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Title:
Resolved CO (1 --> 0) Nuclei in IRAS 14348-1447: Evidence for Massive Bulge Progenitors to Ultraluminous Infrared Galaxies
Authors:
Evans, A. S.; Surace, J. A.; Mazzarella, J. M.
Publication:
The Astrophysical Journal, Volume 529, Issue 2, pp. L85-L88. (ApJ Homepage)
Publication Date:
02/2000
Origin:
UCP
ApJ Keywords:
GALAXIES: ACTIVE, GALAXIES: INDIVIDUAL: ALPHANUMERIC: IRAS 14348-1447, GALAXIES: ISM, INFRARED: GALAXIES, ISM: MOLECULES, RADIO LINES: GALAXIES
DOI:
10.1086/312465
Bibliographic Code:
2000ApJ...529L..85E

Abstract

High-resolution, CO (1 --> 0) interferometry of the ultraluminous infrared galaxy IRAS 14348-1447 is presented. The merger system has a molecular gas mass of ~3x1010 Msolar and a projected nuclear separation of 4.8 kpc (3.5"), making it one of the most molecular gas-rich galaxies known and an ideal candidate for studying the intermediate stages of an ultraluminous merger event. The CO morphology shows two molecular gas components associated with the stellar nuclei of the progenitors, consistent with the idea that the molecular disks are gravitationally bound by the dense bulges of the progenitor galaxies as the interaction proceeds. In contrast, less luminous infrared galaxies observed to date with projected nuclear separations of <~5 kpc show a dominant CO component between the stellar nuclei. This discrepancy may be an indication that the progenitors of mergers with lower infrared luminosity do not possess massive bulges and that the gas is stripped during the initial encounter. A comparison of the CO and radio luminosities of the northeast and southwest components of IRAS 14348-1447 show them to have comparable radio and CO flux ratios of f(NE)/f(SW)~0.6, possibly indicating that the amount of star-forming molecular gas in the progenitors is correlated with the supernovae rate. The estimate of molecular gas masses of the nuclei and the extent of the radio emission are used to infer that the nuclei of IR 14348-1447 have gas densities comparable to the cores of elliptical galaxies.
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