Pulsars, transients and relativistic astrophysics

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Abundance Gradients from Massive, Early-Type Stars — the Milky Way and Beyond

Chapter in Chemical Evolution from Zero to High Redshift, Springer Nature (1999) 24-29
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Completeness and confusion in the identification of Lyman-break galaxies

HY-REDSHIFT UNIVERSE: GALAXY FORMATION AND EVOLUTION AT HIGH REDSHIFT 193 (1999) 513-516

Authors:

G Cotter, T Haynes, JC Baker, ME Jones, R Saunders
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High-z radio galaxies and the 'youth-redshift degeneracy'

ASTR SOC P 193 (1999) 75-78

Authors:

KM Blundell, S Rawlings

Abstract:

We discuss a unifying explanation for many 'trends with redshift' of radio galaxies which includes the relevance of their ages (time since their jet triggering event), and the marked dependence of their ages on redshift due to the selection effect of imposing a flux-limit. We briefly describe some important benefits which this 'youth-redshift degeneracy' brings.
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Infrared spectroscopic variability of Cygnus X-3

Symposium - International Astronomical Union Cambridge University Press (CUP) 193 (1999) 358-359

Authors:

Margaret M Hanson, Rob P Fender, GG Pooley
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No evidence for a 'redshift cut-off' for the most powerful classical double radio sources

ASTR SOC P 193 (1999) 90-93

Authors:

MJ Jarvis, S Rawlings, CJ Willott, KM Blundell, S Eales, M Lacy

Abstract:

We use three samples (3CRR, 6CE and 6C*) to investigate the radio luminosity function (RLF) for the 'most powerful' low-frequency selected radio sources. We find that the data are well fitted by a model with a constant ca-moving space density at high redshift as well as by one with a declining co-moving space density above some particular redshift. This behaviour is very similar to that inferred for steep-spectrum radio quasars by Willott et al (1998) in Line with the expectations of Unified Schemes. We conclude that there is as yet no evidence for a 'redshift cutoff' in the co-moving space densities of powerful classical double radio sources, and rule out a art-off at z less than or similar to 2.5.
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