Properties of the point-like sources in the XMM-LSS field Olga Melnyk and XMM-LSS collaboration N. Clerc, L. Chiappetti, A. Elyiv, P.Gandhi, E.Gosset, M. Pierre, M. Plionis, T.Sadibekova, M.Salvato, P.-G. Sprimont, J.Surdej

XMM-LSS survey One of the largest view of the deep X- ray sky, coverage extends to 11 deg 2 (99 XMM pointings) One of the largest view of the deep X- ray sky, coverage extends to 11 deg 2 (99 XMM pointings) Software Clusters of galaxies Sacley team Spectroscopy Point sources (AGN) Liege team Data Base Milan

Main goals of work: It is well-known that galaxy properties strongly depend on local environment (morphology, color, star-formation etc.) What is the main influence on galaxy properties: intrinsic evolution or influence of environment? As X-ray selected AGNs we can see at high redshifts, studying of their environment gives us the possibility to understand better scenario of AGN formation and connection between AGN and large-scale structure at early epoch; Providing the classification of X-ray sources that complete XMM-LSS survey; Providing the classification of X-ray sources that complete XMM-LSS survey; Studying the local environment of AGN and their host galaxies. Studying the local environment of AGN and their host galaxies.

Main steps: To define AGN sample and subsamples: soft (0.5-2 keV) and hard band (2-10 keV) band population; To define AGN sample and subsamples: soft (0.5-2 keV) and hard band (2-10 keV) band population; To find Optical/Near-infrared/ Infrared/Ultraviolet counterparts of X-ray sources; To find Optical/Near-infrared/ Infrared/Ultraviolet counterparts of X-ray sources; To find the spectroscopic or compute the photometric redshifts; To find the spectroscopic or compute the photometric redshifts; To define local 2D and 3D environments. To define local 2D and 3D environments.

AGN in XMM-LSS+Subaru field

Sample of X-ray point-like sources and counterparts We have 2169 X-ray sources with counterparts in optical (CFHT) and infrared (Swire/IRAC) counterparts with good probabilities and some of them have also near-infrared (UKIDSS) and/or ultraviolet (GALEX) counterparts; RA(DEC)_Opt - RA(DEC)_Sw < 0.5'‘; RA(DEC)_Opt - RA(DEC)_Sw < 0.5'‘; RA(DEC)_Opt - RA(DEC)_Uki < 0.5'‘; RA(DEC)_Opt - RA(DEC)_Uki < 0.5'‘; RA(DEC)_Opt - RA(DEC)_GALEX < 1'‘; RA(DEC)_Opt - RA(DEC)_GALEX < 1'‘; RA(DEC)_Opt - RA(DEC)_Spec < 1''. RA(DEC)_Opt - RA(DEC)_Spec < 1''. 15% of the sample have spectroscopic redshifts; 15% of the sample have spectroscopic redshifts; The rest of the sample has the photometric redshifts. The rest of the sample has the photometric redshifts. Probability=1-exp(-πn(>m)∙r2), that the association between an X- ray source and its counterpart results from random fluctuations: p<0.01 “good” counterpart; 0.01<p<0.03 “fair” counterpart; p>0.03 “bad” counterpart.

Difference of coordinates between counterparts Optical-Infrared Optical-UKIDSS Optical-Spectra Optical-UV

extended sources point-like sources Photo-z vs. spectro-z relation for the 355 spectroscopically observed sources. The solid line corresponds to z_ph = z_sp, the dashed lines correspond to z_ph=z_sp± 0.15(1+z_sp). The GAL/QSO classification corresponds to the extended/point-like dominated sample Photometric redshifts using 13 bands σ Δz/(1+z_sp) =0.11: 0.08 for extended sources 0.11 for point-like sources 25% of outliers: 8% for extended sources 27% for point-like sources

Redshift distributions. We did not show 14 objects with z_ph > 4. The average value of redshifts and standard deviation are: =1.26± 0.84 for the whole sample and =1.23± 0.85 for the spectro-z sample, alone.

Template distribution of all sources. The template numbers (identifiers) correspond to 1 - blue starforming galaxy, 2 - S0, 3 - Sb, 4 - Sc, 5 - M82 starburst, 6- I22491 Starburst/ULIRG, 7 - Seyfert 1.8, 8 - Seyfert 2, S0-QSO hybrid, 18 - Mrk231 (Seyfert 1/BALQSO), I22491-QSO hybrid, I22491-QSO hybrid with UV, 28 - QSO high luminosity with UV, 29 - QSO low luminosity with UV, 30 - QSO high IR luminosity with UV. Non-active galaxies Obscured QSO/AGN Unobscured QSO/AGN

R mag - hard band flux for the GALs and QSOs samples according to the template classification. X/O>10: Extremely red objects (EROs) with R-K>5 Type II (highly obscured) AGN; high-redshift passive ellipticals; dusty-starforming galaxies. We choose high-z obscured candidates: X/O>10 and νF24/νFR >10 ∩ R-[3.6]≥4

Spectroscopically classified sources Photometrically classified sources

SampleN {HR} 1/2 photo-GALs with z>1 and Lx>10 43 erg/s photo-GALs z>1 and Lx>10 44 erg/s All photo-GALs All photo- obscured AGN/QSO All photo- unobscured AGN/QSO All spectro-GALs All spectro-QSOs High-z obscured candidates % (80%) of the sources with HR>-0.3 (-0.2) are obscured (COSMOS results).

Classifications 1291 QSOs and 692 GALs according to templates 1291 QSOs and 692 GALs according to templates Template/spectroscopic: 66/86=77% of GALs; 208/229=91% of QSOs; Template/spectroscopic: 66/86=77% of GALs; 208/229=91% of QSOs; 732 “IRAC” QSO = template QSO 732/1291 = 56% (from total template QSO); 732/768 = 95% (from visible IRAC template QSO); 732 “IRAC” QSO = template QSO 732/1291 = 56% (from total template QSO); 732/768 = 95% (from visible IRAC template QSO); 135/152 = 89% spectral QSO in IRAC 135/152 = 89% spectral QSO in IRAC 704 sources are template QSO, IRAC QSO and have Lx>2x10 42 erg/s: 55% 704 sources are template QSO, IRAC QSO and have Lx>2x10 42 erg/s: 55%

CFHT+ABC r-band field without overlaps (black area). The sample of z_ph+z_sp counterparts N=1983 (red dots). Environmental properties Δ(r)= (ρ(r)- )/, Where is the mean value of density of each dm for the whole sample

Δ(r)

Blue starforming and spiral galaxies Early type galaxies Starburst and Sy Δ(r)

Conclusions For all the considered samples, we note that the significance of the overdensity (in σ units) increases with the value of dm. Whole sample and soft subsample show the significant overdensities contrary to hard band. We didn't find the significant differences in the nature of the only soft and the only hard sources. For the template-classified objects, we note some tendencies in the overdensities. Blue starforming galaxies and spiral (Sb and Sc) galaxies (#1,3,4) show some overdensities (from 2.4 to 4.3 σ) in the first bins; S0 (#2) galaxies show very significant overdensities at dm = 1 mag and at dm=0.2 mag. The high value of local overdensity (200 kpc) can signify about the presence of close satellites around these early type galaxies. For the QSO template-classified objects, we do not see any significant overdensity.