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High Energy Large Area Surveys, the history of accretion in the Universe and galaxy evolution

High Energy Large Area Surveys, the history of accretion in the Universe and galaxy evolution. Fabrizio Fiore and the HELLAS2XMM collaboration:

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High Energy Large Area Surveys, the history of accretion in the Universe and galaxy evolution

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  1. High Energy Large Area Surveys, the history of accretion in the Universeand galaxy evolution Fabrizio Fiore and the HELLAS2XMM collaboration: (A. Baldi, M. Brusa, N. Carangelo, P. Ciliegi, F. Cocchia, A. Comastri, V. D’Elia, C. Feruglio, F. La Franca, R. Maiolino, G. Matt, M. Mignoli, S. Molendi, G.C. Perola, S. Puccetti, C. Vignali) + M. Elvis, P. Severgnini, N. Sacchi, N. Menci, A. Cavaliere, G. Pareschi, O. Citterio...

  2. Hard X-ray Surveys • Most direct probe of the super-massive black hole (SMBH) accretion activity, recorded in the CXB spectral energy density • SMBH census • Strong constraints to models for the formation and evolution of structure in the Universe AGN number and luminosity evolution AGN clustering and its evolution

  3. The Cosmic X-ray Background

  4. Hard X-ray Surveys • Most direct probe of the super-massive black hole (SMBH) accretion activity, recorded in the CXB spectral energy density • SMBH census • Strong constraints to models for the formation and evolution of structure in the Universe AGN number and luminosity evolution AGN clustering and its evolution

  5. XMM/Chandra Surveys • Wide and medium-deep several deg2 30-100 sources/XMM field, Fx  10-14 50% of the CXB • LX-Z diagram coverage • Rare and peculiar sources, avoid cosmic variance • Relatively “easy” multi-wavelength follow-up (ESO-VLT,3.6m, ATCA, VLA, TNG & Chandra) HELLAS2XMM CDFNCDFS Lockman Hole

  6. The HELLAS2XMM survey - 1.5 deg2 of sky covered, 232 2-10keV sources down to F 2-10keV=610-15 cgs - nearly completephotometry down to R~25 - nearly complete spectroscopy down to R~24: 160 z - 100 broad line AGN; 41 narrow line AGN and gal. 16 have logLX>44  QSO2! - 11 XBONGs; 1 star; 3 groups of galaxies - 40 sources with X/O>8,19 z - 6 broad line AGN; 13 narrow line AGN (12 QSO2!) Fiore et al. 2003 A&A, Cocchia et al. in preparation

  7. X-ray to optical flux ratio 15-20% of the sources have X/O>10 over a large flux range 30-40% have X/O>3. Optical identification of sources with X/O>3-10 is possible in the shallower surveys! HELLAS2XMM CDFNSSA13Lockman Hole Large area surveys at Fx10-14can be used to gain info on the fainter sources, making the remaining half of the CXB!!!

  8. High X/O = QSO2! Mignoli, Cocchia et al. 2004

  9. X-ray obscured AGNPerola, Puccetti et al. 2004 A&A PKS0537_111 R=25 X/O=50 logNH  23 PKS0312_22 QSO1 z=2.14 X/O=3.1 logNH=22.8 PKS0537_153 R>25 X/O>21 logNH  23 PKS0537_11a QSO2 z=0.981 LX=44.2 X/O=30 logNH=22.2

  10. XBONGs O = type 1 AGN =type 2 AGN = Early type Gals.

  11. The HELLAS2XMM survey in a context HELLAS2XMM – 1.5 deg2 - 232 sources F2-10keV10-14 cgs Fiore et al. 2003 Lockman Hole - 0.09 deg2 - 55 sources F2-10keV510-15 cgs (Mainieri et al 2002) CDFN - 0.037 deg2 - 88 sources F2-10keV10-15 cgs CDFN - 0.051 deg2 - 44 sources F2-10keV310-15 cgs (Barger et al. 2002) CDFS - 0.037 deg2 - 80 sources F2-10keV10-15 cgs CDFS - 0.051 deg2 - 43 sources F2-10keV310-15 cgs SSA13 - 0.015 deg2 - 20 sources F2-10keV410-15 cgs Barger et al. 2001 HEAO1 (Grossan) - 26,000 deg2 - 63 sources F2-10keV210-11 cgs

  12. The evolution of number and luminosity densities Non parametric determination Fiore et al. 2003 A&A

  13. Black hole mass density A ~ 5x1039 erg s-1Mpc-3 A (1-) LBol BH ~ ——————  c2 LX =0.1 LBol/LX=40 BH ~ 3x10-5MΘ Yr-1Mpc-3 BH ~ 4x105MΘ Mpc-3 . .

  14. 2-10 keV AGN luminosity function models Solid = observed dashed = best fit LDDE with constant NH distribution La Franca et al. 2005

  15. 2-10 keV AGN luminosity function models LDDE with variable absorbed AGN fraction La Franca et al. 2005

  16. Fraction of obscured AGN La Franca et al. 2005

  17. Comparison with CDM HC modelsMenci,Fiore,Perola & Cavaliere 2004 Processes of galaxy formation and evolution described by a semi-analytic model. Galaxy interactions: main triggers of accretion (Cavaliere & Vittorini 2000) L(2-10keV)=0.01 L(bol.) no other parameter tuning

  18. Comparison with CDM HC modelsMenci,Fiore,Perola & Cavaliere 2004

  19. CXB Resolved fraction LogL<43.5 43.5<LogL<44.5 LogL>44.5 Menci et al 2004

  20. Summary • most of the CXB <6-8keV is resolved in sources • Black Hole mass density ~2 times higher than that estimated from optical and soft X-rays: better agreement with CXB estimates and with local space density • Differential evolution of number and luminosity densities. • Nice agreement between the evolution of luminous QSO and CDM HC models. Problems with low luminosity AGN?  Revision of Unified Schemes

  21. Revision of Unified Schemes Mild .

  22. Revision of Unified Schemes Strong: Low L Seyfers and powerful QSO: different populations. A working scenario: Seyferts – associated to galaxies with merging histories characterized by small mass progenitors. Feedback is effective in self-regulating accretion and SF, cold gas is left available for subsequent nuclear activation produced by loose galaxy encounters (fly-by). QSOs – associated to galaxies with large mass progenitors. Feedback is less effective, most gas is quickly converted in stars and accreted during a few major mergers at high Eddington rates. The obscuration properties of the two populations can be different in term of geometry, gas density, covering factor, ionization state, metallicity, dust content etc..

  23. What’s next ? • 1) Paucity of high z logLX<44.5 sources? Real or are we missing highly obscured AGNs? • 2) Compare the obscuration properties of Seyfert 2 galaxies and QSO2 • 3) Deconvolve accr. rate and BH mass: • 4) Seyfert-QSO/galaxy clustering and its evolution

  24. 1) Paucity of Seyfert like sources @ z>1 is real? Or, is it, at least partly, a selection effect? Are we missing in Chandra and XMM surveys highly obscured (NH1024 cm-2) AGN? Which are common in the local Universe…

  25. Imaging surveys up to 8-10 keV (ASCA,BSAX, Chandra, XMM): • most of the CXB <6-7 keV is resolved in sources. But only 40-50% in the 5-10 keV band. Few % E>10keV. The light-up and evolution of obscured accreting SMBH is still largely unknown Worsley et a. 2004

  26. What’s needed? • Sensitive observations at the peak of the CXB (~20-40 keV) to probe highly X-ray obscured AGN • But.. How deep should we go? • …and how hard should we go?

  27. Residual CXB after subtracting the resolved fraction below 10 keV Comastri 2004 We need to resolve: 80% of CXB @10-30keV (similar to Chandra and XMM deep fields below 10 keV) 50% of CXB @ 20-40keV

  28. CXB fraction >50% res.CXB >80% res.CXB F(20-40keV)< 710-15 cgs or 0.75 Crab 10-15 cgs or 0.1 Crab F(10-30keV)< 10-14 cgs or 0.65 Crab 210-15 cgs or 0.13 Crab

  29. What’s next (3) Franceschini et al. 1999 Marconi et al 2004 Deconvolve accr. rate and BH mass: • Optically unobscured AGN: MBH from broad line FWHM • Optically obscured AGN: MBH from bulge light

  30. Unobscured sources A detailed spectral analysis allows to make use of the correlations between FWHM of the broad emission lines and BH masses Spectroscopy  FWHM emission lines  MBH Mclure & Jarvis 2002 Vestergaard 2002

  31. Obscured sources The nucleus is obscured so we can study the host galaxy Imaging  Morphology  Bulge  MBH Mc Lure et al. 2002 Log(MBH/Mo) = -0.5 MR – 2.96

  32. Hellas2XMM BPM16274 #69 B/T = 1 Pks0312 #31 B/T = 0.8

  33. The GOODS sample Weextended our analisys to a sample of optically obscured sources in the Great Observatories Origins Deep Survey (GOODS) fields taking advantage of the superior quality of the HST images Z band Ks band

  34. B/T =0.39 B/T =0.5

  35. MBH, L/LEDD of obscured and unobscured AGN * = broad line AGN

  36. What’s next (4) AGN clustering D’Elia et al. 2004

  37. AGN clusteringD’Elia et al. 2004 0=10’’

  38. ELAIS S1 XMM-SWIREX-ray sources clustering and evolution XMM PN+MOS  50ks net expo. 0.5 deg2479 X-ray sources R=16.8 R=17.1 45’

  39. FX=1.510-13 cgs

  40. ELAIS S1 XMM-SWIRE 6 extended sources in the 0.5 deg2 field R=19.5 FX=1.510-14 R=20.3

  41. ELAIS-S1 number counts Unobscured Obscured

  42. Clustering in the ELAIS-S1 field 2-10 keV: 0=11+/-6 arcsec 0.5-2keV 0=4+/-2.5 arcsec

  43. What’s next • How galaxy activity traces the cosmic WEB (direct comparison with models for the evolution of the structure in the universe) COSMOS! ACS-XMM-VIMOS-Chandra

  44. COSMOS multiwavelength project “COSMOS is an HST/ACS Treasury project (..) Goal: Interplay between Large Scake Structure, evolution and formation of galaxies, dark matter and AGNs” Need to go to larger scales  2 sq. deg.

  45. COSMOS project: overview MULTIWAVELENGTH DATA Scheduled/observed: HST/ACS (600 orbits), XMM-Newton (0.8 Ms), SUBARU (b,v,r,i,z), VLA, GALEX, CFHT, Mambo … proposed: Chandra (1.4 Ms), XMM (additional 0.8 Ms) + Spitzer (200 orbits), VLT/VIMOS (70 nights) http://www.astro.caltech.edu/cosmos/ http://www.ifa.hawaii.edu/~Eaussel/Cosmos/multiwavelength.html

  46. 800 ksec XMM-Newton Cosmos field PI: G. Hasinger; 25 pointings 32 ksec each XMM pn true color image (courtesy I. Lehmann)

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