We present a study of the host galaxies of active galactic nucleus (AGN) selected from the zCOSMOS survey to establish if accretion onto supermassive black holes (SMBHs) and star formation are explicitly linked up to z similar to 1. We identify 152 galaxies that harbor AGN, based on their X-ray emission (L0.5-10keV > 10(42) erg s(-1)) detected by XMM-Newton observations of 7543 galaxies (i(acs) < 22.5). Star formation rates (SFRs), including those weighted by stellar mass, of a subsample are determined using the [O II]lambda 3727 emission-line luminosity, corrected for an AGN contribution based on the observed [O III]lambda 5007 strength or that inferred by their hard (2-10 keV) X-ray luminosity. We find that an overwhelming majority of AGN host galaxies have significant levels of star formation with a distribution spanning similar to 1-100 M-circle dot yr(-1); their average SFR is higher than that of galaxies with equivalent stellar mass (M-* > 4 x 10(10) M-circle dot). The close association between AGN activity and star formation is further substantiated by an increase in the fraction of galaxies hosting AGN with the youthfulness of their stars as indicated by the rest-frame color (U-V) and spectral index D-n(4000); we demonstrate that a mass-selected sample is required to alleviate an artificial peak in the AGN fraction falling in the transition region due to the fact that many "blue cloud" galaxies have low mass-to-light ratios in luminosity-limited samples. We also find that the SFRs of AGN hosts evolve with cosmic time in a manner that closely mirrors the overall galaxy population and naturally explains the low SFRs in AGNs (z < 0.3) from the SDSS. We conclude that the conditions most conducive for AGN activity are a massive host galaxy and a large reservoir of gas. Furthermore, a direct correlation between mass-accretion rate onto SMBHs and SFR is shown to be weak although the average ratio (similar to 10(-2)) is constant with redshift, effectively shifting the evidence for a co-evolution scenario in a statistical manner to smaller physical scales (i.e., within the same galaxies). The order-of-magnitude increase in this ratio compared to the locally measured value of M-BH/M-bulge is consistent with an AGN lifetime substantially shorter than that of star formation. Our findings illustrate an intermittent scenario with underlying complexities regarding fueling over vastly different physical (and temporal) scales yet to be firmly determined.

ONGOING AND CO-EVOLVING STAR FORMATION IN zCOSMOS GALAXIES HOSTING ACTIVE GALACTIC NUCLEI / Silverman, J. D.; Lamareille, F.; Maier, C.; Lilly, S. J.; Mainieri, V.; Brusa, M.; Cappelluti, N.; Hasinger, G.; Zamorani, G.; Scodeggio, M.; Bolzonella, M.; Contini, T.; Carollo, C. M.; Jahnke, K.; Kneib, J. -P.; Le Fèvre, O.; Merloni, A.; Bardelli, S.; Bongiorno, A.; Brunner, H.; Caputi, K.; Civano, F.; Comastri, A.; Coppa, G.; Cucciati, O.; de la Torre, S.; de Ravel, L.; Elvis, M.; Finoguenov, A.; Fiore, F.; Franzetti, P.; Garilli, B.; Gilli, R.; Iovino, A.; Kampczyk, P.; Knobel, C.; Kovač, K.; Le Borgne, J. -F.; Le Brun, V.; Mignoli, M.; Pello, R.; Peng, Y.; Montero, E. Perez; Ricciardelli, E.; Tanaka, M.; Tasca, L.; Tresse, L.; Vergani, D.; Vignali, C.; Zucca, E.; Bottini, D.; Cappi, A.; Cassata, P.; Fumana, M.; Griffiths, R.; Kartaltepe, J.; Koekemoer, A.; Marinoni, C.; Mccracken, H. J.; Memeo, P.; Meneux, B.; Oesch, P.; Porciani, C.; Salvato, M.. - In: THE ASTROPHYSICAL JOURNAL. - ISSN 0004-637X. - 696:1(2009), pp. 396-410. [10.1088/0004-637X/696/1/396]

ONGOING AND CO-EVOLVING STAR FORMATION IN zCOSMOS GALAXIES HOSTING ACTIVE GALACTIC NUCLEI

Coppa, G.;
2009

Abstract

We present a study of the host galaxies of active galactic nucleus (AGN) selected from the zCOSMOS survey to establish if accretion onto supermassive black holes (SMBHs) and star formation are explicitly linked up to z similar to 1. We identify 152 galaxies that harbor AGN, based on their X-ray emission (L0.5-10keV > 10(42) erg s(-1)) detected by XMM-Newton observations of 7543 galaxies (i(acs) < 22.5). Star formation rates (SFRs), including those weighted by stellar mass, of a subsample are determined using the [O II]lambda 3727 emission-line luminosity, corrected for an AGN contribution based on the observed [O III]lambda 5007 strength or that inferred by their hard (2-10 keV) X-ray luminosity. We find that an overwhelming majority of AGN host galaxies have significant levels of star formation with a distribution spanning similar to 1-100 M-circle dot yr(-1); their average SFR is higher than that of galaxies with equivalent stellar mass (M-* > 4 x 10(10) M-circle dot). The close association between AGN activity and star formation is further substantiated by an increase in the fraction of galaxies hosting AGN with the youthfulness of their stars as indicated by the rest-frame color (U-V) and spectral index D-n(4000); we demonstrate that a mass-selected sample is required to alleviate an artificial peak in the AGN fraction falling in the transition region due to the fact that many "blue cloud" galaxies have low mass-to-light ratios in luminosity-limited samples. We also find that the SFRs of AGN hosts evolve with cosmic time in a manner that closely mirrors the overall galaxy population and naturally explains the low SFRs in AGNs (z < 0.3) from the SDSS. We conclude that the conditions most conducive for AGN activity are a massive host galaxy and a large reservoir of gas. Furthermore, a direct correlation between mass-accretion rate onto SMBHs and SFR is shown to be weak although the average ratio (similar to 10(-2)) is constant with redshift, effectively shifting the evidence for a co-evolution scenario in a statistical manner to smaller physical scales (i.e., within the same galaxies). The order-of-magnitude increase in this ratio compared to the locally measured value of M-BH/M-bulge is consistent with an AGN lifetime substantially shorter than that of star formation. Our findings illustrate an intermittent scenario with underlying complexities regarding fueling over vastly different physical (and temporal) scales yet to be firmly determined.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11696/71443
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