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The XMM-Newton hard band wide angle Survey Nicoletta Carangelo and Silvano Molendi (IASF-MI(CNR)) Epic Consortium Meeting Palazzo Steri, Palermo, 14-16 October 2003
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The Cosmic X-ray Background 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: N H
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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. 1999 Several works but all affected by selection effects, incompleteness problems or by biases related to the absorption
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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
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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
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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
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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]=3 10 -14 erg cm -2 s -1 The XMM-Newton hard band wide angle Survey: the sample
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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. 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)
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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 0.4 -10 keV ENERGY RANGE
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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-(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
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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
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X/OFiore et al. 2003 Survey [7-11] keV (Hellas2XMM [2-10] keV) 0.1-355%40% 3-1021%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
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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 ~ 10 23 cm -2 L [2-10] keV=1.5 10 44 erg s - 1 QSO2 Carangelo et al. 2003 (astro-ph/0309732)
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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. 2003 X/O-(R-K) see Mignoli et al. 2003
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