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首页> 外文期刊>The Journal of the American Association of Variable Star Observers >Anchoring the Universal Distance Scale Via a Wesenheit Template
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Anchoring the Universal Distance Scale Via a Wesenheit Template

机译：通过Wesenheit模板锚定通用距离尺度

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摘要

A VI Wesenheit diagram featuring SX Phoenicis, δ Scuti, RR Lyrae, and type II and classical Cepheid variables is calibrated by means of geometric-based distances inferred from HST, Hipparcos, and VLBA observations (n= 30). The distance to a target population follows from the offset between the observed Wesenheit magnitudes and the calibrated template. The method is evaluated by ascertaining the distance moduli for the LMC (μ_0 = 18.43 = 0.03 ox ) and the globular clusters w Cen, M54, M13, M3, and M15. The results agree with estimates cited in the literature, although a nearer distance to M13 is favored (pending confirmation of the data's photometric zero-point) and observations of variables near the core of M15 suffer from photometric contamination. The calibrated LMC data are subsequently added to the Wesenheit template since that galaxy exhibits precise OGLE photometry for innumerable variables of differing classes. that includes recent observations for δ Scuti variables indicating the stars follow a steeper VI Wesenheit function than classical Cepheids pulsating in the fundamental mode. VI photometry for the calibrators is tabulated to facilitate further re search, and includes new observations acquired via the AAVSO"s robotic telescope network (e.g., VY Pyx: V = 7.25 and V> – I = 0.67).
机译：通过从HST，Hipparcos和VLBA观测值推断出的基于几何的距离（n = 30）来校准包含SX腓尼基，δScuti，RR Lyrae和II型以及经典造父变星的VI Wesenheit图。到目标种群的距离是从观测到的Wesenheit量级与校准模板之间的偏移量得出的。通过确定LMC（μ_0= 18.43 = 0.03 ox）和球状星团w Cen，M54，M13，M3和M15的距离模量来评估该方法。尽管与M13的距离更近（有待确认数据的光度零点），并且M15核心附近变量的观测值受到光度污染，但结果与文献中引用的估计值一致。随后将校准的LMC数据添加到Wesenheit模板中，因为该星系针对不同类别的无数变量显示了精确的OGLE光度法。其中包括对δScuti变量的最新观测结果，表明恒星遵循的经典Wepheheit函数比经典造父变星在基本模式下脉动时更陡峭。校准器的VI光度测定结果已制成表格，以便于进一步研究，并包括通过AAVSO的自动望远镜网络获得的新观测值（例如，VY Pyx：V = 7.25和V> – I = 0.67）。

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