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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