1 / 14

The XMM-Newton hard band wide angle Survey

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. The Cosmic X-ray Background. Giacconi et al. 1962.

bianca-campbell
Télécharger la présentation

The XMM-Newton hard band wide angle Survey

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 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

  2. The Cosmic X-ray Background Giacconi et al. 1962 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 XRB as superposition of unabsorbed and absorbed AGNs KEY INGREDIENT: NH Comastri et al. 1995

  3. Gilli et al. 1999 The Cosmic X-ray Background:critical parameters of the model • Lack of any X-ray luminosity function for Type 2 AGNs • Absorbing column density (NH) 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 Several works but all affected by selection effects, incompleteness problems or by biases related to the absorption

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

  5. 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

  6. 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 texp>10 ksec • WithFull Frame Observations in PN

  7. The XMM-Newton hard band wide angle Survey: the sample • 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

  8. 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: the sample Cross-correlation of the 80 source X-ray position • 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 NED DSS For 47 sources optical counterpart visible in the R plates (Rlim=21) R≤22-23 Fiore et al. 2003

  9. Automatic Spectral pipeline Automatic Spectral pipeline Cleaned event files BACKGROUND SPETRUM rbkg=3rext SOURCE SPECTRUM 30”<rext<45” PN(single,double,s+d)-MOS1-MOS2-MOS(=MOS1+MOS2) 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 SPECTRAL MODEL IN THE 0.4 -10 keV ENERGY RANGE

  10. 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 wide angle Survey:preliminary spectral characterization Model wabs(pow) in the 2-10 keV band Preliminary measure of NH ~30-35% with NH>1022

  11. High 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 ellipticals See Fiore et al. 2003, Mignoli et al. 2003 The XMM-Newton hard band wide angle Survey:preliminary multiwavelength study Redshift and luminosity distribution key parameters to test synthesis models of XRB A large fraction of obscured AGNs resides in objects with an extreme X/O

  12. 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

  13. z wabs[1](mekal[2]+zwabs[3](pexrav[4]+zgauss[5]) z=0.31±0.03 NH~ 1023 cm-2 L[2-10]keV=1.5 1044 erg s-1 The XMM-Newton hard band wide angle Survey: a particular example QSO2 Carangelo et al. 2003 (astro-ph/0309732)

  14. 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 NH bias • NH distribution • XLF of absorbed objects • THIS IS THE BEST WE CAN DO WITH THE CURRENT GENERATION OF X-RAY SATELLITES • Future • Optical follow-up TNG & ESO 3.6m • Multiwavelength properties: X/O-L[2-10] see Fiore et al. 2003 X/O-(R-K) see Mignoli et al. 2003

More Related