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• W2179835331 abstract "It has been 22 years since Jack Baldwin first noticed that there was an inverse correlation between the equivalent width of the C iv emission line and the apparent luminosity of bright quasars. (See J. A. Baldwin, E. J. Wampler, & C. M. Gaskell, ApJ, 338, 630 [1989] for a review and further references.) By using this “Baldwin effect” correlation to calibrate the relative luminosity of quasars, the scatter in the quasar Hubble diagram can be reduced by about a factor of 10. For high-redshift quasars, the data have sufficiently low scatter to discriminate between the different popular cosmologies at high redshift. Early efforts, which ignored possible redshift evolution in the Baldwin effect, give Hubble diagrams that require a high value for q0 ( ). This means that either the Baldwin effect has q ∼ 5 0 strong redshift evolution or the high-redshift quasars are telling us that there was a strong deceleration during the early expansion of the universe. At the end of 1998 May an international conference on the Baldwin effect, “Quasars as Standard Candles for Cosmology,” was held in La Serena, Chile, to review the progress in our understanding of the physical processes important in quasar nuclei where the broad emission lines are formed. It is hoped that with a deeper understanding of quasar central engine chemistry and physics, the source of the Baldwin effect can be identified and understood. It would then be possible to identify any agents that could lead to systematic differences between quasars at different redshifts. In the first talk of the conference, Nick Suntzeff reviewed the new, very accurate data from the distant supernovae (SNe) programs. These data, which have now reached SNe out to redshift 1, indicate that q0 is very small, or possibly negative. If both the quasar data and the SN data are to be believed, then the universe has evolved from an early decelerating universe to the present accelerating universe. The SN data are very convincing. While the scatter in the quasar data is much larger, at redshifts above 2, different models of the universe give very different Hubble diagrams, and small scatter is not needed to distinguish between the models. A much more serious concern is the possible evolution of the Baldwin effect with redshift. Malmquist bias is not likely to be important because quasar subsamples, selected in narrow redshift intervals, show similar Baldwin effect slopes. The zero-point offset of the different" @default.
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• W2179835331 date "1998-11-01" @default.
• W2179835331 modified "2023-09-27" @default.
• W2179835331 title "Conference Highlights: Quasars as Standard Candles for Cosmology" @default.
• W2179835331 doi "https://doi.org/10.1086/316258" @default.
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