The Team Keck Treasury Redshift Survey of the GOODS-North Field

Wirth, Gregory D.; Willmer, Christopher N. A.; Amico, Paola; Chaffee, Frederic H.; Goodrich, Robert W.; Kwok, S.; Lyke, James E.; Mader, J.; Tran, H. D.; Barger, A. J.; Cowie, L. L.; Capak, P.; Coil, Alison L.; Cooper, Michael C.; Conrad, Al; Davis, Marc; Faber, S. M.; Hu, E. M.; Koo, David C.; Mignant, D. Le; Newman, Jeffrey A.; Songaila, A.

doi:10.1086/420999

Cited by 281 publications

(306 citation statements)

References 35 publications

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“…In fact, at 16 < R < 24, deep Chandra observations have picked up all of the color-selected quasars identified by the COMBO-17 survey in their fields of view (Wolf et al 2004). Moreover, deep Chandra observations have picked up all of the spectroscopically identified broad-line AGNs in the highly spectroscopically complete (to R ¼ 24:5; Cowie et al 2004b;Wirth et al 2004) ACS GOODS-North region of the CDF-N (see x 3).…”

Section: X-ray Luminositiesmentioning

confidence: 99%

The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei

et al. 2005

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We use highly spectroscopically complete deep and wide-area Chandra surveys to determine the cosmic evolution of hard X-ray-selected active galactic nuclei (AGNs). For the deep fields, we supplement the spectroscopic redshifts with photometric redshifts to assess where the unidentified sources are likely to lie. We find that the median redshifts are fairly constant with X-ray flux at z $ 1.We classify the optical spectra and measure the FWHM line widths. Most of the broad-line AGNs show essentially no visible absorption in X-rays, whereas the sources without broad lines (FWHM < 2000 km s À1 ; ''optically narrow'' AGNs) show a wide range of absorbing column densities. We determine hard X-ray luminosity functions for all spectral types with L X ! 10 42 ergs s À1 and for broad-line AGNs alone. At z < 1:2, both are well described by pure luminosity evolution, with L * evolving as (1 þ z) 3:2AE0:8 for all spectral types and as (1 þ z) 3:0AE1:0 for broad-line AGNs alone. Thus, all AGNs drop in luminosity by almost an order of magnitude over this redshift range. We show that this observed drop is due to AGN downsizing rather than to an evolution in the accretion rates onto the supermassive black holes.We directly compare our broad-line AGN hard X-ray luminosity functions with the optical QSO luminosity functions and find that at the bright end they agree extremely well at all redshifts. However, the optical QSO luminosity functions do not probe faint enough to see the downturn in the broad-line AGN hard X-ray luminosity functions and even appear to be missing some sources at the lowest luminosities they probe.We find that broad-line AGNs dominate the number densities at the higher X-ray luminosities, while optically narrow AGNs dominate at the lower X-ray luminosities. We rule out galaxy dilution as a partial explanation for this effect by measuring the nuclear UV/optical properties of the Chandra sources using the Hubble Space Telescope Advanced Camera for Surveys GOODS-North data. The UV/optical nuclei of the optically narrow AGNs are much weaker than expected if the optically narrow AGNs were similar to the broad-line AGNs. We therefore postulate the need for a luminosity-dependent unified model. An alternative possibility is that the broad-line AGNs and the optically narrow AGNs are intrinsically different source populations. We cover both interpretations by constructing composite spectral energy distributions-including long-wavelength data from the mid-infrared to the submillimeterby spectral type and by X-ray luminosity. We use these spectral energy distributions to infer the bolometric corrections (from hard X-ray luminosities to bolometric luminosities) needed to map the accretion history.We determine the accreted supermassive black hole mass density for all spectral types and for broad-line AGNs alone, using the observed evolution of the hard X-ray energy density production rate and our inferred bolometric corrections. We find that only about one-half to one-quarter of the supermassive black hole mass ...

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Section: X-ray Luminositiesmentioning

confidence: 99%

The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei

et al. 2005

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“…In the CDF-N we used spectroscopic redshifts from DEEP3 (Cooper et al 2011) as well as the surveys of Trouille et al (2008); Barger et al (2008); Reddy et al (2006); Wirth et al (2004); Cowie et al (2004) and Steidel et al (2003).…”

Section: Spectroscopic Redshiftsmentioning

confidence: 99%

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

Aird

Coil

Georgakakis

et al. 2015

Monthly Notices of the Royal Astronomical Society

373

559

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We present new measurements of the evolution of the X-ray luminosity functions (XLFs) of unabsorbed and absorbed Active Galactic Nuclei (AGNs) out to z ∼ 5. We construct samples containing 2957 sources detected at hard (2-7 keV) X-ray energies and 4351 sources detected at soft (0.5-2 keV) energies from a compilation of Chandra surveys supplemented by wide-area surveys from ASCA and ROSAT. We consider the hard and soft X-ray samples separately and find that the XLF based on either (initially neglecting absorption effects) is best described by a new flexible model parametrization where the break luminosity, normalization and faint-end slope all evolve with redshift. We then incorporate absorption effects, separately modelling the evolution of the XLFs of unabsorbed (20 < log N H < 22) and absorbed (22 < log N H < 24) AGNs, seeking a model that can reconcile both the hard-and soft-band samples. We find that the absorbed AGN XLF has a lower break luminosity, a higher normalization, and a steeper faint-end slope than the unabsorbed AGN XLF out to z ∼ 2. Hence, absorbed AGNs dominate at low luminosities, with the absorbed fraction falling rapidly as luminosity increases. Both XLFs undergo strong luminosity evolution which shifts the transition in the absorbed fraction to higher luminosities at higher redshifts. The evolution in the shape of the total XLF is primarily driven by the changing mix of unabsorbed and absorbed populations.

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“…In this study we use spectroscopic redshifts coming from a combination of various studies (Cohen et al 2000;Wirth et al 2004;Cowie et al 2004;Le Fèvre et al 2004;Mignoli et al 2005;Vanzella et al 2006;Reddy et al 2006;Barger et al 2008;Cimatti et al 2008;Kurk et al in prep. for GMASS redshifts and finally Stern et al in prep.).…”

Section: Redshiftsmentioning

confidence: 99%

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

Magnelli

Elbaz

Chary

et al. 2011

A&A

352

422

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Aims. We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24 and 70 μm imaging of the GOODS North and South fields. Methods. We use an extraction technique based on prior source positions at shorter wavelengths to build the 24 and 70 μm source catalogs. The majority (93%) of the sources have a spectroscopic (39%) or a photometric redshift (54%) and, in our redshift range of interest (i.e., 1.3 < z < 2.3) ∼20% of the sources have a spectroscopic redshift. To extend our study to lower 70 μm luminosities we perform a stacking analysis and we characterize the observed L 24/(1+z) vs. L 70/(1+z) correlation. Using spectral energy distribution (SED) templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24 and 70 μm luminosities. We then compute the infrared LF at z ∼ 1.55 ± 0.25 and z ∼ 2.05 ± 0.25. Results. We observe the break in the infrared LF up to z ∼ 2.3. The redshift evolution of the infrared LF from z = 1.3 to z = 2.3 is consistent with a luminosity evolution proportional to (1 + z) 1.0±0.9 combined with a density evolution proportional to (1 + z) −1.1±1.5 . At z ∼ 2, luminous infrared galaxies (LIRGs: 10 11 L < L IR < 10 12 L ) are still the main contributors to the total comoving infrared luminosity density of the Universe. At z ∼ 2, LIRGs and ultra-luminous infrared galaxies (ULIRGs: 10 12 L < L IR ) account for ∼49% and ∼17% respectively of the total comoving infrared luminosity density of the Universe. Combined with previous results using the same strategy for galaxies at z < 1.3 and assuming a constant conversion between the infrared luminosity and star-formation rate (SFR) of a galaxy, we study the evolution of the SFR density of the Universe from z = 0 to z = 2.3. We find that the SFR density of the Universe strongly increased with redshift from z = 0 to z = 1.3, but is nearly constant at higher redshift out to z = 2.3. As part of the online material accompanying this article, we present source catalogs at 24 μm and 70 μm for both the GOODS-North and -South fields.

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The Team Keck Treasury Redshift Survey of the GOODS-North Field

Cited by 281 publications

References 35 publications

The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei

The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

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