infrared selected highly obscured qso

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INFRARED SELECTED HIGHLY OBSCURED QSO C. Feruglio (INAF-OAR) & F. Fiore, E. Piconcelli, R. Maiolino, + many others (OABo, UniBo, MPE, ASDC)

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INFRARED SELECTED HIGHLY OBSCURED QSO. C. Feruglio (INAF-OAR) & F. Fiore, E. Piconcelli, R. Maiolino, + many others (OABo, UniBo, MPE, ASDC). High MIR/O High luminosity obscured AGN. SAMPLE SELECTION. High MIR/Optical flux ratio indicates the presence of an obscured AGN. - PowerPoint PPT Presentation

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Page 1: INFRARED SELECTED HIGHLY OBSCURED  QSO

INFRARED SELECTEDHIGHLY OBSCURED QSO

C. Feruglio (INAF-OAR)

& F. Fiore, E. Piconcelli, R. Maiolino,

+ many others (OABo, UniBo, MPE, ASDC)

Page 2: INFRARED SELECTED HIGHLY OBSCURED  QSO

SAMPLE SELECTION

High MIR/Optical flux ratio indicates the presence of an obscured AGN

Strong correlation of MIR/O with

24 um luminosity for moderately obscured AGN

Recalls the correlation between

X/O and L(2-10 keV) for moderately obscured AGN selected in X-rays

X-ray samples; GOODS-MUSIC, ELAIS-S1, HELLAS2XMM (Pozzi et al 2007)

Filled symbols=moderately obscured AGN

High MIR/O

High luminosity obscured AGN

Page 3: INFRARED SELECTED HIGHLY OBSCURED  QSO

SAMPLE SELECTION

This selection is equilvalent to SFR (IR) >> SFR (UV)

(Fiore et al 2007)

MIR/O correlated with R-K color

Bimodal distribution of R-K for sourcess with MIR/O>1000, separate population

Page 4: INFRARED SELECTED HIGHLY OBSCURED  QSO

F24um/FR >1000 R-K>4.5

The stack produces a detection in both soft and

hard bands

F24um/FR <100 R-K>4.5

Detection only in 0.3-1.5 keV

0.3-1.5 keV 1.5-4 keV

0.3-1.5 keV 1.5-4 keV

(Fiore et al 2007)

Page 5: INFRARED SELECTED HIGHLY OBSCURED  QSO

A new population of CT AGN

Fiore et al. 2007

Stack of Chandra images excluding X-ray detections

Using the observed counts rate and hardness ratios we evaluated the fraction of highly obscured AGN (logNH>24) in the samples

Assuming a reasonable LIR/LX ratio, a flat NH distribution from logNH=24-26 and a reflection component =1% of the direct one

Page 6: INFRARED SELECTED HIGHLY OBSCURED  QSO

HIGH MIR/O SWIRE SOURCES

Blue circles = XMM pointings; Red polygons = Chandra ACIS-I and ACIS-S pointings

Elais N1 Elais N2 Elais S1

Lockman Hole XMM-LSS

Large area (50 deg2) with sensitive IR (Spitzer) and optical data,

suitable for searching for type2 QSO

Small fraction covered with shallow X-ray observations below 10 keV

~ 30% of the high MIR/O sources with XMM/Chandra coverage are detected below 10 keV

Page 7: INFRARED SELECTED HIGHLY OBSCURED  QSO

SWIRE highly obscured QSO

About 30 SWIRE sources with

MIR/O > 2000 Flux(24um) > 2 mJy and R-mag(3.6um)>4.5

SWIRE

CDFS X-ray sources

SWIRE

Page 8: INFRARED SELECTED HIGHLY OBSCURED  QSO

Bright MIPS sources

Fl 24 um > 4 mJy

with faint optical counterparts (R>24)

Page 9: INFRARED SELECTED HIGHLY OBSCURED  QSO

The template obscured QSO: IRAS 09104+4109

Template Compton-thick QSO

High L(IR)/Lx ratio

No PAH emission features in IRS spectrum

IR SED dominated by the AGN

Abell 112690#75

(Pozzi et al 2007)IRAS 09

IRAS 09 SDSS spectrum

Page 10: INFRARED SELECTED HIGHLY OBSCURED  QSO

Use the observed SED and L(24 um) to evaluate

L(2-10 keV)

for high MIR/O sources

The template obscured QSO: IRAS 09104+4109

L(2-10 keV) = 8.8 1044 cgs

rest

log(

L

/ L

2-1

0 k

eV )

Page 11: INFRARED SELECTED HIGHLY OBSCURED  QSO

Candidate highly obscured QSO

targets for Simbol-X

SW110013.92+581034.9 SW163515.61+405607 z = 1.5

L (24 um) = 5.8 1045

L (2-10 keV) = 4.7 1044

z = 1

L (24 um) = 3.2 1045

L (2-10 keV) = 1.1 1044

IRAS09104+4109

SWIRE

Page 12: INFRARED SELECTED HIGHLY OBSCURED  QSO

Simbol-X view of SW110013.92+581034.9 z=1 Binned, bkg-subtracted, 200 ks spectrum;

A typical Compton-thick source spctrum is assumed :

NH = 2 1024 cm-2 , Gamma=1.8, EW(Fe Ka )= 1keV

Normalization of the reflected vs transmitted component : A_refl/A_trans =0.2 (e.g. Circinus, Matt et al. 99)

L(2-10 keV) = 1.1 1044 cgs intermediate luminosity AGNF(2-10 keV) = 7.1 10 -15 cgs F(20-40 keV)=1.7 -14 cgs

Page 13: INFRARED SELECTED HIGHLY OBSCURED  QSO

Simbol-X view of SW163515.61+405607 z=1.5

The same model with T_exp=300 ks

SX allows to constrain NH for the most heavily obcured AGN up to z=2

with ~ 30% error at 2 sigma

L(2-10 keV)=3.03 1044 ,

F(2-10 keV)=1.07 10 -14 cgs, F(20-40 keV)=1.7 10-14 cgs

Page 14: INFRARED SELECTED HIGHLY OBSCURED  QSO

We selected a sample of ~ 30 candidate type 2 QSOs using deep IR and optical photometry in the SWIRE fields These are going to be targets of several present and future observatories (Chandra, XMM, Herschel, ALMA...)

We used the SED of IRAS09104+4109 and Abell112690 to evaluate the intrinsic X-ray luminosity

Assuming NH typical of a Compton thick AGN we obtained simulations of SX observationsThe simulations show that the sources are detected up to 60 keV and the 90% uncertainty on NH is < 30%

SX Observations of this sample of IR selected QSOs will allow us to : 1) obtain a complete census of SMBH up to z 1.5-2 ;

2) obtain a well constrained NH distribution

Conclusions