Hostname: page-component-7479d7b7d-c9gpj Total loading time: 0 Render date: 2024-07-11T08:30:57.690Z Has data issue: false hasContentIssue false
  • English
  • Français

A Distance Scale from the IR Magnitude/HI Velocity Width Relation

Published online by Cambridge University Press:  19 July 2016

M. Aaronson
M. Aaronson*
Affiliation:
Steward Observatory, University of Arizona, Tucson, Arizona 85721 U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A summary is given of recent work using the IR/H I method, arguably the best global distance indicator presently available. Reflex motion toward the microwave dipole anisotropy has been seen relative to a sample of nearby galaxy clusters; this result is contrasted with the somewhat divergent conclusions obtained by Burstein et al. from a similar study of elliptical galaxies. A best guess calibration of the IR/H I zero point continues to lead to a high value for the expansion rate. This finding cannot be explained by appealing to Malmquist bias, as demonstrated by a straightforward linearity test of the velocity-distance relation. However, all current estimates of the Hubble constant are plagued by the large uncertainties to the distances of nearby calibrating galaxies, a problem whose full solution probably must await the launch of the Hubble Space Telescope.

Type
Chapter III. The Classical Quantities of Cosmology
Information
Symposium - International Astronomical Union , Volume 124: Observational Cosmology , 1987 , pp. 187 - 195
Copyright
Copyright © Reidel 1987 

References

Aaronson, M., Bothun, G., Mould, J., Huchra, J., Schommer, R. A., and Cornell, M. E.: 1986, Ap. J., 302, 536 (ABMHSC).CrossRefGoogle Scholar
Aaronson, M., Huchra, J., Mould, J., Schechter, P. L., and Tully, R. B.: 1982, Ap. J., 258, 64 (AHMST).Google Scholar
Aaronson, M., and Mould, J.: 1986, Ap. J., 303, 1.CrossRefGoogle Scholar
Balona, L. A., and Shobbrook, R. R.: 1984, M.N.R.A.S., 211, 375.Google Scholar
Blanco, V. M., and Blanco, B. M.: 1985, Mem. Soc. Astron. Ital., 56, 15.Google Scholar
Bothun, G.: 1986, private communication.Google Scholar
Burstein, D., Davies, R. L., Dressler, A., Faber, S. M., Lynden-Bell, D., Terlevich, R., and Wegner, G.: 1986, in “Galaxy Distances and Deviations from Universal Expansion,” ed. Madore, B. F. and Tully, R. B. (NATO: Brussels); and private communication (BDDFLTW).Google Scholar
Caldwell, J. A. R., and Coulson, I. M.: 1986, M.N.R.A.S., 218, 223.Google Scholar
Caldwell, J. A. R., and Coulson, I. M.: 1987, in preparation.Google Scholar
Chiosi, C., and Pigatto, L.: 1986, Ap. J., 308, 1.Google Scholar
Christian, C. A., and Schommer, R. A.: 1986, preprint.Google Scholar
Collins, A., Joseph, R. D., and Robertson, N. A.: 1986, NATURE, 320, 506.Google Scholar
Conti, P. S., Garmany, C. D., and Massey, P. 1986, A. J., 92, 48.Google Scholar
de Vaucouleurs, G.: 1980, Pub. A.S.P., 92, 579.CrossRefGoogle Scholar
Eggen, O. J.: 1977, Ap. J. Suppl., 34, 1.CrossRefGoogle Scholar
Freedman, W. L.: 1985, in “IAU Colloqiuium 82, Cepheids: Theory and Observation,” ed. Madore, B. F. (Cambridge: Cambridge University Press), p. 225.Google Scholar
Frenk, C. S., and White, S. D. M.: 1982, M.N.R.A.S., 198, 173.Google Scholar
Graham, J. A.: 1984, in “Structure and Evolution of the Magellanic Clouds,” ed. van den Bergh, S. and de Boer, K. S. (Dordrecht: Reidel), p. 207.CrossRefGoogle Scholar
Kerr, F. J., and Lynden-Bell, D.: 1986, M.N.R.A.S., 221, 1023.Google Scholar
Kraan-Korteweg, R. C., Cameron, L. M., and Tammann, G.: 1986, in “Galaxy Distances and Deviations from Universal Expansion,” ed. Madore, B. F. and Tully, R. B. (NATO: Brussels).Google Scholar
Lilje, P. B., Yahil, A., and Jones, B. J. T.: 1986, Ap. J., 307, 91.Google Scholar
Lucey, J. R., Currie, M. J., and Dickens, R. J.: 1986, M.N.R.A.S., 221, 453.Google Scholar
Martin, W. L., Warren, P. R., and Feast, M. W.: 1979, M.N.R.A.S., 188, 139.CrossRefGoogle Scholar
Menzies, J. W., and Whitelock, P. A.: 1985, M.N.R.A.S., 212, 783.CrossRefGoogle Scholar
Pritchet, C. J., and van den Bergh, S.: 1986, preprint.Google Scholar
Reid, I. N., and Strugnell, P. R.: 1986, M.N.R.A.S., 221, 887.Google Scholar
Reid, M. J., et al.: 1987, in “Star Formation,” ed. Peimbert, M. and and Jugaku, J. (Dordrecht: Reidel).Google Scholar
Schmidt, E. G.: 1984, Ap. J., 285, 501.Google Scholar
Sandage, A.: 1986, private communication.Google Scholar
Sandage, A., and Carlson, G.: 1983, Ap. J. (Letters), 267, L25.Google Scholar
Sandage, A., and Tammann, G. A.: 1984, NATURE, 307, 326.Google Scholar
Schommer, R. A.: 1986, in “Galaxy Distances and Deviations from Universal Expansion,” ed. Madore, B. F. and Tully, R. B. (NATO: Brussels).Google Scholar
Schommer, R. A., Olszewski, E. W., and Aaronson, M.: 1984, Ap. J. (Letters), 285, L53.Google Scholar
Seidel, E., Da Costa, G. S., and Demarque, P.: 1986, preprint.Google Scholar
Vittorio, N., Juszkiewicz, R., and Davis, M.: 1986, NATURE, 323, 132.Google Scholar
Walker, A. R.: 1985, M.N.R.A.S., 212, 343.Google Scholar
Yahil, A.: 1986, private communication.Google Scholar