Globular clusters and the Mira period–luminosity relation
Globular clusters and the Mira period–luminosity relation
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球状星团和米拉周期-光度关系
DOI：
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发表时间：
2001
期刊：
影响因子：
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通讯作者：
J. Menzies
中科院分区：
文献类型：
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作者：
M. Feast;Patricia Whitelock;J. Menzies
基于亚矮星的喜巴谷视差的球状星团距离尺度已经被用来估计星团Miras的MK，包括小麦哲伦云（SMC）球状星团ngc121中的一个。这导致Mira红外周期-光度（PL）关系的零点，PL(K)，与附近场Miras的Hipparcos视差得到的结果很好地一致。这两个估计的平均值加上LMC Miras的数据得出大麦哲伦云（LMC）的距离模量为18:60 ^ 0:10，与经金属量校正的造父变星模量O18:59^， 0:10 u明显一致。本文还讨论了利用发光渐近巨支星（AGB）作为星系外星群指标的问题。
A globular cluster distance scale based on Hipparcos parallaxes of subdwarfs has been used to derive estimates of MK for cluster Miras, including one in the Small Magellanic Cloud (SMC) globular cluster NGC 121. These lead to a zero-point of the Mira infrared period ‐luminosity (PL) relation, PL(K ), in good agreement with that derived from Hipparcos parallaxes of nearby field Miras. The mean of these two estimates together with data on LMC Miras yields a Large Magellanic Cloud (LMC) distance modulus of 18:60 ^ 0:10 in evident agreement with a metallicity-corrected Cepheid modulus O18:59^ , 0:10U. The use of luminous asymptotic giant branch (AGB) stars as extragalactic population indicators is also discussed.