The Tully-Fisher relation and H-0

被引：65

作者：

Giovanelli, R

Haynes, MP

daCosta, LN

Freudling, W

Salzer, JJ

Wegner, G

机构：

[1] CORNELL UNIV,NATL ASTRON & IONOSPHERE CTR,ITHACA,NY 14953

[2] EUROPEAN SO OBSERV,D-85748 GARCHING,GERMANY

[3] OBSERV NACL,RIO JANEIRO,BRAZIL

[4] SPACE TELESCOPE EUROPEAN COORDINATING FACIL,D-85748 GARCHING,GERMANY

[5] WESLEYAN UNIV,DEPT ASTRON,MIDDLETOWN,CT 06457

[6] DARTMOUTH COLL,DEPT PHYS & ASTRON,HANOVER,NH 03755

来源：

ASTROPHYSICAL JOURNAL | 1997年 / 477卷 / 01期

基金：

美国国家科学基金会;

关键词：

cosmology; distance scale; large-scale structure of universe; observations; galaxies; distances and redshifts; infrared;

D O I：

10.1086/310521

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The use of the Tully-Fisher (TF) relation for the determination of H-0 relies on the availability of an adequate template TF relation and of reliable primary distances. Here we use a TF template relation with the best available kinematical zero point, obtained from a sample of 24 clusters of galaxies extending to cz similar to 9000 km s(-1), and the most recent set of Cepheid distances for galaxies fit for TF use. The combination of these two ingredients yields H-0 = 69 +/- 5 km s(-1) Mpc(-1). The approach is significantly more accurate than the more common application with single cluster (e.g., Virgo, Coma) samples.

引用

页码：L1 / L4

页数：4

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