X-ray spectral properties of active galactic nuclei in the Chandra

By P. Tozzi, R. Gilli, V. Mainieri, G. Risaliti, Piero Rosati, Stefano Borgani, R. Giacconi, G. Hasinger, M. Nonino, A. Streblyanska and 1 more. 2006

297 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/a10f5f41226c00f5ae14dfb4da4d7a62aeb1bd93

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1. P. Hopkins
2. D. M. Alexander
3. W. N. Brandt
4. E. Daddi
5. L. Hernquist
6. R. Somerville
7. R. Dav'e
8. P. Santini

Citations in the corpus

• Spitzer Power-Law Active Galactic Nucleus Candidates in the Chandra Deep Field-North (2007, methodology): “The intrinsic photon index was drawn from the distribution of Tozzi et al (2006), as measured for the brightest 30 sources in their sample:Γ = 1.81± 0.20.”
• ONGOING AND CO-EVOLVING STAR FORMATION IN zCOSMOS GALAXIES HOSTING ACTIVE GALACTIC NUCLEI (2008, background): “…AGN (LX ∼ 10 43 erg s−1), detected in medium-to-deep X-ray observations, have been shown to be ideal laboratories for the study of their host galaxies due to their low optical brightness which in many cases is due to their nuclear obscuration (e.g., Tozzi et al. 2006; Mainieri et al. 2007).”
• The synthesis of the cosmic X-ray background in the Chandra and XMM-Newton era (2006, methodology): “In particular Akylas et al. (2006) suggestedhat the apparent increase in the obscured AGN fraction with redshift is due to a systematic overestimate of the column densiti s measured in high redshift sources where the absorption cut–off is shifted towards low energies (see also Tozzi et al. 2006).”
• An Observational Determination of the Bolometric Quasar Luminosity Function (2006, methodology): “…estimate these dispersions in the power-law components of our modeling from the observed distributions, assuming that they are normally distributed: o 0:125 (Richards et al. 2003; comparing the mean o in each observed quartile), ¼ 0:30 (Tozzi et al. 2006), and ox ¼ 0:075Y0:14 (Steffen et al. 2006).”
• The incidence of obscuration in active galactic nuclei (2013, background): “Large, systematic studies of their spectral energy distribution (SED) clearly show that the intrinsic shape of the X-ray continuum can be characterized by a power law in the 2– 10 keV energy range, with a relative narrow distribution of slopes: 〈 〉 = 1.8 ± 0.2 (Nandra & Pounds 1994; Steffen et al. 2”
• The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer (2007, methodology): “In the CDF-S, we used the catalogs published by Giacconi et al. (2002, see also Tozzi et al. 2006) for the 1 Ms Chandra Deep Field-South Survey, identifying 3% of our IRAC sources as X-ray emitters (2% of the I-band sample).”
• Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, background): “In particular, they calculated the expected fraction between observed and unabsorbed 2–10 keV X-ray luminosity, by assuming a canonical AGN X-ray spectrum (absorbed power-law with photon index Γ=1.8; Tozzi et al. 2006), and as a function of obscuration in the range 21 < log(NH/cm −2) < 24.”
• What drives the growth of black holes (2011, background): “6 of Brandt & Hasinger 2005) out to z ≈ 1–2, even in the presence of large amounts of absorption (up-to NH ≈ 1023–1024 cm−2; e.g., Tozzi et al. 2006; Raimundo et al. 2010; Alexander et al. 2011; Comastri et al. 2011; Feruglio et al. 2011); AGNs ≈ 1–2 orders of magnitude brighter can be identified…”
• IDENTIFYING LUMINOUS ACTIVE GALACTIC NUCLEI IN DEEP SURVEYS: REVISED IRAC SELECTION CRITERIA (2012, methodology): “…an apparent discrepancy whose proposed explanations include spectral variability, host galaxy dilution, and disappearance of the broad-line region in AGN accreting at L/LEdd ≤ 0.01 (e.g., Tozzi et al. 2006; Page et al. 2006; Caccianiga et al. 2007; Trouille et al. 2009; Trump et al. 2009, 2011b,a).”
• Unveiling Obscured Accretion in the Chandra Deep Field-South (2007, background): “Indeed, these sources are among the most obscured ones in the Tozzi et al (2006) analysis, all having column densities higher than a few×1022 cm−2 and 2 having column densities as high as 1024 cm−2.”
• A synthesis model for AGN evolution: supermassive black holes growth and feedback modes (2008, unknown): “No significant trend with redshift is instead evident, similarly to what is known for the spectral properties of type I AGN in the X-ray band alone (Vignali, Brandt & Schneider 2003; Tozzi et al. 2006; Steffen et al. 2006).”
• THE SPACE DENSITY OF COMPTON-THICK ACTIVE GALACTIC NUCLEUS AND THE X-RAY BACKGROUND (2009, methodology): “However, no overlap is found between the reflection-dominated CT AGN candidates reported by Tozzi et al. (2006) and the flat-spectrum sources of Georgantopoulos et al. (2007).”
• A Catalog of Galaxy Clusters Observed by XMM-Newton (2007, background): “There is considerable discussion concerning the uniformity of this emission over the sky and what the true form of the spectrum is (e.g., whether the slope changes for energies less than 1 keV, Tozzi et al. 2006).”
• TOWARD THE STANDARD POPULATION SYNTHESIS MODEL OF THE X-RAY BACKGROUND: EVOLUTION OF X-RAY LUMINOSITY AND ABSORPTION FUNCTIONS OF ACTIVE GALACTIC NUCLEI INCLUDING COMPTON-THICK POPULATIONS (2014, result): “We find that the observed CTK AGN fractions at various flux limits in the 2–10 keV (or 0.5–8 keV) band reported by Tozzi et al. (2006), Hasinger et al. (2007), Brunner et al. (2008), and Brightman & Ueda (2012) are generally in good agreements with the model prediction.”
• A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys (2013, methodology): “Here we use Cash statistics in our analysis, whereas previous works have used χ2, the two being known to produce systematic differences in (Tozzi et al. 2006).”
• The mean star formation rate of X-ray selected active galaxies and its evolution from z~2.5: results from PEP-Herschel (2012, background): “This is governed mostly by selection effects (Tozzi et al. 2006).”
• THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION (2013, background): “These surveys have resolved 70– 90% of the 0.5–10 keV XRB (e.g., Worsley et al. 2005; Hickox & Markevitch 2006; Xue et al. 2012), revealing obscured and unobscured AGNs out to z ∼ 5–6 (e.g., Tozzi et al. 2006; Brusa et al. 2009; see Brandt & Alexander 2010 for a recent review).”
• Dust covering factor, silicate emission, and star formation in luminous QSOs (2007, result): “…has been noted in various X-ray surveys (Ueda et al., 2003; Steffen et al., 2003; La Franca et al., 2005; Akylas et al., 2006; Barger et al., 2005; Tozzi et al., 2006; Simpson, 2005), although the results have been questioned by other authors (e.g. Dwelly & Page, 2006; Treister & Urry, 2005; Wang…”