Caunto et al. 1979

Caunto, V.M., S.-H. Hsieh, and J.R. Owen, 1979: Scale covariance and G-varying cosmology. III. The (m,z), (θ_m,z), (θ_t,z), and (N(m),m) tests. Astrophys. J. Supp. Series, 41, 263-300, doi:10.1086/190619.

Within the context of the recently proposed scale-covariant cosmology we present in this paper: (a) the full solution to Einstein gravitational equations in atomic units for a matter-dominated universe, (b) the study of the magnitude versus redshift relation for elliptical galaxies, (c) the derivation of the evolutionaary parameter used in (b), (d) the isophotal angular diameters versus redshifts, (e) the metric angular parameters versus red-shifts, and finally (f) the N(m) versus magnitude relation for QSOs and their m versus z relation.

The results, both in graphical and tabular form, are presented for the four gauges [i.e., relation between G and the scale function β(t)] introduced and studied in previous works.

No contradiction between the new theory and the data is found with any of the tests studied.

If we chose the gauges with ε < 0, β ~ t^-ε, as suggested by a recent analysis of the time variation, of the Moon's period, only an open universe can fit the data.

For the gauges with ε > 0, the results become very familiar to those of standard cosmology.

As for QSOs, since we cannot evaluate the evolutionary parameter as we did in the case of elliptical galaxies, we determine it by requiring that the log N(m) versus m relation has an average slope derived from recently published data. It is shown that such an evolutionary parameter yields a satusfactory m versus z relation for QSOs. When the same procedure is applied to standard cosmology, the results are less satisfactory.

Consideration concerning the radiation-dominated universe are briefly discussed at the end. Finally, we introduce the concept of "lens effect" (section VIII). The time dependence of G can be thought of as indicating that gravitational phenomena, when viewed through atomic measurements, can be either magnified or reduced, thus changing the relation between density of matter and space curvature. The implications of this new feature for the geometry of the universe are discussed.

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Caunto, V.M., Hsieh, S.-H., and Owen, J.R.: Scale covariance and G-varying cosmology. III. The (m,z), (θ_m,z), (θ_t,z), and (N(m),m) tests, Astrophys. J. Supp. Series, 41, 263-300, doi:10.1086/190619, 1979.

Caunto, V.M., S.-H. Hsieh, and J.R. Owen (1979), Scale covariance and G-varying cosmology. III. The (m,z), (θ_m,z), (θ_t,z), and (N(m),m) tests, Astrophys. J. Supp. Series, 41, 263-300, doi:10.1086/190619.

Caunto, V.M., S.-H. Hsieh, and J.R. Owen, 1979: Scale covariance and G-varying cosmology. III. The (m,z), (θ_m,z), (θ_t,z), and (N(m),m) tests. Astrophys. J. Supp. Series, 41, 263-300, doi:10.1086/190619.

Caunto, V.M., Hsieh, S.-H., & Owen, J.R. 1979, Astrophys. J. Supp. Series, 41, 263, doi:10.1086/190619.

Caunto VM, Hsieh S-H, Owen JR. Scale covariance and G-varying cosmology. III. The (m,z), (θ_m,z), (θ_t,z), and (N(m),m) tests, Astrophys J Supp Series 1979;41:263-300. doi:10.1086/190619.

V.M. Caunto, S.-H. Hsieh, J.R. Owen, Astrophys. J. Supp. Series 41, 263-300, doi:10.1086/190619 (1979).