Andrii ElyivAndrii Elyiv

and and

XMM-LSS collaborationXMM-LSS collaboration

The correlation function analysisof AGN in the XMM-LSS survey

ImportanceImportance of the deep of the deep surveyssurveys

► The description of the objects along the wide range The description of the objects along the wide range of of redshifts “time machines” redshifts “time machines” luminosities luminosities

► Rich statistics of the different types of objectsRich statistics of the different types of objects► Large Scale Structure studyingLarge Scale Structure studying► The clue on The clue on δρδρ//ρρ at high z at high z► Cosmological parametersCosmological parameters► Measurements of AGN evolutionMeasurements of AGN evolution► Environment of different types of AGNEnvironment of different types of AGN► Relation between AGN activity and dark matter halo Relation between AGN activity and dark matter halo

hostshosts

Types of objects in X-ray Types of objects in X-ray surveyssurveys

►ObscuredObscured and and Unobscured AGNUnobscured AGN

►Optically faint X-ray sourcesOptically faint X-ray sources

► X-ray bright, optically normal galaxiesX-ray bright, optically normal galaxies

► SStarbursttarburst galaxies galaxies

►Groups and clusters of galaxiesGroups and clusters of galaxies

►Galactic starsGalactic stars

z ≈ 1.5–5

XMM and Chandra surveysXMM and Chandra surveys

shallower

deep

wid

e

narro

w

Log(N)-Log(S) for soft band∼ 30000 sources ∼ 125.5 deg2 sky area5-20 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 arcmin2 CDF-S - 1 Ms, 391 arcmin2

a few hundreds sources

The CDF-S and CDF-N ACFAngular clustering scale as a function of the flux limit

Main conclusion: a strong dependence of the clustering strength on the subsample flux limit

XXL surveyXXL survey

►two extragalactic regions of 25 degtwo extragalactic regions of 25 deg22

►at a depth of ~ 5at a depth of ~ 5xx1010-15-15 erg/s/cm erg/s/cm22  ►10 ks XMM10 ks XMM-Newton-Newton observations observations►The main goalThe main goal

to constrain the Dark Energy equation of to constrain the Dark Energy equation of state using clusters of galaxies. state using clusters of galaxies.

cluster scaling laws cluster scaling laws studies of AGNs. studies of AGNs.

XMM-LSS surveyXMM-LSS survey► at high galactic latitudeat high galactic latitude, near , near celestial equator celestial equator ► 11 deg11 deg22 of 99 adjacent XMM pointings of 99 adjacent XMM pointings::

91 from the XMM-LSS programme91 from the XMM-LSS programme,, ranging from ranging from 77 to 27 ks, to 27 ks, 8 from the Subaru Deep Survey, ranging from 40 to 80 ks. 8 from the Subaru Deep Survey, ranging from 40 to 80 ks.

► 7.0007.000 detected detected sources sources brighterbrighter 1010-15-15 erg/s/cm2 in the soft erg/s/cm2 in the soft band. band.

► mostmost of the sources are of the sources are the the AGNAGNss or stars (point-like sources). or stars (point-like sources).► the others the others are mainly clusters of galaxies are mainly clusters of galaxies and aand a few very few very

nearby galaxies (extended sources).nearby galaxies (extended sources).

► the main goals of the XMM-LSS survey is to study the cosmic the main goals of the XMM-LSS survey is to study the cosmic network underlined by clusters of galaxiesnetwork underlined by clusters of galaxies as well as AGN as well as AGN distributiondistribution

5170 point like sources10.2 deg2

20’

Main principle: keep the smallest off-axis distance

1. soft and hard bands2. adjacent pointings

Flux redistribution problemFlux redistribution problem

true flux F+ Poisson noise

Flux limit of XMM-Newton

Log(N)-Log(S) distributionsLog(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 catalogwith 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 soft band

CFA for the hard band CFA for the hard band

ConlusionsConlusions

► 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 1.85.

► 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.