#Author Last NameAuthor First NameEmail AddressInstitutionTitleAbstractPresentationDiscussionSplinter SessionSession
1CoilAlisonacoil@as.arizona.eduUniversity of ArizonaClustering of AGN and QSOs at z=1Using galaxies from the DEEP2 Redshift Survey and AGN from the AEGIS/Chandra survey and QSOs from SDSS, I present the cross-correlation function of AGN/QSOs and 'normal' galaxies at z=1. Using the known clustering of DEEP2 galaxies, this leads to an estimate of the bias and typical host dark matter halo mass of AGN/QSOs as a function of X-ray luminosity, which constrains AGN formation models.oralAre AGN really created/fueled by mergers and what evidence do we have for that?Tuesday: AGN correlation functions, LSS, environments4
2GeorgakakisAntonisage@ic.ac.ukImperial CollegeThe environment of AGN at z~1I will present results on the environment of X-ray selected AGN at z~1 using data from the Extended Groth strip International Survey (AEGIS) which combines (among others) deep (200ks per field) wide-area (0.5deg2) Chandra observations with extensive optical spectroscopy to R~24mag. The 3-D information is exploited to quantify the local density in the vicinity of an X-ray source by measuring the projected surface density of galaxies within a radius defined by the 3rd nearest neighbour. The main result is that X-ray selected AGN at z~1 avoid underdense regions at the 99.89% confidence level. Moreover, although the overall AGN population shares the same (rich) environment with optical galaxies of similar U-B and M_B, there is also tentative evidence (96%) that AGN with blue host-galaxy colors (U-B<1) reside in denser environments compared to optical galaxies. The results above can be understood as a consequence of the whereabouts of massive galaxies, capable of hostin! g supermassive black holes at their centers, with available cold gas reservoirs, the fuel for AGN activity. At z~1 an increasing fraction of such systems are found in dense regions.oralAGN/host-galaxy co-evolution Link between AGN and environment differences among AGN samples selected at different wavelengths, e.g. IR, X-ray, opticalMonday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments4
3GilliRobertoroberto.gilli@bo.astro.itINAF-Osservatorio Astronomico di BolognaThe spatial clustering of X-ray selected AGNWe discuss the 3D clustering properties of AGN selected by X-ray surveys with different area and sensitivity. The measurements performed in the 0.1 deg2 Chandra Msec Fields are compared with those obtained in the 0.4 deg2 CLASXS and 81 deg2 NEP surveys. We also present preliminary results on the spatial clustering of ~300 AGN selected in the 2 deg2 XMM-COSMOS field, where a highly significant (~8sigma) clustering signal has been detected. The issue of cosmic variance is discussed. Finally, we investigate the relation between AGN clustering amplitude vs X-ray luminosity, redshift and obscuration.oralI think an important issue to discuss is the XLF and evolution of obscured AGN, particularly of Compton-thick sources. These are particularly relevant to understand the CXRB and compute the relic SMBH mass function. Another important issue is explore is the relation between AGN clustering and AGN luminosity, redshift and obscuration, which would tell us how these objects form and evolve in the cosmic web.Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments4
4KenterAlmusakenter@cfa.harvard.eduSAO We present results from the XBootes survey. This survey consists of 126 separate Chandra ACIS-~I observations each of approximately 5000 seconds in duration. The observations comprise a field of view of $\sim$ 9 degree$^{2}$ and are part of the multi-wavelength NOAO Deep Wide Field Survey (NDWFS). 3293 x-ray sources have been detected with flux~$\geq 8\times 10^{-15} ($0.5-7$~keV). These X-ray data are combined with optical observations and the combined data set is observed with the multi-fiber spectrograph (HECTOSPEC) as part of the AGN and Galaxy Evolution Survey (AGES). We present results on large scale structure, redshift distribution, and the three dimensional 2-point correlation.oral Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments4 5MiyajiTakamitsumiyaji@cmu.eduCarnegie Mellon UniversityAGN Clustering and Environments in X-ray SurveysClustering properties and environments of active galactic nuclei provide yet another key to understanding the formation/triggering mechanism of AGN activities. I review the current status of AGN clustering and environment studies from X-ray surveys and discuss their implications for AGN formation/evolution and cosmology. Topics include comparisons amonng AGN correlation functions from various X-ray and opticl surveys, statistical challenges in the correlation function analysis, and the evolution of AGN clustering/bias with redshift. I further overview the implications of the AGN clusterings in terms of dark-matter halo occupation, typical lifetime of AGN activities, and cosmolgy. Future prospects are discussed.oralHow to best use remaining lifetime of Chandra and XMM? Prospective future missions and their role in X-ray survey science.Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments4 6PlionisManolismplionis@inaoep.mxIAA-NOA, Greece & INAOE-MexicoHIGH-Z XRAY AGN CLUSTERING AND COSMOLOGICAL IMPLICATIONSI present recent results of the high-redshift X-ray selected AGN clustering, based on the XMM/2dF survey. Using the luminosity-dependent density evolution luminosity function we find that the spatial clustering lengths, derived using Limber's inversion equation, are$\sim 16$and 19$h^{-1}$Mpc respectively (for the comoving clustering evolution model) while the median redshifts of the soft and hard X-ray sources are${\bar z}\sim 1.2$and 0.75, respectively. Within the framework of flat cosmological models we find that these results support a model with$\Omega_m \simeq 0.26$,$\sigma_8\simeq 0.75$, w$\simeq -0.9$(in excellent agreement with the 3 year WMAP results). We also find the present day bias of X-ray AGNs to be$b_o\simeq 2\$.oral Monday: Type I and II AGN, Absorption, XBONGs, Tuesday: AGN correlation functions, LSS, environments4
7StewartGordongcs@star.le.ac.ukDept. of Physics and Astronomy, Leicester UniversityCosmic Variance From the 2XMM Catalogue G C Stewart, M G Watson, S Mateos, R SmithNumber counts from 2XMM serendipitous catalogue number counts are used to probe the cosmic variance at a range of depths and scales.The high sensitivity, wide-field and large sky coverage of this catalogue are ideal for this analysis. The results are used in combination with results from the deep surveys of Chandra and XMM to constrain the fluctuation amplitudes at a typical redshift of 1-2. Comparison with results obtained using other techniques can be used to investigate the bias parameter and how well for various source populations`light' traces the matter fluctuations.oral Monday: X-ray luminosity functions and evolution, Tuesday: AGN correlation functions, LSS, environments4