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Properties of the point-like sources in the XMM-LSS field

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. Software Clusters of galaxies Sacley team. Spectroscopy

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Properties of the point-like sources in the XMM-LSS field

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  1. 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

  2. SoftwareClusters of galaxies Sacley team Spectroscopy Point sources(AGN)Liege team Data BaseMilan XMM-LSS survey • One of the largest view of the deep X-ray sky, coverage extends to 11 deg2 (99 XMM pointings)

  3. 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; • Studying the local environment of AGN and their host galaxies.

  4. Main steps: • 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 the spectroscopic or compute the photometric redshifts; • To define local 2D and 3D environments.

  5. AGN in XMM-LSS+Subaru field

  6. Sample of X-ray point-like sources and counterparts • 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. • 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)_Uki < 0.5'‘; • RA(DEC)_Opt - RA(DEC)_GALEX < 1'‘; • RA(DEC)_Opt - RA(DEC)_Spec < 1''. • 15% of the sample have spectroscopic redshifts; • The rest of the sample has the photometric redshifts.

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

  8. extended sourcespoint-like sources Photometric redshifts using 13 bands σΔz/(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 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

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

  10. Non-active galaxies Obscured QSO/AGN Unobscured QSO/AGN 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, 9 - 17 S0-QSO hybrid, 18 - Mrk231 (Seyfert 1/BALQSO), 19-24 I22491-QSO hybrid, 25-27 I22491-QSO hybrid with UV, 28 - QSO high luminosity with UV, 29 - QSO low luminosity with UV, 30 - QSO high IR luminosity with UV.

  11. We choose high-z obscured candidates: X/O>10 and νF24/νFR >10 ∩ R-[3.6]≥4 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>5Type II (highly obscured) AGN; high-redshift passive ellipticals; dusty-starforming galaxies.

  12. Spectroscopically classified sources Photometrically classified sources

  13. 50% (80%) of the sources with HR>-0.3 (-0.2) are obscured (COSMOS results).

  14. Classifications • 1291 QSOs and 692 GALs according to templates • Template/spectroscopic:66/86=77% of GALs;208/229=91% of QSOs; • 732 “IRAC” QSO = template QSO732/1291 = 56% (from total template QSO); 732/768 = 95% (from visible IRAC template QSO); • 135/152 = 89% spectral QSO in IRAC • 704 sources are template QSO, IRAC QSO and have Lx>2x1042 erg/s: 55%

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

  16. Δ(r) Δ(r)

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

  18. 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.

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