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• W1939777949 endingPage "87" @default.
• W1939777949 startingPage "87" @default.
• W1939777949 abstract "We present results from a ≈100 ks Chandra observation of the 2QZ Cluster 1004+00 structure at z = 2.23 (hereafter 2QZ Clus). 2QZ Clus was originally identified as an overdensity of four optically-selected QSOs at z = 2.23 within a 15 × 15 arcmin2 region. Narrow-band imaging in the near-IR (within the K band) revealed that the structure contains an additional overdensity of 22 z = 2.23 Hα-emitting galaxies (HAEs), resulting in 23 unique z = 2.23 HAEs/QSOs (22 within the Chandra field of view). Our Chandra observations reveal that three HAEs in addition to the four QSOs harbor powerfully accreting supermassive black holes (SMBHs), with 2–10 keV luminosities of ≈(8–60) × 1043 erg s−1 and X-ray spectral slopes consistent with unobscured active galactic nucleus (AGN). Using a large comparison sample of 210 z = 2.23 HAEs in the Chandra-COSMOS field (C-COSMOS), we find suggestive evidence that the AGN fraction increases with local HAE galaxy density. The 2QZ Clus HAEs reside in a moderately overdense environment (a factor of ≈2 times over the field), and after excluding optically-selected QSOs, we find that the AGN fraction is a factor of ≈3.5+3.8−2.2 times higher than C-COSMOS HAEs in similar environments. Using stacking analyses of the Chandra data and Herschel SPIRE observations at 250 μm, we respectively estimate mean SMBH accretion rates () and star formation rates (SFRs) for the 2QZ Clus and C-COSMOS samples. We find that the mean 2QZ Clus HAE stacked X-ray luminosity is QSO-like (L2-10 keV ≈ [6–10] × 1043 erg s−1), and the implied /SFR ≈ (1.6–3.2) × 10−3 is broadly consistent with the local MBH/M⋆ relation and z ≈ 2 X-ray selected AGN. In contrast, the C-COSMOS HAEs are on average an order of magnitude less X-ray luminous and have /SFR ≈ (0.2–0.4) × 10−3, somewhat lower than the local MBH/M⋆ relation, but comparable to that found for z ≈ 1–2 star-forming galaxies with similar mean X-ray luminosities. We estimate that a periodic QSO phase with duty cycle ≈2%–8% would be sufficient to bring star-forming galaxies onto the local MBH/M⋆ relation. This duty cycle is broadly consistent with the observed C-COSMOS HAE AGN fraction (≈0.4%–2.3%) for powerful AGN with LX ≳ 1044 erg s−1. Future observations of 2QZ Clus will be needed to identify key factors responsible for driving the mutual growth of the SMBHs and galaxies." @default.
• W1939777949 created "2016-06-24" @default.
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• W1939777949 date "2013-02-20" @default.
• W1939777949 modified "2023-10-16" @default.
• W1939777949 title "CONCURRENT SUPERMASSIVE BLACK HOLE AND GALAXY GROWTH: LINKING ENVIRONMENT AND NUCLEAR ACTIVITY IN<i>z</i>= 2.23 Hα EMITTERS" @default.
• W1939777949 cites W1492972489 @default.
• W1939777949 cites W1575728940 @default.
• W1939777949 cites W1681070356 @default.
• W1939777949 cites W1924766263 @default.
• W1939777949 cites W1938555805 @default.
• W1939777949 cites W1975780632 @default.
• W1939777949 cites W1977796024 @default.
• W1939777949 cites W1985952407 @default.
• W1939777949 cites W1991788629 @default.
• W1939777949 cites W2015353002 @default.
• W1939777949 cites W2025968438 @default.
• W1939777949 cites W2029445285 @default.
• W1939777949 cites W2030627151 @default.
• W1939777949 cites W2048186190 @default.
• W1939777949 cites W2054131667 @default.
• W1939777949 cites W2067509014 @default.
• W1939777949 cites W2081265738 @default.
• W1939777949 cites W2081879654 @default.
• W1939777949 cites W2088761263 @default.
• W1939777949 cites W2090459210 @default.
• W1939777949 cites W2096017091 @default.
• W1939777949 cites W2100336040 @default.
• W1939777949 cites W2101701816 @default.
• W1939777949 cites W2104127586 @default.
• W1939777949 cites W2106708461 @default.
• W1939777949 cites W2110021525 @default.
• W1939777949 cites W2112152942 @default.
• W1939777949 cites W2115659244 @default.
• W1939777949 cites W2118265220 @default.
• W1939777949 cites W2121173473 @default.
• W1939777949 cites W2125383073 @default.
• W1939777949 cites W2125489913 @default.
• W1939777949 cites W2129276959 @default.
• W1939777949 cites W2129760210 @default.
• W1939777949 cites W2130843916 @default.
• W1939777949 cites W2131150711 @default.
• W1939777949 cites W2131546154 @default.
• W1939777949 cites W2132711591 @default.
• W1939777949 cites W2133030092 @default.
• W1939777949 cites W2134770152 @default.
• W1939777949 cites W2138158862 @default.
• W1939777949 cites W2147024658 @default.
• W1939777949 cites W2147847259 @default.
• W1939777949 cites W2151119306 @default.
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• W1939777949 cites W2158454843 @default.
• W1939777949 cites W2162125418 @default.
• W1939777949 cites W2165265292 @default.
• W1939777949 cites W3098347591 @default.
• W1939777949 cites W3099149995 @default.
• W1939777949 cites W3099428329 @default.
• W1939777949 cites W3099471130 @default.
• W1939777949 cites W3099949614 @default.
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• W1939777949 doi "https://doi.org/10.1088/0004-637x/765/2/87" @default.
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