Mergers as an Omega estimator. [For curvature of universe determination]
Mergers as an Omega estimator. [For curvature of universe determination]
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作为 Omega 估算师进行合并。
DOI：
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发表时间：
1990
期刊：
影响因子：
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通讯作者：
R. Carlberg
中科院分区：
文献类型：
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作者：
R. Carlberg
正在合并或强烈相互作用的星系的分数的红移依赖是一个陡峭的函数欧米茄，并取决于相互作用的两两速度色散的截止速度的比率。对于典型的星系，合并率显示为（1 + z）exp m，其中m约为4.51（Ω）exp 0.42，对于Ω接近1和CDM类宇宙学。指数m对最大合并速度、星系质量和背景宇宙学的依赖性相对较弱，因为在星系形成的红移较低（z约为2）的宇宙学周围有很小的变化。光学星系和红外天文望远镜星系的m估计值大约是3-4，但不确定性很大。如果类星体的演化遵循星系合并的演化，并且类星体的m大于4，则Omega大于0.8。参考文献21篇。
The redshift dependence of the fraction of galaxies which are merging or strongly interacting is a steep function of Omega and depends on the ratio of the cutoff velocity for interactions to the pairwise velocity dispersion. For typical galaxies the merger rate is shown to vary as (1 + z)exp m, where m is about 4.51 (Omega)exp 0.42, for Omega near 1 and a CDM-like cosmology. The index m has a relatively weak dependence on the maximum merger velocity, the mass of the galaxy, and the background cosmology, for small variations around a cosmology with a low redshift, z of about 2, of galaxy formation. Estimates of m from optical and IRAS galaxies have found that m is about 3-4, but with very large uncertainties. If quasar evolution follows the evolution of galaxy merging and m for quasars is greater than 4, then Omega is greater than 0.8. 21 refs.