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Article Contents

ABSTRACT

1.INTRODUCTION
1.1.Scope of this article - HzRGs
1.2.History
1.3.Hunting for HzRGs
1.4.Redshift distribution of HzRGs
1.5.Constituents of HzRGs

2.RELATIVISTIC PLASMA
2.1.HzRGS and low-redshift radio galaxies
2.2.Radio sizes and morphologies. Size as an evolutionary clock
2.3.Radio size vs redshift correlation
2.4.Radio spectral index vs redshift correlation
2.5.Nonthermal X-ray emission

3.GAS AND DUST
3.1.Hot ionised gas - Radio depolarization
3.2.Warm ionized gas
3.3.Neutral Gas
3.4.Molecular Gas
3.5.Dust

4.STARS
4.1.Old stars: HzRGs as the most massive galaxies
4.2.Young stars - UV absorption lines
4.3.The alignment effect - Jet-induced star formation

5.ACTIVE GALACTIC NUCLEUS (AGN)
5.1.Hidden or dormant quasar - The Unification Church
5.2.Supermassive black hole - Powerhouse of the AGN
5.3.Extinction of the "dinosaurs"

6.NATURE OF HzRG HOSTS - MASSIVE FORMING GALAXIES
6.1.The Spiderweb Galaxy - a case study

7.ENVIRONMENT OF HzRGS - PROTOCLUSTERS
7.1.Finding protoclusters using HzRGs
7.2.Properties of radio-selected protoclusters
7.3.Are radio-selected protoclusters typical?
7.4.Protocluster evolution

8.CONCLUSIONS AND FUTURE

9.APPENDIX: KNOWN HzRGs

REFERENCES