Andrii Elyiv and XMM-LSS collaboration The correlation function analysis of AGN in the XMM-LSS survey

Importance of the deep surveys ► The description of the objects along the wide range of  redshifts “time machines”  luminosities ► Rich statistics of the different types of objects ► Large Scale Structure studying ► The clue on δρ/ρ at high z ► Cosmological parameters ► Measurements of AGN evolution ► Environment of different types of AGN ► Relation between AGN activity and dark matter halo hosts

Types of objects in X-ray surveys ► Obscured and Unobscured AGN ► Optically faint X-ray sources ► X-ray bright, optically normal galaxies ► Starburst galaxies ► Groups and clusters of galaxies ► Galactic stars z ≈ 1.5–5

XMM and Chandra surveys shallower deep wide narrow

Log(N)-Log(S) for soft band ∼ sources ∼ deg 2 sky area 5-20 ks Main results: Positive clustering signals in the soft (10σ) and hard (5σ ) bands Dependency of the clustering strength on the flux limit Obscured and unobscured objects share similar clustering properties Best-fit correlation length Correlation function

CDF-N - 2 Ms, 448 arcmin 2 CDF-S - 1 Ms, 391 arcmin 2 a few hundreds sources The CDF-S and CDF-N ACF Angular clustering scale as a function of the flux limit Main conclusion: a strong dependence of the clustering strength on the subsample flux limit

XXL survey ► two extragalactic regions of 25 deg 2 ► at a depth of ~ 5x erg/s/cm 2 ► at a depth of ~ 5x erg/s/cm 2 ► 10 ks XMM-Newton observations ► The main goal  to constrain the Dark Energy equation of state using clusters of galaxies.  cluster scaling laws  studies of AGNs.

XMM-LSS survey ► at high galactic latitude, near celestial equator ► 11 deg 2 of 99 adjacent XMM pointings:  91 from the XMM-LSS programme, ranging from 7 to 27 ks,  8 from the Subaru Deep Survey, ranging from 40 to 80 ks. ► detected sources brighter erg/s/cm2 in the soft band. ► most of the sources are the AGNs or stars (point-like sources). ► the others are mainly clusters of galaxies and a few very nearby galaxies (extended sources). ► the main goals of the XMM-LSS survey is to study the cosmic network underlined by clusters of galaxies as well as AGN distribution

5170 point like sources 10.2 deg 2

20’ Main principle: keep the smallest off-axis distance 1. soft and hard bands 2. adjacent pointings

Flux redistribution problem true flux F + Poisson noise Flux limit of XMM-Newton

Log(N)-Log(S) distributions

Main steps: - to reconstruct the true Log(N)-Log(S) distribution -to generate the random catalogs according to flux distribution taking into account the detection probability of the sources with flux at different: - off-axis distance - exposures - backgrounds Two-point correlation function (Hamilton 1993) -DD(θ) – number of pair from real catalog with size in the range [θ, θ+d θ] -RR(θ) – average number of pair in random catalogs - DR(θ) – average number of data-random pairs

CFA for the soft band

CFA for the hard band

Conlusions ► ► The LogN-LogS distribution for the soft and hard bands are found to be in good agreement with the results from the work of Gandhi at al. (2006). Using 11 sq. deg. from the XMM-LSS and Subaru fields, we have extended the LogN- LogS to smaller fluxes. ► ► The resulting power-law slopes for all considered subsamples and both bands are found to be quite similar, between 1.67 and ► ► The scale of CF is found to be substantially smaller in the soft band (0.4" - 5.9") than in the hard band (3.8"- 35.1"). ► ► Flux limitation does not significantly change the CF parameters in the soft band.