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dc.contributor.authorPage, M. J.-
dc.contributor.authorStevens, J. A.-
dc.contributor.authorMittaz, J. P. D.-
dc.contributor.authorCarrera, Francisco J.-
dc.date.accessioned2008-05-04T18:55:01Z-
dc.date.available2008-05-04T18:55:01Z-
dc.date.issued2002-02-05-
dc.identifier.citationScience 294(5551): 2516-2518 (2001)en_US
dc.identifier.issn0036-8075-
dc.identifier.urihttp://hdl.handle.net/10261/3978-
dc.description.abstractThe correlation, found in nearby galaxies, between black hole mass and stellar bulge mass implies that the formation of these two components must be related. Here we report submillimeter photometry of eight x-ray absorbed active galactic nuclei which have luminosities and redshifts characteristic of the sources that produce the bulk of the accretion luminosity in the universe. The four sources with the highest redshifts are detected at 850 microns, with flux densities between 5.9 and 10.1 milliJanskies, and hence are ultraluminous infrared galaxies. Interpreting the submillimeter flux as emission from dust heated by starbursts, these results suggest that the majority of stars in spheroids were formed at the same time as their central black holes built up most of their mass by accretion, accounting for the observed demography of massive black holes in the local universe. The skewed rate of submillimeter detection with redshift is consistent with a high redshift epoch of star formation in radio quiet active galactic nuclei, similar to that seen in radio galaxies.en_US
dc.format.extent128877 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoengen_US
dc.publisherAmerican Association for the Advancement of Scienceen_US
dc.relation.isversionofPreprint-
dc.rightsopenAccessen_US
dc.subjectBlack holesen_US
dc.subjectStellar bulgesen_US
dc.subjectMass correlationen_US
dc.subjectAccretion luminosityen_US
dc.subjectSubmillimeter fluxen_US
dc.subjectAstrophysicsen_US
dc.titleSubmillimeter evidence for the coeval growth of massive black holes and galaxy bulgesen_US
dc.typeartículoen_US
dc.identifier.doi10.1126/science.1065880-
dc.description.peerreviewedPeer revieweden_US
dc.relation.publisherversionhttp://dx.doi.org/10.1126/science.1065880-
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