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

LSS fieldLSS field

Olga Melnyk and XMM-LSS collaborationOlga Melnyk and XMM-LSS collaboration

N. Clerc, L. Chiappetti, A. Elyiv, P.Gandhi, E.Gosset, M. Pierre, M. N. Clerc, L. Chiappetti, A. Elyiv, P.Gandhi, E.Gosset, M. Pierre, M. Plionis, T.Sadibekova, M.Salvato, P.-G. Sprimont, J.SurdejPlionis, T.Sadibekova, M.Salvato, P.-G. Sprimont, J.Surdej

XMM-LSS surveyXMM-LSS survey

One of the largest view of the One of the largest view of the deep X-ray sky, coverage extends deep X-ray sky, coverage extends to 11 degto 11 deg2 2

(99 XMM pointings)(99 XMM pointings)

SoftwareClusters of galaxies

Sacley team

SpectroscopyPoint sources (AGN)

Liege teamData BaseMilan

Main goals of work:Main goals of work:

It is well-known that galaxy properties strongly depend It is well-known that galaxy properties strongly depend on local environment (morphology, color, star-on local environment (morphology, color, star-formation etc.)formation etc.)

What is the main influence on galaxy properties: What is the main influence on galaxy properties: intrinsic evolution or influence of environment? intrinsic evolution or influence of environment?

As X-ray selected AGNs we can see at high redshifts, As X-ray selected AGNs we can see at high redshifts, studying of their environment gives us the possibility studying of their environment gives us the possibility to understand better scenario of AGN formation and to understand better scenario of AGN formation and connection between AGN and large-scale structure at connection between AGN and large-scale structure at early epoch;early epoch;

Providing the classification of X-ray sources that Providing the classification of X-ray sources that complete XMM-LSS survey;complete XMM-LSS survey;

Studying the local environment of AGN and their host Studying the local environment of AGN and their host galaxies.galaxies.

Main steps:Main steps:

To define AGN sample and subsamples: To define AGN sample and subsamples: soft (0.5-2 keV) and hard band (2-10 soft (0.5-2 keV) and hard band (2-10 keV) band population;keV) band population;

To find Optical/Near-infrared/To find Optical/Near-infrared/Infrared/Ultraviolet counterparts of X-ray Infrared/Ultraviolet counterparts of X-ray sources;sources;

To find the spectroscopic or compute the To find the spectroscopic or compute the photometric redshifts;photometric redshifts;

To define local 2D and 3D environments.To define local 2D and 3D environments.

AGN in XMM-LSS+Subaru AGN in XMM-LSS+Subaru fieldfield

Sample of X-ray point-Sample of X-ray point-like sources and like sources and counterpartscounterpartsWe have 2169 X-ray sources with counterparts in We have 2169 X-ray sources with counterparts in

optical (CFHT) and infrared (Swire/IRAC) optical (CFHT) and infrared (Swire/IRAC) counterparts with good probabilities and some of counterparts with good probabilities and some of them have also near-infrared (UKIDSS) and/or them have also near-infrared (UKIDSS) and/or ultraviolet (GALEX) counterparts;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(-Probability=1-exp(-ππn(>m)∙r2),n(>m)∙r2),that the association between an that the association between an X-ray source and its counterpart X-ray source and its counterpart results from random results from random fluctuations:fluctuations:

p<0.01 “good” counterpart;p<0.01 “good” counterpart;0.01<0.01<p<0.03p<0.03 “fair” “fair”

counterpart;counterpart;p>0.03 “bad” counterpart.p>0.03 “bad” counterpart.

Difference of coordinates Difference of coordinates between counterpartsbetween counterparts

Optical-Infrared

Optical-UKIDSS

Optical-Spectra

Optical-UV

extended sourcespoint-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

σΔz/(1+z_sp)=0.11:

0.08 for extended sources0.11 for point-like sources

25% of outliers:

8% for extended sources27% 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: <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.

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.

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>5Type II (highly obscured) AGN; high-redshift passive ellipticals; dusty-starforming galaxies.

We choose high-z obscured candidates:X/O>10 andνF24/νFR >10 ∩ R-[3.6]≥4

Spectroscopically classified sources

Photometrically classified sources

Sample N <z> {HR}1/2 <HR>

photo-GALs with z>1 and Lx>1043 erg/s 151 1.38 -1 -0.57

photo-GALs z>1 and Lx>1044 erg/s 57 1.61 -0.38 -0.28

All photo-GALs 605 0.79 -1 -0.59

All photo- obscured AGN/QSO 183 0.82 -0.52 -0.45

All photo- unobscured AGN/QSO 880 1.68 -0.58 -0.55

All spectro-GALs 86 0.36 -0.61 -0.47

All spectro-QSOs 229 1.56 -0.59 -0.51

High-z obscured candidates 133 1.54 -0.29 -0.16

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

ClassificationsClassifications

1291 QSOs and 692 GALs according to 1291 QSOs and 692 GALs according to templatestemplates

Template/spectroscopicTemplate/spectroscopic::66/86=66/86=7777% of GALs;% of GALs;208/229=208/229=9191% of QSOs;% of QSOs;

732 “IRAC” QSO = template QSO732 “IRAC” QSO = template QSO732/1291 = 732/1291 = 5656% (from total template QSO); % (from total template QSO); 732/768 = 732/768 = 9595% (from visible IRAC template % (from visible IRAC template QSO);QSO);

135/152 = 135/152 = 8989% spectral QSO in IRAC% spectral QSO in IRAC 704 sources are template QSO, IRAC QSO 704 sources are template QSO, IRAC QSO

and have Lx>2x10and have Lx>2x104242 erg/s: erg/s: 5555%%

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)-< ρ >)/< ρ >,

Where < ρ >is the mean value ofdensity of each dm for the whole sample

Δ(r)

Δ(r)

Blue starforming and spiral galaxies

Early type galaxies

Starburst and SyΔ(r)

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.