The XMM-Newton hard The XMM-Newton hard band wide angle Surveyband wide angle SurveyNicoletta Carangelo and Silvano Molendi (IASF-Nicoletta Carangelo and Silvano Molendi (IASF-

MI(CNR))MI(CNR))

Epic Consortium Meeting Palazzo Steri, Palermo, 14-16 October 2003

The Cosmic X-ray The Cosmic X-ray BackgroundBackground

Giacconi et al. 1962

XRB as superposition of unabsorbed and absorbed

AGNs

Comastri et al. 1995

Several self-consistent synthesis models (e.g.

Madau,Ghisellini & Fabian 1994; Comastri et al. 1995;

Gilli, Salvati & Hasinger 2001), Franceschini, Braito

& Fadda 2002; Gandhi & Fabian 2003) of the XRB based on the unification

schemes of AGNs

KEY INGREDIENT: NH

Lack of any X-ray luminosity function for Type 2 AGNsLack of any X-ray luminosity function for Type 2 AGNs Absorbing column density (NAbsorbing column density (NHH) distribution: assumed ) distribution: assumed

to be independent of z and L and has been treated ad to be independent of z and L and has been treated ad free parameter in the fitting procedurefree parameter in the fitting procedure

IS THE ONLY PARAMETER IN THE MODEL IS THE ONLY PARAMETER IN THE MODEL THAT HAS NOT BEEN CONSTRAINED BY ANY THAT HAS NOT BEEN CONSTRAINED BY ANY

DIRECT MEASUREMENTDIRECT MEASUREMENT

The Cosmic X-ray The Cosmic X-ray Background:Background:

critical parameters of the critical parameters of the modelmodel

Gilli et al. 1999

Several works but all affected by selection

effects, incompleteness

problems or by biases related to the

absorption

Obtain a more reliable NH distribution according to criteria independent of absorption effects

GOAL

We need….

HARD BAND

[7-11] keV

The less biased against absorbed

objectsAccurate X-ray Spectroscopy and characterization of the sources

XMM

High XMM throughput

+

selection of bright objects

XMM-Newton Serendipitous XMM-Newton Serendipitous Survey in the hard band [7-11] Survey in the hard band [7-11]

keVkeV

GOAL

To build a local reference sample less affected that any other by NH

bias Study its properties and compare these with those of other deeper and non local samples

NH distribution: a solid determination from direct spectral modelling

Constrain the XRLF of absorbed objects and the unification schemes and AGN synthesis models of the XRB

Relative importance of the reflection component and EW of the Fe lines

The XMM-Newton hard The XMM-Newton hard band wide angle Survey: band wide angle Survey:

the samplethe sampleAnalyzed ALL XMM-EPIC fields including Target of

Opportunity Observations (ToO), publically available before October 1st 2003 selected

following these criteria

Objects at high galactic latitude |b|>27 and excluding Magellanic Clouds

With exposure time texp>10 ksec

With Full Frame Observations in PN

A total of 140 fields observed A total of 140 fields observed

Survey covers about 40 square degreesSurvey covers about 40 square degrees Searching for rare objectsSearching for rare objects

A total of A total of 8080 sources have been detected in the [7- sources have been detected in the [7-11] keV band down to a limiting flux of about F[7-11] keV band down to a limiting flux of about F[7-11]=3 1011]=3 10-14-14 erg cm erg cm-2-2 s s-1-1

The XMM-Newton hard The XMM-Newton hard band wide angle Survey: band wide angle Survey:

the samplethe sample

Cross-correlation of the 80 Cross-correlation of the 80 source X-ray position source X-ray position

The XMM-Newton hard band The XMM-Newton hard band wide angle Survey: wide angle Survey:

the samplethe sampleNED

For 15 objetcs the optical counterpart is known with a measured z

For 5 objects more than one optical counterpart within 0.2’ with measured z DSS For 47 sources optical

counterpart visible in the R plates (Rlim=21)

R≤22-23Fiore et al. 2003

HELLAS2XMM (Baldi et al. 2002)

CDFN (Barger et al. 2002)

LH (Baldi et al. 2001; Mainieri et al. 2002)

SSA13 (Mushotzky et al. 2000; Barger et al. 2001)

The XMM-Newton hard band The XMM-Newton hard band wide angle Survey: wide angle Survey:

data handlingdata handlingData reduction using the XMM-SAS v5.4Data reduction using the XMM-SAS v5.4

Baldi et al. (2002) pipeline implemented Baldi et al. (2002) pipeline implemented for [7-11] keV bandfor [7-11] keV band

Merge together the MOS and PN images to

increase the S/N of the sources

Automatic Spectral pipeline

Cleaned event files

SOURCE SPECTRUM30”<rext<45”

BACKGROUND SPETRUMrbkg=3rext

PN(single,double,s+d)-MOS1-MOS2-MOS(=MOS1+MOS2)

Automatic Spectral pipeline

SPECTRAL MODEL IN THE 0.4 -10 keV ENERGY RANGE

The XMM-Newton hard band The XMM-Newton hard band wide angle Survey:wide angle Survey:preliminary spectral preliminary spectral

characterizationcharacterization Model wabs(pow) in the 2-10 keV band

Preliminary measure of NH~30-35% with NH>1022

HELLAS2XMM-(4.5-10 keV): sp.analy

HELLAS2XMM-HR (Baldi et al. 2002)

CDFS (Giacconi et al. 2002)

ASCA MSS (Ueda et al. 2001)

Piccinotti et al. 1982

Comastri et al. 2001

The XMM-Newton hard band The XMM-Newton hard band wide angle Survey:wide angle Survey:

preliminary multiwavelength preliminary multiwavelength studystudy

A large fraction of obscured AGNs resides in objects with an extreme

X/O

Redshift and luminosity

distribution key parameters to test synthesis models of

XRBHigh X/O •Hard spectra

•Correlation X/O-L[2-10] for optically obscured AGNs

•Large majority are Ty2 QSO

•NIR observations:

•Correlations R-K colors and X/O: X/O>10 R-K>5

•Host galaxies are ellipticalsSee Fiore et al. 2003, Mignoli et al. 2003

X/O Fiore et al. 2003 Survey [7-11] keV(Hellas2XMM [2-10] keV)

0.1-3 55% 40%

3-10 21% 14%

>10 24% 46%

Survey in the hard band and at high X-ray flux

Best method to find objects with extreme X/O and for which optical follow-up is

attainable with present class of telescopes

The XMM-Newton hard The XMM-Newton hard band wide angle Survey: band wide angle Survey:

a particular example a particular example

wabs[1](mekal[2]+zwabs[3](pexrav[4]+zgauss[5])

z

z=0.31±0.03 NH~ 1023 cm-2

L[2-10]keV=1.5 1044 erg s-1

QSO2

Carangelo et al. 2003 (astro-ph/0309732)

ConclusionConclusion

XMM survey in the hard [7-11] keV band which allows for the XMM survey in the hard [7-11] keV band which allows for the first time to perform an accurate spectral analysis and first time to perform an accurate spectral analysis and caracterization of a local reference sample less affected than caracterization of a local reference sample less affected than any other by Nany other by NHH bias bias

NNHH distribution distribution XLF of absorbed objectsXLF of absorbed objects

THIS IS THE BEST WE CAN DO WITH THE CURRENT THIS IS THE BEST WE CAN DO WITH THE CURRENT GENERATION OF X-RAY SATELLITES GENERATION OF X-RAY SATELLITES

FutureFutureOptical follow-upOptical follow-up TNG & ESO 3.6mTNG & ESO 3.6m

Multiwavelength properties: Multiwavelength properties: X/O-L[2-10] X/O-L[2-10] see Fiore et al. see Fiore et al. 20032003

X/O-(R-K) X/O-(R-K) see Mignoli see Mignoli et al. 2003et al. 2003