Review article, published in "Astrophysics Update 2 - topical and timely reviews on astronomy and astrophysics". Ed. John W. Mason. Springer/Praxis books. ISBN: 3-540-30312-X. 53
astro-ph/0603031

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Abstract. Ever since their discovery in the 1970's, UltraLuminous InfraRed Galaxies (ULIRGs; classically L_ir > 10¹² L) have fascinated astronomers with their immense luminosities, and frustrated them due to their singularly opaque nature, almost in equal measure. Over the last decade, however, comprehensive observations from the X-ray through to the radio have produced a consensus picture of local ULIRGs, showing that they are mergers between gas rich galaxies, where the interaction triggers some combination of dust-enshrouded starburst and AGN activity, with the starburst usually dominating. Very recent results have thrown ULIRGs even further to the fore. Originally they were thought of as little more than a local oddity, but the latest IR surveys have shown that ULIRGs are vastly more numerous at high redshift, and tantalizing suggestions of physical differences between high and low redshift ULIRGs hint at differences in their formation modes and local environment. In this review we look at recent progress on understanding the physics and evolution of local ULIRGs, the contribution of high redshift ULIRGs to the cosmic infrared background and the global history of star formation, and the role of ULIRGs as diagnostics of the formation of massive galaxies and large-scale structures.

Table of Contents

INTRODUCTION

The Biggest and the Brightest

Overview

THE DISCOVERY OF ULIRGs

THE PHYSICS OF LOCAL ULIRGs

Optical to mid-IR Imaging

Optical & near-IR Spectroscopy

Mid-infrared spectroscopy

Radio Continuum Studies: AGN vs Luminous Radio Supernovae

Molecular gas: CO & HCN Observations

Maser Emission

X-Ray Emission

THE EMERGING PICTURE OF ULIRGs: LOCAL UNIVERSE

ULIRGs AT HIGH REDSHIFT

The cosmic infrared background

Resolving the CIB: LIRGs and ULIRGs at 0 < z < 1.5

Resolving the CIB: ULIRGs at z > 1.5

ULIRGs AND LARGE-SCALE STRUCTURE

OPEN QUESTIONS AND NEW DIRECTIONS

ACKNOWLEDGEMENTS

REFERENCES