A catalogue of the Chandra Deep Field South with multi-colour classification and photometric redshifts from COMBO-17

Wolf, Christian; Meisenheimer, K.; Kleinheinrich, M.; Borch, Andrea; Dye, S.; Gray, Meghan E.; Wisotzki, L.; Bell, Eric F.; Rix, H. W.; Cimatti, A.; Hasinger, G.; Szokoly, G.

doi:10.1051/0004-6361:20040525

Cited by 392 publications

(542 citation statements)

References 30 publications

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“…Since broad-line AGNs are straightforward to identify spectroscopically, even in the so-called redshift ''desert'' at z $ 1:5 2, and since the bulk of the sources in the total X-ray samples have now been spectroscopically observed (see Table 1), we do not need to worry that broad-line AGNs are making up a substantial fraction of the unidentified population. 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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“…2, we summarize our results and compare the H-ATLAS dust temperatures with dust temperatures in the literature for a variety of sub-mm bright galaxies. These samples are: (i) the sources in BLAST detected above 5σ in at least one of the BLAST bands with either a COMBO-17 (Wolf et al 2004) or a SWIRE photometric redshift (Rowan-Robinson et al 2008) and Spitzer-MIPS 70 and 160 μm fluxes (Dye et al 2009; β = 1.5 fixed); (ii) local ULIRGS observed with SCUBA at 450 and 850 μm and complemented with IRAS 60 and 100 μm fluxes ; β varied); (iii) SCUBA sub-mm galaxies detected at better than 3σ at 850 μm and having redshifts determined from Keck-I spectroscopy (Chapman et al 2005; β = 1.5 fixed); and (iv) local IRAS-selected galaxies with 60 and 100 μm fluxes complemented with SCUBA 850 μm (Dunne et al 2000; β varied).…”

Section: Dust Temperature Distributionmentioning

confidence: 99%

Herschel-ATLAS: Dust temperature and redshift distribution of SPIRE and PACS detected sources using submillimetre colours

Amblard¹,

Cooray²,

Serra³

et al. 2010

A&A

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110

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We present colour-colour diagrams of detected sources in the Herschel-ATLAS science demonstration field from 100 to 500 μm using both PACS and SPIRE. We fit isothermal modified black bodies to the spectral energy distribution (SED) to extract the dust temperature of sources with counterparts in Galaxy And Mass Assembly (GAMA) or SDSS surveys with either a spectroscopic or a photometric redshift. For a subsample of 330 sources detected in at least three FIR bands with a significance greater than 3σ, we find an average dust temperature of (28 ± 8) K. For sources with no known redshift, we populate the colour-colour diagram with a large number of SEDs generated with a broad range of dust temperatures and emissivity parameters, and compare to colours of observed sources to establish the redshift distribution of this sample. For another subsample of 1686 sources with fluxes above 35 mJy at 350 μm and detected at 250 and 500 μm with a significance greater than 3σ, we find an average redshift of 2.2 ± 0.6.

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“…The I band magnitudes successively grow from left to right until the emission drops below the spectroscopic sensitivity limit of 8-10 m class telescopes, leaving a lack of spectroscopically identified sources on the on the right-hand side of the plot close to the sensitivity limit. In the CDF-S it is possible to fill this spectroscopic desert with photo-z thanks to a combination of the deep multiwavelength photometry available through GOODS, GEMS and COMBO-17 in this field (Szokoly et al 2004, Zheng et al 2004, Mainieri et al 2005, Wolf et al 2004, Grazian et al 2006. As a result, it is possible to obtain 95% redshift completeness for the CDF-S. Redshift completeness of X-ray flux limited samples is vital to produce statistically and systematically reliable results.…”

Section: Deep Surveysmentioning

confidence: 99%

Evolution of supermassive black holes

Müller

Hasinger

2011

Black Holes

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The cosmological evolution of supermassive black holes (SMBHs) seems to be intimately linked to their host galaxies. Active galactic nuclei (AGN) can be probed by deep X-ray surveys. We review results from large X-ray selected samples including first results from the XMM-Newton COSMOS survey. A new picture arises from the fact that high-luminosity AGN grow earlier than low-luminosity AGN. In particular, the space density of low-luminosity AGN exhibits a significant decline for redshifts above z=1. This "anti-hierarchical" growth scenario of SMBHs can be explained by two modes of accretion with different efficiency. The population of Comptonthick sources plays a key role in our understanding of the BH growth history. Their space density and redshift distribution is relevant to estimate the SMBH mass function. A comparison with the relic SMBH mass distribution in the local Universe constrains the average radiative efficiency and Eddington ratio of the accretion. We discuss a new synthesis model of Compton-thin and Compton-thick sources that is in concordance with deep X-ray observations and in particular predicts the right level of contribution of the Compton-thick source population observed in the Chandra Deep Field South observations as well as the first INTEGRAL and Swift catalogues of AGN. Currently, one of the most important problems is the evolution of obscuration with redshift.

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A catalogue of the Chandra Deep Field South with multi-colour classification and photometric redshifts from COMBO-17

Cited by 392 publications

References 30 publications

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

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

Herschel-ATLAS: Dust temperature and redshift distribution of SPIRE and PACS detected sources using submillimetre colours

Evolution of supermassive black holes

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