Submillimeter galaxiesIntroductionSubmm-wave emission from galaxiesThe power source for dusty galaxiesContinuum emission from dustThe emission spectrum, dust mass and temperatureThe observed SEDs of dusty galaxiesLine emissionLine emission contribution to continuum detectionsThe observability of high-redshift dusty galaxiesSubmm-wave selection effectsDeep submm-wave surveysSubmm observations of known high-redshift galaxies and QSOsAlternative strategy for deep submm surveysDetermining redshifts of submm galaxiesPhotometric redshifts from far-IR SEDsRadio--submm photometric redshiftsThe observed properties of submm-selected galaxiesConfusionConfusion and follow-up observations of submm galaxiesMulti-waveband follow-up studiesOptical/near-IRUltradeep radio imagesCO rotation line emission and continuum mm-wave interferometryX-ray observationsMid- and far-IR observationsA gallery of follow-up resultsClustering propertiesSubmm galaxy luminosity functions and their relationship with other populationsOptically selected Lyman-break galaxies (LBGs)Extremely red objects (EROs)Faint radio galaxiesActive galaxies and X-ray sourcesGamma-ray burst (GRB) host galaxiesProspects for the follow-up observations in the futureModeling the evolution of submm galaxiesAn array of possible treatmentsObservational tests of modelsModeling the detailed astrophysics of the submm galaxiesThe global evolution of dust-enshrouded galaxiesGravitational lensing in the submm wavebandMagnification biasConditions for exploiting submm lensing by galaxiesProspects for the lensing studies in the futureFuture developments in submm cosmologyNew technologies for instrumentationNew telescopesFuture capabilities and progressSummary: key questions and targets for the futureAcknowledgementsReferencesPhysics Reports 369 (2002) 111–176www.elsevier.com/locate/physrepSubmillimeter galaxiesAndrew W. Blaina; b; ∗, Ian Smailc, R.J. Ivisond, J.-P. Kneibe, David T. FrayerfaDepartment of Astronomy, Caltech, Pasadena, CA 91125, USAbInstitute of Astronomy, Madingley Road, Cambridge CB3 0HA, UKcDepartment of Physics, University of Durham, South Road, Durham DH1 3LE, UKdInstitute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, UKeObservatoire Midi-Pyr-en-ees, 14 Avenue E. Belin, F-31400 Toulouse, FrancefSIRTF Science Center, Caltech, Pasadena, CA 91125, USAReceived 1 January 2002editor: M.P. KamionkowskiAbstractA cosmologically signi4cant population of very luminous high-redshift galaxies has recently been discoveredat submillimeter (submm) wavelengths. Advances in submm detector technologies have opened this newwindow on the distant Universe. Here we discuss the properties of the high-redshift submm galaxies, theirsigni4cance for our understanding of the process of galaxy formation, and the selection e7ects that apply todeep submm surveys. The submm galaxies generate a signi4cant fraction of the energy output of all the galaxiesin the early Universe. We emphasize the importance of studying a complete sample of submm galaxies, andstress that because they are typically very faint in other wavebands, these follow-up observations are verychallenging. Finally, we discuss the surveys that will be made using the next generation of submm-waveinstruments under development.c 2002 Elsevier Science B.V. All rights reserved.PACS: 98.80.Es; 98.62.−gKeywords: Dust extinction; Observational cosmology; Galaxy evolution; Galaxy formation; Gravitational lensing; RadiocontinuumContents1. Introduction ........................................................................................ 1132. Submm-wave emission from galaxies .................................................................. 1162.1. The power source for dusty galaxies .............................................................. 1172.2. Continuum emission from dust ................................................................... 119∗Corresponding author. Department of Astronomy, Caltech, Pasadena, CA 91125, USA.E-mail address: [email protected] (A.W. Blain).0370-1573/02/$ - see front matterc 2002 Elsevier Science B.V. All rights reserved.PII: S 0370-1573(02)00134-5112 A.W. Blain et al. / Physics Reports 369 (2002) 111–1762.2.1. The emission spectrum, dust mass and temperature ........................................... 1202.3. The observed SEDs of dusty galaxies ............................................................. 1222.4. Line emission .................................................................................. 1242.4.1. Line emission contribution to continuum detections .......................................... 1252.5. The observability of high-redshift dusty galaxies .................................................... 1262.6. Submm-wave selection e7ects .................................................................... 1272.7. Deep submm-wave surveys ...................................................................... 1292.8. Submm observations of known high-redshift galaxies and QSOs ...................................... 1302.9. Alternative strategy for deep submm surveys ....................................................... 1332.10. Determining redshifts of submm galaxies .......................................................... 1342.10.1. Photometric redshifts from far-IR SEDs..................................................... 1342.10.2. Radio–submm photometric redshifts ........................................................ 1363. The observed properties of submm-selected galaxies ..................................................... 1393.1. Confusion ..................................................................................... 1433.1.1. Confusion and follow-up observations of submm galaxies ..................................... 1443.2. Multi-waveband follow-up studies ................................................................ 1453.2.1. Optical=near-IR .......................................................................... 1483.2.2. Ultradeep radio images ................................................................... 1493.2.3. CO rotation line emission and continuum mm-wave interferometry ............................. 1493.2.4. X-ray observations ....................................................................... 1503.2.5. Mid- and far-IR observations .............................................................. 1503.3. A gallery of follow-up results