G. A. Galazutdinov, T. A. Santander, E. Babina, J. Krełowski
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引用次数: 0
Abstract
We measured the equivalent widths (\(EW\)s) of interstellar Ti II absorption lines at \(\lambda\) 3383.759 for about 250 reddened objects and found a good correlation of the \(EW\)s with distances to the background stars, estimated using Gaia DR3 parallaxes. Hipparcos trigonometric parallaxes were used for very bright objects which were not observed by Gaia. The Ti II based distance estimation procedure is similar to the well known Ca II-method (Megier et al., 2005, 2009). However, there are at least 3 advantages of the Ti II method: in contrast to interstellar Ca II H and K lines, blending of Ti II with stellar lines is not an issue even for late B stars; Ti II is to a much less extent influenced by the saturation effect; only a single line must be measured, i.e. there is only a single measurement error to be taken into account. The relation of between Ti II \(EW\) and distance is given by simple equation \(d\approx 30EW\), where \(d\) is the distance in pc and \(EW\) is the equivalent width of the Ti II \(\lambda\) 3383.759 line in mÅ.
摘要我们测量了大约250个变红天体在\(\lambda\) 3383.759处的星际Ti II吸收线的等效宽度（\(EW\)s），发现\(EW\)s与利用盖亚DR3视差估算的背景恒星的距离有很好的相关性。对于盖亚没有观测到的非常明亮的天体，则使用了Hipparcos三角视差。基于 Ti II 的距离估算程序与众所周知的 Ca II 方法类似（Megier 等人，2005 年，2009 年）。不过，Ti II 方法至少有三个优点：与星际 Ca II H 和 K 线相比，Ti II 与恒星线的混合即使对于晚期 B 星也不是问题；Ti II 受饱和效应的影响要小得多；只需测量一条线，即只需考虑一个测量误差。Ti II （EW）和距离之间的关系由简单的方程 \(d\approx 30EW\) 给出，其中 \(d\) 是以 pc 为单位的距离，\(EW\) 是以 mÅ 为单位的 Ti II （\lambda）383.759 线的等效宽度。
期刊介绍：
Astrophysical Bulletin is an international peer reviewed journal that publishes the results of original research in various areas of modern astronomy and astrophysics, including observational and theoretical astrophysics, physics of the Sun, radio astronomy, stellar astronomy, extragalactic astronomy, cosmology, and astronomy methods and instrumentation.
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