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Herschel ATLAS: The cosmic star formation history of quasar host galaxies

AutorSerjeant, S.; Herranz, D. ; López-Caniego, M.
Palabras claveGalaxies: active
Infrared: galaxies
Quasars: general
Galaxies: formation
Submillimeter: galaxies
Galaxies: starburst
Fecha de publicación2010
EditorEDP Sciences
CitaciónAstronomy and Astrophysics 518: L7 (2010)
ResumenWe present a derivation of the star formation rate per comoving volume of quasar host galaxies, derived from stacking analyses of far-infrared to mm-wave photometry of quasars with redshifts 0 < z < 6 and absolute I-band magnitudes -22 > IAB > -32 We use the science demonstration observations of the first ~16 deg2 from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) in which there are 240 quasars from the Sloan Digital Sky Survey (SDSS) and a further 171 from the 2dF-SDSS LRG and QSO (2SLAQ) survey. We supplement this data with a compilation of data from IRAS, ISO, Spitzer, SCUBA and MAMBO. H-ATLAS alone statistically detects the quasars in its survey area at >5σ at 250,350 and 500 μm. From the compilation as a whole we find striking evidence of downsizing in quasar host galaxy formation: low-luminosity quasars with absolute magnitudes in the range -22 > IAB > -24 have a comoving star formation rate (derived from 100 μm rest-frame luminosities) peaking between redshifts of 1 and 2, while high-luminosity quasars with IAB < -26 have a maximum contribution to the star formation density at z ~ 3. The volume-averaged star formation rate of -22 > IAB > -24 quasars evolves as (1 + z)2.3±0.7 at z < 2, but the evolution at higher luminosities is much faster reaching (1 + z)10±1 at -26 > IAB > -28. We tentatively interpret this as a combination of a declining major merger rate with time and gas consumption reducing fuel for both black hole accretion and star formation.
Descripción5 páginas, 2 figuras, 1 tabla.-- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia with important participation from NASA.-- et al.
Versión del editorhttp://dx.doi.org/10.1051/0004-6361/201014565
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