这对文章的第二篇文章描述了一种替代技术，通过使用两个位于山顶的激光器，在距离真空中波长分别为589.16 nm和819.71 nm的谐振约4 GHz的光频率下，实现与本文所述技术相似但更亮的LPRS。

英文摘要：

The largest uncertainty on measurements of dark energy using type Ia supernovae is presently due to systematics from photometry; specifically to the relative uncertainty on photometry as a function of wavelength in the optical spectrum. We show that a precise constraint on relative photometry between the visible and near-infrared can be achieved in upcoming surveys (such as in LSST at the Vera C. Rubin Observatory) via a mountaintop-located laser source tuned to the 342.78 nm vacuum excitation wavelength of neutral sodium atoms. Using a high-power (500 W) laser modified from laser guide star studies, this excitation will produce an artificial star (which we term a "laser photometric ratio star," or LPRS) of de-excitation light in the mesosphere that is observable from the ground at approximately 20 magnitude (i.e., well within the expected single-image magnitude limit of LSST) at wavelengths in vacuum of 589.16 nm, 589.76 nm, 818.55 nm, and 819.70 nm, with the sum of the numbers of 589.16 nm and 589.76 nm photons produced by this process equal to the sum of the numbers of 818.55 nm and 819.70 nm photons, establishing a precise calibration ratio between, for example, the LSST r and z filters. This technique can thus provide a novel mechanism for establishing a spectrophotometric calibration ratio of unprecedented precision, from above most of the Earth's atmosphere, for upcoming telescopic observations across astronomy and atmospheric physics. This article is the first in a pair of articles on this topic. The second article of the pair describes an alternative technique to achieve a similar, but brighter, LPRS than the technique described in this paper, by using two mountaintop-located lasers, at optical frequencies approximately 4 GHz away from resonances at wavelengths in vacuum of 589.16 nm and 819.71 nm respectively.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

↑