Andrii Elyiv and XMM-LSS collaboration

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

2. 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

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

4. XMM and Chandra surveys shallower narrow wide deep

5. 2XMM survey (Ebrero et al. 2009) Log(N)-Log(S) for soft band Best-fit correlation length ∼ 30000 sources ∼ 125.5 deg2 sky area 5-20 ks Correlation function • 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

6. Chandra Deep Field North and South Surveys (Plionis et al. 2009) Angular clustering scale as a function of the flux limit The CDF-S and CDF-N ACF Main conclusion: a strong dependence of the clustering strength on the subsample flux limit CDF-N - 2 Ms, 448 arcmin2 CDF-S - 1 Ms, 391 arcmin2 a few hundreds sources

7. XXL survey • two extragalactic regions of 25 deg2 • at a depth of ~ 5x10-15 erg/s/cm2 • 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.

8. XMM-LSS survey • at high galactic latitude, near celestial equator • 11 deg2 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. • 7.000 detected sources brighter10-15 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

9. XMM-LSS field: soft band [0.5 – 2 keV] 5170 point like sources 10.2 deg2

10. XMM-LSS field: overlap problem 1. soft and hard bands 2. adjacent pointings 20’ Main principle: keep the smallest off-axis distance

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

12. Probability curves for different exposures

13. Probability curves for different off-axis distances

14. Probability curves for different backgrounds

15. Log(N)-Log(S) distributions

16. Procedure of CF determination • 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

17. CFA for the soft band

18. CFA for the hard band

19. Conlusions • The LogN-LogS distribution for the soft and hardbands are found to be in good agreement with the resultsfrom the work of Gandhi at al. (2006). Using 11 sq. deg.from the XMM-LSS and Subaru fields, we have extendedthe LogN-LogS to smaller fluxes. • The resulting power-law slopes for all consideredsubsamples and both bands are found to be quite similar,between 1.67 and 1.85. • The scale of CF is found to be substantiallysmaller in the soft band (0.4" - 5.9") than in the hardband (3.8"- 35.1"). • Flux limitation does not significantly change the CF parameters in the soft band.