The XMM-Newton hard band wide angle Survey Nicoletta Carangelo and Silvano Molendi (IASF-MI(CNR)) Epic Consortium Meeting Palazzo Steri, Palermo, October 2003

The Cosmic X-ray Background Giacconi et al XRB as superposition of unabsorbed and absorbed AGNs Comastri et al 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: N H

 Lack of any X-ray luminosity function for Type 2 AGNs  Absorbing column density (N H ) distribution: assumed to be independent of z and L and has been treated ad free parameter in the fitting procedure IS THE ONLY PARAMETER IN THE MODEL THAT HAS NOT BEEN CONSTRAINED BY ANY DIRECT MEASUREMENT The Cosmic X-ray Background: critical parameters of the model Gilli et al Several works but all affected by selection effects, incompleteness problems or by biases related to the absorption

Obtain a more reliable N H distribution according to criteria independent of absorption effects GOAL We need…. HARD BAND [7-11] keV The less biased against absorbed objects Accurate X-ray Spectroscopy and characterization of the sources XMM High XMM throughput + selection of bright objects XMM-Newton Serendipitous Survey in the hard band [7-11] keV

GOAL To build a local reference sample less affected that any other by N H bias  Study its properties and compare these with those of other deeper and non local samples  N H 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 band wide angle Survey: the sample Analyzed 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 t exp >10 ksec  With Full Frame Observations in PN

 A total of 140 fields observed  Survey covers about 40 square degrees Searching for rare objects  A total of 80 sources have been detected in the [7-11] keV band down to a limiting flux of about F[7-11]= erg cm -2 s -1 The XMM-Newton hard band wide angle Survey: the sample

Cross-correlation of the 80 source X-ray position The XMM-Newton hard band wide angle Survey: the sample NED  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 DSSFor 47 sources optical counterpart visible in the R plates (R lim =21) R≤22-23 Fiore et al 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 wide angle Survey: data handling Data reduction using the XMM-SAS v5.4 Baldi et al. (2002) pipeline implemented for [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 SPECTRUM 30”<r ext <45” BACKGROUND SPETRUM r bkg =3r ext PN(single,double,s+d)-MOS1-MOS2-MOS(=MOS1+MOS2) Automatic Spectral pipeline SPECTRAL MODEL IN THE keV ENERGY RANGE

The XMM-Newton hard band wide angle Survey: preliminary spectral characterization Model wabs(pow) in the 2-10 keV band Preliminary measure of N H ~30-35% with N H >10 22 HELLAS2XMM-( keV): sp.analy HELLAS2XMM-HR (Baldi et al. 2002) CDFS (Giacconi et al. 2002) ASCA MSS (Ueda et al. 2001) Piccinotti et al Comastri et al. 2001

The XMM-Newton hard band wide angle Survey: preliminary multiwavelength study 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 XRB High X/OHard 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 ellipticals See Fiore et al. 2003, Mignoli et al. 2003

X/OFiore et al Survey [7-11] keV (Hellas2XMM [2-10] keV) %40% %14% >1024%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 band wide angle Survey: a particular example wabs[1](mekal[2]+zwabs[3](pexrav[4]+zgauss[5]) z z=0.31±0.03 N H ~ cm -2 L [2-10] keV= erg s - 1 QSO2 Carangelo et al (astro-ph/ )

Conclusion  XMM survey in the hard [7-11] keV band which allows for the first time to perform an accurate spectral analysis and caracterization of a local reference sample less affected than any other by N H bias  N H distribution  XLF of absorbed objects  THIS IS THE BEST WE CAN DO WITH THE CURRENT GENERATION OF X-RAY SATELLITES  Future  Optical follow-upTNG & ESO 3.6m  Multiwavelength properties: X/O-L[2-10] see Fiore et al X/O-(R-K) see Mignoli et al. 2003