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Ultraluminous Infrared Galaxies

Published online by Cambridge University Press:  25 May 2016

D.B. Sanders ,
J.A. Surace  and
C.M. Ishida
D.B. Sanders
Affiliation:
Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
J.A. Surace
Affiliation:
Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
C.M. Ishida
Affiliation:
Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA

Abstract

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At luminosities above ~ 1011L⊙, infrared galaxies become the dominant population of extragalactic objects in the local Universe (z < 0.5), being more numerous than optically selected starburst and Seyfert galaxies, and QSOs at comparable bolometric luminosity. At the highest luminosities, ultraluminous infrared galaxies (ULIGs: Lir > 1012L⊙), outnumber optically selected QSOs by a factor of ~ 1.5–2. All of the nearest ULIGs (z <0.1) appear to be advanced mergers that are powered by both a circumnuclear starburst and AGN, both of which are fueled by an enormous concentration of molecular gas (~ 1010M⊙) that has been funneled into the merger nucleus. ULIGs may represent a primary stage in the formation of massive black holes and elliptical galaxy cores. The intense circumnuclear starburst that accompanies the ULIG phase may also represent a primary stage in the formation of globular clusters, and the metal enrichment of the intergalactic medium by gas and dust expelled from the nucleus due to the combined forces of supernova explosions and powerful stellar winds.

Type
Nuclear Activity
Information
Symposium - International Astronomical Union , Volume 186: Galaxy Interactions at High and Low Redshift , 1999 , pp. 289 - 294
Copyright
Copyright © Kluwer 1999 

References

Armus, L., Heckman, T.M., & Miley, G.K. 1989, ApJ, 347, 727 CrossRefGoogle Scholar
Barnes, J.E., & Hernquist, L. 1992, ARAA, 30, 705 Google Scholar
Bryant, P.M., & Scoville, N.Z. 1996, ApJ, 457, 678 Google Scholar
Clements, D.L., et al. 1996, MNRAS, 279, 459 Google Scholar
Heckman, T.M., Armus, L., & Miley, G.K. 1987, AJ, 93, 276 Google Scholar
Kim, D.-C. 1995, , University of Hawaii Google Scholar
Kormendy, J., & Richstone, D. 1995, ARAA, 33, 581 Google Scholar
Kormendy, J., & Sanders, D.B. 1992, ApJ, 390, L53 CrossRefGoogle Scholar
Magorrian, J., et al. 1998, AJ, 115, 2285 CrossRefGoogle Scholar
Melnick, J., & Mirabel, I.F. 1990, A&A, 231, L9 Google Scholar
Mihos, J.C., & Hernquist, L. 1994, ApJ, 431, L9 CrossRefGoogle Scholar
Murphy, T.W., et al. 1996, A.J., 111, 1025 CrossRefGoogle Scholar
Perault, M. 1987, , University of Paris Google Scholar
Sanders, D.B., & Mirabel, I.F. 1996, ARAA, 34, 725 Google Scholar
Sanders, D.B., Scoville, N.Z., & Soifer, B.T. 1991, ApJ, 370, 158 Google Scholar
Sanders, D.B., et al. 1987, ApJ, 312, L5 CrossRefGoogle Scholar
Sanders, D.B., et al. 1988a, ApJ, 325, 74 CrossRefGoogle Scholar
Sanders, D.B., et al. 1988b, ApJ, 328, L35 CrossRefGoogle Scholar
Sanders, D.B., et al. 1995, AJ, 110, 1993 Google Scholar
Sanders, D.B., et al. 1998, ApJS, in preparation Google Scholar
Schweizer, F. 1982, ApJ, 252, 455 Google Scholar
Scoville, N.Z., et al. 1989, ApJ, 345, L25 Google Scholar
Scoville, N.Z., Sargent, A.I., Sanders, D.B., & Soifer, B.T. 1991, ApJ, 366, L5 Google Scholar
Soifer, B.T., et al. 1987, ApJ, 320, 238 Google Scholar
Soifer, B.T., et al. 1998, ApJ, submitted Google Scholar
Surace, J.A., & Sanders, D.B. 1999, ApJ, 512, 162 CrossRefGoogle Scholar
Surace, J.A. 1998, , University of Hawaii Google Scholar
Surace, J.A., et al. 1998, ApJ, 492, 116 CrossRefGoogle Scholar
Wright, G.S., James, P.A., Joseph, R.D., & McLean, I.S. 1990, Nature, 344, 417 Google Scholar