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- W1972308849 abstract "Approximately 20%-30% of 1.4 ≲ z ≲ 2.5 galaxies with KVega < 22 detected with Spitzer MIPS at 24 μm show excess mid-IR emission relative to that expected based on the rates of star formation measured from other multiwavelength data. These galaxies also display some near-IR excess in Spitzer IRAC data, with an SED peaking longward of 1.6 μm in the rest frame, indicating the presence of warm dust emission usually absent in star-forming galaxies. Stacking Chandra data for the mid-IR excess galaxies yields a significant hard X-ray detection at rest-frame energies >6.2 keV. The stacked X-ray spectrum rises steeply at >10 keV, suggesting that these sources host Compton-thick AGNs with column densities NH ≳ 1024 cm-2 and an average, unobscured X-ray luminosity L2-8 keV ≈ (1-4) × 1043 ergs s-1. Their sky density (~3200 deg-2) and space density (~2.6 × 10-4 Mpc-3) are twice those of X-ray-detected AGNs at z ≈ 2, and much larger than those of previously known Compton-thick sources at similar redshifts. The mid-IR excess galaxies are part of the long sought after population of distant heavily obscured AGNs predicted by synthesis models of the X-ray background. The fraction of mid-IR excess objects increases with galaxy mass, reaching ~50%-60% for M ~ 1011 M☉, an effect likely connected with downsizing in galaxy formation. The ratio of the inferred black hole growth rate from these Compton-thick sources to the global star formation rate at z = 2 is similar to the mass ratio of black holes to stars in local spheroids, implying concurrent growth of both within the precursors of today's massive galaxies." @default.
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- W1972308849 date "2007-11-20" @default.
- W1972308849 modified "2023-09-30" @default.
- W1972308849 title "Multiwavelength Study of Massive Galaxies at<i>z</i> ∼ 2. II. Widespread Compton‐thick Active Galactic Nuclei and the Concurrent Growth of Black Holes and Bulges" @default.
- W1972308849 cites W1497175568 @default.
- W1972308849 cites W1582758454 @default.
- W1972308849 cites W1914598719 @default.
- W1972308849 cites W1961625706 @default.
- W1972308849 cites W1965134192 @default.
- W1972308849 cites W1966503522 @default.
- W1972308849 cites W1968646907 @default.
- W1972308849 cites W1970660289 @default.
- W1972308849 cites W1972507852 @default.
- W1972308849 cites W1973939397 @default.
- W1972308849 cites W1976615408 @default.
- W1972308849 cites W1979115990 @default.
- W1972308849 cites W1981769908 @default.
- W1972308849 cites W1981936828 @default.
- W1972308849 cites W1985952407 @default.
- W1972308849 cites W1986486448 @default.
- W1972308849 cites W1989738078 @default.
- W1972308849 cites W2001198139 @default.
- W1972308849 cites W2002044265 @default.
- W1972308849 cites W2002467915 @default.
- W1972308849 cites W2006316173 @default.
- W1972308849 cites W2007125765 @default.
- W1972308849 cites W2011087021 @default.
- W1972308849 cites W2011881697 @default.
- W1972308849 cites W2013375438 @default.
- W1972308849 cites W2016121098 @default.
- W1972308849 cites W2017450908 @default.
- W1972308849 cites W2018489450 @default.
- W1972308849 cites W2020747414 @default.
- W1972308849 cites W2021194233 @default.
- W1972308849 cites W2022429453 @default.
- W1972308849 cites W2025338816 @default.
- W1972308849 cites W2027713091 @default.
- W1972308849 cites W2027744705 @default.
- W1972308849 cites W2028229318 @default.
- W1972308849 cites W2030944204 @default.
- W1972308849 cites W2035199026 @default.
- W1972308849 cites W2036319176 @default.
- W1972308849 cites W2036920580 @default.
- W1972308849 cites W2039847154 @default.
- W1972308849 cites W2042692850 @default.
- W1972308849 cites W2052151970 @default.
- W1972308849 cites W2055686415 @default.
- W1972308849 cites W2057015950 @default.
- W1972308849 cites W2070952256 @default.
- W1972308849 cites W2074175398 @default.
- W1972308849 cites W2074255988 @default.
- W1972308849 cites W2074320758 @default.
- W1972308849 cites W2075831123 @default.
- W1972308849 cites W2079227246 @default.
- W1972308849 cites W2081248194 @default.
- W1972308849 cites W2085122822 @default.
- W1972308849 cites W2089065940 @default.
- W1972308849 cites W2089107762 @default.
- W1972308849 cites W2090459210 @default.
- W1972308849 cites W2092504858 @default.
- W1972308849 cites W2100739331 @default.
- W1972308849 cites W2103924419 @default.
- W1972308849 cites W2109104929 @default.
- W1972308849 cites W2110833048 @default.
- W1972308849 cites W2122471784 @default.
- W1972308849 cites W2124219338 @default.
- W1972308849 cites W2125977823 @default.
- W1972308849 cites W2127772312 @default.
- W1972308849 cites W2128089313 @default.
- W1972308849 cites W2129276959 @default.
- W1972308849 cites W2129760210 @default.
- W1972308849 cites W2129883223 @default.
- W1972308849 cites W2132007051 @default.
- W1972308849 cites W2132711591 @default.
- W1972308849 cites W2135894620 @default.
- W1972308849 cites W2144320326 @default.
- W1972308849 cites W2147847259 @default.
- W1972308849 cites W2150995848 @default.